On the spectroscopic nature of the cool evolved Am star HD151878

NASA Astrophysics Data System (ADS)

Freyhammer, L. M.; Elkin, V. G.; Kurtz, D. W.

2008-10-01

Recently, Tiwari, Chaubey & Pandey detected the bright component of the visual binary HD151878 to exhibit rapid photometric oscillations through a Johnson B filter with a period of 6min (2.78mHz) and a high, modulated amplitude up to 22mmag peak-to-peak, making this star by far the highest amplitude rapidly oscillating Ap (roAp) star known. As a new roAp star, HD151878 is of additional particular interest as a scarce example of the class in the northern sky, and only the second known case of an evolved roAp star - the other being HD116114. We used the FIbre-fed Echelle Spectrograph at the Nordic Optical Telescope to obtain high time-resolution spectra at high dispersion to attempt to verify the rapid oscillations. We show here that the star at this epoch is spectroscopically stable to rapid oscillations of no more than a few tens of ms-1. The high-resolution spectra furthermore show the star to be of type Am rather than Ap and we show the star lacks most of the known characteristics for roAp stars. We conclude that this is an Am star that does not pulsate with a 6-min period. The original discovery of pulsation is likely to be an instrumental artefact. Based on observations collected at the Nordic Optical Telescope as part of programme 36-418. E-mail: lfreyham@gmail.com

Large amplitude change in spot-induced rotational modulation of the Kepler Ap star KIC 2569073

NASA Astrophysics Data System (ADS)

Drury, Jason A.; Murphy, Simon J.; Derekas, Aliz; Sódor, Ádám; Stello, Dennis; Kuehn, Charles A.; Bedding, Timothy R.; Bognár, Zsófia; Szigeti, László; Szakáts, Róbert; Sárneczky, Krisztián; Molnár, László

2017-11-01

An investigation of the 200 × 200 pixel `superstamp' images of the centres of the open clusters NGC 6791 and NGC 6819 allows for the identification and study of many variable stars that were not included in the Kepler target list. KIC 2569073 (V = 14.22), is a particularly interesting variable Ap star that we discovered in the NGC 6791 superstamp. With a rotational period of 14.67 d and 0.034 mag variability, it has one of the largest peak-to-peak variations of any known Ap star. Colour photometry reveals an antiphase correlation between the B band, and the V, R and I bands. This Ap star is a rotational variable, also known as an α2 CVn star, and is one of only a handful of Ap stars observed by Kepler. While no change in spot period or amplitude is observed within the 4 yr Kepler time series, the amplitude shows a large increase compared to ground-based photometry obtained two decades ago.

VizieR Online Data Catalog: New IR photometric study of Ap and Am stars (Chen+, 2017)

NASA Astrophysics Data System (ADS)

Chen, P. S.; Liu, J. Y.; Shan, H. G.

2018-05-01

In the General Catalog of Ap and Am stars (Renson & Manfroid 2009, Cat. III/260) 8265 stars are included in which, as Renson & Manfroid (2009, Cat. III/260) described, only 426 stars are of the "well known confirmed sample". We take these 426 stars as our working sample. The cross-identifications of 2MASS/WISE counterparts for all Ap, Am, and HgMn stars listed in this paper are made from Cutri et al. (2012, Cat. II/311) by using the radius of 2 arcsec. All 426 Ap, Am, and HgMn stars have 2MASS and/or WISE counterparts, which are listed in Table 3. The cross-identifications of IRAS counterparts are made according to the positional error ellipse of the source, because it has a 95% confidence level (IRAS Explanatory Supplement, Beichman et al. 1988, Cat. II/274). Finally, 202 stars are found to have the IRAS counterparts from IRAS PSC/FSC, which is listed in Table 4. (5 data files).

Analysis of stratification of Cr with depth in the atmospheres of normal and CP stars.

NASA Astrophysics Data System (ADS)

Savanov, I. S.

We present the results of analysis of stratification of Cr with depth in the atmospheres of normal, Am, HgMn and Ap stars. On the base of high resolution CCD-spectrograms obtained with spectrograph of 2.6-meter Shajn reflector using synthetic spectrum technique analysis of eight Cr II lines (30 multiplet) located in the wings of Hb Hydrogen line. For all investigated Am stars as well as for HgMn components of 46 Dra we suspect the similar small increase of Cr abundance in the upper atmosphere. For the hot spotted Ap stars α2 CVn and 17 Com we do not find evidence for the inhomogeneity distribution of Chromium while for the group of cool Ap stars (β CrB, HR 7575, 10 Aql and γ Equ) the increase of Cr abundance with depth was found. Detailed modelling of Cr II line profiles was performed in order to obtain vertical distributions of this element in the atmospheres of several Ap and Am stars. Our results for cool Ap stars were compared with vertical Cr distribution calculated by J.Babel using the diffusion theory and magnetically confined wind for Ap star 53 Cam (e.g. Astronomy and Astrophysics, v.258, p.449-463, 1992). It was shown that our observational material cannot be interpreted using hypothesis of depth-dependent microturbulent velocity. While the investigation of β CrB we demonstrate that obtained results insignificantly depend upon the uncertainties of the parameters of models of atmospheres.

An investigation of the rapid spectral variability of the AP stars 53 Cam, 41 Tau, and Beta CrB on the basis of the K CA II and H-delta lines

NASA Astrophysics Data System (ADS)

Kuvshinov, V. M.; Plachinda, S. I.

The flux is shown to vary with the phase of the period of axial rotation. For 53 Cam and Beta CrB, this variability is smooth and is well correlated with the intensity of the mean surface magnetic field. It is pointed out that in the case of 53 Cam, an analogous dependence between the equivalent width of the K Ca II line and the phase of the period of rotation was obtained by Faraggiana (1973). It is considered significant that the correlations between the flux in the K line and the intensity of the mean surface magnetic field for 53 Cam and Beta CrB have the same sign. With 41 Tau, as with the effective magnetic field, no smooth relationship is found between the fluxes in the K Ca II and H-delta lines and the phase of the period of rotation.

Importin Beta Plays an Essential Role in the Regulation of the LysRS-Ap4A Pathway in Immunologically Activated Mast Cells ▿

PubMed Central

Carmi-Levy, Irit; Motzik, Alex; Ofir-Birin, Yifat; Yagil, Zohar; Yang, Christopher Maolin; Kemeny, David Michael; Han, Jung Min; Kim, Sunghoon; Kay, Gillian; Nechushtan, Hovav; Suzuki, Ryo; Rivera, Juan; Razin, Ehud

2011-01-01

We recently reported that diadenosine tetraphosphate hydrolase (Ap4A hydrolase) plays a critical role in gene expression via regulation of intracellular Ap4A levels. This enzyme serves as a component of our newly described lysyl tRNA synthetase (LysRS)-Ap4A biochemical pathway that is triggered upon immunological challenge. Here we explored the mechanism of this enzyme's translocation into the nucleus and found its immunologically dependent association with importin beta. Silencing of importin beta prevented Ap4A hydrolase nuclear translocation and affected the local concentration of Ap4A, which led to an increase in microphthalmia transcription factor (MITF) transcriptional activity. Furthermore, immunological activation of mast cells resulted in dephosphorylation of Ap4A hydrolase, which changed the hydrolytic activity of the enzyme. PMID:21402779

Suppressed phase variations in a high amplitude rapidly oscillating Ap star pulsating in a distorted quadrupole mode

NASA Astrophysics Data System (ADS)

Holdsworth, Daniel L.; Saio, H.; Bowman, D. M.; Kurtz, D. W.; Sefako, R. R.; Joyce, M.; Lambert, T.; Smalley, B.

2018-05-01

We present the results of a multisite photometric observing campaign on the rapidly oscillating Ap (roAp) star 2MASS 16400299-0737293 (J1640; V = 12.7). We analyse photometric B data to show the star pulsates at a frequency of 151.93 d-1 (1758.45 μHz; P = 9.5 min) with a peak-to-peak amplitude of 20.68 mmag, making it one of the highest amplitude roAp stars. No further pulsation modes are detected. The stellar rotation period is measured at 3.674 7 ± 0.000 5 d, and we show that rotational modulation due to spots is in antiphase between broad-band and B observations. Analysis and modelling of the pulsation reveals this star to be pulsating in a distorted quadrupole mode, but with a strong spherically symmetric component. The pulsational phase variation in this star is suppressed, leading to the conclusion that the contribution of ℓ > 2 components dictate the shape of phase variations in roAp stars that pulsate in quadrupole modes. This is only the fourth time such a strong pulsation phase suppression has been observed, leading us to question the mechanisms at work in these stars. We classify J1640 as an A7 Vp SrEu(Cr) star through analysis of classification resolution spectra.

Pulsation in Chemically Peculiar Stars

NASA Astrophysics Data System (ADS)

Sachkov, M.

2015-04-01

Chemically peculiar stars offer the opportunity to study the interaction of strong magnetic fields, rotation, and pulsation. The rapidly oscillating chemically peculiar A stars (roAp) are a subgroup of the chemically peculiar magnetic A stars. They are high-overtone, low-degree p-mode pulsators. Until recently, the classical asteroseismic analysis, i.e., frequency analysis, of these stars was based on ground and space photometric observations. Significant progress was achieved through the access to the uninterrupted, ultra-high-precision data from the MOST, COROT, and Kepler satellites. Over the last ten years, the studies of roAp stars have been altered drastically from the observational point of view through the usage of time-resolved, high-resolution spectra. Their unusual pulsation characteristics, caused by the interplay between short vertical lengths of pulsation waves and strong stratification of chemical elements, allow us to examine the upper roAp atmosphere in more detail than is possible for any star except the Sun. In this paper a review of the results of recent studies of the pulsations of roAp stars is presented.

Chromosome localization of human genes for clathrin adaptor polypeptides AP2{beta} and AP50 and the clathrin-binding protein, VCP

DOE Office of Scientific and Technical Information (OSTI.GOV)

Druck, T.; Gu, Y.; Prabhala, G.

1995-11-01

Clathrin-coated vesicles, involved in endocytosis and Golgi processing, have a surface lattice containing clathrin triskelia and stoichiometric amounts of additional components termed {open_quotes}assembly proteins,{close_quotes} or APs. The AP form at the plasma membrane, AP2, is composed of two large subunits of 100-115 kDa, denoted AP2{alpha} and AP2{beta}, a medium chain of 50 kDa, designated AP50, and a small chain. We have determined human chromosomal locations of genes for a large AP2{beta} (CLAPB1) and a medium (CLAPM1) AP subunit and of a novel clathrin-binding protein, VCP, that binds clathrin simultaneously with A1`s. Chromosomal in situ hybridization of a human genomic clonemore » demonstrated that the CLAPM1 gene mapped to chromosome region 3q28. The gene for the CLAPB1 large subunit was mapped to 17q11.2-q12 by PCR amplification of an AP2{beta} fragment from a panel of rodent-human hybrid DNAs. To map the human VCP sequence, a human-specific probe was made by RT-PCR of human mRNA using oligonucleotide primers from conserved regions of the porcine sequence. The amplified human fragment served as probe on Southern blots of hybrid DNAs to determine that the human VCP locus maps to chromosome region 9pter-q34. 13 refs., 2 figs.« less

Molecular cloning and nucleotide sequence of the alpha and beta subunits of allophycocyanin from the cyanelle genome of Cyanophora paradoxa.

PubMed Central

Bryant, D A; de Lorimier, R; Lambert, D H; Dubbs, J M; Stirewalt, V L; Stevens, S E; Porter, R D; Tam, J; Jay, E

1985-01-01

The genes for the alpha- and beta-subunit apoproteins of allophycocyanin (AP) were isolated from the cyanelle genome of Cyanophora paradoxa and subjected to nucleotide sequence analysis. The AP beta-subunit apoprotein gene was localized to a 7.8-kilobase-pair Pst I restriction fragment from cyanelle DNA by hybridization with a tetradecameric oligonucleotide probe. Sequence analysis using that oligonucleotide and its complement as primers for the dideoxy chain-termination sequencing method confirmed the presence of both AP alpha- and beta-subunit genes on this restriction fragment. Additional oligonucleotide primers were synthesized as sequencing progressed and were used to determine rapidly the nucleotide sequence of a 1336-base-pair region of this cloned fragment. This strategy allowed the sequencing to be completed without a detailed restriction map and without extensive and time-consuming subcloning. The sequenced region contains two open reading frames whose deduced amino acid sequences are 81-85% homologous to cyanobacterial and red algal AP subunits whose amino acid sequences have been determined. The two open reading frames are in the same orientation and are separated by 39 base pairs. AP alpha is 5' to AP beta and both coding sequences are preceded by a polypurine, Shine-Dalgarno-type sequence. Sequences upstream from AP alpha closely resemble the Escherichia coli consensus promoter sequences and also show considerable homology to promoter sequences for several chloroplast-encoded psbA genes. A 56-base-pair palindromic sequence downstream from the AP beta gene could play a role in the termination of transcription or translation. The allophycocyanin apoprotein subunit genes are located on the large single-copy region of the cyanelle genome. PMID:2987916

Pulsating Stars in the ASAS-3 Database. I. beta Cephei Stars

NASA Astrophysics Data System (ADS)

Pigulski, A.

2005-06-01

We present results of an analysis of the ASAS-3 data for short-period variables from the recently published catalog of over 38000 stars. Using the data available in the literature we verify the results of the automatic classification related to \\beta Cep pulsators. In particular, we find that 14 stars in the catalog can be classified unambiguously as new beta Cep stars. By means of periodogram analysis we derive the frequencies and amplitudes of the excited modes. The main modes in the new beta Cep stars have large semi-amplitudes, between 35 and 80 mmag. Up to four modes were found in some stars. Two (maybe three) new beta Cep stars are members of southern young open clusters: ASAS 164409-4719.1 belongs to NGC 6200, ASAS 164630-4701.2 is a member of Hogg 22, and ASAS 164939-4431.7 could be a member of NGC 6216. We also analyze the photometry of four known beta Cep stars in the ASAS-3 catalog, namely IL Vel, NSV 24078, V1449 Aql and SY Equ. Finally, we discuss the distribution of beta Cep stars in the Galaxy.

Transforming growth factor-beta 1 (TGF-beta1) promotes IL-2 mRNA expression through the up-regulation of NF-kappaB, AP-1 and NF-AT in EL4 cells.

PubMed

Han, S H; Yea, S S; Jeon, Y J; Yang, K H; Kaminski, N E

1998-12-01

Transforming growth factor beta1 (TGF-beta1) has been previously shown to modulate interleukin 2 (IL-2) secretion by activated T-cells. In the present studies, we determined that TGF-beta1 induced IL-2 mRNA expression in the murine T-cell line EL4, in the absence of other stimuli. IL-2 mRNA expression was significantly induced by TGF-beta1 (0.1-1 ng/ml) over a relatively narrow concentration range, which led to the induction of IL-2 secretion. Under identical condition, we examined the effect of TGF-beta1 on the activity of nuclear factor AT (NF-AT), nuclear factor kappaB (NF-kappaB), activator protein-1 (AP-1) and octamer, all of which contribute to the regulation of IL-2 gene expression. Electrophoretic mobility shift assays showed that TGF-beta1 markedly increased NF-AT, NF-kappaB and AP-1 binding to their respective cognate DNA binding sites, whereas octamer binding remained constant, as compared with untreated cells. Employing a reporter gene expression system with p(NF-kappaB)3-CAT, p(NF-AT)3-CAT and p(AP-1)3-CAT, TGF-beta1 treatment of transfected EL4 cells induced a dose-related increase in chloramphenicol acetyltransferase activity that correlated well with the DNA binding profile found in the electrophoretic mobility shift assay studies. These results show that TGF-beta1, in the absence of any additional stimuli, up-regulates the activity of key transcription factors involved in IL-2 gene expression, including NF-AT, NF-kappaB and AP-1, to help promote IL-2 mRNA expression by EL4 cells.

Accurate age determinations of several nearby open clusters containing magnetic Ap stars

NASA Astrophysics Data System (ADS)

Silaj, J.; Landstreet, J. D.

2014-06-01

Context. To study the time evolution of magnetic fields, chemical abundance peculiarities, and other characteristics of magnetic Ap and Bp stars during their main sequence lives, a sample of these stars in open clusters has been obtained, as such stars can be assumed to have the same ages as the clusters to which they belong. However, in exploring age determinations in the literature, we find a large dispersion among different age determinations, even for bright, nearby clusters. Aims: Our aim is to obtain ages that are as accurate as possible for the seven nearby open clusters α Per, Coma Ber, IC 2602, NGC 2232, NGC 2451A, NGC 2516, and NGC 6475, each of which contains at least one magnetic Ap or Bp star. Simultaneously, we test the current calibrations of Te and luminosity for the Ap/Bp star members, and identify clearly blue stragglers in the clusters studied. Methods: We explore the possibility that isochrone fitting in the theoretical Hertzsprung-Russell diagram (i.e. log (L/L⊙) vs. log Te), rather than in the conventional colour-magnitude diagram, can provide more precise and accurate cluster ages, with well-defined uncertainties. Results: Well-defined ages are found for all the clusters studied. For the nearby clusters studied, the derived ages are not very sensitive to the small uncertainties in distance, reddening, membership, metallicity, or choice of isochrones. Our age determinations are all within the range of previously determined values, but the associated uncertainties are considerably smaller than the spread in recent age determinations from the literature. Furthermore, examination of proper motions and HR diagrams confirms that the Ap stars identified in these clusters are members, and that the presently accepted temperature scale and bolometric corrections for Ap stars are approximately correct. We show that in these theoretical HR diagrams blue stragglers are particularly easy to identify. Conclusions: Constructing the theoretical HR diagram of a nearby open cluster makes possible an accurate age determination, with well defined uncertainty. This diagnostic of a cluster also provides a useful tool for studying unusual stars such as Ap stars and blue stragglers. Table 3 is available in electronic form at http://www.aanda.org

Intelligent error correction method applied on an active pixel sensor based star tracker

NASA Astrophysics Data System (ADS)

Schmidt, Uwe

2005-10-01

Star trackers are opto-electronic sensors used on-board of satellites for the autonomous inertial attitude determination. During the last years star trackers became more and more important in the field of the attitude and orbit control system (AOCS) sensors. High performance star trackers are based up today on charge coupled device (CCD) optical camera heads. The active pixel sensor (APS) technology, introduced in the early 90-ties, allows now the beneficial replacement of CCD detectors by APS detectors with respect to performance, reliability, power, mass and cost. The company's heritage in star tracker design started in the early 80-ties with the launch of the worldwide first fully autonomous star tracker system ASTRO1 to the Russian MIR space station. Jena-Optronik recently developed an active pixel sensor based autonomous star tracker "ASTRO APS" as successor of the CCD based star tracker product series ASTRO1, ASTRO5, ASTRO10 and ASTRO15. Key features of the APS detector technology are, a true xy-address random access, the multiple windowing read out and the on-chip signal processing including the analogue to digital conversion. These features can be used for robust star tracking at high slew rates and under worse conditions like stray light and solar flare induced single event upsets. A special algorithm have been developed to manage the typical APS detector error contributors like fixed pattern noise (FPN), dark signal non-uniformity (DSNU) and white spots. The algorithm works fully autonomous and adapts to e.g. increasing DSNU and up-coming white spots automatically without ground maintenance or re-calibration. In contrast to conventional correction methods the described algorithm does not need calibration data memory like full image sized calibration data sets. The application of the presented algorithm managing the typical APS detector error contributors is a key element for the design of star trackers for long term satellite applications like geostationary telecom platforms.

A quantitative comparison of plaque types in Alzheimer's disease and senile dementia of the Lewy body type.

PubMed

McKenzie, J E; Edwards, R J; Gentleman, S M; Ince, P G; Perry, R H; Royston, M C; Roberts, G W

1996-01-01

In a previous study we reported no difference in the overall beta-amyloid protein (beta AP) load between Alzheimer's disease (AD) and senile dementia of the Lewy body type (SDLT). However, it is possible that differences in the morphology of beta AP plaque types exist, analogous to the differences in cytoskeletal pathology found in these two disorders. We have carried out a quantitative image analysis of plaque subtypes in the temporal lobe of AD (n = 8), SDLT (n = 9) and control (n = 11) cases. Measurements of beta AP load and plaque density were consistently higher in AD and SDLT than in controls. When AD and SDLT cases were compared no differences were seen in either the density or relative proportions of classic and diffuse plaques. Based on these results we suggest that the variation in the clinical course of these diseases reflects differences in the cytoskeletal pathology, whereas the final stages of profound dementia common to both disorders is associated with the deposition of beta AP.

VizieR Online Data Catalog: Variable stars in M31 and M33. V. HR diagram (Humphreys+, 2017)

NASA Astrophysics Data System (ADS)

Humphreys, R. M.; Davidson, K.; Hahn, D.; Martin, J. C.; Weis, K.

2017-09-01

We use the large data set published by Massey+ (2016, J/AJ/152/62), together with our own spectral classifications from Papers II (Humphreys+, 2014, J/ApJ/790/48; III (Gordon+, 2016, J/ApJ/825/50), and IV (Humphreys+, 2017, J/ApJ/836/64), to create a catalog of luminous O-, B-, and A-type stars representative of the hot star populations in M31 and M33. (2 data files).

Analysis of the IRAS Low Resolution Spectra

DTIC Science & Technology

1988-04-01

WITH EU ANDROMEDAE : A CARBON 33 STAR NEAR AN OXYGEN-RICH CIRCUMSTELLAR SHELL (AP J COPYRIGHT - BENSON WORKED AT WELLESLEY COLL., WHILE LITTLE-MARENIN...OR AFGL MONEY) G. MASERS ASSOCIATED WITH TWO CARBON STARS: V778 CYGNI 71 AND EU ANDROMEDAE (ACCEPTED BY AP J FOR PUBLICATION 15 JUL 88; TWO NON...I.R. 1987, "A Water Maser Associated with EU Andromedae . A Carbon Star Near an Oxygen-Rich Circumstcllar Shell," Ap. J. (Letterc), 316, L37-L40. l

Multipurpose active pixel sensor (APS)-based microtracker

NASA Astrophysics Data System (ADS)

Eisenman, Allan R.; Liebe, Carl C.; Zhu, David Q.

1998-12-01

A new, photon-sensitive, imaging array, the active pixel sensor (APS) has emerged as a competitor to the CCD imager for use in star and target trackers. The Jet Propulsion Laboratory (JPL) has undertaken a program to develop a new generation, highly integrated, APS-based, multipurpose tracker: the Programmable Intelligent Microtracker (PIM). The supporting hardware used in the PIM has been carefully selected to enhance the inherent advantages of the APS. Adequate computation power is included to perform star identification, star tracking, attitude determination, space docking, feature tracking, descent imaging for landing control, and target tracking capabilities. Its first version uses a JPL developed 256 X 256-pixel APS and an advanced 32-bit RISC microcontroller. By taking advantage of the unique features of the APS/microcontroller combination, the microtracker will achieve about an order-of-magnitude reduction in mass and power consumption compared to present state-of-the-art star trackers. It will also add the advantage of programmability to enable it to perform a variety of star, other celestial body, and target tracking tasks. The PIM is already proving the usefulness of its design concept for space applications. It is demonstrating the effectiveness of taking such an integrated approach in building a new generation of high performance, general purpose, tracking instruments to be applied to a large variety of future space missions.

Mode identification in Beta Cephei stars

NASA Technical Reports Server (NTRS)

Aizenmen, M. L.; Lesh, J. R.

1980-01-01

The essential observational characteristics related to mode identification are summarized. Major emphasis is placed on the following: both light and velocity amplitudes; typical periods in both light and radial velocity; the light curve for Beta Cephei stars in comparison to the classical Cepheids and RR Lyrae stars; the van Hoof effect with respect to the radial velocity curves in many Beta Cephei stars; and the line profiles of many Beta Cephei stars.

The dichotomy between strong and ultra-weak magnetic fields among intermediate-mass stars

NASA Astrophysics Data System (ADS)

Lignières, François; Petit, Pascal; Aurière, Michel; Wade, Gregg A.; Böhm, Torsten

2014-08-01

Until recently, the detection of magnetic fields at the surface of intermediate-mass main-sequence stars has been limited to Ap/Bp stars, a class of chemically peculiar stars. This class represents no more than 5-10% of the stars in this mass range. This small fraction is not explained by the fossil field paradigm that describes the Ap/Bp type magnetism as a remnant of an early phase of the star-life. Also, the limitation of the field measurements to a small and special group of stars is obviously a problem to study the effect of the magnetic fields on the stellar evolution of a typical intermediate-mass star. Thanks to the improved sensitivity of a new generation of spectropolarimeters, a lower bound to the magnetic fields of Ap/Bp stars, a two orders of magnitude desert in the longitudinal magnetic field and a new type of sub-gauss magnetism first discovered on Vega have been identified. These advances provide new clues to understand the origin of intermediate-mass magnetism as well as its influence on stellar evolution. In particular, a scenario has been proposed whereby the magnetic dichotomy between Ap/Bp and Vega-like magnetism originate from the bifurcation between stable and unstable large scale magnetic configurations in differentially rotating stars. In this paper, we review these recent observational findings and discuss this scenario.

A beta-N-acetylglucosaminyl phosphate diester residue is attached to the glycosylphosphatidylinositol anchor of human placental alkaline phosphatase: a target of the channel-forming toxin aerolysin.

PubMed

Fukushima, Keiko; Ikehara, Yukio; Kanai, Michiko; Kochibe, Naohisa; Kuroki, Masahide; Yamashita, Katsuko

2003-09-19

Glycosylphosphatidylinositol (GPI)-anchored proteins are ubiquitous in eukaryotes. The minimum conserved GPI core structure of all GPI-anchored glycans has been determined as EtN-PO4-6Manalpha1-2Manalpha1-6Manalpha1-4GlcN-myo-inositol-PO3H. Human placental alkaline phosphatase (AP) has been reported to be a GPI-anchored membrane protein. AP carries one N-glycan, (NeuAcalpha2-->3)2Gal2GlcNAc2Man3GlcNAc(+/-Fuc)GlcNAc, and a GPI anchor, which contains an ethanolamine phosphate diester group, as a side chain. However, we found that both sialidase-treated soluble AP (sAP) and its GPI-anchored glycan bound to a Psathyrella velutina lectin (PVL)-Sepharose column, which binds beta-GlcNAc residues. PVL binding of asialo-sAP and its GPI-anchored glycan was diminished by digestion with diplococcal beta-N-acetylhexosaminidase or by mild acid treatment. After sequential digestion of asialo-sAP with beta-N-acetylhexosaminidase and acid phosphatase, the elution patterns on chromatofocusing gels were changed in accordance with the negative charges of phosphate residues. Trypsin-digested sAP was analyzed by liquid chromatography/electrospray ionization mass spectrometry, and the structures of two glycopeptides with GPI-anchored glycans were confirmed as peptide-EtN-PO4-6Manalpha1-->2(GlcNAcbeta1-PO4-->6)Manalpha1-6(+/-EtN-PO4-->)Manalpha1-->4GlcN, which may be produced by endo-alpha-glucosaminidase. In addition to AP, GPI-anchored carcinoembryonic antigen, cholinesterase, and Tamm-Horsfall glycoprotein also bound to a PVL-Sepharose column, suggesting that the beta-N-acetylglucosaminyl phosphate diester residue is widely distributed in human GPI-anchored glycans. Furthermore, we found that the beta-N-acetylglucosaminyl phosphate diester residue is important for GPI anchor recognition of aerolysin, a channel-forming toxin derived from Aeromonas hydrophila.

The Beta Pictoris Phenomenon in A-Shell Stars: Detection of Accreting Gas

NASA Technical Reports Server (NTRS)

Grady, C. A.; Perez, Mario R.; Talavera, A.; McCollum, B.; Rawley, L. A.; England, M. N.; Schlegel, M.

1996-01-01

We present the results of an expanded survey of A-shell stars using IUE high-dispersion spectra and find accreting, circumstellar gas in the line of sight to nine stars, in addition to the previously identified beta Pic, HR 10, and 131 Tau, which can be followed to between +70 and 100 km/s relative to the star. Two of the program stars, HD 88195 and HD 148283, show variable high-velocity gas. Given the small number of IUE spectra for our program stars, detection of high-velocity, accreting gas in 2/3 of the A-shell stars sampled indicates that accretion is an intrinsic part of the A-shell phenomenon and that beta Pic is not unique among main-sequence A stars in exhibiting such activity. Our program stars, as a group, have smaller column densities of high-velocity gas and smaller near-IR excesses compared with beta Pic. These features are consistent with greater central clearing of a remnant debris disk, compared with beta Pic, and suggest that the majority of field A-shell stars are older than beta Pic.

Ap4A and ADP-beta-S binding to P2 purinoceptors present on rat brain synaptic terminals.

PubMed Central

Pintor, J.; Díaz-Rey, M. A.; Miras-Portugal, M. T.

1993-01-01

1. Diadenosine tetraphosphate (Ap4A) a dinucleotide stored and released from rat brain synaptic terminals presents two types of affinity binding sites in synaptosomes. When [3H]-Ap4A was used for binding studies a Kd value of 0.10 +/- 0.014 nM and a Bmax value of 16.6 +/- 1.2 fmol mg-1 protein were obtained for the high affinity binding site from the Scatchard analysis. The second binding site, obtained by displacement studies, showed a Ki value of 0.57 +/- 0.09 microM. 2. Displacement of [3H]-Ap4A by non-labelled Ap4A and P2-purinoceptor ligands showed a displacement order of Ap4A > adenosine 5'-O-(2-thiodiphosphate) (ADP-beta-S) > 5'-adenylyl-imidodiphosphate (AMP-PNP) > alpha,beta-methylene adenosine 5'-triphosphate (alpha,beta-MeATP) in both sites revealed by the Ki values of 0.017 nM, 0.030 nM, 0.058 nM and 0.147 nM respectively for the high affinity binding site and values of 0.57 microM, 0.87 microM, 2.20 microM and 4.28 microM respectively for the second binding site. 3. Studies of the P2-purinoceptors present in synaptosomes were also performed with [35S]-ADP-beta-S. This radioligand showed two binding sites the first with Kd and Bmax values of 0.11 +/- 0.022 nM and 3.9 +/- 2.1 fmol mg-1 of protein respectively for the high affinity binding site obtained from the Scatchard plot. The second binding site showed a Ki of 0.018 +/- 0.0035 microM obtained from displacement curves. 4. Competition studies with diadenosine polyphosphates of [35S]-ADP-beta-S binding showed a displacement order of Ap4A > Ap5A > Ap6A in the high affinity binding site and Ki values of 0.023 nM, 0.081 nM and 5.72 nM respectively.(ABSTRACT TRUNCATED AT 250 WORDS) PMID:8485620

VizieR Online Data Catalog: High quality Spitzer/MIPS obs. of F4-K2 stars (Sierchio+, 2014)

NASA Astrophysics Data System (ADS)

Sierchio, J. M.; Rieke, G. H.; Su, K. Y. L.; Gaspar, A.

2016-11-01

We used specific criteria to draw samples of stars from the entire Spitzer Debris Disk Database (see section 2.1.1). V magnitudes were taken from Hipparcos and transformed to Johnson V. All stars were also required to have observations on the Two Micron All Sky Survey (2MASS) Ks system. Additional measurements were obtained at SAAO on the 0.75m telescope using the MarkII Infrared Photometer (transformed as described by Koen et al. 2007MNRAS.380.1433K), and at the Steward Observatory 61 in telescope using a NICMOS2-based camera with a 2MASS filter set and a neutral density filter to avoid saturation. These measurements will be described in a forthcoming paper (K. Y. L. Su et al., in preparation). The original programs in which our sample stars were measured are identified in Table 1. A large majority (93%) come from seven Spitzer programs: (1) the MIPS Guaranteed Time Observer (GTO) Sun-like star observations (Trilling+ 2008ApJ...674.1086T); (2) Formation and Evolution of Planetary Systems (FEPS; Meyer+ 2006, J/PASP/118/1690); (3) Completing the Census of Debris Disks (Koerner+ 2010ApJ...710L..26K); (4) potential Space Interferometry Mission/Terrestrial Planet Finder (SIM/TPF) targets (Beichman+ 2006ApJ...652.1674B); (5) an unbiased sample of F-stars (Trilling+ 2008ApJ...674.1086T); and (6) two coordinated programs selecting stars on the basis of indicators of youth (Low+ 2005ApJ...631.1170L; Plavchan+ 2009ApJ...698.1068P). See section 2.1.2. (1 data file).

Retinoic acid and Wnt/beta-catenin have complementary roles in anterior/posterior patterning embryos of the basal chordate amphioxus.

PubMed

Onai, Takayuki; Lin, Hsiu-Chin; Schubert, Michael; Koop, Demian; Osborne, Peter W; Alvarez, Susana; Alvarez, Rosana; Holland, Nicholas D; Holland, Linda Z

2009-08-15

A role for Wnt/beta-catenin signaling in axial patterning has been demonstrated in animals as basal as cnidarians, while roles in axial patterning for retinoic acid (RA) probably evolved in the deuterostomes and may be chordate-specific. In vertebrates, these two pathways interact both directly and indirectly. To investigate the evolutionary origins of interactions between these two pathways, we manipulated Wnt/beta-catenin and RA signaling in the basal chordate amphioxus during the gastrula stage, which is the RA-sensitive period for anterior/posterior (A/P) patterning. The results show that Wnt/beta-catenin and RA signaling have distinctly different roles in patterning the A/P axis of the amphioxus gastrula. Wnt/beta-catenin specifies the identity of the ends of the embryo (high Wnt = posterior; low Wnt = anterior) but not intervening positions. Thus, upregulation of Wnt/beta-catenin signaling induces ectopic expression of posterior markers at the anterior tip of the embryo. In contrast, RA specifies position along the A/P axis, but not the identity of the ends of the embryo-increased RA signaling strongly affects the domains of Hox expression along the A/P axis but has little or no effect on the expression of either anterior or posterior markers. Although the two pathways may both influence such things as specification of neuronal identity, interactions between them in A/P patterning appear to be minimal.

Effects of PPADS and suramin on contractions and cytoplasmic Ca2+ changes evoked by AP4A, ATP and alpha, beta-methylene ATP in guinea-pig urinary bladder.

PubMed Central

Usune, S.; Katsuragi, T.; Furukawa, T.

1996-01-01

1. The contraction and intracellular Ca2+ change evoked by diadenosine tetraphosphate (AP4A) were studied in the outer longitudinal muscle of the guinea-pig urinary bladder and compared with those evoked by ATP and alpha, beta-methylene ATP (a P2-purinoceptor agonist). 2. AP4A, ATP and alpha, beta-methylene ATP produced concentration-dependent transient contractions. These contractions were inhibited by PPADS (pyridoralphosphate-6-azophenyl- 2'-4'-disulphonic acid), 0.3- 30 microM, a P2x-purinoceptor antagonist, and suramin, 1-300 microM, a P2-purinoceptor antagonist in a concentration-dependent manner. From Schild plot analysis, the apparent pA2 values for PPADS for contractions evoked by AP4A, ATP and alpha, beta-methylene ATP were 6.86, 6.56, 6.74, and those for suramin were 6.01, 4.59 and 5.12, respectively; the Schild slopes for PPADS were 1.07, 1.14 and 1.06, and, those for suramin 0.75, 1.05 and 1.16, respectively. 3. AP4A (10 microM) and ATP (100 microM) failed to elicit any contraction of the tissue after a desensitization produced by repeated application of alpha, beta-methylene ATP (1 microM). 4. In fluorescence experiments with fura-2, the increases in [Ca2+]i and contraction evoked by AP4A were suppressed by suramin and nifedipine, an L-type Ca2+ channel blocker. 5. These findings suggest that P2x-purinoceptors, which are more sensitive to PPADS than suramin, exist on the outer longitudinal muscles of guinea-pig urinary bladder, and that the AP4A-evoked contraction results from Ca2+ influx. PMID:8646416

Ap stars with resolved magnetically split lines: Magnetic field determinations from Stokes I and V spectra⋆

NASA Astrophysics Data System (ADS)

Mathys, G.

2017-05-01

Context. Some Ap stars that have a strong enough magnetic field and a sufficiently low v sini show spectral lines resolved into their magnetically split components. Aims: We present the results of a systematic study of the magnetic fields and other properties of those stars. Methods: This study is based on 271 new measurements of the mean magnetic field modulus ⟨ B ⟩ of 43 stars, 231 determinations of the mean longitudinal magnetic field ⟨ Bz ⟩ and of the crossover ⟨ Xz ⟩ of 34 stars, and 229 determinations of the mean quadratic magnetic field ⟨ Bq ⟩ of 33 stars. Those data were used to derive new values or meaningful lower limits of the rotation periods Prot of 21 stars. Variation curves of the mean field modulus were characterised for 25 stars, the variations of the longitudinal field were characterised for 16 stars, and the variations of the crossover and of the quadratic field were characterised for 8 stars. Our data are complemented by magnetic measurements from the literature for 41 additional stars with magnetically resolved lines. Phase coverage is sufficient to define the curve of variation of ⟨ B ⟩ for 2 of these stars. Published data were also used to characterise the ⟨ Bz ⟩ curves of variation for 10 more stars. Furthermore, we present 1297 radial velocity measurements of the 43 Ap stars in our sample that have magnetically resolved lines. Nine of these stars are spectroscopic binaries for which new orbital elements were derived. Results: The existence of a cut-off at the low end of the distribution of the phase-averaged mean magnetic field moduli ⟨ B ⟩ av of the Ap stars with resolved magnetically split lines, at about 2.8 kG, is confirmed. This reflects the probable existence of a gap in the distribution of the magnetic field strengths in slowly rotating Ap stars, below which there is a separate population of stars with fields weaker than 2 kG. In more than half of the stars with magnetically resolved lines that have a rotation period shorter than 150 days, ⟨ B ⟩ av > 7.5 kG, while those stars with a longer period all have ⟨ B ⟩ av < 7.5 kG. The difference between the two groups is significant at the 100.0% confidence level. The relative amplitudes of variation of the mean field modulus may tend to be greater in stars with Prot > 100 d than in shorter period stars. The root-mean-square longitudinal fields of all the studied stars but one is less than one-third of their phased-average mean field moduli, which is consistent with the expected behaviour for fields whose geometrical structure resembles a centred dipole. However, moderate but significant departures from the latter are frequent. Crossover resulting from the correlation between the Zeeman effect and the rotation-induced Doppler effect across the stellar surface is definitely detected in stars with rotation periods of up to 130 days and possibly even up to 500 days. Weak, but formally significant crossover of constant sign, has also been observed in a number of longer period stars, which could potentially be caused by pulsation velocity gradients across the depth of the photosphere. The quadratic field is in average 1.3 times greater than the mean field modulus and both of those moments vary with similar relative amplitudes and almost in phase in most stars. Rare exceptions almost certainly have unusual field structures. The distribution of the known values and lower limits of the rotation periods of the Ap stars with magnetically resolved lines indicates that for some of them, Prot must almost certainly reach 300 yr or possibly even much higher values. Of the 43 Ap stars that we studied in detail, 22 are in binary systems. The shortest orbital period Porb of those systems is 27 days. For those non-synchronised Ap binaries for which both the rotation period and the orbital period, or meaningful lower limits thereof, are reliably determined, the distribution of the orbital periods of the systems in which the Ap star has a rotation period that is shorter than 50 days is different from its distribution for those systems in which the rotation period of the Ap star is longer, at a confidence level of 99.6%. The shortest rotation and orbital periods are mutually exclusive: all but one of the non-synchronised systems that contain an Ap component with Prot < 50 d, have Porb > 1000 d. Conclusions: Stars with resolved magnetically split lines represent a significant fraction, of the order of several percent, of the whole population of Ap stars. Most of these stars are genuine slow rotators, whose consideration provides new insight into the long-period tail of the distribution of the periods of Ap stars. Emerging correlations between rotation periods and magnetic properties provide important clues for the understanding of the braking mechanisms that have been at play in the early stages of stellar evolution. The geometrical structures of the magnetic fields of Ap stars with magnetically resolved lines appear in general to depart slightly, but not extremely, from centred dipoles. However, there are a few remarkable exceptions, which deserve further consideration. Confirmation that pulsational crossover is indeed occurring at a detectable level would open the door to the study of non-radial pulsation modes of degree ℓ, which is too high for photometric or spectroscopic observations. How the lack of short orbital periods among binaries containing an Ap component with magnetically resolved lines is related to their (extremely) slow rotation remains to be fully understood, but the very existence of a correlation between the two periods lends support to the merger scenario for the origin of Ap stars. Based on observations collected at the European Southern Observatory, Chile (ESO Programmes 56.E-0688, 56.E-0690, 57.E-0557, 57.E-0637, 58.E-0155, 58.E-0159, 59.E-0372, 59.E-0373, 60.E-0564, 60.E-0565, 61.E-0711, and Period 56 Director Discretionary Time); at Observatoire de Haute Provence (CNRS), France; at Kitt Peak National Observatory, National Optical Astronomy Observatory (NOAO Prop. ID: KP2442; PI: T. Lanz), which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation; and at the Canada-France-Hawaii Telescope (CFHT), which is operated from the summit of Mauna Kea by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. The observations at the Canada-France-Hawaii Telescope were performed with care and respect from the summit of Mauna Kea, which is a significant cultural and historic site.Table 7 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (http://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/601/A14

Predicting the Presence of Companions for Stripped-envelope Supernovae: The Case of the Broad-lined Type Ic SN 2002ap

NASA Astrophysics Data System (ADS)

Zapartas, E.; de Mink, S. E.; Van Dyk, S. D.; Fox, O. D.; Smith, N.; Bostroem, K. A.; de Koter, A.; Filippenko, A. V.; Izzard, R. G.; Kelly, P. L.; Neijssel, C. J.; Renzo, M.; Ryder, S.

2017-06-01

Many young, massive stars are found in close binaries. Using population synthesis simulations we predict the likelihood of a companion star being present when these massive stars end their lives as core-collapse supernovae (SNe). We focus on stripped-envelope SNe, whose progenitors have lost their outer hydrogen and possibly helium layers before explosion. We use these results to interpret new Hubble Space Telescope observations of the site of the broad-lined Type Ic SN 2002ap, 14 years post-explosion. For a subsolar metallicity consistent with SN 2002ap, we expect a main-sequence (MS) companion present in about two thirds of all stripped-envelope SNe and a compact companion (likely a stripped helium star or a white dwarf/neutron star/black hole) in about 5% of cases. About a quarter of progenitors are single at explosion (originating from initially single stars, mergers, or disrupted systems). All of the latter scenarios require a massive progenitor, inconsistent with earlier studies of SN 2002ap. Our new, deeper upper limits exclude the presence of an MS companion star >8-10 {M}⊙ , ruling out about 40% of all stripped-envelope SN channels. The most likely scenario for SN 2002ap includes nonconservative binary interaction of a primary star initially ≲ 23 {M}⊙ . Although unlikely (<1% of the scenarios), we also discuss the possibility of an exotic reverse merger channel for broad-lined Type Ic events. Finally, we explore how our results depend on the metallicity and the model assumptions and discuss how additional searches for companions can constrain the physics that govern the evolution of SN progenitors.

New results of the spectral observations of CP stars

NASA Astrophysics Data System (ADS)

Polosukhina, N. S.; Shavrina, A. V.; Drake, N. A.; Kudryavtsev, D. O.; Smirnova, M. A.

2010-04-01

The lithium problem in Ap-CP stars has been, for a long time, a subject of debate. Individual characteristics of CP stars, such as high abundance of the rare-earth elements presence of magnetic fields, complicate structure of the surface distribution of chemical elements, rapid oscillations of some CP-stars, make the detection of the lithium lines and the determination of the lithium abundance, a difficult task. During the International Meeting in Slovakia in 1996, the lithium problem in Ap-CP stars was discussed. The results of the Li study carried out in CrAO Polosukhina (1973-1976), the works of Hack & Faraggiana (1963), Wallerstein & Hack (1964), Faraggiana et al. (1992-1996) formed the basis of the International project ‘Lithium in the cool CP-stars with magnetic fields’. The main goal of the project was, using systematical observations of Ap-CP stars with phase rotation in the spectral regions of the resonance doublet Li I 6708 Å and subordinate 6104 Å lithium lines with different telescopes, to create a database, which will permit to explain the physical origin of anomalous Li abundance in the atmospheres of these stars.

A Brightness-Referenced Star Identification Algorithm for APS Star Trackers

PubMed Central

Zhang, Peng; Zhao, Qile; Liu, Jingnan; Liu, Ning

2014-01-01

Star trackers are currently the most accurate spacecraft attitude sensors. As a result, they are widely used in remote sensing satellites. Since traditional charge-coupled device (CCD)-based star trackers have a limited sensitivity range and dynamic range, the matching process for a star tracker is typically not very sensitive to star brightness. For active pixel sensor (APS) star trackers, the intensity of an imaged star is valuable information that can be used in star identification process. In this paper an improved brightness referenced star identification algorithm is presented. This algorithm utilizes the k-vector search theory and adds imaged stars' intensities to narrow the search scope and therefore increase the efficiency of the matching process. Based on different imaging conditions (slew, bright bodies, etc.) the developed matching algorithm operates in one of two identification modes: a three-star mode, and a four-star mode. If the reference bright stars (the stars brighter than three magnitude) show up, the algorithm runs the three-star mode and efficiency is further improved. The proposed method was compared with other two distinctive methods the pyramid and geometric voting methods. All three methods were tested with simulation data and actual in orbit data from the APS star tracker of ZY-3. Using a catalog composed of 1500 stars, the results show that without false stars the efficiency of this new method is 4∼5 times that of the pyramid method and 35∼37 times that of the geometric method. PMID:25299950

A brightness-referenced star identification algorithm for APS star trackers.

PubMed

Zhang, Peng; Zhao, Qile; Liu, Jingnan; Liu, Ning

2014-10-08

Star trackers are currently the most accurate spacecraft attitude sensors. As a result, they are widely used in remote sensing satellites. Since traditional charge-coupled device (CCD)-based star trackers have a limited sensitivity range and dynamic range, the matching process for a star tracker is typically not very sensitive to star brightness. For active pixel sensor (APS) star trackers, the intensity of an imaged star is valuable information that can be used in star identification process. In this paper an improved brightness referenced star identification algorithm is presented. This algorithm utilizes the k-vector search theory and adds imaged stars' intensities to narrow the search scope and therefore increase the efficiency of the matching process. Based on different imaging conditions (slew, bright bodies, etc.) the developed matching algorithm operates in one of two identification modes: a three-star mode, and a four-star mode. If the reference bright stars (the stars brighter than three magnitude) show up, the algorithm runs the three-star mode and efficiency is further improved. The proposed method was compared with other two distinctive methods the pyramid and geometric voting methods. All three methods were tested with simulation data and actual in orbit data from the APS star tracker of ZY-3. Using a catalog composed of 1500 stars, the results show that without false stars the efficiency of this new method is 4~5 times that of the pyramid method and 35~37 times that of the geometric method.

A Novel GLP1 Receptor Interacting Protein ATP6ap2 Regulates Insulin Secretion in Pancreatic Beta Cells*

PubMed Central

Dai, Feihan F.; Bhattacharjee, Alpana; Liu, Ying; Batchuluun, Battsetseg; Zhang, Ming; Wang, Xinye Serena; Huang, Xinyi; Luu, Lemieux; Zhu, Dan; Gaisano, Herbert; Wheeler, Michael B.

2015-01-01

GLP1 activates its receptor, GLP1R, to enhance insulin secretion. The activation and transduction of GLP1R requires complex interactions with a host of accessory proteins, most of which remain largely unknown. In this study, we used membrane-based split ubiquitin yeast two-hybrid assays to identify novel GLP1R interactors in both mouse and human islets. Among these, ATP6ap2 (ATPase H+-transporting lysosomal accessory protein 2) was identified in both mouse and human islet screens. ATP6ap2 was shown to be abundant in islets including both alpha and beta cells. When GLP1R and ATP6ap2 were co-expressed in beta cells, GLP1R was shown to directly interact with ATP6ap2, as assessed by co-immunoprecipitation. In INS-1 cells, overexpression of ATP6ap2 did not affect insulin secretion; however, siRNA knockdown decreased both glucose-stimulated and GLP1-induced insulin secretion. Decreases in GLP1-induced insulin secretion were accompanied by attenuated GLP1 stimulated cAMP accumulation. Because ATP6ap2 is a subunit required for V-ATPase assembly of insulin granules, it has been reported to be involved in granule acidification. In accordance with this, we observed impaired insulin granule acidification upon ATP6ap2 knockdown but paradoxically increased proinsulin secretion. Importantly, as a GLP1R interactor, ATP6ap2 was required for GLP1-induced Ca2+ influx, in part explaining decreased insulin secretion in ATP6ap2 knockdown cells. Taken together, our findings identify a group of proteins that interact with the GLP1R. We further show that one interactor, ATP6ap2, plays a novel dual role in beta cells, modulating both GLP1R signaling and insulin processing to affect insulin secretion. PMID:26272612

Circumstellar Structure Around Evolved Stars in the Cygnus-X Star Formation Region

DTIC Science & Technology

2010-06-01

respectively: Jimenez-Esteban et al. 2010, ApJ, 713, 429 and Gvaramadze et al. 2010, MNRAS, in press; and Gvaramadze et al. 2009, MNRAS, 400, 524...F. 1978, ApJ, 222, LI29 Goebel, J. H., & Moseley, S. H. 1985, ApJ, 290, L35 Gutermuth, R. A., et al. 2008, ApJ, 674, 336 Gvaramadze , V. V., et al...2009, MNRAS, 400, 524 Gvaramadze , V. V., et al. 2010, MNRAS, in press Herbig, G. H. 2009, AJ, 138, 1502 Higgs, L. A., Wendker, H. J., & Landecker

CMOS Active Pixel Sensor Star Tracker with Regional Electronic Shutter

NASA Technical Reports Server (NTRS)

Yadid-Pecht, Orly; Pain, Bedabrata; Staller, Craig; Clark, Christopher; Fossum, Eric

1996-01-01

The guidance system in a spacecraft determines spacecraft attitude by matching an observed star field to a star catalog....An APS(active pixel sensor)-based system can reduce mass and power consumption and radiation effects compared to a CCD(charge-coupled device)-based system...This paper reports an APS (active pixel sensor) with locally variable times, achieved through individual pixel reset (IPR).

beta. -Amyloid precursor protein of Alzheimer disease occurs as 110- to 135-kilodalton membrane-associated proteins in neural and nonneural tissues

DOE Office of Scientific and Technical Information (OSTI.GOV)

Selkoe, D.J.; Podlisny, M.B.; Joachim, C.L.

1988-10-01

Progressive cerebral deposition of extracellular filaments composed of the {beta}-amyloid protein ({beta}AP) is a constant feature of Alzheimer disease (AD). Since the gene on chromosome 21 encoding the {beta}AP precursor ({beta}APP) is not known to be altered in AD, transcriptional or posttranslational changes may underlie accelerated {beta}AP deposition. Using two antibodies to the predicted carboxyl terminus of {beta}APP, the authors have identified the native {beta}APP in brain and nonneural human tissues as a 110- to 135-kDa protein complex that is insoluble in buffer and found in various membrane-rich subcellular fractions. These proteins are relatively uniformly distributed in adult brain, abundantmore » in fetal brain, and detected in nonneural tissues that contain {beta}APP mRNA. Similarly sized proteins occur in rat, cow, and monkey brain and in cultured human HL-60 and HeLa cells; the precise patterns in the 110- to 135-kDa range are heterogeneous among various tissues and cell lines. They conclude that the highly conserved {beta}APP molecule occurs in mammalian tissues as a heterogeneous group of membrane-associated proteins of {approx} 120 kDa. Detection of the nonamyloidogenic carboxyl terminus within plaques suggests that proteolytic processing of the {beta}APP into insoluble filaments occurs locally in cortical regions that develop {beta}-amyloid deposits with age.« less

Replacing colour blindness with Depth Perception

NASA Astrophysics Data System (ADS)

Matthews, Jaymie M.

Until recently, most work on rapidly oscillating Ap (roAp) stars has concentrated on rapid single-bandpass photometry, which efficiently samples their short periods even with telescopes of modest aperture. Global campaigns of this nature have yielded eigenfrequency spectra essential to asteroseismology. However, we have reached a threshold where such data must be supplemented with rapid spectroscopy and photometry at many bandpasses if we are to (a) identify the modes in roAp stars, and (b) fully exploit those modes to probe the stars' atmospheres and interiors. Studies by Medupe & Kurtz and Matthews raise the prospect of using the wavelength dependence of oscillation amplitude to map pulsational dynamics and/or atmospheric structure in roAp stars. Also, precise measurements of velocity oscillations through rapid high-resolution spectroscopy suggest that spectral lines from different ions behave differently. Given the chemical stratification and inhomogeneities of peculiar atmospheres, this may be a way to map spherical harmonic modes in 3-D (i.e., depths of upper radial nodes and positions of the surface nodes).

The Galactic O-Star Spectroscopic Survey (GOSSS): new results from the southern stars

NASA Astrophysics Data System (ADS)

Sota, A.; Maíz Apellániz, J.; Barbá, R. H.; Walborn, N. R.; Alfaro, E. J.; Gamen, R. C.; Morrell, N. I.; Arias, J. I.; Penadés Ordaz, M.

2013-05-01

The Galactic O-Star Spectroscopic Survey (GOSSS) is a project that will observe all known Galactic O stars with B < 14 in the blue-violet part of the spectrum with R ˜ 3000. It is based on v2.0 of the the most complete Galactic O star catalog with accurate spectral types (Maíz Apellániz et al. 2004, ApJS, 151, 103; Sota et al. 2008, RevMexAA Conf. Series, 33, 55) that we have recently compiled. We have completed the first part of the main project and recently published the first articles (Walborn et al. 2010, ApJ, 711, 143; Walborn et al. 2011, AJ, 142, 150; Sota et al. 2011, ApJS, 193, 24). GOSSS is part of a bigger project with the next companion surveys: High resolution spectroscopic surveys: OWN, IACOB, IACOB-sweG, NoMaDS, CAFÉ-BEANS High resolution imaging surveys: Astralux, Astralux Sur.

VizieR Online Data Catalog: Solar analogs and twins rotation by Kepler (do Nascimento+, 2014)

NASA Astrophysics Data System (ADS)

Do Nascimento, J.-D. Jr; Garcia, R. A.; Mathur, S.; Anthony, F.; Barnes, S. A.; Meibom, S.; da Costa, J. S.; Castro, M.; Salabert, D.; Ceillier, T.

2017-03-01

Our sample of 75 stars consists of a seismic sample of 38 from Chaplin et al. (2014, J/ApJS/210/1), 35 additional stars selected from the Kepler Input Catalog (KIC), and 16 Cyg A and B. We selected 38 well-studied stars from the asteroseismic data with fundamental properties, including ages, estimated by Chaplin et al. (2014, J/ApJS/210/1), and with Teff and log g as close as possible to the Sun's value (5200 K < Teff < 6060 K and 3.63 < log g < 4.40). This seismic sample allows a direct comparison between gyro- and seismic-ages for a subset of eight stars. These seismic samples were observed in short cadence for one month each in survey mode. Stellar properties for these stars have been estimated using two global asteroseismic parameters and complementary photometric and spectroscopic observations as described by Chaplin et al. (2014, J/ApJS/210/1). The median final quoted uncertainties for the full Chaplin et al. (2014, J/ApJS/210/1) sample were approximately 0.020 dex in log g and 150 K in Teff. (1 data file).

New Results of Spectral Observations of CP Stars in the Li I 6708 Å Spectral Region with the 6-m BTA Telescope

NASA Astrophysics Data System (ADS)

Polosukhina, N.; Shavrina, A.; Drake, N.; Kudryavtsev, D.; Smirnova, M.

The lithium problem in Ap-CP stars has for a long time been a subject of debates. Individual characteristics of CP stars, such as a high abundance of rare-earth elements, the presence of magnetic fields, complex structures of the surface distribution of chemical elements, rapid oscillations of some CP stars, make the detection of lithium lines, and determination of lithium abundance a challenging task. The lithium problem in Ap-CP stars was discussed during the meeting in Slovakia in 1996. The results of the Li study, carried out in CrAO (Polosukhina, 1973 - 1976), the works of Faraggiana & Hack (1963), Wallerstein & Hack (1964), Faraggiana et al. (1992 - 1996) formed the basis of the international project, called Lithium in the Cool CP Stars with Magnetic Fields. The main goal of the project was, using systematical observations of Ap-CP stars with phase rotation in the spectral regions of the resonance doublet Li I 6708 Å and subordinate 6104 Å lithium lines with different telescopes, to create a database, which will permit to explain the physical origin of the anomalous Li abundance in the atmospheres of these stars.

Defective pigment granule biogenesis and aberrant behavior caused by mutations in the Drosophila AP-3beta adaptin gene ruby.

PubMed Central

Kretzschmar, D; Poeck, B; Roth, H; Ernst, R; Keller, A; Porsch, M; Strauss, R; Pflugfelder, G O

2000-01-01

Lysosomal protein trafficking is a fundamental process conserved from yeast to humans. This conservation extends to lysosome-like organelles such as mammalian melanosomes and insect eye pigment granules. Recently, eye and coat color mutations in mouse (mocha and pearl) and Drosophila (garnet and carmine) were shown to affect subunits of the heterotetrameric adaptor protein complex AP-3 involved in vesicle trafficking. Here we demonstrate that the Drosophila eye color mutant ruby is defective in the AP-3beta subunit gene. ruby expression was found in retinal pigment and photoreceptor cells and in the developing central nervous system. ruby mutations lead to a decreased number and altered size of pigment granules in various cell types in and adjacent to the retina. Humans with lesions in the related AP-3betaA gene suffer from Hermansky-Pudlak syndrome, which is caused by defects in a number of lysosome-related organelles. Hermansky-Pudlak patients have a reduced skin pigmentation and suffer from internal bleeding, pulmonary fibrosis, and visual system malfunction. The Drosophila AP-3beta adaptin also appears to be involved in processes other than eye pigment granule biogenesis because all ruby allele combinations tested exhibited defective behavior in a visual fixation paradigm. PMID:10790396

Statistical studies of superflares on G-, K-, M- type stars from Kepler data

NASA Astrophysics Data System (ADS)

Notsu, Yuta; Maehara, Hiroyuki; Honda, Satoshi; Notsu, Shota; Namekata, Kosuke; Ikuta, Kai; Nogami, Daisaku; Shibata, Kazunari

2017-05-01

Flares are thought to be sudden releases of magnetic energy stored around starspots. Recent space high-precision photometry shows “superflares”, 10-104 times more energetic than the largest solar flares, occur on many G, K, M-type stars (e.g., Maehara+2012 Nature). Harmful UV/X-ray radiation and high-energy particles such as protons are caused by such superflares. This may suggest that exoplanet host stars have severe effects on the physical and chemical evolution of exoplanetary atmospheres (cf. Segura+2010 Astrobiology, Takahashi+2016 ApJL).We here present statistical properties of superflares on G, K, M-type stars on the basis of our analyses of Kepler photometric data (Maehara+2012 Nature, Shibayama+2013 ApJS, Notsu+2013 ApJ, Canderaresi+2014 ApJ, Maehara+2015 EPS, Maehara+2017 PASJ). We found more than 5000 superflares on 800 G, K, M-type main-sequence stars, and the occurrence frequency (dN/dE) of superflares as a function of flare energy (E) shows the power-law distribution with the index of -1.8 -1.9. This power-law distribution is consistent with that of solar flares.Flare frequency increases as stellar temperature decreases. As for M-type stars, energy of the largest flares is smaller compared with G,K-type stars, but more frequent “hazardous” flares for the habitable planets since the habitable zone around M-type stars is much smaller compared with G, K-type stars.Rotation period and starspot coverage can be estimated from the quasi-periodic brightness variation of the superflare stars. The intensity of Ca II 8542 line of superflare stars, which is measured from spectroscopic observations with Subaru Telescope, has a well correlation with the brightness variation amplitude (Notsu+2015a&b PASJ).Flare frequency has a correlation with rotation period, and this suggests young rapidly-rotating stars (like “young Sun”) have more severe impacts of flares on the planetary atmosphere (cf. Airapetian+2016 ApJL). Flare energy and frequency also depends on starspot coverage, and this suggests existence of large starspots is important factor of superflares.These statistical properties of superflares discussed here can be one of the basic information for considering the impacts of flares on planet-host stars.

White Dwarf Stars

NASA Astrophysics Data System (ADS)

Kepler, S. O.

2014-10-01

White dwarfs are the evolutionary endpoint for nearly 95% of all stars born in our Galaxy, the final stages of evolution of all low- and intermediate mass stars, i.e., main sequence stars with masses below (8.5± 1.5) M_{odot}, depending on metallicity of the progenitor, mass loss and core overshoot. Massive white dwarfs are intrinsically rare objects, tand produce a gap in the determination of the initial vs. final mass relation at the high mass end (e.g. Weidemann 2000 A&A, 363, 647; Kalirai et al. 2008, ApJ, 676, 594; Williams, Bolte & Koester 2009, ApJ, 693, 355). Main sequences stars with higher masses will explode as SNII (Smartt S. 2009 ARA&A, 47, 63), but the limit does depend on the metallicity of the progenitor. Massive white dwarfs are probably SNIa progenitors through accretion or merger. They are rare, being the final product of massive stars (less common) and have smaller radius (less luminous). Kepler et al. 2007 (MNRAS, 375, 1315), Kleinman et al. 2013 (ApJS, 204, 5) estimate only 1-2% white dwarfs have masses above 1 M_{odot}. The final stages of evolution after helium burning are a race between core growth and loss of the H-rich envelope in a stellar wind. When the burning shell is exposed, the star rapidly cools and burning ceases, leaving a white dwarf. As they cool down, the magnetic field freezes in, ranging from a few kilogauss to a gigagauss. Peculiar type Ia SN 2006gz, SN 2007if, SN 2009dc, SN 2003fg suggest progenitors in the range 2.4-2.8 M_{odot}, and Das U. & Mukhopadhyay B. (2012, Phys. Rev. D, 86, 042001) estimate that the Chandrasekhar limit increases to 2.3-2.6 M_{odot} for extremely high magnetic field stars, but differential rotation induced by accretion could also increase it, according to Hachisu I. et al. 2012 (ApJ, 744, 69). García-Berro et al. 2012, ApJ, 749, 25, for example, proposes double degenerate mergers are the progenitors of high-field magnetic white dwarfs. We propose magnetic fields enhance the line broadening in WDs, causing an overestimated surface gravity, and ultimately determine if these magnetic fields are likely developed through the star's own surface convection zone, or inherited from massive Ap/Bp progenitors. We discovered around 20 000 spectroscopic white dwarfs with the Sloan Digital Sky Survey (SDSS), with a corresponding increase in relatively rare varieties of white dwarfs, including the massive ones (Kleinman et al. 2013, ApJS, 204, 5, Kepler et al. 2013, MNRAS, 439, 2934). The mass distributions of the hydrogen-rich (DA) measured from fitting the spectra with model atmospheres calculated using unidimensinal mixing lenght-theory (MLT) shows the average mass (as measured by the surface gravity) increases apparently below 13 000K for DAs (e.g. Bergeron et al. 1991, ApJ, 367, 253; Tremblay et al. 2011, ApJ, 730, 128; Kleinman et al. 2013). Only with the tridimensional (3D) convection calculations of Tremblay et al. 2011 (A&A, 531, L19) and 2013 (A&A, 552, 13; A&A, 557, 7; arXiv 1309.0886) the problem has finally been solved, but the effects of magnetic fields are not included yet in the mass determinations. Pulsating white dwarf stars are used to measure their interior and envelope properties through seismology, and together with the luminosity function of white dwarf stars in clusters and around the Sun are valuable tools for the study of high density physics, and the history of stellar formation.

A survey for pulsations in A-type stars using SuperWASP

NASA Astrophysics Data System (ADS)

Holdsworth, Daniel L.

2015-12-01

"It is sound judgement to hope that in the not too distant future we shall be competent to understand so simple a thing as a star." - Sir Arthur Stanley Eddington, The Internal Constitution of Stars, 1926 A survey of A-type stars is conducted with the SuperWASP archive in the search for pulsationally variable stars. Over 1.5 million stars are selected based on their (J-H) colour. Periodograms are calculated for light curves which have been extracted from the archive and cleaned of spurious points. Peaks which have amplitudes greater than 0.5 millimagnitude are identified in the periodograms. In total, 202 656 stars are identified to show variability in the range 5-300 c/d. Spectroscopic follow-up was obtained for 38 stars which showed high-frequency pulsations between 60 and 235 c/d, and a further object with variability at 636 c/d. In this sample, 13 were identified to be normal A-type δ Sct stars, 14 to be pulsating metallic-lined Am stars, 11 to be rapidly oscillating Ap (roAp) stars, and one to be a subdwarf B variable star. The spectra were used not only to classify the stars, but to determine an effective temperature through Balmer line fitting. Hybrid stars have been identified in this study, which show pulsations in both the high- and low-overtone domains; an observation not predicted by theory. These stars are prime targets to perform follow-up observations, as a confirmed detection of this phenomenon will have significant impact on the theory of pulsations in A-type stars. The detected number of roAp stars has expanded the known number of this pulsator class by 22 per cent. Within these results both the hottest and coolest roAp star have been identified. Further to this, one object, KIC 7582608, was observed by the Kepler telescope for 4 yr, enabling a detailed frequency analysis. This analysis has identified significant frequency variations in this star, leading to the hypothesis that this is the first close binary star of its type. The observational results presented in this thesis are able to present new challenges to the theory of pulsations in A-type stars, with potentially having the effect of further delaying the full understanding of 'so simple a thing as a star'.

Analysis of magnetic activity of the rapidly rotating stars He 373 and AP 225

NASA Astrophysics Data System (ADS)

Kolbin, A. I.; Tsymbal, V. V.

2017-06-01

Spectroscopic and photometric data for the two rapidly rotating members of the α Persei cluster He 373 and AP 225 are analyzed. Improved estimates have been obtained for the projected equatorial rotation velocities: v sin i = 164 km/s for He 323 and v sin i = 129 km/s for AP 225. Multi-band photometric mapping is used to map the spot distributions on the surfaces of the two stars. The fractional spotted areas S and mean temperature difference Δ T between the unspotted photosphere and the spots are estimated ( S = 7% and Δ T = 1000 K for He 373; S = 9% and Δ T = 800 K for AP 225). The H α line profiles of both stars have variable emission components whose widths are used to deduce the presence of extended regions of emission reaching the corotation radius.

Lithium and Isotopic Ratio Li6/Li7 in Magnetic roAp Stars as an Indicator of Active Processes

NASA Astrophysics Data System (ADS)

Polosukhina, N.; Shavrina, A.; Lyashko, D.; Nesvacil, N.; Drake, N.; Smirnova, M.

2015-04-01

The lines of lithium at 6708 Å and 6103 Å are analyzed in high resolution spectra of some sharp-lined and slowly rotating roAp stars. Three spectral synthesis codes— STARSP, ZEEMAN2, and SYNTHM—were used. New lines of rare earth elements (REE) from the DREAM database and the lines calculated on the basis of the NIST energy levels were included. Magnetic splitting and other line broadening processes were taken into account. For both lithium lines, the enhanced abundances of lithium in the atmospheres of the stars studied are obtained. The lithium abundance determined from the Li 6103 Å line is higher than that from the Li 6708 Å for all the stars. This may be evidence of vertical lithium stratification, abnormal temperature distribution, or unidentified blending of the 6103 Å line. Our work on two roAp stars, HD 83368 and HD 60435 (Shavrina et al. 2001) provides evidence of an enhanced lithium abundance near the magnetic-field poles. We can expect similar effects in the sharp-lined roAp stars. High lithium abundance for all the stars and the estimates of the 6Li/7Li ratio (0.2-0.5) can be explained by production of Li in the cosmic ray spallation reactions in the interstellar medium where the stars were born, and by preservation of the original 6Li and 7Li by strong magnetic fields of these stars. The values of the 6Li/7Li ratio expected from production by cosmic rays are about 0.5-0.8 (Knauth et al. 2003; Webber et al. 2002). New laboratory and theoretical gf-values for REE lines are necessary in order to refine our estimates of lithium abundances and the isotopic ratio.

VizieR Online Data Catalog: UV spectra of classical T Tauri stars (France+, 2014)

NASA Astrophysics Data System (ADS)

France, K.; Schindhelm, E.; Bergin, E. A.; Roueff, E.; Abgrall, H.

2017-06-01

We present 16 objects from the larger GTO + DAO T Tauri star samples described by Ardila et al. (2013ApJS..207....1A; focusing on the hot gas emission lines) and France et al. (2012, J/ApJ/756/171; focusing on the molecular circumstellar environment). Eleven of the 16 sources were observed as part of the DAO of Tau guest observing program (PID 11616; PI: G. Herczeg), four were part of the COS Guaranteed Time Observing program on protoplanetary disks (PIDs 11533 and 12036; PI: J. Green), and we have included archival STIS observations of the well-studied CTTS TW Hya (Herczeg et al. 2002ApJ...572..310H, 2004ApJ...607..369H), obtained through StarCAT (Ayres 2010, J/ApJS/187/149). The targets were selected by the availability of reconstructed Lyα spectra, as this emission line is a critical component to the intrinsic CTTS UV radiation field (Schindhelm et al. 2012ApJ...756L..23S) and has not been uniformly included in recent studies of the CTTS radiation field (e.g., Ingleby et al. 2011AJ....141..127I; Yang et al. 2012, J/ApJ/744/121). Most of the targets were observed with the medium-resolution FUV modes of COS (G130M and G160M; Green et al. 2012ApJ...744...60G). (2 data files).

A magnetic survey of AP stars in young clusters - Preliminary results

NASA Astrophysics Data System (ADS)

Brown, D. N.; Landstreet, J. D.; Thompson, I.

Photoelectric polarimetry of Ap stars was undertaken in order to investigate the role of magnetic fields in the evolution of atmospheric chemical peculiarities and the braking of stellar rotation. The stars are grouped by cluster or association and listed by HD number, and each star's spectral type, reference for classification, number of magnetic observations, and root mean square of the equivalent magnetic field measurements obtained from an expression are shown. The data obtained to date include several new magnetic identifications and display the character of the survey, but are not yet sufficient to support any firm evolutionary conclusions.

Whole Earth Telescope discovery of a strongly distorted quadrupole pulsation in the largest amplitude rapidly oscillating Ap star

NASA Astrophysics Data System (ADS)

Holdsworth, Daniel L.; Kurtz, D. W.; Saio, H.; Provencal, J. L.; Letarte, B.; Sefako, R. R.; Petit, V.; Smalley, B.; Thomsen, H.; Fletcher, C. L.

2018-01-01

We present a new analysis of the rapidly oscillating Ap (roAp) star, 2MASS J19400781 - 4420093 (J1940; V = 13.1). The star was discovered using SuperWASP broad-band photometry to have a frequency of 176.39 d-1 (2041.55 μHz; P = 8.2 min; Holdsworth et al. 2014a) and is shown here to have a peak-to-peak amplitude of 34 mmag. J1940 has been observed during three seasons at the South African Astronomical Observatory, and has been the target of a Whole Earth Telescope campaign. The observations reveal that J1940 pulsates in a distorted quadrupole mode with unusual pulsational phase variations. A higher signal-to-noise ratio spectrum has been obtained since J1940's first announcement, which allows us to classify the star as A7 Vp Eu(Cr). The observing campaigns presented here reveal no pulsations other than the initially detected frequency. We model the pulsation in J1940 and conclude that the pulsation is distorted by a magnetic field of strength 1.5 kG. A difference in the times of rotational maximum light and pulsation maximum suggests a significant offset between the spots and pulsation axis, as can be seen in roAp stars.

FIRST MAGNETIC FIELD MODELS FOR RECENTLY DISCOVERED MAGNETIC {beta} CEPHEI AND SLOWLY PULSATING B STARS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Hubrig, S.; Ilyin, I.; Schoeller, M.

2011-01-01

In spite of recent detections of magnetic fields in a number of {beta} Cephei and slowly pulsating B (SPB) stars, their impact on stellar rotation, pulsations, and element diffusion has not yet been sufficiently studied. The reason for this is the lack of knowledge of rotation periods, the magnetic field strength distribution and temporal variability, and the field geometry. New longitudinal field measurements of four {beta} Cephei and candidate {beta} Cephei stars, and two SPB stars were acquired with FORS 2 at the Very Large Telescope. These measurements allowed us to carry out a search for rotation periods and tomore » constrain the magnetic field geometry for four stars in our sample.« less

Structural Determinants of DNA Binding by a P. falciparum ApiAP2 Transcriptional Regulator

DOE Office of Scientific and Technical Information (OSTI.GOV)

Lindner, Scott E.; De Silva, Erandi K.; Keck, James L.

2010-11-05

Putative transcription factors have only recently been identified in the Plasmodium spp., with the major family of regulators comprising the Apicomplexan Apetala2 (AP2) proteins. To better understand the DNA-binding mechanisms of these transcriptional regulators, we characterized the structure and in vitro function of an AP2 DNA-binding domain from a prototypical Apicomplexan AP2 protein, PF14{_}0633 from Plasmodium falciparum. The X-ray crystal structure of the PF14{_}0633 AP2 domain bound to DNA reveals a {beta}-sheet fold that binds the DNA major groove through base-specific and backbone contacts; a prominent {alpha}-helix supports the {beta}-sheet structure. Substitution of predicted DNA-binding residues with alanine weakened ormore » eliminated DNA binding in solution. In contrast to plant AP2 domains, the PF14{_}0633 AP2 domain dimerizes upon binding to DNA through a domain-swapping mechanism in which the {alpha}-helices of the AP2 domains pack against the {beta}-sheets of the dimer mates. DNA-induced dimerization of PF14{_}0633 may be important for tethering two distal DNA loci together in the nucleus and/or for inducing functional rearrangements of its domains to facilitate transcriptional regulation. Consistent with a multisite binding mode, at least two copies of the consensus sequence recognized by PF14{_}0633 are present upstream of a previously identified group of sporozoite-stage genes. Taken together, these findings illustrate how Plasmodium has adapted the AP2 DNA-binding domain for genome-wide transcriptional regulation.« less

Autonomous star sensor ASTRO APS: flight experience on Alphasat

NASA Astrophysics Data System (ADS)

Schmidt, U.; Fiksel, T.; Kwiatkowski, A.; Steinbach, I.; Pradarutti, B.; Michel, K.; Benzi, E.

2015-06-01

Jena-Optronik GmbH, located in Jena/Germany, has profound experience in designing and manufacturing star trackers since the early 80s. Today the company has a worldwide leading position in supplying geo-stationary and Earth observation satellites with robust and reliable star tracker systems. In the first decade of the new century Jena-Optronik received a development contract (17317/2003/F/WE) from the European Space Agency to establish the technologically challenging elements for which advanced star tracker technologies as CMOS Active Pixel Sensors were being introduced or were considered strategic. This activity was performed in the frame of the Alphabus large platform pre-development lead by ESA and the industrial Joint Project Team consisting of Astrium (now Airbus Defence and Space), Thales Alenia Space and CNES (Centre national d'études spatiales). The new autonomous star tracker, ASTRO APS (Active Pixel Sensor), extends the Jena-Optronik A stro-series CCD-based star tracker products taken the full benefit of the CMOS APS technology. ASTRO APS is a fully autonomous compact star tracker carrying either the space-qualified radiation hard STAR1000 or the HAS2 APS detectors. The star tracker is one of four Technology Demonstration Payloads (TDP6) carried by Alphasat as hosted payload in the frame of a successful Private Public Partnership between ESA and Inmarsat who owns and operates the satellite as part of its geo-stationary communication satellites fleet. TDP6 supports also directly TDP1, a Laser Communication Terminal, for fine pointing tasks. Alphasat was flawlessly brought in orbit at the end of July 2013 by a European Ariane 5 launcher. Only a few hours after launch the star tracker received its switch ON command and acquired nominally within 6 s the inertial 3-axes attitude. In the following days of the early in-orbit operations of Alphasat the TDP6 unit tracked reliably all the spacecraft maneuvers including the 0.1 and 0.2°/s spin stabilization for Sun pointing, all of the apogee engine thrusts, Moon field of view transits and recovered to stable tracking after several Earth and Sun blindings before the spacecraft entered a preliminary Earth pointing in a nominal geo-stationary attitude. The Jena-Optronik TDP6 operation center received daily the star tracker status and attitude data. The huge amount of acquired raw data has been evaluated to characterize the ASTRO APS (STAR1000) star tracker in-orbit performance. The paper will present in detail these data processing activities and will show the extraordinary good results. Due to the diverse transfer orbit satellite operations the key performance star tracker data like attitude random noise, single star noise, star brightness measurement, baffle Sun exclusion angle, temperature control, etc., could be derived and have been compared to the ground based laboratory and field measurements. The ultimate performance parameters achieved and verified as well as the lessons learned from the comparison to the ground test data are summarized in the conclusion of the paper.

Multiplicity among chemically peculiar stars. II. Cool magnetic Ap stars

NASA Astrophysics Data System (ADS)

Carrier, F.; North, P.; Udry, S.; Babel, J.

2002-10-01

We present new orbits for sixteen Ap spectroscopic binaries, four of which might in fact be Am stars, and give their orbital elements. Four of them are SB2 systems: HD 5550, HD 22128, HD 56495 and HD 98088. The twelve other stars are: HD 9996, HD 12288, HD 40711, HD 54908, HD 65339, HD 73709, HD 105680, HD 138426, HD 184471, HD 188854, HD 200405 and HD 216533. Rough estimates of the individual masses of the components of HD 65339 (53 Cam) are given, combining our radial velocities with the results of speckle interferometry and with Hipparcos parallaxes. Considering the mass functions of 74 spectroscopic binaries from this work and from the literature, we conclude that the distribution of the mass ratio is the same for cool Ap stars and for normal G dwarfs. Therefore, the only differences between binaries with normal stars and those hosting an Ap star lie in the period distribution: except for the case of HD 200405, all orbital periods are longer than (or equal to) 3 days. A consequence of this peculiar distribution is a deficit of null eccentricities. There is no indication that the secondary has a special nature, like e.g. a white dwarf. Based on observations collected at the Observatoire de Haute-Provence (CNRS), France. Tables 1 to 3 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/394/151 Appendix B is only available in electronic form at http://www.edpsciences.org

VizieR Online Data Catalog: Basic properties of Kepler and CoRoT targets (Yildiz+, 2016)

NASA Astrophysics Data System (ADS)

Yildiz, M.; Celik Orhan, Z.; Kayhan, C.

2018-01-01

The basic data of certain Kepler (79 stars) and CoRoT (seven stars) target stars, compiled from the literature, are listed in Table A1. Oscillation frequencies of three stars (Procyon A, HD 2151 and HD 146233) were obtained from ground-based observations (Bedding et al., 2010ApJ...713..935B; Bedding et al., 2007ApJ...663.1315B and Bazot et al. 2012, Cat. J/A+A/544/A106, respectively). These stars are also listed in this table, with data for the Sun for comparison. For most stars, we provide B-V and V-K colours (SIMBAD data base) from photometric observations, and surface gravity [log(g)], effective temperature (TeS) and metallicity ([Fe/H]) from spectroscopic observations. (2 data files).

The most interesting roAp target for MONS: HR1217 ?

NASA Astrophysics Data System (ADS)

Knudsen, M. R.

2000-04-01

The roAp star HR1217 is presented as a good and possibly the best roAp target for MONS and the progress of the 1998 3-site STACC Campaign is briefly summarized incl. the first detection of EW oscillation in Hα and Hβ in this star, alongside evidence of EW varying with the phase of rotation. HR1217 has 6 known oscillation frequencies of which the four strongest appear to be rotationally split with photometric amplitudes ~< 1 mmag. The problem with groundbased observations is the 3-day-alias beating with neighbouring peaks which limits our chances for a solid mode id. With 30 days (2.4ṡ Prot) on MONS CAM we should have the needed observational data for doing asteroseismology on a magnetic star at last!

A giant planet imaged in the disk of the young star beta Pictoris.

PubMed

Lagrange, A-M; Bonnefoy, M; Chauvin, G; Apai, D; Ehrenreich, D; Boccaletti, A; Gratadour, D; Rouan, D; Mouillet, D; Lacour, S; Kasper, M

2010-07-02

Here, we show that the approximately 10-million-year-old beta Pictoris system hosts a massive giant planet, beta Pictoris b, located 8 to 15 astronomical units from the star. This result confirms that gas giant planets form rapidly within disks and validates the use of disk structures as fingerprints of embedded planets. Among the few planets already imaged, beta Pictoris b is the closest to its parent star. Its short period could allow for recording of the full orbit within 17 years.

Possible Mg II emission in B stars observed from Copernicus

NASA Technical Reports Server (NTRS)

Kondo, Y.; Whaley, R. S.; Modisette, J. L.; Dufour, R. J.

1976-01-01

Four B stars, Alpha Vir, Beta Cen, Alpha Gru, and Beta Lib, were observed with the Copernicus spectrometer at a resolution of 0.1 A in order to investigate the presence of chromospheric emission. Emission was observed in Beta Cen and Alpha Gru, while the results for Alpha Vir and Beta Lib were inconclusive.

Velocity fields and spectrum peculiarities in Beta Cephei stars

NASA Technical Reports Server (NTRS)

Lesh, J. R.

1980-01-01

The acquisition of short wavelength spectra of Beta Cephei variable stars from the International Ultraviolet Explorer is reported. A total of 122 images of 10 variable stars and 3 comparison stars were obtained. All of the images were observed in the high dispersion mode through a small aperture. The development of image processing methods is also briefly discussed.

First photometric study of two southern eclipsing binaries IS Tel and DW Aps

NASA Astrophysics Data System (ADS)

Özer, S.; Sürgit, D.; Erdem, A.; Öztürk, O.

2017-02-01

The paper presents the first photometric analysis of two southern eclipsing binary stars, IS Tel and DW Aps. Their V light curves from the All Sky Automated Survey were modelled by using Wilson-Devinney method. The final models give these two Algol-like binary stars as having detached configurations. Absolute parameters of the components of the systems were also estimated.

The (BETA) Pictoris Phenomenon Among Herbig Ae/Be Stars

NASA Technical Reports Server (NTRS)

Grady, C. A.; Perez, M. R.; Talavera, A.; Bjorkman, K. S.; deWinter, D.; The, P.-S.; Molster, F. J.; vandenAncker, M. E.; Sitko, M. L.; Morrison, N. D.;

Possible Mg ii emission in B stars observed from Copernicus

DOE Office of Scientific and Technical Information (OSTI.GOV)

Kondo, Y.; Modisette, J.L.; Dufour, R.J.

1976-05-15

Four B stars, ..cap alpha.. Vir, ..beta.. Cen, ..cap alpha.. Gru, and ..beta.. Lib, were observed with the Copernicus Princeton Telescope Spectrometer at a resolution of 0.1 A in order to investigate the presence of chromospheric emission. Emission was observed in ..beta.. Cen and ..cap alpha.. Gru, while the results for ..cap alpha.. Vir and ..beta.. Lib were inconclusive. (AIP)

MALDI, AP/MALDI and ESI techniques for the MS detection of amyloid [beta]-peptides

NASA Astrophysics Data System (ADS)

Grasso, Giuseppe; Mineo, Placido; Rizzarelli, Enrico; Spoto, Giuseppe

2009-04-01

Amyloid [beta]-peptides (A[beta]s) are involved in several neuropathological conditions such as Alzheimer's disease and considerable experimental evidences have emerged indicating that different proteases play a major role in regulating the accumulation of A[beta]s in the brain. Particularly, insulin-degrading enzyme (IDE) has been shown to degrade A[beta]s at different cleavage sites, but the experimental results reported in the literature and obtained by mass spectrometry methods are somehow fragmentary. The detection of A[beta]s is often complicated by solubility issues, oxidation artifacts and spontaneous aggregation/cleavage and, in order to rationalize the different reported results, we analyzed A[beta]s solutions by three different MS approaches: matrix assisted laser desorption ionization-time of flight (MALDI-TOF), atmospheric pressure (AP) MALDI ion trap and electrospray ionization (ESI) ion trap. Differences in the obtained results are discussed and ESI is chosen as the most suitable MS method for A[beta]s detection. Finally, cleavage sites produced by interaction of A[beta]s with IDE are identified, two of which had never been reported in the literature.

Study of Pulsations in the Atmosphere of the roAp star HD 137949

NASA Astrophysics Data System (ADS)

Sachkov, M.; Hareter, M.; Ryabchikova, T.; Wade, G.; Kochukhov, O.; Weiss, W. W.

The roAp star HD 137949 (33 Lib) shows the most complex pulsational behaviour among all roAp stars. Mkrtichian et al. (2003) found nearly anti-phase pulsations of Nd II and Nd III lines, which they attribute to the presence of a pulsation node high in the atmosphere of HD 137949. This was confirmed by Kurtz at al. (2005), who also find that in some REE lines the main frequency, corresponding to 8.27 min, and its harmonic have almost equal RV amplitudes. Based on high accuracy observations Ryabchikova et al. (2007a) studied pulsational characteristics of the HD 137949 atmosphere in detail. In general, spectroscopy provides 3D resolution of modes and allows to search for the photometrically undetectable frequencies. The high-accuracy space photometry provides very high-precision measurements of detected pulsation frequencies and enables an accurate phasing of multi-site spectroscopic data. A combination of simultaneous spectroscopy and photometry represents the most sophisticated asteroseismic dataset for any roAp star. In 2009 the star HD 137949 became a target of an intense observing campaign that combined ground-based spectroscopy with space photometry, obtained with the MOST satellite. We collected 780 spectra using the ESPaDOnS spectrograph mounted on the 3.6 m CFHT telescope; 374 spectra were obtained with the FIES spectrograph mounted on the 2.56-m NOT to perform the time-resolved spectroscopy of HD 137949. In addition, we used 111 UVES spectra (2004) from the ESO archive to check the mode stability. The frequency analysis of the new radial velocity (RV) measurements confirmed the previously reported frequency pattern (two frequencies and the first harmonic of the main frequency), and revealed an additional frequency at 1.991 mHz. The new frequency solution fits perfectly the RV variations from the 2004 and 2009 observational sets providing a strong support for the p-mode stability in the roAp star HD 137949 for at least 5 years.

Autonomous star tracker based on active pixel sensors (APS)

NASA Astrophysics Data System (ADS)

Schmidt, U.

2017-11-01

Star trackers are opto-electronic sensors used onboard of satellites for the autonomous inertial attitude determination. During the last years, star trackers became more and more important in the field of the attitude and orbit control system (AOCS) sensors. High performance star trackers are based up today on charge coupled device (CCD) optical camera heads. The Jena-Optronik GmbH is active in the field of opto-electronic sensors like star trackers since the early 80-ties. Today, with the product family ASTRO5, ASTRO10 and ASTRO15, all marked segments like earth observation, scientific applications and geo-telecom are supplied to European and Overseas customers. A new generation of star trackers can be designed based on the APS detector technical features. The measurement performance of the current CCD based star trackers can be maintained, the star tracker functionality, reliability and robustness can be increased while the unit costs are saved.

Characterization of diadenosine tetraphosphate (Ap4A) binding sites in cultured chromaffin cells: evidence for a P2y site.

PubMed Central

Pintor, J.; Torres, M.; Castro, E.; Miras-Portugal, M. T.

1991-01-01

1. Diadenosine tetraphosphate (Ap4A) a dinucleotide, which is stored in secretory granules, presents two types of high affinity binding sites in chromaffin cells. A Kd value of 8 +/- 0.65 x 10(-11) M and Bmax value of 5420 +/- 450 sites per cell were obtained for the high affinity binding site. A Kd value of 5.6 +/- 0.53 x 10(-9) M and a Bmax value close to 70,000 sites per cell were obtained for the second binding site with high affinity. 2. The diadenosine polyphosphates, Ap3A, Ap4A, Ap5A and Ap6A, displaced [3H]-Ap4A from the two binding sites, the Ki values being 1.0 nM, 0.013 nM, 0.013 nM and 0.013 nM for the very high affinity binding site and 0.5 microM, 0.13 microM, 0.062 microM and 0.75 microM for the second binding site. 3. The ATP analogues displaced [3H]-Ap4A with the potency order of the P2y receptors, adenosine 5'-O-(2 thiodiphosphate) (ADP-beta-S) greater than 5'-adenylyl imidodiphosphate (AMP-PNP) greater than alpha, beta-methylene ATP (alpha, beta-MeATP), in both binding sites. The Ki values were respectively 0.075 nM, 0.2 nM and 0.75 nM for the very high affinity binding site and 0.125 microM, 0.5 microM and 0.9 microM for the second binding site. PMID:1912985

Young Debris Disks With Newly Discovered Emission Features

NASA Astrophysics Data System (ADS)

Ballering, N.

2014-04-01

We analyzed the Spitzer/IRS spectra of young A and F stars that host debris disks with previously unidentified silicate emission features. Such features probe small, warm dust grains in the inner regions of these young systems where terrestrial planet formation may be proceeding (Lisse et al. 2009). For most systems, these regions are too near their host star to be directly seen with high-contrast imaging and too warm to be imaged with submillimeter interferometers. Mid-infrared excess spectra - originating from the thermal emission of the debris disk dust - remain the best data to constrain the properties of the debris in these regions. For each target, we fit physically-motivated model spectra to the data. Typical spectra of unresolved debris disks are featureless and suffer severe degeneracies between the dust location and the grain properties; however, spectra with solid-state emission features provide significantly more information, allowing for a more accurate determination of the dust size, composition, and location (e.g. Chen et al. 2006; Olofsson et al. 2012). Our results shed light on the dynamic properties occurring in the terrestrial regions of these systems. For instance, the sizes of the smallest grains and the nature of the grain size distribution reveal whether the dust originates from steady-state collisional cascades or from stochastic collisions. The properties of the dust grains - such as their crystalline or amorphous structure - can inform us of grain processing mechanisms in the disk. The location of this debris illuminates where terrestrial planet forming activity is occurring. We used results from the Beta Pictoris - which has a well-resolved debris disk with emission features (Li et al. 2012) - to place our results in context. References: Chen et al. 2006, ApJS, 166, 351 Li et al. 2012, ApJ, 759, 81 Lisse et al. 2009, ApJ, 701, 2019 Olofsson et al. 2012, A&A, 542, A90

VizieR Online Data Catalog: Multiplicity among chemically peculiar stars II (Carrier+, 2002)

NASA Astrophysics Data System (ADS)

Carrier, F.; North, P.; Udry, S.; Babel, J.

2002-08-01

We present new orbits for sixteen Ap spectroscopic binaries, four of which might in fact be Am stars, and give their orbital elements. Four of them are SB2 systems: HD 5550, HD 22128, HD 56495 and HD 98088. The twelve other stars are : HD 9996, HD 12288, HD 40711, HD 54908, HD 65339, HD 73709, HD 105680, HD 138426, HD 184471, HD 188854, HD 200405 and HD 216533. Rough estimates of the individual masses of the components of HD 65339 (53 Cam) are given, combining our radial velocities with the results of speckle interferometry and with Hipparcos parallaxes. Considering the mass functions of 74 spectroscopic binaries from this work and from the literature, we conclude that the distribution of the mass ratio is the same for cool Ap stars as for normal G dwarfs. Therefore, the only differences between binaries with normal stars and those hosting an Ap star lie in the period distribution: except for the case of HD 200405, all orbital periods are longer than (or equal to) 3 days. A consequence of this peculiar distribution is a deficit of null eccentricities. There is no indication that the secondary has a special nature, like e.g. a white dwarf. (4 data files).

Some experiments related to L-star instability in rocket motors

NASA Technical Reports Server (NTRS)

Kumar, R. N.; Mcnamara, R. P.

1973-01-01

The influence of condensed phase heterogeneity on the L-star instability of nonmetallized AP/PBAN propellants is explored using four propellants (with monomodal AP particle distributions having 50 per cent weight average points at 11, 39.5, 175, and 350 microns). An economical firing program is used. One-dimensional nature of the Helmholtz mode and the complex nature of the chuff mode are revealed through color movies. The stability boundary on the L-star pressure plot is found to be parabolic. Frequency correlations and many other features reveal the important role of condensed phase details in propellant combustion.

V and K-band Mass-Luminosity Relations for M Dwarf Stars

NASA Astrophysics Data System (ADS)

Benedict, George Frederick; Henry, Todd J.; McArthur, Barbara E.; Franz, Otto; Wasserman, Larry H.; Dieterich, Sergio

2015-08-01

Applying Hubble Space Telescope Fine Guidance Sensor astrometric techniques developed to establish relative orbits for binary stars (Franz et al. 1998, AJ, 116, 1432), determine masses of binary components (Benedict et al. 2001, AJ, 121, 1607), and measure companion masses of exoplanet host stars (McArthur et al. 2010, ApJ, 715, 1203), we derive masses with an average 2% error for 28 components of 14 M dwarf binary star systems. With these and other published masses we update the lower Main Sequence V-band Mass-Luminosity Relation first shown in Henry et al. 1999, ApJ, 512, 864. We demonstrate that a Mass-Luminosity Relation in the K-band has far less scatter. These relations can be used to estimate the masses of the ubiquitous red dwarfs (75% of all stars) to an accuracy of better than 5%.

Reduction of low frequency error for SED36 and APS based HYDRA star trackers

NASA Astrophysics Data System (ADS)

Ouaknine, Julien; Blarre, Ludovic; Oddos-Marcel, Lionel; Montel, Johan; Julio, Jean-Marc

2017-11-01

In the frame of the CNES Pleiades satellite, a reduction of the star tracker low frequency error, which is the most penalizing error for the satellite attitude control, was performed. For that purpose, the SED36 star tracker was developed, with a design based on the flight qualified SED16/26. In this paper, the SED36 main features will be first presented. Then, the reduction process of the low frequency error will be developed, particularly the optimization of the optical distortion calibration. The result is an attitude low frequency error of 1.1" at 3 sigma along transverse axes. The implementation of these improvements to HYDRA, the new multi-head APS star tracker developed by SODERN, will finally be presented.

VizieR Online Data Catalog: Iron abundance of Terzan 5 stars (Massari+, 2014)

NASA Astrophysics Data System (ADS)

Massari, D.; Mucciarelli, A.; Ferraro, F. R.; Origlia, L.; Rich, R. M.; Lanzoni, B.; Dalessandro, E.; Valenti, E.; Ibata, R.; Lovisi, L.; Bellazzini, M.; Reitzel, D.

2017-05-01

This study is based on a sample of stars located within the tidal radius of Terzan 5 (rt~300''; Lanzoni et al. 2010ApJ...717..653L; Miocchi et al. 2013ApJ...774..151M) observed with two different instruments: FLAMES (Pasquini et al. 2002Msngr.110....1P) at the European Southern Observatory (ESO) VLT and DEIMOS (Faber et al. 2003SPIE.4841.1657F) at the Keck II Telescope. The spectroscopic targets have been selected from the optical photometric catalog of Terzan 5 described in Lanzoni et al. (2010ApJ...717..653L) along the brightest portion (I<17) of the red giant branch (RGB). In order to avoid contamination from other sources, we avoided stars with bright neighbors (Ineighbor

Silencing of Smed-betacatenin1 generates radial-like hypercephalized planarians.

PubMed

Iglesias, Marta; Gomez-Skarmeta, Jose Luis; Saló, Emili; Adell, Teresa

2008-04-01

Little is known about the molecular mechanisms responsible for axis establishment during non-embryonic processes such as regeneration and homeostasis. To address this issue, we set out to analyze the role of the canonical Wnt pathway in planarians, flatworms renowned for their extraordinary morphological plasticity. Canonical Wnt signalling is an evolutionarily conserved mechanism to confer polarity during embryonic development, specifying the anteroposterior (AP) axis in most bilaterians and the dorsoventral (DV) axis in early vertebrate embryos. beta-Catenin is a key element in this pathway, although it is a bifunctional protein that is also involved in cell-cell adhesion. Here, we report the characterization of two beta-catenin homologs from Schmidtea mediterranea (Smed-betacatenin1/2). Loss of function of Smed-betacatenin1, but not Smed-betacatenin2, in both regenerating and intact planarians, generates radial-like hypercephalized planarians in which the AP axis disappears but the DV axis remains unaffected, representing a unique example of a striking body symmetry transformation. The radial-like hypercephalized phenotype demonstrates the requirement for Smed-betacatenin1 in AP axis re-establishment and maintenance, and supports a conserved role for canonical Wnt signalling in AP axis specification, whereas the role of beta-catenin in DV axis establishment would be a vertebrate innovation. When considered alongside the protein domains present in each S. mediterranea beta-catenin and the results of functional assays in Xenopus embryos demonstrating nuclear accumulation and axis induction with Smed-betacatenin1, but not Smed-betacatenin2, these data suggest that S. mediterranea beta-catenins could be functionally specialized and that only Smed-betacatenin1 is involved in Wnt signalling.

Documentation for the machine-readable version of the catalogue of individual UBV and UVBY beta observations in the region of the Orion OB1 association

NASA Technical Reports Server (NTRS)

Warren, W. H., Jr.

1982-01-01

The machine-readable files of individual UBV observations of 106 stars in the vicinity of the Orion Nebula (the Sword region) and individual uvby beta observations of 508 stars in all regions of the Orion OB 1 association are described. For the UBV data the stars are identified by their Brun numbers, with cross identifications to the chart numbers used in Warren and Hesser; the uv by beta stars are identified by the aforementioned chart numbers and HD, BD or P ( = pi); numbers in that order of preference.

Pulsational mode-typing in line profile variables. I - Four Beta Cephei stars

NASA Technical Reports Server (NTRS)

Campos, A. J.; Smith, M. A.

1980-01-01

The detailed variations of line profiles in the Beta Cephei-type variable stars Gamma Pegasi, Beta Cephei, Delta Ceti and Sigma Scorpii are modeled throughout their pulsation cycles in order to classify the dominant pulsation mode as radial or nonradial. High-dispersion Reticon observations of the variables were obtained for the Si III line at 4567 A, and line profiles broadened by radial or nonradial pulsations, rotation and radial-tangential macroturbulence were calculated based on a model atmosphere. It is found that only a radial pulsation mode can reproduce the radial velocity amplitude, changes in line asymmetry and uniform line width observed in all four stars. Results are in agreement with the color-to-light arguments of Stamford and Watson (1978), and suggest that radial pulsation plays the dominant role in the observed variations in most Beta Cephei stars. Evidence for shocks or moving shells is also found in visual line data for Sigma Scorpii and an ultraviolet line of Beta Cephei, together with evidence of smooth, secular period changes in Beta Cephei and Delta Ceti.

Hiding in plain sight

NASA Astrophysics Data System (ADS)

Riedel, Adric Richard

2012-05-01

Since the first successful measurements of stellar trigonometric parallax in the 1830s, the study of nearby stars has focused on the highest proper motion stars (micro > 0.18″ yr-1). Those high proper motion stars have formed the backbone of the last 150 years of study of the Solar Neighborhood and the composition of the Galaxy. Statistically speaking, though, there is a population of stars that will have low proper motions when their space motions have been projected onto the sky. At the same time, over the last twenty years, populations of relatively young stars (less than ˜ 100 Myr), most of them with low proper motions, have been revealed near (< 100 pc) the Sun. This dissertation is the result of two related projects: A photometric search for nearby (< 25pc) southern-hemisphere M dwarf stars with low proper motions (micro < 0.18″ yr-1), and a search for nearby (< 100 pc) pre-main-sequence (< 125 Myr old) M dwarf systems. The projects rely on a variety of photometric, spectroscopic, and astrometric analyses (including parallaxes from our program) using data from telescopes at CTIO via the SMARTS Consortium and at Lowell Observatory. Within this dissertation, I describe the identification and confirmation of 23 new nearby low proper motion M dwarf systems within 25 pc, 8 of which are within 15 pc (50% of the anticipated low-proper-motion 15 pc sample). I also report photometric, spectroscopic, and astrometric parameters and identifications for a selection of 25 known and new candidate nearby young M dwarfs, including new low-mass members of the TW Hydra, beta Pictoris, Tucana-Horologium, Argus, and AB Doradus associations, following the methods of my Riedel et al. (2011) paper and its discovery of AP Col, the closest pre-main-sequence star to the Solar System. These low proper motion and nearby star discoveries are put into the context of the Solar Neighborhood as a whole by means of the new RECONS 25 pc Database, to which I have now added (including my Riedel et al. (2010) paper) 81 star systems (4% of the total). INDEX WORDS: Astronomy, Astrometry, Photometry, Spectroscopy, Kinematics, Proper motion, Parallax, Nearby stars, Low-mass stars, Young stars, Pre-main-sequence stars.

In vitro binding of the asialoglycoprotein receptor to the beta adaptin of plasma membrane coated vesicles.

PubMed Central

Beltzer, J P; Spiess, M

1991-01-01

The asialoglycoprotein (ASGP) receptor was used to probe total clathrin-coated vesicle proteins and purified adaptor proteins (APs) which had been fractionated by gel electrophoresis and transferred to nitrocellulose. The receptor was found to interact with proteins of approximately 100 kDa. The cytoplasmic domain of the ASGP receptor subunit H1 fused to dihydrofolate reductase competed for receptor binding to the 100 kDa polypeptide in the plasma membrane-type AP complexes (AP-2). A fusion protein containing the cytoplasmic domain of the endocytic mutant haemagglutinin HA-Y543 also competed, but a protein with the wild-type haemagglutinin sequence did not. This indicates that the observed interaction is specific for the cytoplasmic domain of the receptor and involves the tyrosine signal for endocytosis. When fractionated by gel electrophoresis in the presence of urea, the ASGP receptor binding polypeptide displayed a characteristic shift in electrophoretic mobility identifying it as the beta adaptin. Partial proteolysis of the AP-2 preparation followed by the receptor binding assay revealed that the aminoterminal domain of the beta adaptin contains the binding site for receptors. Images PMID:1935897

A fossil origin for the magnetic field in A stars and white dwarfs.

PubMed

Braithwaite, Jonathan; Spruit, Hendrik C

2004-10-14

Some main-sequence stars of spectral type A are observed to have a strong (0.03-3 tesla), static, large-scale magnetic field, of a chiefly dipolar shape: they are known as 'Ap stars', such as Alioth, the fifth star in the Big Dipper. Following the discovery of these fields, it was proposed that they are remnants of the star's formation, a 'fossil' field. An alternative suggestion is that they could be generated by a dynamo process in the star's convective core. The dynamo hypothesis, however, has difficulty explaining high field strengths and the observed lack of a correlation with rotation. The weakness of the fossil-field theory has been the absence of field configurations stable enough to survive in a star over its lifetime. Here we report numerical simulations that show that stable magnetic field configurations, with properties agreeing with those observed, can develop through evolution from arbitrary, unstable initial fields. The results are applicable equally to Ap stars, magnetic white dwarfs and some highly magnetized neutron stars known as magnetars. This establishes fossil fields as the natural, unifying explanation for the magnetism of all these stars.

Am stars and the influence of binarity on infall

NASA Astrophysics Data System (ADS)

Cowley, Charles R.

2016-01-01

We explore an old idea for the origin of Am star anomalies, possibly related to observations of pollution in white dwarfs (Jura & Young, ARAA, 42, 45, 2014; Gansicke, et al., Arxiv:1505.03142). It must be noted that infall of an earthlike body can explain some, but not all of the abundance anomalies of Am stars.The ingestion of earthlike material by an a star should have observable effects that are larger than for solar-type stars. We follow dynamical arguments discussed, e.g. by Debes, et al. ApJ., 747, 148, 2012), and postulate that gravitational interactions will produce an infalling stream of low angularmomentum bodies.Note that most if not all Am stars are binary. Here we investigate only whether there is an increased frequency of collisions with a close binary relative to a single star.We make quantitative estimates, using analytical 2-body solutions and restricted 3-body calculations with parameters similar to those of the eclipsing Am pair Beta Aur,or WW Aur. We use initial values for the binary similar to those which would lead to a certain collision on a (4M_sun) single star for a parabolic trajectory. All calculations begin with a distance from the center of mass along the axis of a paraboloid of revolution at 3 or 5 AU and such that a marginal collision occurs with a single star. The perpendicular area of this figure is a cross section for a collision. We sample trajectories starting within and near this cross section, for double starsystems. Based on many trials we find it about equally likely-- relative to a single star--that an incoming body will be ejected from the system than that it will collide with one of the stars. Although we have sampled only a fraction of possible parameter space, we find no basis to expect that the binarity of the Am systems makes them more likely to have ingested planetary material.Infall should probably still be considered, along with the generally accepted diffusion scenario, but it does not appear that the binarity of Am stars makes infall significantly more relevant.

The lathyrus toxin, {beta}-N-oxalyl-L-{alpha},{beta}-diaminopropionic acid (ODAP), and homocysteic acid sensitize CA1 pyramidal neurons to cystine and L-2-amino-6-phosphonohexanoic acid

DOE Office of Scientific and Technical Information (OSTI.GOV)

Chase, L.A.; Peterson, N.L.; Koerner, J.F.

2007-02-15

A brief exposure of hippocampal slices to L-quisqualic acid (QUIS) sensitizes CA1 pyramidal neurons 30- to 250-fold to depolarization by certain excitatory amino acids analogues, e.g., L-2-amino-6-phosphonohexanoic acid (L-AP6), and by the endogenous compound, L-cystine. This phenomenon has been termed QUIS sensitization. A mechanism similar to that previously described for QUIS neurotoxicity has been proposed to describe QUIS sensitization. Specifically, QUIS has been shown to be sequestered into GABAergic interneurons by the System x{sub c} {sup -} and subsequently released by heteroexchange with cystine or L-AP6, resulting in activation of non-NMDA receptors. We now report two additional neurotoxins, the Lathyrusmore » excitotoxin, {beta}-N-oxalyl-L-{alpha},{beta}-diaminopropionic acid (ODAP), and the endogenous compound, L-homocysteic acid (HCA), sensitize CA1 hippocampal neurons > 50-fold to L-AP6 and > 10-fold to cystine in a manner similar to QUIS. While the cystine- or L-AP6-mediated depolarization can be inhibited by the non-NMDA receptor antagonist CNQX in ODAP- or QUIS-sensitized slices, the NMDA antagonist D-AP5 inhibits depolarization by cystine or L-AP6 in HCA-sensitized slices. Thus, HCA is the first identified NMDA agonist that induces phosphonate or cystine sensitization. Like QUIS sensitization, the sensitization evoked by either ODAP or HCA can be reversed by a subsequent exposure to 2 mM {alpha}-aminoadipic acid. Finally, we have demonstrated that there is a correlation between the potency of inducers for triggering phosphonate or cystine sensitivity and their affinities for System x{sub c} {sup -} and either the non-NMDA or NMDA receptor. Thus, the results of this study support our previous model of QUIS sensitization and have important implications for the mechanisms of neurotoxicity, neurolathyrism and hyperhomocystinemia.« less

Beta Decay and the Origins of Biological Chirality

NASA Astrophysics Data System (ADS)

van House, James Christopher

1984-06-01

The amino acids and sugars on which terrestrial life is based show maximal optical activity, that is, with rare exceptions, they are composed of D sugars in RNA and DNA and L-amino acids in proteins. Recent quantitative theoretical calculations suggest that the origin of this asymmetry can be causally explained by asymmetric radiolysis of initially racemic mixtures of D and L molecules by the longitudinally polarized electrons emitted in parity violating nuclear (beta) decay. These same theories predict an asymmetry in the rate of orthopositronium formation, Ap(,s), when low energy positron beams with a net helicity form positronium in optically active molecules, and quantitatively connect Ap(,s) to asymmetric radiolysis. This thesis presents the results of a measurement of Ap(,s) in several D, L, and DL amino acids using a polarized low energy positron beam. Limits of Ap(,s) < 3 x 10(' -4) were set on the amino acids leucine, selenocystine, and thyroxine, sufficient to exclude part of the predicted range of Ap(,s) in the last two molecules. These experimental limits improve previous limits on asymmetric radiolysis by a factor of 10('6). A quantitative discussion of the connection between the above limits and the origin of optical activity in living organisms is presented. Details of the development of the high intensity, highly polarized slow positron beam used in these measurements and of the first use of remoderation to form a slow positron beam and provide a timing signal for the beam are presented in the Appendices.

DACH1 inhibits transforming growth factor-beta signaling through binding Smad4.

PubMed

Wu, Kongming; Yang, Ying; Wang, Chenguang; Davoli, Maria A; D'Amico, Mark; Li, Anping; Cveklova, Kveta; Kozmik, Zbynek; Lisanti, Michael P; Russell, Robert G; Cvekl, Ales; Pestell, Richard G

2003-12-19

The vertebrate homologues of Drosophila dachsund, DACH1 and DACH2, have been implicated as important regulatory genes in development. DACH1 plays a role in retinal and pituitary precursor cell proliferation and DACH2 plays a specific role in myogenesis. DACH proteins contain a domain (DS domain) that is conserved with the proto-oncogenes Ski and Sno. Since the Ski/Sno proto-oncogenes repress AP-1 and SMAD signaling, we hypothesized that DACH1 might play a similar cellular function. Herein, DACH1 was found to be expressed in breast cancer cell lines and to inhibit transforming growth factor-beta (TGF-beta)-induced apoptosis. DACH1 repressed TGF-beta induction of AP-1 and Smad signaling in gene reporter assays and repressed endogenous TGF-beta-responsive genes by microarray analyses. DACH1 bound to endogenous NCoR and Smad4 in cultured cells and DACH1 co-localized with NCoR in nuclear dotlike structures. NCoR enhanced DACH1 repression, and the repression of TGF-beta-induced AP-1 or Smad signaling by DACH1 required the DACH1 DS domain. The DS domain of DACH was sufficient for NCoR binding at a Smad4-binding site. Smad4 was required for DACH1 repression of Smad signaling. In Smad4 null HTB-134 cells, DACH1 inhibited the activation of SBE-4 reporter activity induced by Smad2 or Smad3 only in the presence of Smad4. DACH1 participates in the negative regulation of TGF-beta signaling by interacting with NCoR and Smad4.

Analysis of class II (hydrolytic) and class I (beta-lyase) apurinic/apyrimidinic endonucleases with a synthetic DNA substrate.

PubMed Central

Levin, J D; Demple, B

1990-01-01

We have developed simple and sensitive assays that distinguish the main classes of apurinic/apyrimidinic (AP) endonucleases: Class I enzymes that cleave on the 3' side of AP sites by beta-elimination, and Class II enzymes that cleave by hydrolysis on the 5' side. The distinction of the two types depends on the use of a synthetic DNA polymer that contains AP sites with 5'-[32P]phosphate residues. Using this approach, we now show directly that Escherichia coli endonuclease IV and human AP endonuclease are Class II enzymes, as inferred previously on the basis of indirect assays. The assay method does not exhibit significant interference by nonspecific nucleases or primary amines, which allows the ready determination of different AP endonuclease activities in crude cell extracts. In this way, we show that virtually all of the Class II AP endonuclease activity in E. coli can be accounted for by two enzymes: exonuclease III and endonuclease IV. In the yeast Saccharomyces cerevisiae, the Class II AP endonuclease activity is totally dependent on a single enzyme, the Apn1 protein, but there are probably multiple Class I enzymes. The versatility and ease of our approach should be useful for characterizing this important class of DNA repair enzymes in diverse systems. PMID:1698278

Functional characterization of the beta-adrenergic receptor subtypes expressed by CA1 pyramidal cells in the rat hippocampus.

PubMed

Hillman, Kristin L; Doze, Van A; Porter, James E

2005-08-01

Recent studies have demonstrated that activation of the beta-adrenergic receptor (AR) using the selective beta-AR agonist isoproterenol (ISO) facilitates pyramidal cell long-term potentiation in the cornu ammonis 1 (CA1) region of the rat hippocampus. We have previously analyzed beta-AR genomic expression patterns of 17 CA1 pyramidal cells using single cell reverse transcription-polymerase chain reaction, demonstrating that all samples expressed the beta2-AR transcript, with four of the 17 cells additionally expressing mRNA for the beta1-AR subtype. However, it has not been determined which beta-AR subtypes are functionally expressed in CA1 for these same pyramidal neurons. Using cell-attached recordings, we tested the ability of ISO to increase pyramidal cell action potential (AP) frequency in the presence of subtype-selective beta-AR antagonists. ICI-118,551 [(+/-)-1-[2,3-(dihydro-7-methyl-1H-inden-4-yl)oxy]-3-[(1-methylethyl)amino]-2-butanol] and butoxamine [alpha-[1-(t-butylamino)ethyl]-2,5-dimethoxybenzyl alcohol) hydrochloride], agents that selectively block the beta2-AR, produced significant parallel rightward shifts in the concentration-response curves for ISO. From these curves, apparent equilibrium dissociation constant (K(b)) values of 0.3 nM for ICI-118,551 and 355 nM for butoxamine were calculated using Schild regression analysis. Conversely, effective concentrations of the selective beta1-AR antagonists CGP 20712A [(+/-)-2-hydroxy-5-[2-([2-hydroxy-3-(4-[1-methyl-4-(trifluoromethyl)-1H-imidazol-2-yl]phenoxy)propyl]amino)ethoxy]-benzamide methanesulfonate] and atenolol [4-[2'-hydroxy-3'-(isopropyl-amino)propoxy]phenylacetamide] did not significantly affect the pyramidal cell response to ISO. However, at higher concentrations, atenolol significantly decreased the potency for ISO-mediated AP frequencies. From these curves, an apparent atenolol K(b) value of 3162 nM was calculated. This pharmacological profile for subtype-selective beta-AR antagonists indicates that beta2-AR activation is mediating the increased AP frequency. Knowledge of functional AR expression in CA1 pyramidal neurons will aid future long-term potentiation studies by allowing selective manipulation of specific beta-AR subtypes.

VizieR Online Data Catalog: Candidate X-ray OB stars in MYStIX regions (Povich+, 2017)

NASA Astrophysics Data System (ADS)

Povich, M. S.; Busk, H. A.; Feigelson, E. D.; Townsley, L. K.; Kuhn, M. A.

2017-10-01

X-ray point source catalogs for the 18 Massive Young Star-forming Complex Study in Infrared and X-Rays (MYStIX) regions studied here were produced by Kuhn+ (2010, J/ApJ/725/2485 and 2013, J/ApJS/209/27) and Townsley (2014+, J/ApJS/213/1) from archival Chandra Advanced CCD Imaging Camera (ACIS) observations. MYStIX JHKs NIR photometry was obtained from images taken with the United Kingdom Infrared Telescope (UKIRT) Wide-field Camera or from the Two-Micron All-Sky Survey (2MASS). See section 2 for further details. Spitzer MIR photometry at 3.6, 4.5, 5.8, and 8.0um was provided either by the Galactic Legacy Mid-Plane Survey Extraordinaire (GLIMPSE; Benjamin+ 2003PASP..115..953B) or by Kuhn+ (2013, J/ApJS/209/29). (4 data files).

VLA observations of dwarf M flare stars and magnetic stars

NASA Technical Reports Server (NTRS)

Willson, R. F.; Lang, K. R.; Foster, P.

1988-01-01

The VLA has been used to search for 6 cm emission from 16 nearby dwarf M stars, leading to the detection of only one of them - Gliese 735. The dwarf M flare stars AD Leonis and YZ Canis Minoris were also monitored at 6 cm and 20 cm wavelength in order to study variability. Successive oppositely circularly polarized bursts were detected from AD Leo at 6 cm, suggesting the presence of magnetic fields of both magnetic polarities. An impulsive 20-cm burst from YZ CMi preceded slowly varying 6-cm emission. The VLA was also used, unsuccessfully, to search for 6-cm emission from 13 magnetic Ap stars, all of which exhibit kG magnetic fields. Although the Ap magnetic stars have strong dipolar magnetic fields, the failure to detect gyroresonant radiation suggests that these stars do not have hot, dense coronae. The quiescent microwave emission from GL 735 is probably due to nonthermal radiation, since unusually high (H = 50 kG or greater) surface magnetic fields are inferred under the assumption that the 6-cm radiation is the gyroresonant radiation of thermal electrons.

Relation between the Li spots, dipolar magnetic field and other variable phenomena in the roAp star HD 83368

NASA Astrophysics Data System (ADS)

Polosukhina, N.

The detection of remarkable variations in the profile of the resonance doublet Li I 6708 Å with rotational phase of the roAp star HD 83368 (North et al. 1998) prompted us to consider the behaviour of other characteristics of this star. The observational data on magnetic field (Heff), brightness and amplitude of rapid light oscillations of HD 83368 are analyzed. A clear synchronism appears between the variations of the Li line intensity, brightness, magnetic field and pulsation amplitude with rotational phase, which can be explained in terms of a spotted rotator model. Reference: North P., Polosukhina N., Malanushenko V., Hack M., 1998, A&A 333, 644

VizieR Online Data Catalog: Spatial structure of young stellar clusters. I. (Kuhn+, 2014)

NASA Astrophysics Data System (ADS)

Kuhn, M. A.; Feigelson, E. D.; Getman, K. V.; Baddeley, A. J.; Broos, P. S.; Sills, A.; Bate, M. R.; Povich, M. S.; Luhman, K. L.; Busk, H. A.; Naylor, T.; King, R. R.

2015-07-01

The regions included in this study, listed in Table 1, are nearby sites of high-mass star formation that are included in the MYStIX sample (Feigelson et al. 2013ApJS..209...26F). These regions are covered in the near-IR by the UKIRT Infrared Deep Sky Survey (King et al. 2013, J/ApJS/209/28) or Two-Micron All Sky Survey (Skrutskie et al. 2006, VII/233), in the mid-IR by Spitzer IRAC observations (Kuhn et al. 2013, J/ApJS/209/29), and in the X-ray by the ACIS-I array on the Chandra X-Ray Observatory in the 0.5-8.0keV band (Kuhn et al. 2013, J/ApJS/209/27; Townsley et al. 2014, J/ApJS/213/1). Other sources to produce multiwavelength catalogs are described in section 2. The multiwavelength point-source catalogs are combined with a list of spectroscopic OB stars from the literature, and sources are classified probabilistically to obtain a list of MYStIX Probable Complex Members (MPCMs) (Broos et al. 2013, J/ApJS/209/32). (3 data files).

Role of astrocytes in reproduction and neuroprotection.

PubMed

Mahesh, Virendra B; Dhandapani, Krishnan M; Brann, Darrell W

2006-02-26

Hypothalamic astrocytes secrete TGF-beta and 3 alpha,5 alpha-tetrahydro progesterone (3 alpha,5 alpha-THP) in culture. When the astrocyte-conditioned medium (ACM) was incubated with the hypothalamic cell line GT1-7, it resulted in the secretion of GnRH. Immunoneutralization with TGF-beta antibody or ultra-filteration with a 10 kDa cut off filter resulted in attenuation of the GnRH releasing ability of ACM, indicating that TGF-beta was a major factor involved with GnRH release. Treatment with estrogens increases TGF-beta secretion. These observations indicate a significant role of astrocytes in GnRH secretion. Serum-deprivation results in the death of GT1-7 neurons in culture and addition of ACM or TGF-beta to the culture, attenuates cell death. The mechanism of protection from cell death appears to involve phosphorylation of MKK4, JNK, c-Jun(Ser63), and enhancement of AP-1 binding. Co-administration of JNK inhibitors, but not MEK inhibitors attenuated ACM or TGF-beta-induced c-Jun(Ser63) phosphorylation and their neuroprotective effects. These studies suggest that astrocytes can protect neurons, at least in part, by the release of TGF-beta and activation of a c-Jun/AP-1 protective pathway.

A proposed STAR microvertex detector using Active Pixel Sensors with some relevant studies on APS performance

NASA Astrophysics Data System (ADS)

Kleinfelder, S.; Li, S.; Bieser, F.; Gareus, R.; Greiner, L.; King, J.; Levesque, J.; Matis, H. S.; Oldenburg, M.; Ritter, H. G.; Retiere, F.; Rose, A.; Schweda, K.; Shabetai, A.; Sichtermann, E.; Thomas, J. H.; Wieman, H. H.; Bichsel, H.

2006-09-01

A vertex detector that can measure particles with charm or bottom quarks would dramatically expand the physics capability of the STAR detector at RHIC. To accomplish this, we are proposing to build the Heavy Flavor Tracker (HFT) using 2×2 cm Active Pixels Sensors (APS). Ten of these APS chips will be arranged on a ladder (0.28% of a radiation length) at radii of 1.5 and at 5.0 cm. We have examined several properties of APS chips, so that we can characterize the performance of this detector. Using 1.5 GeV/ c electrons, we have measured the charge collected and compared it to the expected charge. To achieve high efficiency, we have considered two different cluster finding algorithms and found that the choice of algorithm is dependent on noise level. We have demonstrated that a Scanning Electron Microscope can probe properties of an APS chip. In particular, we studied several position resolution algorithms. Finally, we studied the properties of pixel pitches from 5 to 30 μm.

THE SOLAR NEIGHBORHOOD. XXVI. AP Col: THE CLOSEST (8.4 pc) PRE-MAIN-SEQUENCE STAR

DOE Office of Scientific and Technical Information (OSTI.GOV)

Riedel, Adric R.; Henry, Todd J.; Jao, Wei-Chun

2011-10-15

We present the results of a multi-technique investigation of the M4.5Ve flare star AP Col, which we discover to be the nearest pre-main-sequence star. These include astrometric data from the CTIO 0.9 m, from which we derive a proper motion of 342.0 {+-} 0.5 mas yr{sup -1}, a trigonometric parallax of 119.21 {+-} 0.98 mas (8.39 {+-} 0.07 pc), and photometry and photometric variability at optical wavelengths. We also provide spectroscopic data, including radial velocity (22.4 {+-} 0.3 km s{sup -1}), lithium equivalent width (EW) (0.28 {+-} 0.02 A), H{alpha} EW (-6.0 to -35 A), vsin i (11 {+-} 1more » km s{sup -1}), and gravity indicators from the Siding Spring 2.3 m WiFeS, Lick 3 m Hamilton echelle, and Keck-I HIRES echelle spectrographs. The combined observations demonstrate that AP Col is the closer of only two known systems within 10 pc of the Sun younger than 100 Myr. Given its space motion and apparent age of 12-50 Myr, AP Col is likely a member of the recently proposed {approx}40 Myr old Argus/IC 2391 Association.« less

Effects of environmental estrogenic chemicals on AP1 mediated transcription with estrogen receptors alpha and beta.

PubMed

Fujimoto, Nariaki; Honda, Hiroaki; Kitamura, Shigeyuki

2004-01-01

There has been much discussion concerning endocrine disrupting chemicals suspected of exerting adverse effects in both wildlife and humans. Since the majority of these compounds are estrogenic, a large number of in vitro tests for estrogenic characteristics have been developed for screening purpose. One reliable and widely used method is the reporter gene assay employing estrogen receptors (ERs) and a reporter gene with a cis-acting estrogen responsive element (ERE). Other elements such as AP1 also mediate estrogenic signals and the manner of response could be quite different from that of ERE. Since this has yet to be explored, the ER mediated AP1 activity in response to a series of environmental estrogens was investigated in comparison with ERE findings. All the compounds exhibited estrogenic properties with ERE-luc and their AP1 responses were quite similar. These was one exception, however, p,p'-DDT (1,1,1,-trichloro-2,2-bis(p-chlorophenyl)ethane) did not exert any AP1-luc activity, while it appeared to be estrogenic at 10(-7) to 10(-5)M with the ERE action. None of the compounds demonstrated ER beta:AP1 activity. These data suggest that significant differences can occur in responses through the two estrogen pathways depending on environmental chemicals.

Magnetic Doppler imaging of Ap stars

NASA Astrophysics Data System (ADS)

Silvester, J.; Wade, G. A.; Kochukhov, O.; Landstreet, J. D.; Bagnulo, S.

2008-04-01

Historically, the magnetic field geometries of the chemically peculiar Ap stars were modelled in the context of a simple dipole field. However, with the acquisition of increasingly sophisticated diagnostic data, it has become clear that the large-scale field topologies exhibit important departures from this simple model. Recently, new high-resolution circular and linear polarisation spectroscopy has even hinted at the presence of strong, small-scale field structures, which were completely unexpected based on earlier modelling. This project investigates the detailed structure of these strong fossil magnetic fields, in particular the large-scale field geometry, as well as small scale magnetic structures, by mapping the magnetic and chemical surface structure of a selected sample of Ap stars. These maps will be used to investigate the relationship between the local field vector and local surface chemistry, looking for the influence the field may have on the various chemical transport mechanisms (i.e., diffusion, convection and mass loss). This will lead to better constraints on the origin and evolution, as well as refining the magnetic field model for Ap stars. Mapping will be performed using high resolution and signal-to-noise ratio time-series of spectra in both circular and linear polarisation obtained using the new-generation ESPaDOnS (CFHT, Mauna Kea, Hawaii) and NARVAL spectropolarimeters (Pic du Midi Observatory). With these data we will perform tomographic inversion of Doppler-broadened Stokes IQUV Zeeman profiles of a large variety of spectral lines using the INVERS10 magnetic Doppler imaging code, simultaneously recovering the detailed surface maps of the vector magnetic field and chemical abundances.

The magnetic fields of Ap stars from high resolution Stokes IQUV spectropolarimetry

NASA Astrophysics Data System (ADS)

Silvester, James

In this thesis we describe the acquisition of high resolution time resolved spectropolarimetric observations of 7 (bright and well understood) Ap stars in Stokes IQUV using the ESPaDOnS and Narval spectropolarimeters at the Canada-France-Hawaii Telescope and the 2m Telescope Bernard Lyot at Pic du Midi Observatory. We compare these observations with those obtained a decade earlier using the MuSiCoS spectropolarimeter to confirm consistency with the older data and provide evidence that both ESPaDOnS and Narval perform as expected in all Stokes parameters. We demonstrate that our refined longitudinal magnetic field and linear polarisation measurements for these 7 stars are of much greater quality than was previously obtained with MuSiCoS and that the global magnetic properties of these stars are stable over a long timescale. The ultimate aim of these new data is to provide a basis from which mapping of both the magnetic field and abundance structures can be performed on our target stars. We then describe magnetic field mapping of the Ap star alpha 2 CVn using these data. This mapping is achieved with the use of tomographic inversion of Doppler-broadened Stokes IQUV profiles of a large variety of spectral lines using the INVERS10 Magnetic Doppler imaging code. We show that not only are the new magnetic field maps of alpha 2 CVn consistent with a previous generation of maps of alpha 2 CVn, but that the same magnetic field topology can be derived from a variety of atomic line sets. This indicates that the magnetic field we derive for alpha2 CVn is a realistic representation of the star's true magnetic topology. Finally we investigate surface abundance structures for alpha 2 CVn for various chemical elements. We investigate the correlation between the location of these abundance features and the magnetic field of alpha 2 CVn. We will demonstrate that whilst the magnetic field plays a role in the formation of abundance structures, the current theoretical framework does not fully explain what we find from our maps. Ultimately this work motivates future mapping of Ap stars by confirming the reliability of both the instrument and associated data and the mapping technique itself.

Exocomet Signatures Around the A-shell Star Phi Leonis

NASA Technical Reports Server (NTRS)

Eiroa, C.; Rebollido, I.; Montesinos, B.; Villaver, E.; Absil, O.; Henning, Th.; Bayo, A.; Canovas, H.; Carmona, A.; Chen, Ch.;

UBV and H. beta. photometry of faint early-type stars in Crux and Centaurus

DOE Office of Scientific and Technical Information (OSTI.GOV)

Muzzio, J.C.; Feinstein, A.; Orsatti, A.M.

1976-08-01

UBV and H..beta.. photoelectric observations of faint early-type stars in a small region in Crux near the open cluster Hogg 15 and another in Centaurus are presented. The data suggest large absorption in Crux and small absorption in Centaurus. The spread in the distance moduli of the observed stars seems to be in agreement with the view that a spiral arm is seen tangentially near l = 305/sup 0/.

DISK AROUND STAR MAY BE WARPED BY UNSEEN PLANET

NASA Technical Reports Server (NTRS)

2002-01-01

NASA's Hubble Space Telescope has provided strong evidence for the existence of a roughly Jupiter-sized planet orbiting the star Beta Pictoris. Detailed Hubble images of the inner region of the 200-billion mile diameter dust disk encircling the star reveal an unexpected warp. Researchers say the warp can be best explained as caused by the gravitational pull of an unseen planet. The suspected planet would dwell within a five-billion mile wide clear zone in the center of the disk. This zone has long been suspected of harboring planets that swept it clear of debris, but the Hubble discovery provides more definitive evidence that a planet is there. (Alternative theories suggest the clear zone is empty because it is too warm for ice particles to exist.) 'We were surprised to find that the innermost region of the disk is orbiting in a different plane from the rest of the disk,' says Chris Burrows (Space Telescope Science Institute, Baltimore, Maryland, and the European Space Agency) who is presenting his results at the meeting of the American Astronomical Society in San Antonio, Texas. As he analyzed Hubble images, taken in January 1995 with the Wide Field Planetary Camera 2, Burrows discovered an unusual bulge in the nearly edge-on disk, which was mirrored on the other side of the star. 'Such a warp cannot last for very long,' says Burrows. 'This means that something is still twisting the disk and keeping out of a basic flat shape.' 'The presence of the warp is strong though indirect evidence for the existence of planets in this system. If Beta Pictoris had a solar system like ours, it would produce a warp like the one we see.' Burrows concludes, 'The Beta Pictoris system seems to contain at least one planet not too dissimilar from Jupiter in size and orbit. Rocky planets like Earth might circle Beta Pictoris as well. However, there is no evidence for these yet. Any planet will be at least a billion- times fainter than the star, and presently impossible to view directly, even with Hubble.' An alterative explanation of the warp is that the disk could have been perturbed by a passing star However this is very unlikely because only the inner region of the disk is affected. Burrows estimates that there is a one in 400,000 chance for Beta Pictoris to have such a close encounter with another star. 'Though Beta Pictoris is probably at least 100 million years old, other explanations for the warp do not allow it to last for very long.' The size of the warp allows Burrows to roughly measure the mass of the orbiting body. 'It must lie well within the warp, probably within the clear zone that exists around Beta Pictoris.' On the other hand, he points out, it cannot be too close to the star because its gravitational pull would cause the star to 'jiggle,' and such radial velocity variations have never been seen in Beta Pictoris. Burrows estimates the planet is from one-twentieth to twenty times the mass of Jupiter. The planet must lie within the range of distances typical of planetary distances within our solar system -- from about Earth's distance from the Sun to about Pluto's distance from the Sun (Pluto is roughly 30 times father from the Sun than Earth.) If the suspected planet were as far from Beta Pictoris as Jupiter is from our Sun, it also would have about the same mass as Jupiter. The planet's orbit must be inclined by about three degrees to the plane of the Beta Pictoris disk, and this is typical of the inclinations of the orbits of the planets in our solar system. The star is located 50 light-years away in the southern constellation Pictor (Painter's Easel). Though its precise age is not known, Beta Pictoris is generally considered a mature, main sequence star, slightly hotter than our Sun. Detections of substellar objects orbiting nearby stars have recently been reported for two other normal (i.e., main sequence) stars -- Gliese 229 and 51 Pegasus. However, Beta Pictoris is the only candidate that looks like it might possess a planetary system similar to our own. Beta Pictoris also is the only known star with a circumstellar disk of gas and dust that can be optically imaged. Despite the presence of dust around approximately one-third of the brightest nearby stars -- as deduced from NASA's Infrared Astronomy Satellite (IRAS) data -- ground-based telescope imaging has not detected other disks. Several Hubble programs are currently in progress to search for these disks. The NICMOS (Near Infrared Camera and Multi-Object Spectrometer), to be installed on Hubble during the February 1997 servicing mission, will provide a near-infrared capability needed for this type of search. * * * * * The Space Telescope Science Institute is operated by the Association of Universities for Research in Astronomy, Inc. (AURA), for NASA, under contract with the Goddard Space Flight Center, Greenbelt, MD. The Hubble Space Telescope is a project of international cooperation between NASA and the European Space Agency (ESA).

Investigation of the shell stars omicron and theta Per, and of the eclipsing binary beta Lyr

NASA Technical Reports Server (NTRS)

Plavec, M.

1975-01-01

All three stars showed rather complicated spectra, which require a very detailed spectroscopic analysis. The far UV spectrum of Beta Lyrae is clearly peculiar, with a multitude of emission lines not observed on any other star so far scanned with Copernicus. This made this star at once the most interesting and also, in a sense, easier to study. The other two stars display a spectrum rich in absorption lines, some of them being fairly broad (as expected for photospheric lines of rapidly rotating objects), some sharp. The later were clearly non-photospheric lines. An attempt was made to distinguish the circumstellar from the interstellar components.

A method of semi-quantifying β-AP in brain PET-CT 11C-PiB images.

PubMed

Jiang, Jiehui; Lin, Xiaoman; Wen, Junlin; Huang, Zhemin; Yan, Zhuangzhi

2014-01-01

Alzheimer's disease (AD) is a common health problem for elderly populations. Positron emission tomography-computed tomography (PET-CT)11C-PiB for beta-P (amyloid-β peptide, β-AP) imaging is an advanced method to diagnose AD in early stage. However, in practice radiologists lack a standardized value to semi-quantify β-AP. This paper proposes such a standardized value: SVβ-AP. This standardized value measures the mean ratio between the dimension of β-AP areas in PET and CT images. A computer aided diagnosis approach is also proposed to achieve SVβ-AP. A simulation experiment was carried out to pre-test the technical feasibility of the CAD approach and SVβ-AP. The experiment results showed that it is technically feasible.

A Binary Nature of the Marginal CP Star Sigma Sculptoris

NASA Astrophysics Data System (ADS)

Janík, Jan; Krtička, Jiří; Mikulášek, Zdeněk; Zverko, Juraj; Pintado, Olga; Paunzen, Ernst; Prvák, Milan; Skalický, Jan; Zejda, Miloslav; Adam, Christian

2018-05-01

The A2 V star σ Scl was suspected of being a low-amplitude rotating variable of the Ap-type star by several authors. Aiming to decide whether the star is a variable chemically peculiar (CP) star, we searched for the photometric and spectroscopic variability, and determined chemical abundances of σ Scl. The possible variability was tested using several types of periodograms applied to the photometry from Long-Term Photometry of Variables project (LTPV) and Hipparcos. Sixty spectrograms of high signal-to-noise (S/N) were obtained and used for chemical analysis of the stellar atmosphere and for looking for spectral variability that is symptomatic for the CP stars. We did not find any signs of the light variability or prominent chemical peculiarity, that is specific for the CP stars. The only exception is the abundance of scandium, which is significantly lower than the solar one and yttrium and barium, which are strongly overabundant. As a by-product of the analysis, and with the addition of 29 further spectra, we found that σ Scl is a single-lined spectroscopic binary with orbital period of 46.877(8) d. We argue that σ Scl is not an Ap star, but rather a marginal Am star in SB1 system. The spectral energy distribution of the binary reveals infrared excess due to circumstellar material.

VizieR Online Data Catalog: Star-forming potential in the Perseus complex (Mercimek+, 2017)

NASA Astrophysics Data System (ADS)

Mercimek, S.; Myers, P. C.; Lee, K. I.; Sadavoy, S. I.

2018-05-01

We used published catalogs of cores and YSOs at different wavelengths ranging from sub-millimeter (850 μm) to infrared (1.25 μm). We focus on seven clumps in Perseus, which Sadavoy et al. (2014ApJ...787L..18S) showed in their Figure 1. They defined these clumps and their boundaries using a fitted Herschel-derived column density map. The column density threshold of AV~7 mag is proposed as a star formation threshold by Andre et al. (2010A&A...518L.102A), Lada et al. (2010ApJ...724..687L), and Evans et al. (2014ApJ...782..114E) and is equal to N(H2)~5x1021/cm2 (see also, Kirk et al. 2006, J/ApJ/646/1009; Andre et al. 2010A&A...518L.102A). We considered a core or YSO to be associated with a clump if it is located within the AV=7 mag contour of that clump from Sadavoy et al. (2014ApJ...787L..18S). We define a "source" to be a starless core or a YSO. (7 data files).

VizieR Online Data Catalog: Kinematics of young associations/clusters (Tetzlaff+, 2010)

NASA Astrophysics Data System (ADS)

Tetzlaff, N.; Neuhaeuser, R.; Hohle, M. M.; Maciejewski, G.

2010-03-01

Given a distance of 1kpc and typical neutron star velocities of 100-500km/s (Arzoumanian et al. 2002ApJ...568..289A; Hobbs et al., 2005, Cat. J/MNRAS/360/974) and maximum ages of 5Myr for neutron stars to be detectable in the optical (see cooling curves in Gusakov et al. 2005MNRAS.363..555G and Popov, Grigorian & Blaschke 2006, Phys. Rev. C, 74, 025803), we restricted our search for birth associations and clusters of young nearby neutron stars to within 3kpc. We chose a sample of OB associations and young clusters (we use the term `association' for both in the following) within 3kpc from the Sun with available kinematic data and distance. We collected those from Dambis, Mel'nik & Rastorguev (2001AstL...27...58D) and Hoogerwerf (2001A&A...365...49H) and associations to which stars from the Galactic O-star catalogue from Maiz-Apellaniz et al. (2004, Cat. J/ApJS/151/103) are associated with. Furthermore, we added young local associations (YLA) from Fernandez, Figueras & Torra (2008A&A...480..735F) since they are possible hosts of a few SNe in the near past. We also included the Hercules-Lyrae association (Her-Lyr) and the Pleiades and massive star-forming regions (Reipurth 2008, ASP Monograph Publ. Vol. 4 and Vol. 5). We set the lower limit of the association age to 2Myr to account for the minimum lifetime of a progenitor star that can produce a neutron star (progenitor mass smaller than 30M⊙ see e.g. Heger et al. 2003ApJ...591..288H). The list of all explored associations and their properties can be found in Appendix A. Coordinates as well as heliocentric velocity components are given for a right-handed coordinate system with the x-axis pointing towards the galactic centre and y is positive in the direction of galactic rotation. (2 data files).

Mining the HST "Advanced Spectral Library (ASTRAL) - Hot Stars": The High Definition UV Spectrum of the Ap Star HR 465

NASA Astrophysics Data System (ADS)

Carpenter, Kenneth G.; Ayres, T. R.; Nielsen, K. E.; Kober, G. V.; Wahlgren, G. M.; Adelman, S. J.; Cowley, C. R.

2014-01-01

The "Advanced Spectral Library (ASTRAL) Project: Hot Stars" is a Hubble Space Telescope (HST) Cycle 21 Treasury Program (GO-13346: Ayres PI). It is designed to collect a definitive set of representative, high-resolution ( 30,000-100,000), high signal/noise (S/N>100), and full UV coverage 1200 - 3000 A) spectra of 21 early-type stars, utilizing the high-performance Space Telescope Imaging Spectrograph (STIS). The targets span the range of spectral types between early-O and early-A, including both main sequence and evolved stars, fast and slow rotators, as well as chemically peculiar (CP) and magnetic objects. These extremely high-quality STIS UV echelle spectra will be available from the HST archive and, in post-processed and merged form, at http://casa.colorado.edu ayres/ASTRAL/. The UV "atlases" produced by this program will enable investigations of a broad range of problems -- stellar, interstellar, and beyond -- for many years to come. We offer a first look at one of the earliest datasets to come out of this observing program, a "high definition" UV spectrum of the Ap star HR 465, which was chosen as a prototypical example of an A-type magnetic CP star. HR 465 has a global magnetic field of ~2200 Gauss. Earlier analyses of IUE spectra show strong iron-peak element lines, along with heavy elements such as Ga and Pt, while being deficient in the abundance of some ions of low atomic number, such as carbon. We demonstrate the high quality of the ASTRAL data and present the identification of spectral lines for a number of elements. By comparison of the observed spectra with calculated spectra, we also provide estimates of element abundances, emphasizing heavy elements, and place these measurements in the context of earlier results for this and other Ap stars.

Correlation of nitric oxide and other free radicals with the severity of acute pancreatitis and complicated systemic inflammatory response syndrome.

PubMed

Que, Ri-sheng; Cao, Li-ping; Ding, Guo-ping; Hu, Jun-an; Mao, Ke-jie; Wang, Gui-feng

2010-05-01

To investigate the correlation of nitric oxide (NO) and other free radicals with the severity of acute pancreatitis (AP) and complicated systemic inflammatory response syndrome (SIRS). Fifty AP patients (24 simple AP patients and 26 patients with AP complicated by SIRS) were involved in the study. Fifty healthy volunteers were included as controls. Acute Physiology and Chronic Health Evaluation II (APACHE II) scores were evaluated, and plasma NO, plasma lipid peroxides, plasma vitamin E, plasma beta-carotene, whole-blood glutathione (GSH), and the activity of plasma GSH peroxidase were measured. Compared with the control group, the APACHE II scores heightened in the AP group, and the SIRS group had the highest APACHE II scores (P < 0.005, P < 0.001, respectively). Plasma NO and plasma lipid peroxides increased with the heightening APACHE II scores, demonstrating a significant linear positive correlation (r = 0.618, r = 0.577, respectively; P < 0.001). Plasma vitamin E, plasma beta-carotene, whole-blood GSH, and the activity of plasma GSH peroxidase decreased with the heightening APACHE II scores, demonstrating a significant linear negative correlation (r = -0.600, r = -0.609, r = -0.559, r = -0.592, respectively; P < 0.001). Nitric oxide and other free radicals take part in the aggravation of oxidative stress and oxidative injury and may play important roles in the pathogenesis of AP and SIRS. It may be valuable to measure free radicals to predict the severity of AP.

Multiperiodicity in the Light Variations of the Beta Cephei Star Beta Crucis

NASA Technical Reports Server (NTRS)

Cuypers, J.; Aerts, C.; Buzasi, D.; Catanzarite, J.; Conrow, T.; Laher, R.

2002-01-01

High-resolution spectroscopic observations have led recently to the discovery that the beta Cephei star beta Crucis (Mimosa) is multiperiodic with at least three non-radial pulsation modes. Data obtained by the star tracker of the WIRE satellite have now allowed us to confirm this multiperiodicity in the light variations. A total of 5 million observations covering 17 days was analyzed and the three main periods we find in this work are in perfect agreement with the results derived from the line profile variations. The photometric amplitudes are small (3, 2.7 and 0.6 millimag for the dominant modes), but this is not surprising in view of the mode identifications derived earlier from the line profiles. Additional periods of low-amplitude modes (between 0.2-0.3 mmag) are also derived, including one suggested earlier by the radial velocity data.

Physical properties of gas disks around shell stars with and without dust

NASA Technical Reports Server (NTRS)

Grady, Carol A.

1992-01-01

Analysis of archival IRAS and IUE data has resulted in: (1) identification of 8 new A star proto-planetary candidates; (2) detection of a mass outflow event around Beta Pic (subsequently confirmed by the 1991 July HST observation); and (3) confirmation of the suggestion by Waters et al. (1988) that 51 Oph is a protoplanetary system similar to beta Pic with the detection of high density, high velocity, collisionally ionized accreting gas in the line of sight toward this star.

Pulsations in the atmosphere of the rapidly oscillating star 33 Lib

NASA Astrophysics Data System (ADS)

Sachkov, M.; Hareter, M.; Ryabchikova, T.; Wade, G.; Kochukhov, O.; Shulyak, D.; Weiss, W. W.

2011-10-01

In 2009, the rapidly oscillating peculiar A-type (roAp) star 33 Lib was the target of an intense observing campaign, combining ground-based spectroscopy with space photometry obtained with the Microvariability and Oscillation of STars (MOST) satellite. We collected 780 spectra using the Echelle Spectro Polarimetric Device for the Observation of Stars (ESPaDOnS) spectrograph attached at the 3.6-m Canada-France-Hawaii Telescope and 374 spectra with the Fibre-fed Echelle Spectrograph attached at the 2.56-m Nordic Optical Telescope to perform time-resolved spectroscopy of 33 Lib. In addition, we used 111 Ultraviolet and Visual Echelle Spectrograph (UVES) spectra (2004) from the European Southern Observatory archive to check mode stability. Frequency analysis of the new radial velocity (RV) measurements confirms the previously reported frequency pattern (two frequencies and the first harmonic of the main one) and reveals an additional frequency at 1.991 mHz. The new frequency solution perfectly reproduces the RV variations from the 2004 and 2009 observational sets, providing strong support for p mode stability in this roAp star over at least 5 years.

TAK1 regulates NF-{Kappa}B and AP-1 activation in airway epithelial cells following RSV infection

DOE Office of Scientific and Technical Information (OSTI.GOV)

Dey, Nilay; Liu Tianshuang; Garofalo, Roberto P.

2011-09-30

Respiratory syncytial virus (RSV) is the most common cause of epidemic respiratory diseases in infants and young children. RSV infection of airway epithelial cells induces the expression of immune/inflammatory genes through the activation of a subset of transcription factors, including Nuclear Factor-{kappa}B (NF-{kappa}B) and AP-1. In this study, we have investigated the signaling pathway leading to activation of these two transcription factors in response to RSV infection. Our results show that IKK{beta} plays a key role in viral-induced NF-{kappa}B activation, while JNK regulates AP-1-dependent gene transcription, as demonstrated by using kinase inactive proteins and chemical inhibitors of the two kinases.more » Inhibition of TAK1 activation, by overexpression of kinase inactive TAK1 or using cells lacking TAK1 expression, significantly reduced RSV-induced NF-{kappa}B and AP-1 nuclear translocation and DNA-binding activity, as well as NF-{kappa}B-dependent gene expression, identifying TAK1 as an important upstream signaling molecule regulating RSV-induced NF-{kappa}B and AP-1 activation. - Highlights: > IKK{beta} is a major kinase involved in RSV-induced NF-{kappa}B activation. > JNK regulates AP-1-dependent gene transcription in RSV infection. > TAK1 is a critical upstream signaling molecule for both pathways in infected cells.« less

DOE Office of Scientific and Technical Information (OSTI.GOV)

A Kolyada; C Lee; A De Biasio

{beta}2GPI is a major antigen for autoantibodies associated with antiphospholipid syndrome (APS), an autoimmune disease characterized by thrombosis and recurrent pregnancy loss. Only the dimeric form of {beta}2GPI generated by anti-{beta}2GPI antibodies is pathologically important, in contrast to monomeric {beta}2GPI which is abundant in plasma. We created a dimeric inhibitor, A1-A1, to selectively target {beta}2GPI in {beta}2GPI/antibody complexes. To make this inhibitor, we isolated the first ligand-binding module from ApoER2 (A1) and connected two A1 modules with a flexible linker. A1-A1 interferes with two pathologically important interactions in APS, the binding of {beta}2GPI/antibody complexes with anionic phospholipids and ApoER2. Wemore » compared the efficiency of A1-A1 to monomeric A1 for inhibition of the binding of {beta}2GPI/antibody complexes to anionic phospholipids. We tested the inhibition of {beta}2GPI present in human serum, {beta}2GPI purified from human plasma and the individual domain V of {beta}2GPI. We demonstrated that when {beta}2GPI/antibody complexes are formed, A1-A1 is much more effective than A1 in inhibition of the binding of {beta}2GPI to cardiolipin, regardless of the source of {beta}2GPI. Similarly, A1-A1 strongly inhibits the binding of dimerized domain V of {beta}2GPI to cardiolipin compared to the monomeric A1 inhibitor. In the absence of anti-{beta}2GPI antibodies, both A1-A1 and A1 only weakly inhibit the binding of pathologically inactive monomeric {beta}2GPI to cardiolipin. Our results suggest that the approach of using a dimeric inhibitor to block {beta}2GPI in the pathological multivalent {beta}2GPI/antibody complexes holds significant promise. The novel inhibitor A1-A1 may be a starting point in the development of an effective therapeutic for antiphospholipid syndrome.« less

Spleen tyrosine kinase mediates high glucose-induced transforming growth factor-{beta}1 up-regulation in proximal tubular epithelial cells

DOE Office of Scientific and Technical Information (OSTI.GOV)

Yang, Won Seok; Chang, Jai Won; Han, Nam Jeong

The role of spleen tyrosine kinase (Syk) in high glucose-induced intracellular signal transduction has yet to be elucidated. We investigated whether Syk is implicated in high glucose-induced transforming growth factor-{beta}1 (TGF-{beta}1) up-regulation in cultured human proximal tubular epithelial cells (HK-2 cell). High glucose increased TGF-{beta}1 gene expression through Syk, extracellular signal-regulated kinase (ERK), AP-1 and NF-{kappa}B. High glucose-induced AP-1 DNA binding activity was decreased by Syk inhibitors and U0126 (an ERK inhibitor). Syk inhibitors suppressed high glucose-induced ERK activation, whereas U0126 had no effect on Syk activation. High glucose-induced NF-{kappa}B DNA binding activity was also decreased by Syk inhibitors. Highmore » glucose increased nuclear translocation of p65 without serine phosphorylation of I{kappa}B{alpha} and without degradation of I{kappa}B{alpha}, but with an increase in tyrosine phosphorylation of I{kappa}B{alpha} that may account for the activation of NF-{kappa}B. Both Syk inhibitors and Syk-siRNA attenuated high glucose-induced I{kappa}B{alpha} tyrosine phosphorylation and p65 nuclear translocation. Depletion of p21-activated kinase 2 (Pak2) by transfection of Pak2-siRNA abolished high glucose-induced Syk activation. In summary, high glucose-induced TGF-{beta}1 gene transcription occurred through Pak2, Syk and subsequent ERK/AP-1 and NF-{kappa}B pathways. This suggests that Syk might be implicated in the diabetic kidney disease.« less

From the Milky Way to differing galaxy environments: filling critical gaps in our knowledge of star formation and its interplay with dust, and in stellar and galaxy evolution.

NASA Astrophysics Data System (ADS)

Bianchi, Luciana

2018-01-01

Rest-frame UV, uniquely sensitive to luminous, short-lived hot massive stars, trace and age-date star formation across galaxies, and is very sensitive to dust, whose properties and presence are closely connected to star formation.With wide f-o-v and deep sensitivity in two broad filters,FUV and NUV,GALEX delivered the first comprehensive UV view of large nearby galaxies, and of the universe to z~2 (e.g.,Bianchi 2014 ApSS 354,103), detected star formation at the lowest rates, in environments where it was not seen before and not expected (e.g. Bianchi 2011 ApSS 335,51; Thilker+2009 Nature 457,990;2007 ApJS 173,538), triggering a new era of investigations with HST and large ground-based telescopes. New instrument technology and modeling capabilities make it now possible and compelling to solve standing issues. The scant UV filters available (esp. FUV) and the wide gap in resolution and f-o-v between GALEX and HST leaves old and new questions open. A chief limitation is degeneracies between physical parameters of stellar populations (age/SFR) and hot stars, and dust (e.g. Bianchi+ 2014 JASR 53,928).We show sample model simulations for filter optimization to provide critical measurements for the science objectives. We also demonstrate how adequate FUV+NUV filters, and resolution, allow us to move from speculative interpretation of UV data to unbiased physical characterization of young stellar populations and dust, using new data from UVIT, which, though smaller than CETUS, has better resolution and filter coverage than GALEX.Also, our understanding of galaxy chemical enrichment is limited by critical gaps in stellar evolution; GALEX surveys enabled the first unbiased census of the Milky Way hot-WD population (Bianchi+2011 MNRAS, 411,2770), which we complement with SDSS, Pan-STARRS, and Gaia data to fill such gaps (Bianchi et al.2018, ApSS). Such objects in CETUS fields (deeper exposures, more filters, and the first UV MOS) will be much better characterized, enabling "Galactic archeology" investigations not possible otherwise.

Association of papillomavirus E6 proteins with either MAML1 or E6AP clusters E6 proteins by structure, function, and evolutionary relatedness

PubMed Central

Brimer, Nicole

2017-01-01

Papillomavirus E6 proteins bind to LXXLL peptide motifs displayed on targeted cellular proteins. Alpha genus HPV E6 proteins associate with the cellular ubiquitin ligase E6AP (UBE3A), by binding to an LXXLL peptide (ELTLQELLGEE) displayed by E6AP, thereby stimulating E6AP ubiquitin ligase activity. Beta, Gamma, and Delta genera E6 proteins bind a similar LXXLL peptide (WMSDLDDLLGS) on the cellular transcriptional co-activator MAML1 and thereby repress Notch signaling. We expressed 45 different animal and human E6 proteins from diverse papillomavirus genera to ascertain the overall preference of E6 proteins for E6AP or MAML1. E6 proteins from all HPV genera except Alpha preferentially interacted with MAML1 over E6AP. Among animal papillomaviruses, E6 proteins from certain ungulate (SsPV1 from pigs) and cetacean (porpoises and dolphins) hosts functionally resembled Alpha genus HPV by binding and targeting the degradation of E6AP. Beta genus HPV E6 proteins functionally clustered with Delta, Pi, Tau, Gamma, Chi, Mu, Lambda, Iota, Dyokappa, Rho, and Dyolambda E6 proteins to bind and repress MAML1. None of the tested E6 proteins physically and functionally interacted with both MAML1 and E6AP, indicating an evolutionary split. Further, interaction of an E6 protein was insufficient to activate degradation of E6AP, indicating that E6 proteins that target E6AP co-evolved to separately acquire both binding and triggering of ubiquitin ligase activation. E6 proteins with similar biological function clustered together in phylogenetic trees and shared structural features. This suggests that the divergence of E6 proteins from either MAML1 or E6AP binding preference is a major event in papillomavirus evolution. PMID:29281732

ERalpha and AP-1 interact in vivo with a specific sequence of the F promoter of the human ERalpha gene in osteoblasts.

PubMed

Lambertini, Elisabetta; Tavanti, Elisa; Torreggiani, Elena; Penolazzi, Letizia; Gambari, Roberto; Piva, Roberta

2008-07-01

Estrogen-responsive genes often have an estrogen response element (ERE) positioned next to activator protein-1 (AP-1) binding sites. Considering that the interaction between ERE and AP-1 elements has been described for the modulation of bone-specific genes, we investigated the 17-beta-estradiol responsiveness and the role of these cis-elements present in the F promoter of the human estrogen receptor alpha (ERalpha) gene. The F promoter, containing the sequence analyzed here, is one of the multiple promoters of the human ERalpha gene and is the only active promoter in bone tissue. Through electrophoretic mobility shift (EMSA), chromatin immunoprecipitation (ChIP), and re-ChIP assays, we investigated the binding of ERalpha and four members of the AP-1 family (c-Jun, c-fos, Fra-2, and ATF2) to a region located approximately 800 bp upstream of the transcriptional start site of exon F of the human ERalpha gene in SaOS-2 osteoblast-like cells. Reporter gene assay experiments in combination with DNA binding assays demonstrated that F promoter activity is under the control of upstream cis-acting elements which are recognized by specific combinations of ERalpha, c-Jun, c-fos, and ATF2 homo- and heterodimers. Moreover, ChIP and re-ChIP experiments showed that these nuclear factors bind the F promoter in vivo with a simultaneous occupancy stimulated by 17-beta-estradiol. Taken together, our findings support a model in which ERalpha/AP-1 complexes modulate F promoter activity under conditions of 17-beta-estradiol stimulation. (c) 2008 Wiley-Liss, Inc.

The impact of IUE on binary star studies

NASA Technical Reports Server (NTRS)

Plavec, M. J.

1981-01-01

The use of IUE observations in the investigation of binary stars is discussed. The results of data analysis of several classes of binary systems are briefly reviewed including zeta Aurigae and VV Cephei stars, mu Sagittarii, epsilon Aurigae, beta Lyrae and the W Serpentis stars, symbiotic stars, and the Algols.

Regulation of rat mesangial cell growth by diadenosine phosphates.

PubMed Central

Heidenreich, S; Tepel, M; Schlüter, H; Harrach, B; Zidek, W

1995-01-01

The newly recognized human endogenous vasoconstrictive dinucleotides, diadenosine pentaphosphate (AP5A) and diadenosine hexaphosphate (AP6A), were tested for growth stimulatory effects in rat mesangial cells (MC). Both AP5A and AP6A stimulated growth in micromolar concentrations. The growth stimulatory effect exceeded that of ATP, alpha,beta-methylene ATP, adenosine 5'-O-(3-thio)triphosphate and UTP. Both diadenosine phosphates potentiated the growth response to platelet-derived growth factor, but not to insulin-like growth factor-1. To further elucidate the site of action in the cell cycle, RNA and protein synthesis were assessed. AP5 and AP6A stimulated protein synthesis, but not RNA formation. Furthermore, both agents increased cytosolic free Ca2+ concentration. It is concluded that AP5A and AP6A may play a regulatory role in MC growth as progression factors and possibly modify MC proliferation in glomerular disease. PMID:7769127

Magnetic Doppler imaging considering atmospheric structure modifications due to local abundances: a luxury or a necessity?

NASA Astrophysics Data System (ADS)

Kochukhov, O.; Wade, G. A.; Shulyak, D.

2012-04-01

Magnetic Doppler imaging is currently the most powerful method of interpreting high-resolution spectropolarimetric observations of stars. This technique has provided the very first maps of stellar magnetic field topologies reconstructed from time series of full Stokes vector spectra, revealing the presence of small-scale magnetic fields on the surfaces of Ap stars. These studies were recently criticised by Stift et al., who claimed that magnetic inversions are not robust and are seriously undermined by neglecting a feedback on the Stokes line profiles from the local atmospheric structure in the regions of enhanced metal abundance. We show that Stift et al. misinterpreted published magnetic Doppler imaging results and consistently neglected some of the most fundamental principles behind magnetic mapping. Using state-of-the-art opacity sampling model atmosphere and polarized radiative transfer codes, we demonstrate that the variation of atmospheric structure across the surface of a star with chemical spots affects the local continuum intensity but is negligible for the normalized local Stokes profiles except for the rare situation of a very strong line in an extremely Fe-rich atmosphere. For the disc-integrated spectra of an Ap star with extreme abundance variations, we find that the assumption of a mean model atmosphere leads to moderate errors in Stokes I but is negligible for the circular and linear polarization spectra. Employing a new magnetic inversion code, which incorporates the horizontal variation of atmospheric structure induced by chemical spots, we reconstructed new maps of magnetic field and Fe abundance for the bright Ap star α2 CVn. The resulting distribution of chemical spots changes insignificantly compared to the previous modelling based on a single model atmosphere, while the magnetic field geometry does not change at all. This shows that the assertions by Stift et al. are exaggerated as a consequence of unreasonable assumptions and extrapolations, as well as methodological flaws and inconsistencies of their analysis. Our discussion proves that published magnetic inversions based on a mean stellar atmosphere are highly robust and reliable, and that the presence of small-scale magnetic field structures on the surfaces of Ap stars is indeed real. Incorporating horizontal variations of atmospheric structure in Doppler imaging can marginally improve reconstruction of abundance distributions for stars showing very large iron overabundances. But this costly technique is unnecessary for magnetic mapping with high-resolution polarization spectra.

Spectrophotometry of peculiar B and A stars. XIV - 56 Arietis, 41 Tauri, 25 Sextantis, HD 170973, HD 205087, and HD 215441

NASA Astrophysics Data System (ADS)

Adelman, S. J.

1983-03-01

Optical region spectrophotometry of six relatively hot Ap stars is presented. Additional scans of 56 Ari extend the results of an earlier paper in this series. The data for 41 Tau, 25 Sex, HD 170973, and HD 215441 are studied as a function of phase. The observations of HD 205087 are inconclusive about its variability although they show spectrophotometrically that it is a definite Ap star. The observations of HD 215441 show a prominent λ5200 broad, continuum feature with an unusual shape. However, when the data are corrected for interstellar reddening, the energy distribution resembles those of other silicon stars. The λ5200 feature is found to be variable in phase with the U-B and B-V colors and with the magnetic field strength. This feature is strongest when the Balmer jump is smallest, the Paschen continuum the bluest according to B-V, and the surface magnetic field strength the largest.

Performance Analysis of Modified Accelerative Preallocation MAC Protocol for Passive Star-Coupled WDMA Networks

NASA Astrophysics Data System (ADS)

Yun, Changho; Kim, Kiseon

2006-04-01

For the passive star-coupled wavelength-division multiple-access (WDMA) network, a modified accelerative preallocation WDMA (MAP-WDMA) media access control (MAC) protocol is proposed, which is based on AP-WDMA. To show the advantages of MAP-WDMA as an adequate MAC protocol for the network over AP-WDMA, the channel utilization, the channel-access delay, and the latency of MAP-WDMA are investigated and compared with those of AP-WDMA under various data traffic patterns, including uniform, quasi-uniform type, disconnected type, mesh type, and ring type data traffics, as well as the assumption that a given number of network stations is equal to that of channels, in other words, without channel sharing. As a result, the channel utilization of MAP-WDMA can be competitive with respect to that of AP-WDMA at the expense of insignificantly higher latency. Namely, if the number of network stations is small, MAP-WDMA provides better channel utilization for uniform, quasi-uniform-type, and disconnected-type data traffics at all data traffic loads, as well as for mesh and ring-type data traffics at low data traffic loads. Otherwise, MAP-WDMA only outperforms AP-WDMA for the first three data traffics at higher data traffic loads. In the aspect of channel-access delay, MAP-WDMA gives better performance than AP-WDMA, regardless of data traffic patterns and the number of network stations.

Nicergoline, a drug used for age-dependent cognitive impairment, protects cultured neurons against beta-amyloid toxicity.

PubMed

Caraci, Filippo; Chisari, Mariangela; Frasca, Giuseppina; Canonico, Pier Luigi; Battaglia, Angelo; Calafiore, Marco; Battaglia, Giuseppe; Bosco, Paolo; Nicoletti, Ferdinando; Copani, Agata; Sortino, Maria Angela

2005-06-14

Nicergoline, a drug used for the treatment of Alzheimer's disease and other types of dementia, was tested for its ability to protect neurons against beta-amyloid toxicity. Pure cultures of rat cortical neurons were challenged with a toxic fragment of beta-amyloid peptide (betaAP(25-35)) and toxicity was assessed after 24 h. Micromolar concentrations of nicergoline or its metabolite, MDL, attenuated betaAP(25-35)-induced neuronal death, whereas MMDL (another metabolite of nicergoline), the alpha1-adrenergic receptor antagonist, prazosin, or the serotonin 5HT-2 receptor antagonist, methysergide, were inactive. Nicergoline increased the basal levels of Bcl-2 and reduced the increase in Bax levels induced by beta-amyloid, indicating that the drug inhibits the execution of an apoptotic program in cortical neurons. In mixed cultures of rat cortical cells containing both neurons and astrocytes, nicergoline and MDL were more efficacious than in pure neuronal cultures in reducing beta-amyloid neurotoxicity. Experiments carried out in pure cultures of astrocytes showed that a component of neuroprotection was mediated by a mechanism of glial-neuronal interaction. The conditioned medium of cultured astrocytes treated with nicergoline or MDL for 72-96 h (collected 24 h after drug withdrawal) was neuroprotective when transferred to pure neuronal cultures challenged with beta-amyloid. In cultured astrocytes, nicergoline increased the intracellular levels of transforming-growth factor-beta and glial-derived neurotrophic factor, two trophic factors that are known to protect neurons against beta-amyloid toxicity. These results raise the possibility that nicergoline reduces neurodegeneration in the Alzheimer's brain.

Quantitative electroencephalography analysis in university students with hazardous alcohol consumption, but not alcohol dependence.

PubMed

Núñez-Jaramillo, Luis; Vega-Perera, Paulo; Ramírez-Lugo, Leticia; Reyes-López, Julián V; Santiago-Rodríguez, Efraín; Herrera-Morales, Wendy V

2015-07-08

Hazardous alcohol consumption is a pattern of consumption that leads to a higher risk of harmful consequences either for the user or for others. This pattern of alcohol consumption has been linked to risky behaviors, accidents, and injuries. Individuals with hazardous alcohol consumption do not necessarily present alcohol dependence; thus, a study of particular neurophysiological correlates of this alcohol consumption pattern needs to be carried out in nondependent individuals. Here, we carried out a quantitative electroencephalography analysis in health sciences university students with hazardous alcohol consumption, but not alcohol dependence (HAC), and control participants without hazardous alcohol consumption or alcohol dependence (NHAC). We analyzed Absolute Power (AP), Relative Power (RP), and Mean Frequency (MF) for beta and theta frequency bands under both eyes closed and eyes open conditions. We found that participants in the HAC group presented higher beta AP at centroparietal region, as well as lower beta MF at frontal and centroparietal regions in the eyes closed condition. Interestingly, participants did not present any change in theta activity (AP, RP, or MF), whereas previous reports indicate an increase in theta AP in alcohol-dependent individuals. Our results partially resemble those found in alcohol-dependent individuals, although are not completely identical, suggesting a possible difference in the underlying neuronal mechanism behind alcohol dependence and hazardous alcohol consumption. Similarities could be explained considering that both hazardous alcohol consumption and alcohol dependence are manifestations of behavioral disinhibition.

VizieR Online Data Catalog: K giant stars along Sagittarius streams (Ren+, 2017)

NASA Astrophysics Data System (ADS)

Ren, H.-B.; Shi, W.-B.; Zhang, X.; Tang, Y.-K.; Zhang, Y.; Hou, Y.-H.; Wang, Y.-F.

2017-08-01

Law & Majewski (2010ApJ...714..229L) provided a Sgr model that has 105 points with angular position, distance and radial velocity. By using the model of Law & Majewski (2010ApJ...714..229L), we selected K giant samples belonging to the leading Sgr stream. (1 data file).

VizieR Online Data Catalog: Masses and ages of red giants (Martig+, 2016)

NASA Astrophysics Data System (ADS)

Martig, M.; Fouesneau, M.; Rix, H.-W.; Ness, M.; Meszaros, S.; Garcia-Hernandez, D. A.; Pinsonneault, M.; Serenelli, A.; Silva Aguirre, V.; Zamora, O.

2016-10-01

The APOKASC project is the spectroscopic follow-up by APOGEE (Majewski et al. 2015, in prep., as part of the third phase of the Sloan Digital Sky Survey, SDSS-III; Eisenstein et al., 2011AJ....142...72E) of stars with asteroseismology data from the Kepler Asteroseismic Science Consortium (KASC). The first version of the APOKASC catalogue (Pinsonneault et al., 2014, Cat. J/ApJS/215/19) contains seismic and spectroscopic measurements for 1989 giants, with the spectroscopic information corresponding to APOGEE's Data Release 10 (DR10; Ahn et al., 2014ApJS..211...17A). In this work, we keep the same original sample of 1989 stars and their seismic parameters, but update their Teff and abundances to DR12 values (Alam et al., 2015ApJS..219...12A; Holtzman et al., 2015AJ....150..148H). (2 data files).

Spectrophotometry of peculiar B and A stars. XVIII - The helium rich variable stars HR 1890, Sigma Orionis E, and HD 37776

NASA Technical Reports Server (NTRS)

Adelman, S. J.; Pyper, D. M.

1985-01-01

Optical region spectrophotometry at 3300-7850 A has been obtained for three helium rich stars, HR 1890, Sigma Ori E, and HD 37776, of the Orion OB1 Association. New uvby-beta photometry of HR 1890 and HD 37776 as well as published data are also used to investigate the variability of these stars. A new period of 1.53862 days was determined for HD 37776. For all three stars H-beta varies in antiphase with strong He I lines. The spectrophotometric bandpass containing the strong He I line at 4471 A varies in phase with the R index of Pedersen and Thomsen (1977). Evidence is found for weak absorption features which appear to be an extension of the 5200 A feature seen in cooler CP stars.

The null result of a search for pulsational variations of the surface magnetic field in the roAp star γ Equulei

NASA Astrophysics Data System (ADS)

Kochukhov, O.; Ryabchikova, T.; Landstreet, J. D.; Weiss, W. W.

2004-06-01

We describe an analysis of the time-resolved measurements of the surface magnetic field in the roAp star γEqu. We have obtained a high-resolution and high signal-to-noise (S/N) spectroscopic time series, and the magnetic field was determined using Zeeman-resolved profiles of the FeII 6149.25 Åand FeI 6173.34 Ålines. Contrary to recent reports, we do not find any evidence of magnetic variability with pulsation phase, and derive an upper limit of 5-10 G for pulsational modulation of the surface magnetic field in γEqu.

The magnetic field of the double-lined spectroscopic binary system HD 5550

NASA Astrophysics Data System (ADS)

Alecian, E.; Tkachenko, A.; Neiner, C.; Folsom, C. P.; Leroy, B.

2016-05-01

Context. The origin of fossil fields in intermediate- and high-mass stars is poorly understood, as is the interplay between binarity and magnetism during stellar evolution. Thus we have begun a study of the magnetic properties of a sample of intermediate-mass and massive short-period binary systems as a function of binarity properties. Aims: This paper specifically aims to characterise the magnetic field of HD 5550, a double-lined spectroscopic binary system of intermediate mass. Methods: We gathered 25 high-resolution spectropolarimetric observations of HD 5550 using the instrument Narval. We first fitted the intensity spectra using Zeeman/ATLAS9 LTE synthetic spectra to estimate the effective temperatures, microturbulent velocities, and the abundances of some elements of both components, as well as the light ratio of the system. We then applied the multi-line least-square deconvolution (LSD) technique to the intensity and circularly polarised spectra, which provided us with mean LSD I and V line profiles. We fitted the Stokes I line profiles to determine the radial and projected rotational velocities of both stars. We then analysed the shape and evolution of the V profiles using the oblique rotator model to characterise the magnetic fields of both stars. Results: We confirm the Ap nature of the primary, which has previously been reported, and find that the secondary displays spectral characteristics typical of an Am star. While a magnetic field is clearly detected in the lines of the primary, no magnetic field is detected in the secondary in any of our observations. If a dipolar field were present at the surface of the Am star, its polar strength must be below 40 G. The faint variability observed in the Stokes V profiles of the Ap star allowed us to propose a rotation period of 6.84-0.39+0.61 d, which is close to the orbital period (~6.82 d), suggesting that the star is synchronised with its orbit. By fitting the variability of the V profiles, we propose that the Ap component hosts a dipolar field inclined with the rotation axis at an angle β = 156 ± 17 ° and a polar strength Bd = 65 ± 20 G. The field strength is the weakest known for an Ap star. Based on the BinaMIcS Large Programme (PI: C. Neiner, runID: L131N02) obtained at the Telescope Bernard Lyot (USR5026) operated by the Observatoire Midi-Pyrénées, Université de Toulouse (Paul Sabatier), Centre National de la Recherche Scientifique of France.

Associations of anti-beta2-glycoprotein I autoantibodies with HLA class II alleles in three ethnic groups.

PubMed

Arnett, F C; Thiagarajan, P; Ahn, C; Reveille, J D

1999-02-01

To determine any HLA associations with anti-beta2-glycoprotein I (anti-beta2GPI) antibodies in a large, retrospectively studied, multiethnic group of 262 patients with primary antiphospholipid antibody syndrome (APS), systemic lupus erythematosus (SLE), or another connective tissue disease. Anti-beta2GPI antibodies were detected in sera using an enzyme-linked immunosorbent assay. HLA class II alleles (DRB1, DQA1, and DQB1) were determined by DNA oligotyping. The HLA-DQB1*0302 (DQ8) allele, typically carried on HLA-DR4 haplotypes, was associated with anti-beta2GPI when compared with both anti-beta2GPI-negative SLE patients and ethnically matched normal controls, especially in Mexican Americans and, to a lesser extent, in whites. Similarly, when ethnic groups were combined, HLA-DQB1*0302, as well as HLA-DQB1*03 alleles overall (DQB1*0301, *0302, and *0303), were strongly correlated with anti-beta2GPI antibodies. The HLA-DR6 (DR13) haplotype DRB1*1302; DQB1*0604/5 was also significantly increased, primarily in blacks. HLA-DR7 was not significantly increased in any of these 3 ethnic groups, and HLA-DR53 (DRB4*0101) was increased in Mexican Americans only. Certain HLA class II haplotypes genetically influence the expression of antibodies to beta2GPI, an important autoimmune response in the APS, but there are variations in HLA associations among different ethnic groups.

The discovery of nonthermal radio emission from magnetic Bp-Ap stars

NASA Technical Reports Server (NTRS)

Drake, Stephen A.; Abbott, David C.; Bastian, T. S.; Bieging, J. H.; Churchwell, E.

1987-01-01

In a VLA survey of chemically peculiar B- and A-type stars with strong magnetic fields, five of the 34 stars observed have been identified as 6 cm continuum sources. Three of the detections are helium-strong early Bp stars (Sigma Ori E, HR 1890, and Delta Ori C), and two are helium weak, silicon-strong stars with spectral types near A0p (IQ Aur = HD 34452, Babcock's star = HD 215441). The 6 cm luminosities L6 (ergs/s Hz) range from log L6 = 16.2 to 17.9, somewhat less than the OB supergiants and W-R stars. Three-frequency observations indicate that the helium-strong Bp stars are variable nonthermal sources.

UV-CONTINUUM SLOPES AT z {approx} 4-7 FROM THE HUDF09+ERS+CANDELS OBSERVATIONS: DISCOVERY OF A WELL-DEFINED UV COLOR-MAGNITUDE RELATIONSHIP FOR z {>=} 4 STAR-FORMING GALAXIES

DOE Office of Scientific and Technical Information (OSTI.GOV)

Bouwens, R. J.; Franx, M.; Labbe, I.

2012-08-01

Ultra-deep Advanced Camera for Surveys (ACS) and WFC3/IR HUDF+HUDF09 data, along with the wide-area GOODS+ERS+CANDELS data over the CDF-S GOODS field, are used to measure UV colors, expressed as the UV-continuum slope {beta}, of star-forming galaxies over a wide range of luminosity (0.1L*{sub z=3} to 2L*{sub z=3}) at high redshift (z {approx} 7 to z {approx} 4). {beta} is measured using all ACS and WFC3/IR passbands uncontaminated by Ly{alpha} and spectral breaks. Extensive tests show that our {beta} measurements are only subject to minimal biases. Using a different selection procedure, Dunlop et al. recently found large biases in their {beta}more » measurements. To reconcile these different results, we simulated both approaches and found that {beta} measurements for faint sources are subject to large biases if the same passbands are used both to select the sources and to measure {beta}. High-redshift galaxies show a well-defined rest-frame UV color-magnitude (CM) relationship that becomes systematically bluer toward fainter UV luminosities. No evolution is seen in the slope of the UV CM relationship in the first 1.5 Gyr, though there is a small evolution in the zero point to redder colors from z {approx} 7 to z {approx} 4. This suggests that galaxies are evolving along a well-defined sequence in the L{sub UV}-color ({beta}) plane (a 'star-forming sequence'?). Dust appears to be the principal factor driving changes in the UV color {beta} with luminosity. These new larger {beta} samples lead to improved dust extinction estimates at z {approx} 4-7 and confirm that the extinction is essentially zero at low luminosities and high redshifts. Inclusion of the new dust extinction results leads to (1) excellent agreement between the star formation rate (SFR) density at z {approx} 4-8 and that inferred from the stellar mass density; and (2) to higher specific star formation rates (SSFRs) at z {approx}> 4, suggesting that the SSFR may evolve modestly (by factors of {approx}2) from z {approx} 4-7 to z {approx} 2.« less

Cometary Dust in the Debris Disks of HD 31648 and HD 163296: Two "Baby" (BETA) Pictoris Stars

NASA Technical Reports Server (NTRS)

Sitko, Michael L.; Grady, Carol A.; Lynch, David K.; Russell, Ray W.; Hanner, Martha S.; Hanner, Martha S.

1999-01-01

The debris disks surrounding the pre-main-sequence stars HD 31648 and HD 163296 were observed spectroscopically between 3 and 14 microns. Both stars possess a silicate emission feature at 10 microns that resembles that of the star beta Pictoris and those observed in solar system comets. The structure of the band is consistent with a mixture of olivine and pyroxene material, plus an underlying continuum of unspecified origin. The similarity in both size and structure of the silicate band suggests that the material in these systems had a processing history similar to that in our own solar system prior to the time that the grains were incorporated into comets.

VizieR Online Data Catalog: Srg tidal tails red giants properties (Zhang+, 2017)

NASA Astrophysics Data System (ADS)

Zhang, X.; Shi, W. B.; Chen, Y. Q.; Zhao, G.; Carrell, K.; Zhao, J. K.; Ruan, G. P.; Liang, Y. C.; Zhou, L.; Ren, H. B.; Zhang, Y.; Hou, Y. H.; Wang, Y. F.

2016-10-01

The list of 1100 RGB stars in Sgr streams is selected from SDSS DR9 with Law & Majewski (2010ApJ...714..229L) model. For each star equatorial coordinates, [Fe/H], distance, Vgsr, Lambda, X, Y and Z are given. Each star is also marked with L1, L2, T1, T2 to show in which stream it locates. (1 data file).

VizieR Online Data Catalog: Velocities of RGB stars in the Leo II dwarf galaxy (Spencer+, 2017)

NASA Astrophysics Data System (ADS)

Spencer, M. E.; Mateo, M.; Walker, M. G.; Olszewski, E. W.; McConnachie, A. W.; Kirby, E. N.; Koch, A.

2018-05-01

We use radial velocity data from four studies. The first set comprises 31 red giant branch (RGB) stars with a median radial velocity error of 3 km/s (Vogt et al. 1995AJ....109..151V). It contains the first spectroscopic observations of RGB stars in Leo II, and remained the only kinematic data set for over a decade. The second study, by Koch et al. (2007, J/AJ/134/566, hereafter KK07), consists of radial velocities for 171 member stars. KK07 published average velocities taken during three epochs between 2003 and 2004. The third data set comes from Kirby et al. (2010, J/ApJS/191/352). They used Keck/DEIMOS to obtain medium resolution spectroscopy for the purpose of chemical abundance measurements, but also extracted radial velocities to help identify member stars. The fourth and final data set is published in Spencer et al. (2017, J/ApJ/836/202), which contains radial velocities for 175 member stars. Fifty of these have two or more observations, which were taken over the course of eight years with Hectochelle (Szentgyorgyi et al. 1998SPIE.3355..242S) on the Multiple Mirror Telescope. This data set contains five epochs between the years 2006 and 2013. (1 data file).

VizieR Online Data Catalog: KIC star parallaxes from asteroseismology vs Gaia (Huber+, 2017)

NASA Astrophysics Data System (ADS)

Huber, D.; Zinn, J.; Bojsen-Hansen, M.; Pinsonneault, M.; Sahlholdt, C.; Serenelli, A.; Aguirre, V. S.; Stassun, K.; Stello, D.; Tayar, J.; Bastien, F.; Bedding, T. R.; Buchhave, L. A.; Chaplin, W. J.; Davies, G. R.; Garcia, R. A.; Latham, D. W.; Mathur, S.; Mosser, B.; Sharma, S.

2018-03-01

Our sample consists of dwarfs, subgiants, and red giants from the APOGEE-Kepler Asteroseismic Science Consortium (APOKASC, Pinsonneault+ J/ApJS/215/19), supplemented with seismic detections using Kepler short-cadence data from Chaplin+ (2014MNRAS.445..946C) and Huber+ (2013, J/ApJ/767/127). (2 data files).

Synthesis, self-assembly, and drug-loading capacity of well-defined cyclodextrin-centered drug-conjugated amphiphilic A(14)B(7) Miktoarm star copolymers based on poly(epsilon-caprolactone) and poly(ethylene glycol).

PubMed

Gou, Peng-Fei; Zhu, Wei-Pu; Shen, Zhi-Quan

2010-04-12

Novel drug-conjugated amphiphilic A(14)B(7) miktoarm star copolymers composed of 14 poly(epsilon-caprolactone) (PCL) arms and 7 poly(ethylene glycol) (PEG) arms with beta-cyclodextrin (beta-CD) as core moiety were synthesized by the combination of controlled ring-opening polymerization (CROP) and "click" chemistry. (1)H NMR, FT-IR, and SEC-MALLS analyses confirmed the well-defined A(14)B(7) miktoarm star architecture. These amphiphilic miktoarm star copolymers could self-assemble into multimorphological aggregates in aqueous solution, which were characterized by dynamic light scattering (DLS) and transmission electron microscopy (TEM). Moreover, the drug-loading efficiency and drug-encapsulation efficiency of the drug-conjugated miktoarm star copolymers were higher than those of the corresponding non-drug-conjugated miktoarm star copolymers.

The Importance of Comprehensive Cam Correction: Radiographic Parameters Are Predictive of Patient-Reported Outcome Measures at 2 Years After Hip Arthroscopy.

PubMed

Lansdown, Drew A; Kunze, Kyle; Ukwuani, Gift; Waterman, Brian R; Nho, Shane J

2018-06-01

The specific influence of preoperative and postoperative radiographic measurements on patient-reported outcome measures after hip arthroscopy for femoroacetabular impingement (FAI) remains unclear. To investigate the relationship between radiographic measurements and 2-year outcomes after hip arthroscopy for the treatment of FAI. Case series; Level of evidence, 4. A clinical registry of patients undergoing primary hip arthroscopy for FAI between January 1, 2012, and December 31, 2014, was queried. Outcome measures included the Hip Outcome Score (HOS) Activities of Daily Living (ADL), HOS Sport-Specific Subscale (SSS), modified Harris Hip Score (mHHS), and visual analog scale (VAS) for pain and satisfaction. Preoperative and postoperative radiographic measurements were recorded. Univariate analysis was conducted to identify relationships between all radiographic and demographic variables and outcome scores. A multivariate regression analysis, controlling for demographic factors, was used to identify independent associations between radiographic measurements on plain radiographs and patient-reported outcomes. The authors identified 707 patients who underwent primary hip arthroscopic management for FAI who were included for analysis. Two-year outcome surveys were completed for 78% to 84% of patients. The mean age of the patients was 33.2 ± 12.3 years, and 64.4% of the patients (n = 456) were female. The mean anteroposterior (AP) alpha angle decreased by 34.3° ( P < .0001), false profile alpha angle by 25.2° ( P < .0001), Dunn lateral alpha angle by 28.9° ( P < .0001), lateral center edge angle by 2.6° ( P < .0001), and anterior center edge angle by 3.4° ( P < .0001). The HOS-ADL score increased from 65.7 ± 18.7 preoperatively to 85.9 ± 16.7 postoperatively ( P < .0001), HOS-SSS increased from 43.4 ± 23.1 to 72.6 ± 27.2 ( P < .0001), and mHHS increased from 57.7 ± 14.0 to 79.1 ± 17.2 ( P < .0001). With multivariate analysis, independent predictors of the postoperative HOS-ADL score included the preoperative false profile alpha angle (beta = -0.16, P = .028). Independent predictors of HOS-SSS score were preoperative AP alpha angle (beta = -0.33, P = .032) and preoperative false profile alpha angle (beta = -0.28, P = .041). For the postoperative mHHS score, independent predictors included preoperative AP alpha angle (beta = -0.18, P = .046), preoperative false profile alpha angle (beta = -0.20, P = .014), and postoperative false profile alpha angle (beta = -0.48, P = .035). The preoperative AP alpha angle (beta = 0.28, P = .024) was a significant predictor for the postoperative VAS pain score. The preoperative false profile alpha angle (beta = -0.34, P = .040) was a significant predictor for the postoperative VAS satisfaction score. The authors observed that radiographic measurements, specifically the preoperative false profile alpha angle, AP alpha angle, and postoperative false profile alpha angle, are independent predictors of 2-year clinical outcomes. The femoral-side measurements were the strongest independent predictors of outcomes, especially measurements of the anterior and lateral-based CAM lesion.

VizieR Online Data Catalog: Star-forming galaxies in near-IR (Martins+, 2013)

NASA Astrophysics Data System (ADS)

Martins, L. P.; Rodriguez-Ardila, A.; Diniz, S.; Riffel, R.; de Souza, R.

2014-10-01

The sample used here was presented in Martins et al. (2013MNRAS.431.1823M) and is a subset of the one presented in the magnitude-limited optical spectroscopic survey of nearby bright galaxies of Ho, Filippenko & Sargent (1995, Cat. J/ApJS/98/477, hereafter HO95). These galaxies are sources defined by Ho, Filippenko & Sargent (1997, Cat. J/ApJS/112/315, hereafter HO97) as those composed of 'nuclei dominated by emission lines from regions of active star formation (HII or starburst nuclei)'. In addition, five galaxies, classified as non-star forming in the optical, dominated by old stellar population and with no detected emission lines, were included as a control sample. All spectra were obtained at the NASA 3m Infrared Telescope Facility (IRTF) in two observing runs (2007 and 2008) - the same data from Martins et al. (2013MNRAS.431.1823M). (2 data files).

Very Wide Binaries

NASA Astrophysics Data System (ADS)

Olling, Robert; Shaya, E.

2011-01-01

We develop Bayesian statistical methods for discovering and assigning probabilities to physical stellar companions. The probabilities depend on similarities in "corrected" proper motion, parallax, and the phase-space density of field stars. Very wide binaries with separations over 10,000 AU have recently been predicted to form during the dissolution process of low-mass star clusters. In this case, these wide systems would still carry information about the density and size of the star cluster in which they formed. Alternatively, Galactic tides and weak interactions with passing stars peel off stars from such very wide binaries in less than 1/2 of a Hubble time. In the past, these systems have been used to rule in/out MACHOs or less compact dark (matter) objects. Ours is the first all-sky survey to locate escaped companions that are still drifting along with each other, long after their binary bond has been broken. We test stars for companionship up to an apparent separation of 8 parsec: 10 to 100 times wider than previous searches. Among Hipparcos stars within 100 pc, we find about 260 systems with separations between 0.01 and 1 pc, and another 190 with separation from 1 to 8 parsec. We find a number of previously unnoticed naked-eye companions, among which: Capella & 50 Per; Alioth, Megrez & Alcor; gamma & tau Cen; phi Eri & eta Hor; 62 & 63 Cnc; gamma & tau Per; zeta & delta Hya; beta01, beta02 & beta03 Tuc; 44 & 58 Oph and pi & rho Cep. At least 15 of our candidates are exoplanet host stars.

V and K-band Mass-Luminosity Relations for M dwarf Stars

NASA Astrophysics Data System (ADS)

Benedict, G. Fritz; Henry, Todd J.; McArthur, Barbara; Franz, Otto G.; Wasserman, Lawrence H.; Dieterich, Sergio

2015-01-01

Applying Hubble Space Telescope Fine Guidance Sensor astrometric techniques developed to establish relative orbits for binary stars (Franz et al. 1998, AJ, 116, 1432), determine masses of binary components (Benedict et al. 2001, AJ, 121, 1607), and measure companion masses of exoplanet host stars (McArthur et al. 2010, ApJ, 715, 1203), we derive masses with an average 2.1% error for 24 components of 12 M dwarf binary star systems. Masses range 0.08 to 0.40 solar masses. With these we update the lower Main Sequence V-band Mass-Luminosity Relation first shown in Henry et al. (1999, ApJ, 512, 864). We demonstrate that a Mass-Luminosity Relation in the K-band has far less scatter than in the V-band. For the eight binary components for which we have component magnitude differences in the K-band the RMS residual drops from 0.5 magnitude in the V-band to 0.05 magnitude in the K-band. These relations can be used to estimate the masses of the ubiquitous red dwarfs that account for 75% of all stars, to an accuracy of 5%, which is much better than ever before.

Opposite Smad and chicken ovalbumin upstream promoter transcription factor inputs in the regulation of the collagen VII gene promoter by transforming growth factor-beta.

PubMed

Calonge, María Julia; Seoane, Joan; Massagué, Joan

2004-05-28

A critical component of the epidermal basement membrane, collagen type VII, is produced by keratinocytes and fibroblasts, and its production is stimulated by the cytokine transforming growth factor-beta (TGF-beta). The gene, COL7A1, is activated by TGF-beta via Smad transcription factors in cooperation with AP1. Here we report a previously unsuspected level of complexity in this regulatory process. We provide evidence that TGF-beta may activate the COL7A1 promoter by two distinct inputs operating through a common region of the promoter. One input is provided by TGF-beta-induced Smad complexes via two Smad binding elements that function redundantly depending on the cell type. The second input is provided by relieving the COL7A1 promoter from chicken ovalbumin upstream promoter transcription factor (COUP-TF)-mediated transcriptional repression. We identified COUP-TFI and -TFII as factors that bind to the TGF-beta-responsive region of the COL7A1 promoter in an expression library screening. COUP-TFs bind to a site between the two Smad binding elements independently of Smad or AP1 and repress the basal and TGF-beta-stimulated activities of this promoter. We provide evidence that endogenous COUP-TF activity represses the COL7A1 promoter. Furthermore, we show that TGF-beta addition causes a rapid and profound down-regulation of COUP-TF expression in keratinocytes and fibroblasts. The results suggest that TGF-beta signaling may exert tight control over COL7A1 by offsetting the balance between opposing Smad and COUP-TFs.

VLA observations of A and B stars with kilogauss magnetic fields

NASA Technical Reports Server (NTRS)

Drake, S. A.; Abbott, D. C.; Linsky, J. L.; Bieging, J. H.; Churchwell, E.

1985-01-01

The serendipitous discovery that the star Sigma Ori E is a 3.5 mJy radio continuum source at 6 cm has stimulated a radio survey of other early-type stars with strong magnetic fields. No Ap stars have been detected of the eight observed, with typical 3-sigma upper limits of 0.5 mJy at 2 cm. Of the six Bp stars examined, only HR 1890, a helium-strong star, was detected. Possible emission mechanisms for the observed radio emission are discussed, and it is concluded that nonthermal emission seems the most plausible, on the basis of the present data.

The complex magnetic field topology of the cool Ap star 49 Cam

NASA Astrophysics Data System (ADS)

Silvester, J.; Kochukhov, O.; Rusomarov, N.; Wade, G. A.

2017-10-01

49 Cam is a cool magnetic chemically peculiar star that has been noted for showing strong, complex Zeeman linear polarization signatures. This paper describes magnetic and chemical surface maps obtained for 49 Cam using the Invers10 magnetic Doppler imaging code and high-resolution spectropolarimetric data in all four Stokes parameters collected with the ESPaDOnS and Narval spectropolarimeters at the Canada-France-Hawaii Telescope and Pic du Midi Observatory. The reconstructed magnetic field maps of 49 Cam show a relatively complex structure. Describing the magnetic field topology in terms of spherical harmonics, we find significant contributions of modes up to ℓ = 3, including toroidal components. Observations cannot be reproduced using a simple low-order multipolar magnetic field structure. 49 Cam exhibits a level of field complexity that has not been seen in magnetic maps of other cool Ap stars. Hence, we concluded that relatively complex magnetic fields are observed in Ap stars at both low and high effective temperatures. In addition to mapping the magnetic field, we also derive surface abundance distributions of nine chemical elements, including Ca, Sc, Ti, Cr, Fe, Ce, Pr, Nd and Eu. Comparing these abundance maps with the reconstructed magnetic field geometry, we find no clear relationship of the abundance distributions with the magnetic field for some elements. However, for other elements some distinct patterns are found. We discuss these results in the context of other recent magnetic mapping studies and theoretical predictions of radiative diffusion.

Spectral Irradiance Calibration in the Infrared. 4; 1.2-35um Spectra of Six Standard Stars

NASA Technical Reports Server (NTRS)

Cohen, Martin; Witteborn, Fred C.; Walker, Russell G.; Bregman, Jesse D.; Wooden, Diane H.

1995-01-01

We present five new absolutely calibrated continuous stellar spectra from 1.2 to 35 microns, constructed as far as possible from actual observed spectral fragments taken from the ground, the Kuiper Airborne Observatory (KAO), and the IRAS Low Resolution Spectrometer (LRS). These stars, Beta Peg, Delta Boo, Beta And, Beta Gem, and Delta Hya, augment our already created complete absolutely calibrated spectrum for a Tau. All these spectra have a common calibration pedigree. The wavelength coverage is ideal for calibration of many existing and proposed ground-based, airborne, and satellite sensors.

Spectral Irradiance Calibration in the Infrared. Part 4; 1.2 - 35 microns Spectra of Six Standard Stars

NASA Technical Reports Server (NTRS)

Cohen, Martin; Witteborn, Fred C.; Walker, Russell G.; Bregman, Jesse D.; Wooden, Diane H.

1995-01-01

We present five new absolutely calibrated continuous stellar spectra from 1.2 to 35 microns, constructed as far as possible from actual observed spectral fragments taken from the ground, the Kuiper Airborne Observatory (KAO), and the IRAS Low Resolution Spectrometer (LRS). These stars- beta Peg, alpha Boo, beta And, beta Gem, and alpha Hya-augment our already created complete absolutely calibrated spectrum for alpha Tau. All these spectra have a common calibration pedigree. The wavelength coverage is ideal for calibration of many existing and proposed ground-based, airborne, and satellite sensors.

ASTE Surveys of Galactic Star-Forming Regions

NASA Astrophysics Data System (ADS)

Kohno, Kotaro

2008-05-01

We report some recent highlights on the observational studies of Galactic star formation based on surveys using the Atacama Submillimeter Telescope Experiment (ASTE), a new 10 m telescope in the Atacama desert in northern Chile (Kohno et al., 2008, ApSS, 313, 279). The highlights will include (1) a large scale CO(3-2) imaging survey of the Galactic Center, unveiling the presence of numerous compact high velocity clouds with high CO(3-2)/CO(1-0) ratios as a "fossil” of the recent burst of star formation in the Galactic Center region (Oka et al., 2007, PASJ, 59, 15; Nagai et al., 2007, PASJ, 59, 25; Tanaka et al., 2007, PASJ, 59, 323), (2) a large scale CO(3-2) imaging survey of the Sgr arm and inter-am regions, revealing the distinct difference on the morphology and physical property of molecular gas between the arm and inter-arm regions for the first time (Sawada, Koda, et al., in prep.), and (3) a wide area 1.1 mm imaging survey of Southern low mass star-forming regions such as Chamaeleon and Lupus molecular clouds using the bolometer camera AzTEC (Wilson et al., 2008, MNRAS, in press) mounted on ASTE, yielding detections of starless cores with a very low mass detection limist down to 0.1 solar masses (Hiramatsu, Tsukagoshi, Kawabe et al., in prep.). Related topics on the massive star-forming regions in very nearby galaxies such as LMC (Minamidani et al., 2008, ApJS, in press) and M 33 (Tosaki et al., 2007, ApJ, 664, L27; Onodera et al., in prep.; Komugi et al., in prep.) will also be reviewed.

Vector space methods of photometric analysis. II - Refinement of the MK grid for B stars. III - The two components of ultraviolet reddening

NASA Technical Reports Server (NTRS)

Massa, D.

1980-01-01

This paper discusses systematic errors which arise from exclusive use of the MK system to determine reddening. It is found that implementation of uvby, beta photometry to refine the qualitative MK grid substantially reduces stellar mismatch error. A working definition of 'identical' ubvy, beta types is investigated and the relationship of uvby to B-V color excesses is determined. A comparison is also made of the hydrogen based uvby, beta types with the MK system based on He and metal lines. A small core correlated effective temperature luminosity error in the MK system for the early B stars is observed along with a breakdown of the MK luminosity criteria for the late B stars. The second part investigates the wavelength dependence of interstellar extinction in the ultraviolet wavelength range observed with the TD-1 satellite. In this study the sets of identical stars employed to find reddening are determined more precisely than in previous studies and consist only of normal, nonsupergiant stars. A multivariate analysis of variance techniques in an unbiased coordinate system is used for determining the wavelength dependence of reddening.

VizieR Online Data Catalog: Spectroscopically Identified Hot Subdwarf Stars (Kilkenny+ 1988)

NASA Astrophysics Data System (ADS)

Kilkenny, D.; Heber, U.; Drilling, J. S.

1996-05-01

Prior to 1986 there were around 200 spectroscopically classified hot subdwarf stars. The Palomar-Green survey (Green et al., 1986ApJS...61..305G) detected over 900 hot subdwarfs, mostly in the North Galactic Cap and mostly previously unknown objects; the Kitt-Peak_Downes survey found another 60 near the Galactic Plane (Downes, 1986ApJS...61..569D). These form the basis of the present catalog but new subdwarfs are continually being found by spectroscopic surveys of photographically discovered faint blue star samples; examples are the work of Wegner and his co-workers on the Kiso survey (Wegner et al., 1985AJ.....90.1511W, 1986AJ.....91..139W, 1987AJ.....94.1271W) and of Kilkenny and Muller (1987) on southern discoveries by Luyten and collaborators (e.g. Haro and Luyten, 1962, Cat. III/74; Luyten and Anderson, 1958, 1959, 1967, "A Search for Faint Blue Stars"). Only stars for which a spectroscopic classification exists have been included. There is a significant probability that stars with only photometric classifications can be normal high-latitude B stars, white dwarfs or cataclysmic variable, for example. Hot subdwarfs in binary systems have been included but not planetary nebulae nuclei classified 'sd' since the latter have been catalogued elsewhere. Although there is not a universally accepted classification scheme for hot subdwarfs, it is fairly clear that the main criterion is a surface gravity higher than that of hot main sequence stars but less than that of hot white dwarfs. Also, hot subdwarf stars typically show helium abundance anomalies. (3 data files).

Independet Component Analyses of Ground-based Exoplanetary Transits

NASA Astrophysics Data System (ADS)

Silva Martins-Filho, Walter; Griffith, Caitlin Ann; Pearson, Kyle; Waldmann, Ingo; Biddle, Lauren; Zellem, Robert Thomas; Alvarez-Candal, Alvaro

2016-10-01

Most observations of exoplanetary atmospheres are conducted when a "Hot Jupiter" exoplanet transits in front of its host star. These Jovian-sized planets have small orbital periods, on the order of days, and therefore a short transit time, making them more ameanable to observations. Measurements of Hot Jupiter transits must achieve a 10-4 level of accuracy in the flux to determine the spectral modulations of the exoplanetary atmosphere. In order to accomplish this level of precision, we need to extract systematic errors, and, for ground-based measurements, the effects of Earth's atmosphere, from the signal due to the exoplanet, which is several orders of magnitudes smaller. Currently, the effects of the terrestrial atmosphere and the some of the time-dependent systematic errors are treated by dividing the host star by a reference star at each wavelength and time step of the transit. More recently, Independent Component Analyses (ICA) have been used to remove systematic effects from the raw data of space-based observations (Waldmann 2014,2012; Morello et al.,2015,2016). ICA is a statistical method born from the ideas of the blind-source separation studies, which can be used to de-trend several independent source signals of a data set (Hyvarinen and Oja, 2000). One strength of this method is that it requires no additional prior knowledge of the system. Here, we present a study of the application of ICA to ground-based transit observations of extrasolar planets, which are affected by Earth's atmosphere. We analyze photometric data of two extrasolar planets, WASP-1b and GJ3470b, recorded by the 61" Kuiper Telescope at Stewart Observatory using the Harris B and U filters. The presentation will compare the light curve depths and their dispersions as derived from the ICA analysis to those derived by analyses that ratio of the host star to nearby reference stars.References: Waldmann, I.P. 2012 ApJ, 747, 12, Waldamann, I. P. 2014 ApJ, 780, 23; Morello G. 2015 ApJ, 806; Morello et al. 2016 ApJ, 820, 86; Hyvarinen, A., and Oja, E. 2000 IEEE Transactions on Neural Networks, 13, 411.

VizieR Online Data Catalog: NuSTAR hard X-ray survey of the Galactic Center. II. (Hong+, 2016)

NASA Astrophysics Data System (ADS)

Hong, J.; Mori, K.; Hailey, C. J.; Nynka, M.; Zhang, S.; Gotthelf, E.; Fornasini, F. M.; Krivonos, R.; Bauer, F.; Perez, K.; Tomsick, J. A.; Bodaghee, A.; Chiu, J.-L.; Clavel, M.; Stern, D.; Grindlay, J. E.; Alexander, D. M.; Aramaki, T.; Baganoff, F. K.; Barret, D.; Barriere, N.; Boggs, S. E.; Canipe, A. M.; Christensen, F. E.; Craig, W. W.; Desai, M. A.; Forster, K.; Giommi, P.; Grefenstette, B. W.; Harrison, F. A.; Hong, D.; Hornstrup, A.; Kitaguchi, T.; Koglin, J. E.; Madsen, K. K.; Mao, P. H.; Miyasaka, H.; Perri, M.; Pivovaroff, M. J.; Puccetti, S.; Rana, V.; Westergaard, N. J.; Zhang, W. W.; Zoglauer, A.

2018-02-01

Observations of the GC region with NuSTAR began in 2012 July, shortly after launch. The original survey strategy for the GC region was to match the central 2°x0.7° region covered by the Chandra X-ray Observatory (Wang et al. 2002Natur.415..148W; Muno et al. 2009, J/ApJS/181/110). The field of views (FOVs) of neighboring NuSTAR observations in the survey were designed to overlap with each other by ~40%. Multiple observations of the same region with relatively large FOV offsets tend to average out the vignetting effects of each observation, enabling a more uniform coverage of the region. Multiple observations are also suitable for monitoring long term X-ray variability of sources in the region. Even when observing a single target, the NuSTAR observation is often broken up into two or more segments with relatively large pointing offsets to allow an efficient subtraction of a detector coordinate-dependent background component (e.g., Mori et al. 2013ApJ...770L..23M). (4 data files).

Erratum: ``A Low-Latitude Halo Stream around the Milky Way'' (ApJ, 588, 824 [2003])

NASA Astrophysics Data System (ADS)

Yanny, Brian; Newberg, Heidi Jo; Grebel, Eva K.; Kent, Steve; Odenkirchen, Michael; Rockosi, Connie M.; Schlegel, David; Subbarao, Mark; Brinkmann, Jon; Fukugita, Masataka; Ivezic, Željko; Lamb, Don Q.; Schneider, Donald P.; York, Donald G.

2004-04-01

The zero points of the stellar templates used to measure radial velocity in the main body of this paper have been found to be systematically in error. Correction of the radial velocities significantly increases the derived circular velocity of the stars in the planar stream, to 215+/-25 km s-1. The velocity dispersion of the stream is somewhat lower than earlier results with the modified analysis. Two types of stars were studied in this paper. The original template for stars of type F, used to study the ``Monoceros arc'' Galactic structure, was incorrectly zero-pointed by 20 km s-1. The original template for stars of type A, used to measure the Sagittarius dwarf tidal stream, produced radial velocities systematically shifted by 49 km s-1. In both cases, the sign of the error is such that for nearly all stars, the correct values of the heliocentric radial velocities are lower than those originally quoted. A cross-correlation of Sloan Digital Sky Survey (SDSS) spectra with templates from the ELODIE survey (C. Soubiran, D. Katz, & R. Cayrel, ApJ, 588, 824 [2003]) was performed to find new radial velocities for each star (D. Schlegel 2003, private communication). This showed that our radial velocities were systematically shifted by an amount that depends on the type of the star observed and the original template against which it was cross-correlated. To determine the measurement error with the new templates, we identified 445 F-type stars and 1109 A-type stars that had been observed twice by the SDSS. These stars were chosen with the color and magnitude criteria used to select stars in Figures 6 and 9. The errors in the F stars were a good match to a Gaussian with a σ of 28 km s-1. The errors in the A star comparison were significantly non-Gaussian, with large tails. A χ2 fit to a Gaussian (similar to the technique we use in this paper to measure the width of the streams) yielded a σ of 35 km s-1. Dividing by sqrt(2) to reflect two independent measurements, we derive a random error of 20 km s-1 for F stars and 25 km s-1 for A stars. The template matching errors in these blue (type A) stars using ELODIE spectral templates are somewhat larger than the errors with our previous analysis, but we found it useful to use ELODIE spectral templates to ensure that the zero points were accurate. We also examined the measured stellar stream dispersions. Electronic versions of Figures 2, 6, and 9 of our paper are presented here with the corrected radial velocity determinations. The data were selected as described in the original paper. Table 1 has been regenerated in its entirety, replacing columns (8) and (10). The radial velocity in column (8) has been replaced with the radial velocity determined from cross-correlation with ELODIE templates. The status flag in column (10) now indicates stars which were used to generate Figure 2. A ``0'' indicates that the star was either outside the color box or had a high cross-correlation error, and a ``1'' indicates that the star was used to fit stream properties. Table 2 has been regenerated using the new results as well. Column (10) has been added to indicate the estimated number of spectra in the stream component. These numbers are used to compute the error in radial velocity, as described in the original paper. Column (11) shows the corrected circulation velocities, which are now consistent with those given in J. D. Crane, S. R. Majewski, H. J. Rocha-Pinto, P. M. Frinchaboy, M. F. Skrutskie, & D. R. Law (ApJ, 588, 824 [2003]). Note that the velocity dispersions of the planar stream are even tighter than originally measured, strengthening the case that the motion is coherent. Note that the mean velocity of the Sagittarius stream in the direction (l,b)=(165deg,-55deg) is -160 km s-1, in line with recent simulations by D. Martinez-Delgado, M. A. Gomez-Flechoso, A. Aparicio, & R. Carrera (2004, ApJ, in press [astro-ph/0308009]). We would like to acknowledge Steve Majewski, who initially pointed out to us that radial velocities for stars he had measured in the halo streams were different from our radial velocities by 20-50 km s-1 (J. D. Crane, S. R. Majewski, H. J. Rocha-Pinto, P. M. Frinchaboy, M. F. Skrutskie, & D. R. Law, ApJ, 588, 824 [2003]). We also acknowledge T. Beers, C. Prieto, and R. Wilhelm for an independent radial velocity analysis, with which we could compare our measured radial velocities.

EVOLUTION OF INTERMEDIATE-MASS X-RAY BINARIES DRIVEN BY THE MAGNETIC BRAKING OF AP/BP STARS. I. ULTRACOMPACT X-RAY BINARIES

DOE Office of Scientific and Technical Information (OSTI.GOV)

Chen, Wen-Cong; Podsiadlowski, Philipp, E-mail: chenwc@pku.edu.cn

2016-10-20

It is generally believed that ultracompact X-ray binaries (UCXBs) evolved from binaries consisting of a neutron star accreting from a low-mass white dwarf (WD) or helium star where mass transfer is driven by gravitational radiation. However, the standard WD evolutionary channel cannot produce the relatively long-period (40–60 minutes) UCXBs with a high time-averaged mass-transfer rate. In this work, we explore an alternative evolutionary route toward UCXBs, where the companions evolve from intermediate-mass Ap/Bp stars with an anomalously strong magnetic field (100–10,000 G). Including the magnetic braking caused by the coupling between the magnetic field and an irradiation-driven wind induced bymore » the X-ray flux from the accreting component, we show that intermediate-mass X-ray binaries (IMXBs) can evolve into UCXBs. Using the MESA code, we have calculated evolutionary sequences for a large number of IMXBs. The simulated results indicate that, for a small wind-driving efficiency f = 10{sup −5}, the anomalous magnetic braking can drive IMXBs to an ultra-short period of 11 minutes. Comparing our simulated results with the observed parameters of 15 identified UCXBs, the anomalous magnetic braking evolutionary channel can account for the formation of seven and eight sources with f = 10{sup −3}, and 10{sup −5}, respectively. In particular, a relatively large value of f can fit three of the long-period, persistent sources with a high mass-transfer rate. Though the proportion of Ap/Bp stars in intermediate-mass stars is only 5%, the lifetime of the UCXB phase is ≳2 Gyr, producing a relatively high number of observable systems, making this an alternative evolutionary channel for the formation of UCXBs.« less

Tracking the Obscured Star Formation Along the Complete Evolutionary Merger Sequence of LIRGs

NASA Astrophysics Data System (ADS)

Diaz-Santos, Tanio

2014-10-01

We propose to obtain WFC3 narrow-band Pa-beta imaging of a sample of 24 nearby luminous infrared (IR) galaxies (LIRGs) from the Great Observatories All-sky LIRG survey (GOALS) selected to be in advanced stages of interaction. LIRGs account for half of the obscured star formation of the Universe at z ~ 1-2, and they represent a key population in galaxy formation and evolution. We will use the Pa-beta images to trace the ionized gas in LIRGs and study its spatial distribution from scales of ~ 100 pc to up to several kpc, probing the youngest, massive stars formed in the most buried environments of LIRGs due to the interaction process. This will allow us to measure how the gas in the center of mergers is converted into stars, which eventually leads to the build-up of a nuclear stellar cusp and the "inside-out" growth of bulges. We will also create spatially-resolved Pa-beta equivalent width maps to search for age gradients across the galaxies and correlate the distribution of Pa-beta emission with that of un-obscured star clusters detected in the UV and optical with HST on the same spatial scales. Finally, we will combine our data with previous studies mainly focused on isolated and early-stage interacting LIRG systems to analyze the size and compactness of the starburst along the complete merger sequence of LIRGs. The requested data represent a critical missing piece of information that will allow us to understand both the physics of merger-induced star formation and the applicability of local LIRGs as templates for high-z interacting starburst galaxies.

LYNX: A Linked Eulerian and Lagrangian Code. Volume II. LYNX Computer Listing

DTIC Science & Technology

1975-11-01

177« 178« 179» ISO* 18|» 182« 183» IBM * 185* 1B6« 187» 198« 189« 190« |f|i 192» 193« 194» 195» 196« 197» 198» 199* 200» 201...XPLC ID) ,Y(JD) ,TAUI ID) ,YB(IJD) .FBI IJD) ,T 1 3B ( ID ) • XCT I IJD) »VOBUjD» ,ZZ(NN0IM) ,VV(NND1M) »OBFUL •BETA tAP •OTCP iTP ...CELL CONTAINING PARTICLE NO I. •OB IOUFUL •BETA »AP •UTCP iTP •COMPEN ,SHEN •YP1 »YP2 •KMAX ,KBAR • 1JMA< ,IK»UX

Diadenosine tetraphosphate-gating of recombinant pancreatic ATP-sensitive K(+) channels.

PubMed

Jovanovic, S; Jovanovic, A

2001-02-01

Diadenosine tetraphosphate (Ap4A) has been recently discovered in the pancreatic beta cells where targets ATP-sensitive K(+) (K(ATP)) channels, depolarizes the cell membrane and induces insulin secretion. However, whether Ap4A inhibit pancreatic K(ATP) channels by targeting protein channel complex itself was unknown. Therefore, we coexpressed pancreatic K(ATP) channel subunits, Kir6.2 and SUR1, in COS-7 cells and examined the effect of Ap4A on the single channel behavior using the inside-out configuration of the patch-clamp technique. Ap4A inhibited channel opening in a concentration-dependent manner. Analysis of single channels demonstrated that Ap4A did not change intraburst kinetic behavior of K(ATP) channels, but rather decreased burst duration and increased between-burst duration. It is concluded that Ap4A antagonizes K(ATP) channel opening by targeting channel subunits themselves and by keeping channels longer in closed interburst states.

Preparation, crystallization and preliminary X-ray crystallographic studies of diadenosine tetraphosphate hydrolase from Shigella flexneri 2a.

PubMed

Hu, Wenxin; Wang, Qihai; Bi, Ruchang

2005-12-01

Diadenosine tetraphosphate (Ap4A) hydrolase (EC 3.6.1.41) hydrolyzes Ap4A symmetrically in prokaryotes. It plays a potential role in organisms by regulating the concentration of Ap4A in vivo. To date, no three-dimensional structures of proteins with significant sequence homology to this protein have been determined. The 31.3 kDa Ap4A hydrolase from Shigella flexneri 2a has been cloned, expressed and purified using an Escherichia coli expression system. Crystals of Ap4A hydrolase have been obtained by the hanging-drop technique at 291 K using PEG 550 MME as precipitant. Ap4A hydrolase crystals diffract X-rays to 3.26 A and belong to space group P2(1), with unit-cell parameters a = 118.9, b = 54.6, c = 128.5 A, beta = 95.7 degrees.

A search for strong, ordered magnetic fields in Herbig Ae/Be stars

NASA Astrophysics Data System (ADS)

Wade, G. A.; Bagnulo, S.; Drouin, D.; Landstreet, J. D.; Monin, D.

2007-04-01

The origin of magnetic fields in intermediate- and high-mass stars is fundamentally a mystery. Clues towards solving this basic astrophysical problem can likely be found at the pre-main-sequence (PMS) evolutionary stage. With this work, we perform the largest and most sensitive search for magnetic fields in PMS Herbig Ae/Be (HAeBe) stars. We seek to determine whether strong, ordered magnetic fields, similar to those of main-sequence Ap/Bp stars, can be detected in these objects, and if so, to determine the intensities, geometrical characteristics, and statistical incidence of such fields. 68 observations of 50 HAeBe stars have been obtained in circularly polarized light using the FORS1 spectropolarimeter at the ESO VLT. An analysis of both Balmer and metallic lines reveals the possible presence of weak longitudinal magnetic fields in photospheric lines of two HAeBe stars, HD 101412 and BF Ori. Results for two additional stars, CPD-53 295 and HD 36112, are suggestive of the presence of magnetic fields, but no firm conclusions can be drawn based on the available data. The intensity of the longitudinal fields detected in HD 101412 and BF Ori suggest that they correspond to globally ordered magnetic fields with surface intensities of order 1 kG. On the other hand, no magnetic field is detected in 4 other HAeBe stars in our sample in which magnetic fields had previously been confirmed. Monte Carlo simulations of the longitudinal field measurements of the undetected stars allow us to place an upper limit of about 300 G on the general presence of aligned magnetic dipole magnetic fields, and of about 500 G on perpendicular dipole fields. Taking into account the results of our survey and other published results, we find that the observed bulk incidence of magnetic HAeBe stars in our sample is 8-12 per cent, in good agreement with that of magnetic main-sequence stars of similar masses. We also find that the rms longitudinal field intensity of magnetically detected HAeBe stars is about 200 G, similar to that of Ap stars and consistent with magnetic flux conservation during stellar evolution. These results are all in agreement with the hypothesis that the magnetic fields of main-sequence Ap/Bp stars are fossils, which already exist within the stars at the PMS stage. Finally, we explore the ability of our new magnetic data to constrain magnetospheric accretion in Herbig Ae/Be stars, showing that our magnetic data are not consistent with the general occurrence in HAeBe stars of magnetospheric accretion as described by the theories of Königl and Shu et al.. Based on observations from the ESO telescopes at the La Silla Paranal Observatory under programme ID 072.C-0447, DDT-272.C-5063, 074.C-0442. E-mail: wade-g@rmc.ca

VizieR Online Data Catalog: Spitzer h and {chi} Persei candidate members (Cloutier+, 2014)

NASA Astrophysics Data System (ADS)

Cloutier, R.; Currie, T.; Rieke, G. H.; Kenyon, S. J.; Balog, Z.; Jayawardhana, R.

2017-08-01

The IRAC (Fazio et al. 2004ApJS..154...39F) observed h and {chi} Persei on October 30, 2008 (AOR IDs 2182740, 21828608, 21828096, 21828864, 21828352, and 2182912). Solar activity was normal to below average. Zodical emission ranged between ~0.02 and 2 MJy/sr from 3.6 um to 8 um. Image processing and photometry were performed separately for the short-exposure and long-exposure frames. The MIPS (Rieke et al. 2004ApJS..154...25R) imaged h and {chi} Persei on 2008 March 15-16, 2008 October 25-26, and 2009 March 26 and 29 as a part of General Observation Programs 40690 and 50664 (PI: Scott Kenyon). To identify and characterize disks surrounding h and {chi} Persei stars, we combine Spitzer data with optical/near-IR data for likely cluster members, updating the list from Currie et al. (2010, J/ApJS/186/191) with a more accurate one of 13956 stars (Table 1). (3 data files).

Pulsation in the presence of a strong magnetic field: the roAp star HD166473

NASA Astrophysics Data System (ADS)

Mathys, G.; Kurtz, D. W.; Elkin, V. G.

2007-09-01

Phase-resolved high-resolution, high signal-to-noise ratio (S/N) observations of the strongly magnetic roAp star HD166473 are analysed. HD166473 was selected as the target of this study because it has one of the strongest magnetic fields of all the roAp stars known with resolved magnetically split lines. Indeed, we show that enhanced pulsation diagnosis can be achieved from consideration of the different pulsation behaviour of the π and σ Zeeman components of the resolved spectral lines. This study is based on a time-series of high spectral resolution observations obtained with the Ultraviolet and Visual Echelle Spectrograph of the Very Large Telescope of the European Southern Observatory. Radial velocity variations due to pulsation are observed in rare earth lines, with amplitudes up to 110ms-1. The variations occur with three frequencies, already detected in photometry, but which can in this work be determined with better precision: 1.833, 1.886 and 1.928mHz. The pulsation amplitudes and phases observed in the rare earth element lines vary with atmospheric height, as is the case in other roAp stars studied in detail. Lines of Fe and of other (mostly non-rare earth) elements do not show any variation to very high precision (1.5ms-1 in the case of Fe). The low amplitudes of the observed variations do not allow the original goal of studying differences between the behaviour of the resolved Zeeman line components to be reached; the S/N achieved in the radial velocity determinations is insufficient to establish definitely the possible existence of such differences. Yet the analysis provides a tantalizing hint at the occurrence of variations of the mean magnetic field modulus with the pulsation frequency, with an amplitude of 21 +/- 5G. Based on observations collected at the European Southern Observatory, Paranal, Chile, as part of programme 067.D-0272. E-mail: gmathys@eso.org

Multiperiodicity in the Light Variations of the Beta Cephei Star Beta Crucis

NASA Technical Reports Server (NTRS)

Cuypers, J.; Aerts, C.; Buzasi, D.; Catanzarite, J.; Conrow, T.; Laher, R.

2002-01-01

High-resolution spectroscopic observations have led recently to the discovery that the P Cephei star Beta Crucis (Mimosa) is multiperiodic with at least three non-radial pulsation modes. Data obtained by the star tracker of the WIRE satellite have now allowed us to confirm this multiperiodicity in the light variations. A total of five million observations covering 17 days was analyzed and the three main periods we find in this work are in perfect agreement with the results derived from the line profile variations. The photometric amplitudes are small (3, 2.7 and 0.6 millimag for the dominant modes), but this is not surprising in view of the mode identifications derived earlier from the line profiles. Additional periods of low-amplitude modes (between 0.2-0.3 mmag) are also derived, including one suggested earlier by the radial velocity data.

Uranium lines in the spectra of peculiar A stars - A search for recent r-process events

NASA Technical Reports Server (NTRS)

Cowley, C. R.; Adelman, S. J.

1975-01-01

Uranium wavelengths in the spectra of Ap stars are studied to see if they give any indication of a recent r-process event. It is concluded that there is no credible evidence for an admixture of uranium-235 in these stars, which would imply such an event. The evidence, though negative, is badly confused by blending of lines, and a final judgement must wait for an observational clarification of the situation.

NEW MEMBERS OF THE SCORPIUS-CENTAURUS COMPLEX AND AGES OF ITS SUB-REGIONS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Song, Inseok; Zuckerman, B.; Bessell, M. S.

2012-07-15

We have spectroscopically identified {approx}100 G-, K-, and M-type members of the Scorpius-Centaurus complex. To deduce the age of these young stars we compare their Li {lambda}6708 absorption line strengths against those of stars in the TW Hydrae association and {beta} Pictoris moving group. These line strengths indicate that Sco-Cen stars are younger than {beta} Pic stars whose ages of {approx}12 Myr have previously been derived from a kinematic traceback analysis. Our derived age, {approx}10 Myr, for stars in the Lower Centaurus Crux and Upper Centaurus Lupus subgroups of ScoCen is younger than previously published ages based on the movingmore » cluster method and upper main-sequence fitting. The discrepant ages are likely due to an incorrect (or lack of) cross-calibration between model-dependent and model-independent age-dating methods.« less

Spectral Irradiance Calibration in the Infrared. Part 4; 1.2-35 micrometer Spectra of Six Standard Stars

NASA Technical Reports Server (NTRS)

Cohen, Martin; Witteborn, Fred C.; Walker, Russell, G.; Bregman, Jesse D.; Wooden, Diane H.

1995-01-01

Five new absolutely calibrated continuous stellar spectra from 1.2 to 35 microns are presented. The spectra were constructed as far as possible from actual observed spectral fragments taken from the ground, the Kuiper Airborne Observatory (KAO), and the IRAS Low Resolution Spectrometer (LRS). These stars (beta Peg, alpha Boo, beta And, beta Gem, and alpha Hya) augment the author's already created complete absolutely calibrated spectrum for alpha Tau. All these spectra have a common calibration pedigree. The wavelength coverage is ideal for calibration of many existing and proposed ground-based, airborne, and satellite sensors.

Calibration of H-alpha/H-beta Indexes for Emission Line Objects

NASA Astrophysics Data System (ADS)

Hintz, Eric G.; Joner, Michael D.

2016-01-01

In Joner and Hintz (2015) they report on a standard star system for calibration of H-alpha and H-beta observations. This work was based on data obtained with the Dominion Astrophysical Observatory 1.2-m telescope. As part of the data acquisition for that project, a large number of emission line objects were also observed. We will report on the preliminary results for the emission line data set. This will include a comparison of equivalent width measurements of each line with the matching index. We will also examine the relation between the absorption line objects previously published and the emission line objects, along with a discussion of the transition point. Object types included are Be stars, high mass x-ray binaries, one low mass x-ray binary, Herbig Ae/Be stars, pre-main sequence stars, T Tauri stars, young stellar objects, and one BY Draconis star. Some of these objects come from Cygnus OB-2, NGC 659, NGC 663, NGC 869 and NGC 884.

Star formation induced by cloud-cloud collisions and galactic giant molecular cloud evolution

NASA Astrophysics Data System (ADS)

Kobayashi, Masato I. N.; Kobayashi, Hiroshi; Inutsuka, Shu-ichiro; Fukui, Yasuo

2018-05-01

Recent millimeter/submillimeter observations towards nearby galaxies have started to map the whole disk and to identify giant molecular clouds (GMCs) even in the regions between galactic spiral structures. Observed variations of GMC mass functions in different galactic environments indicates that massive GMCs preferentially reside along galactic spiral structures whereas inter-arm regions have many small GMCs. Based on the phase transition dynamics from magnetized warm neutral medium to molecular clouds, Kobayashi et al. (2017, ApJ, 836, 175) proposes a semi-analytical evolutionary description for GMC mass functions including a cloud-cloud collision (CCC) process. Their results show that CCC is less dominant in shaping the mass function of GMCs than the accretion of dense H I gas driven by the propagation of supersonic shock waves. However, their formulation does not take into account the possible enhancement of star formation by CCC. Millimeter/submillimeter observations within the Milky Way indicate the importance of CCC in the formation of star clusters and massive stars. In this article, we reformulate the time-evolution equation largely modified from Kobayashi et al. (2017, ApJ, 836, 175) so that we additionally compute star formation subsequently taking place in CCC clouds. Our results suggest that, although CCC events between smaller clouds are more frequent than the ones between massive GMCs, CCC-driven star formation is mostly driven by massive GMCs ≳ 10^{5.5} M_{⊙} (where M⊙ is the solar mass). The resultant cumulative CCC-driven star formation may amount to a few 10 percent of the total star formation in the Milky Way and nearby galaxies.

Organic Molecules and Water in the Inner Disks of T Tauri Stars

DTIC Science & Technology

2011-05-11

603 Knez, C., et al. 2007, BAAS , 211, 5005 Kruger, A. J., Richter, M. J., Carr, J. S., Najita, J. R., Doppmann, G. W., & Seifahrt, A. 2011, ApJ, 729...Close, L. M., Hinz, P. M., Hoffmann, W. F., Greene, T. P., Males, J. R., & Beck , T. L. 2010, ApJ, 711, 1280 Tappe, A., Lada, C. J., Black, J. H

Large-scale Organized Magnetic Fields in O, B and A Stars

NASA Astrophysics Data System (ADS)

Mathys, G.

2009-06-01

The status of our current knowledge of magnetic fields in stars of spectral types ranging from early F to O is reviewed. Fields with large-scale organised structure have now been detected and measured throughout this range. These fields are consistent with the oblique rotator model. In early F to late B stars, their occurrence is restricted to the subgroup of the Ap stars, which have the best studied fields among the early-type stars. Presence of fields with more complex topologies in other A and late B stars has been suggested, but is not firmly established. Magnetic fields have not been studied in a sufficient number of OB stars yet so as to establish whether they occur in all or only in some subset of these stars.

Abundance analysis of roAp stars. IV. HD24712

NASA Astrophysics Data System (ADS)

Ryabchikova, T. A.; Landstreet, J. D.; Gelbmann, M. J.; Bolgova, G. T.; Tsymbal, V. V.; Weiss, W. W.

1997-11-01

We present the first abundance analysis of the rapidly oscillating chemically peculiar star HD24712, and determine a T_eff,=7250K, log {g},=4.3, and xi_t ,=1kms(-1) . Microturbulence seems to be entirely simulated by a magnetic field with a polar field strength of 4.4kG and of dipolar structure, both of which are supported by our polarimetric observations. Rotation of HD24712 and a spotty surface distribution of the elements result in different mean abundances for different (magnetic) phases. Our results do not support the hypothesis of a monotonic correlation between the amplitude of abundance variations and the atomic number Z, and we present arguments in favour of one of the rotation periods (Prot=12\\fd 4610) discussed in the literature. Rare earth elements are the most overabundant elements relative to the sun, and they have the largest abundance amplitude during a rotation cycle; only Mg has a larger amplitude. For HD24712 we find a clear overabundance of Co while most of the other iron peak elements are underabundant. A comparison of the abundance pattern with the other three roAp stars analyzed so far by us concludes the paper. A systematic difference between surface gravities obtained from spectroscopy and from both asteroseismology and evolutionary tracks is found for the roAp stars HD 24712, alpha Cir, and gamma Equ. Based on observations obtained with the Canada-France-Hawaii telescope, operated by the National Research Council of Canada, the Centre Centre National de la Recherche Scientifique de France, and the University of Hawaii, and on observations obtained at CARSO, Las Campanas, Chile

SEARCHING FOR YOUNG JUPITER ANALOGS AROUND AP COL: L-BAND HIGH-CONTRAST IMAGING OF THE CLOSEST PRE-MAIN-SEQUENCE STAR

DOE Office of Scientific and Technical Information (OSTI.GOV)

Quanz, Sascha P.; Avenhaus, Henning; Meyer, Michael R.

2012-08-01

The nearby M-dwarf AP Col was recently identified by Riedel et al. as a pre-main-sequence star (age 12-50 Myr) situated only 8.4 pc from the Sun. The combination of its youth, distance, and intrinsically low luminosity make it an ideal target to search for extrasolar planets using direct imaging. We report deep adaptive optics observations of AP Col taken with VLT/NACO and Keck/NIRC2 in the L band. Using aggressive speckle suppression and background subtraction techniques, we are able to rule out companions with mass m {>=} 0.5-1 M{sub Jup} for projected separations a > 4.5 AU, and m {>=} 2more » M{sub Jup} for projected separations as small as 3 AU, assuming an age of 40 Myr using the COND theoretical evolutionary models. Using a different set of models, the mass limits increase by a factor of {approx}>2. The observations presented here are the deepest mass-sensitivity limits yet achieved within 20 AU on a star with direct imaging. While Doppler radial velocity surveys have shown that Jovian bodies with close-in orbits are rare around M-dwarfs, gravitational microlensing studies predict that 17{sup +6}{sub -9}% of these stars host massive planets with orbital separations of 1-10 AU. Sensitive high-contrast imaging observations, like those presented here, will help to validate results from complementary detection techniques by determining the frequency of gas giant planets on wide orbits around M-dwarfs.« less

VizieR Online Data Catalog: 61 main-sequence and subgiant oscillations (Appourchaux+, 2012)

NASA Astrophysics Data System (ADS)

Appourchaux, T.; Chaplin, W. J.; Garcia, R. A.; Gruberbauer, M.; Verner, G. A.; Antia, H. M.; Benomar, O.; Campante, T. L.; Davies, G. R.; Deheuvels, S.; Handberg, R.; Hekker, S.; Howe, R.; Regulo, C.; Salabert, D.; Bedding, T. R.; White, T. R.; Ballot, J.; Mathur, S.; Silva Aguirre, V.; Elsworth, Y. P.; Basu, S.; Gilliland, R. L.; Christensen-Dalsgaard, J.; Kjeldsen, H.; Uddin, K.; Stumpe, M. C.; Barclay, T.

2017-11-01

Kepler observations are obtained in two different operating modes: long cadence (LC) and short cadence (SC) (Gilliland et al., 2010ApJ...713L.160G; Jenkins et al., 2010ApJ...713L..87J). This work is based on SC data. For the brightest stars (down to Kepler magnitude, Kp~=12), SC observations can be obtained for a limited number of stars (up to 512 at any given time) with a faster sampling cadence of 58.84876s (Nyquist frequency of ~8.5mHz), which permits a more precise transit timing and the performance of asteroseismology. Kepler observations are divided into three-month-long quarters (Q). A subset of 61 solar-type stars observed during quarters Q5-Q7 (March 22, 2010 to December 22, 2010) were chosen because they have oscillation modes with high signal-to-noise ratios. This length of data gives a frequency resolution of about 0.04uHz. (2 data files).

Periodic spectrum variations in helium-rich stars

NASA Technical Reports Server (NTRS)

Walborn, N. R.

1982-01-01

Spectroscopic observations of four helium-rich stars are presented. In HD 37776, antiphase variations of Si III and He I have been found, which represent another point of similarity to the Ap phenomenon. The remarkable H-alpha emission variations in Sigma Ori E are illustrated with uniform phase coverage, and strict periodicity over a five-year interval is shown. A radial-velocity study of HD 64740 shows constancy to within the accuracy of the observations. Finally, Delta Ori B is confirmed as a helium-rich star.

VizieR Online Data Catalog: Distances to RRab stars from WISE and Gaia (Sesar+, 2017)

NASA Astrophysics Data System (ADS)

Sesar, B.; Fouesneau, M.; Price-Whelan, A. M.; Bailer-Jones, C. A. L.; Gould, A.; Rix, H.-W.

2017-10-01

To constrain the period-luminosity-metallicity (PLZ) relations for RR Lyrae stars in WISE W1 and W2 bands, we use TGAS trigonometric parallaxes (barω), spectroscopic metallicities ([Fe/H]; Fernley+ 1998, J/A+A/330/515), log-periods (logP, base 10), and apparent magnitudes (m; Klein+ 2014, J/MNRAS/440/L96) for 102 RRab stars within ~2.5kpc from the Sun. The E(B-V) reddening at a star's position is obtained from the Schlegel+ (1998ApJ...500..525S) dust map. (1 data file).

VizieR Online Data Catalog: Fundamental parameters of Kepler stars (Silva Aguirre+, 2015)

NASA Astrophysics Data System (ADS)

Silva Aguirre, V.; Davies, G. R.; Basu, S.; Christensen-Dalsgaard, J.; Creevey, O.; Metcalfe, T. S.; Bedding, T. R.; Casagrande, L.; Handberg, R.; Lund, M. N.; Nissen, P. E.; Chaplin, W. J.; Huber, D.; Serenelli, A. M.; Stello, D.; van Eylen, V.; Campante, T. L.; Elsworth, Y.; Gilliland, R. L.; Hekker, S.; Karoff, C.; Kawaler, S. D.; Kjeldsen, H.; Lundkvist, M. S.

2016-02-01

Our sample has been extracted from the 77 exoplanet host stars presented in Huber et al. (2013, Cat. J/ApJ/767/127). We have made use of the full time-base of observations from the Kepler satellite to uniformly determine precise fundamental stellar parameters, including ages, for a sample of exoplanet host stars where high-quality asteroseismic data were available. We devised a Bayesian procedure flexible in its input and applied it to different grids of models to study systematics from input physics and extract statistically robust properties for all stars. (4 data files).

VizieR Online Data Catalog: Abundances of late-type stars (Roederer+, 2014)

NASA Astrophysics Data System (ADS)

Roederer, I. U.; Jacobson, H. R.; Thanathibodee, T.; Frebel, A.; Toller, E.

2017-01-01

We obtained observations covering the NUV spectral range from the Barbara A. Mikulski Archive for Space Telescopes (MAST). These observations were taken using the medium- or high-resolution echelle gratings in the Space Telescope Imaging Spectrograph (STIS; Kimble et al. 1998ApJ...492L..83K; Woodgate et al. 1998PASP..110.1183W) on board the Hubble Space Telescope (HST). Spectra downloaded from the MAST have been reduced by the calstis pipeline and combined by Ayres (2010, Cat. J/ApJS/187/149). Spectra obtained previously by our own observing programs were reduced by the calstis pipeline and processed as described in Roederer et al. (2012ApJS..203...27R, 2014ApJ...791...32R) and Placco et al. (2014ApJ...790...34P). (4 data files).

Effect of diadenosine tetraphosphate (AP4A) on coronary arterial microvessels in the beating canine heart.

PubMed

Sugimura, A; Kanatsuka, H; Tanikawa, T; Ong, B H; Shirato, K

2000-11-01

Diadenosine tetraphosphate (AP4A) can be released from activated platelets and the present study examined its effect on coronary arterial microvessels. The role of purinoceptors in the coronary microcirculation in vivo was also investigated. In open chest dogs, coronary arterioles were observed using a microscope with a floating objective. In Protocol 1, AP4A (1, 10, 100 and 1,000 micromol/L) was superfused onto the heart surface before and during the superfusion of 10 micromol/L of 8-phenyltheophylline (8-PT), a P1 purinoceptor blocker. In Protocol 2, AP4A (0.1, 1, 10, and 100 nmol x kg(-1) x min(-1)) was infused into the left anterior descending coronary artery before and during the superfusion of 10 micromol/L of 8-PT. In addition to 8-PT, 30 micromol/L of pyridoxalphosphate-6-azophenyl 2',4'-disulphonic acid (PPADS), a P2X purinoceptor blocker in Protocol 3, or 300 micromol/L of N(omega)-nitro-L-arginine (LNNA) in Protocol 4, was continuously superfused, and 4 doses of AP4A were cumulatively superfused as in Protocol 1. In Protocol 5, 10 micromol/L of alpha,beta-methylene ATP, an agonist of P2X purinoceptors, was superfused for 60 min. Superfused AP4A dilated arterioles in a dose-dependent manner. The magnitude of dilatation was greater in smaller arterioles (small vessel < or = 150 microm: 24.5+/-2.2% vs large vessel > 150 microm: 10.6+/-1.5% at a dose of 1,000 micromol/L, p<0.001). On the other hand, intraluminally applied AP4A also dilated arterioles, but no size dependency was shown. In the presence of 8-PT, vasodilatory responses to superfused and intraluminally applied AP4A were attenuated and the lower doses of AP4A constricted arterioles. This vasoconstrictor effect was not affected by PPADS. The vasodilatory effect of the higher doses of AP4A was almost abolished in the presence of LNNA. Alpha,beta-methylene ATP had no effect on coronary microvascular diameters. AP4A has bidirectional effects on coronary arterial microvessels: vasodilatory effects mediated by P1 purinoceptors and NO, which might be mediated by P2Y purinoceptors, and a vasoconstrictor effect, which is not mediated by P2X purinoceptors.

An Atlas of O-C Diagrams of Eclipsing Binary Stars

NASA Astrophysics Data System (ADS)

Kreiner, Jerzy M.; Kim, Chun-Hwey; Nha, Il-Seong

The Atlas contains data for 1,138 eclipsing binaries represented by 91,798 minima timings, collected from the usual international and local journals, observatory publications and unpublished minima. Among this source material there is a considerable representation of amateur astronomers. Some timings were found in the card-index catalogue of the Astronomical Observatory of the Jagiellonian University, Cracow. Stars were included in the Atlas provided that they satisfied 3 criteria: (1) at least 20 minima had been times; (2) these minima spanned at least 2,500 cycles; and (3) the 2,500 cycles represented no fewer than 40 years. Some additional stars not strictly satisfying these criteria were also included if useful information was available. For each star, the Atlas contains the (O-C) diagram calculated by the authors and a table of general information containing: binary characteristics; assorted catalogue numbers; the statistics of the collected minima timings; the light elements (light ephemeris); comments and literature references. All of the data and diagrams in the Atlas are also available in electronic form on the Internet at http://www.as.ap.krakow.pl/o- c".

Extended 60 μm Emission from Nearby Mira Variables

NASA Astrophysics Data System (ADS)

Bauer, W. H.; Stencel, R. E.

1993-01-01

Circumstellar dust envelopes around some optically visible late-type stars are so extensive that they are detectable as extended at an arc-minute scale by the IRAS survey observations (Stencel, Pesce and Bauer 1988, Astron. J 95, 141; Hawkins 1990, Astron. Ap. 229, L8). The width of the IRAS scan profiles at 10% of peak intensity is an indicator of source extension. Wyatt and Cahn (1983, Ap. J. 275, 225) presented a sample of 124 Mira variables in the solar neighborhood. Of this sample, 11 Miras which show silicate emission are bright enough at 60 microns for a significant determination of the width of a scan at 10% of peak flux. Individual scans and maps were examined in order to determine whether any observed extension was associated with the central star. Five stars showed significant extension apparently due to mass loss from the central star: R Leo, o Cet, U Ori, R Cas and R Hor. IRAS LRS spectra, point source fluxes and observed extensions of these sources are compared to the predictions of model dust shells which assume steady mass loss. This work was supported in part by NASA grant NAG 5-1213 to Wellesley College.

Short communication: use of the BetaStar Plus assay for detection of ceftiofur antimicrobial residues in milk from individual cows following intramammary treatment for mastitis.

PubMed

Grooms, D L; Norby, B; Grooms, K E; Jagodzinski, E N; Erskine, R J; Halbert, L W; Coetzee, J F; Wulf, L; Rice, J A

2015-09-01

Development and use of on-farm assays to detect antimicrobial residues in milk is important to reduce the risk of violative residues in marketed milk. The objective of this study was to evaluate the effectiveness of a lateral-flow immunodiagnostic assay (BetaStar Plus, Neogen Corp., Lansing, MI) in detecting ceftiofur residues in milk from individual cows treated for mastitis. This assay is currently approved by the US Federal Drug Administration (FDA) for detecting β-lactam residues in commingled milk. Forty-five dairy cows with clinical mastitis from 4 dairy farms were enrolled and treated intramammary with 125 mg of ceftiofur hydrochloride (Spectramast LC, Zoetis, Madison, NJ) according to the manufacturer's label recommendation. Composite milk samples were collected (A) before first intramammary antimicrobial treatment, (B) before the last intramammary antimicrobial treatment, (C) the last milking of the product-labeled milk withhold, (D) the first milking after the product-labeled milk withhold had been met, and (E) 72 h after the product-labeled milk withhold had been met. Samples were tested using the BetaStar Plus assay within 48 h of collection. Parallel samples were analyzed by liquid chromatography-tandem mass spectrometry (LC-MS/MS) and for somatic cell count and milk components. The BetaStar Plus assay identified 6.7, 60.0, 46.7, 22.2, and 6.7% positive samples at each of the respective time points. The assay had sensitivity and specificity of 100 and 84.7%, respectively, compared with liquid chromatography-tandem mass spectrometry analysis using FDA published residue tolerance levels for ceftiofur (or ceftiofur metabolites) as a threshold. The BetaStar Plus assay could be useful for detecting ceftiofur residues in milk from individual cows following intramammary treatment for mastitis before the milk is shipped for processing. Copyright © 2015 American Dairy Science Association. Published by Elsevier Inc. All rights reserved.

VizieR Online Data Catalog: Cosmic evolution of long gamma-ray burst luminosity (Deng+, 2016)

NASA Astrophysics Data System (ADS)

Deng, C.-M.; Wang, X.-G.; Guo, B.-B.; Lu, R.-J.; Wang, Y.-Z.; Wei, J.-J.; Wu, X.-F.; Liang, E.-W.

2018-02-01

Our sample includes only the redshift-known long GRBs observed with Swift/BAT from 2005 January to 2015 April. Low-luminosity GRBs are excluded since they may belong to another distinct population (e.g., Chapman et al. 2007MNRAS.382L..21C; Liang et al. 2007ApJ...662.1111L; Lu et al. 2010ApJ...725.1965L). Although the durations of some GRBs, such as GRB 050724 and GRB 060614, are larger than 2s, we do not include them in our sample since they may be from merger of compact stars (Berger et al. 2005Natur.438..988B; Gehrels et al. 2006Natur.444.1044G; Zhang et al. 2007ApJ...655L..25Z, 2009ApJ...703.1696Z). The afterglow and host galaxy observations of the high-z SGRB GRB 090426 (T90=1.2s) show that it may be from the collapse of a massive star (Antonelli et al. 2009A&A...507L..45A; Xin et al. 2011MNRAS.410...27X). We thus include this GRB in our sample. We finally obtain a sample of 258 GRBs. They are reported in Table 1. (1 data file).

Erratum: ``On the Evolution of Star-forming Galaxies'' (ApJ, 615, 209 [2004])

NASA Astrophysics Data System (ADS)

Hopkins, A. M.

2007-01-01

The star formation rate (SFR) density values reported in my 2004 paper for the data taken from D. W. Hogg et al. (ApJ, 615, 209 [2004]) are in error. The original cosmology conversion factor used was incorrect, and the values listed in Table 2 for both C1 and ρ˙*com are in error. Moreover, the (incorrect) value reported for C1 was not that used in calculating the (incorrect) values of ρ˙*com. The correct cosmology conversion leads to SFR density values that are smaller than those given in the original paper by amounts decreasing monotonically from ~43% for the z=0.2 bin to ~30% for the z=1.2 bin, as indicated by A. M. Hopkins & J. F. Beacom (ApJ, 615, 209 [2004]), who show an updated version of the star formation history diagram (compare their Fig. 1 with my original Fig. 1). The correct SFR density values are given here in a new Table 1, which has the same format as Table 2 of my original paper, although the table notes are omitted here. Apart from the location of the corresponding data points in Figure 1, this error does not significantly alter any of the results or conclusions of the original paper. I thank Chun Ly for bringing this error to my attention.

Effects of physiological versus pharmacological beta-carotene supplementation on cell proliferation and histopathological changes in the lungs of cigarette smoke-exposed ferrets.

PubMed

Liu, C; Wang, X D; Bronson, R T; Smith, D E; Krinsky, N I; Russell, R M

2000-12-01

There remains a remarkable discordance between the results of observational epidemiological studies and intervention trials using beta-carotene as a potential chemopreventive agent. One question that needs to be examined is whether the adverse outcomes of human beta-carotene trials are related to the large doses of beta-carotene that were administered. In the present study, ferrets were given a physiological (low) dose or a pharmacological (high) dose of beta-carotene supplementation (0.43 mg versus 2.4 mg/kg body wt/day, which is equivalent to 6 mg versus 30 mg/day in humans) and exposed to cigarette smoke for 6 months. We investigated the effects of these doses of beta-carotene on retinoid concentrations, expression of retinoic acid receptors (RARs), activator protein 1 (AP-1; c-Jun and c-Fos), cyclin D1, proliferating cellular nuclear antigen (PCNA), and histopathological changes in the lungs of both normal and cigarette smoke-exposed ferrets. Thirty-six male ferrets were treated in six groups-control, smoke-exposed (SM), low-dose beta-carotene (LBC), high-dose beta-carotene (HBC), low-dose beta-carotene plus smoke exposure (LBC+SM) or high-dose beta-carotene plus smoke exposure (HBC+SM)-for 6 months. Retinoic acid concentration and RAR beta gene expression, but not expression of RAR alpha and RAR gamma, was reduced in the lung tissue of HBC+SM, HBC, SM and LBC+SM ferrets, but not in that of LBC ferrets, as compared with the control group. Expression of AP-1 and PCNA was greater in HBC+SM, HBC, SM and LBC+SM ferrets, but not in the LBC ferrets, as compared with the control group. Increased amounts of cyclin D1 and keratinized squamous metaplasia were observed in the lung tissue of HBC+SM, HBC and SM groups but not in that of the LBC+SM, LBC or control groups. These data suggest that, in contrast with a pharmacological dose of beta-carotene, a physiological dose of beta-carotene in smoke-exposed ferrets has no potentially detrimental effects and may afford weak protection against lung damage induced by cigarette smoke.

Measurements of Beta Lyrae at the Pine Mountain Observatory Summer Workshop 2011

NASA Astrophysics Data System (ADS)

Carro, Joseph; Chamberlain, Rebecca; Schuler, Marisa; Varney, Timothy; Ewing, Robert; Genet, Russell

2012-04-01

As part of the Pine Mountain Observatory Summer Workshop 2011, high school and college students joined with an experienced observer to learn the use of a telescope, astrometric techniques, and measure a double star. This workshop was the first time these students operated a telescope, and, thus, constituted an educational experience for them as they used the telescope and took the measurements. The double star Beta Lyrae was measured resulting in a separation of 44.3 arc seconds and a position angle of 151.6 degrees. The Washington Double Star catalog (2009 data) lists a separation of 45.4 arc seconds and a position angle of 148 degrees.

Chemical Compositions of Young Stars in the Leading Arm of the Magellanic System

NASA Astrophysics Data System (ADS)

Zhang, L.; Moni Bidin, C.; Casetti-Dinescu, D. I.; Mendez, R. A.; Girard, T. M.; Korchagin, V. I.; Vieira, K.; van Altena, W. F.; Zhao, G.

2017-07-01

Seven element abundances (He, C, N, O, Mg, Si, and S) and kinematics were determined for eight O-/B- type stars, based on high resolution spectra taken with the MIKE instrument on the Magellan 6.5m Clay telescope (program ID: CN2014A-057). The sample is selected from 42 candidates Casetti-Dinescu et al.(2014, ApJL, 784, L37) of membership in the Leading Arm (LA) of the Magellanic System. After investigating the relationship between abundances and kinematics parameters, we found that five stars have kinematics compatible with LA membership, i.e. RV>100kms-1. For the five possible LA member stars, Mg abundance is significantly lower than that of the remaining two that are kinematical members of the Galactic disk, and is more close to the LMC values. Distances to the LA members indicate that they are at the edge of the Galactic disk, while ages are of the order of ˜ 50-70 Myr, lower than the dynamical age of the LA, suggesting a single star-forming episode in the LA. VLSR of the LA members decreases with decreasing Magellanic longitude, confirming the results of previous LA gas studies (McClure-Griffiths et al.2008, ApJ, 673, L143). Our abundance and kinematic results for the LA member stars demonstrate that parts of the LA are hydrodynamically interacting with the gaseous Galactic disk, forming young stars that are chemically distinct from those in the Galactic disk. These results can provide constraints to future models for the Magellanic leading material.

The roAp star α Circinus as seen by BRITE-Constellation

NASA Astrophysics Data System (ADS)

Weiss, W. W.; Fröhlich, H.-E.; Pigulski, A.; Popowicz, A.; Huber, D.; Kuschnig, R.; Moffat, A. F. J.; Matthews, J. M.; Saio, H.; Schwarzenberg-Czerny, A.; Grant, C. C.; Koudelka, O.; Lüftinger, T.; Rucinski, S. M.; Wade, G. A.; Alves, J.; Guedel, M.; Handler, G.; Mochnacki, St.; Orleanski, P.; Pablo, B.; Pamyatnykh, A.; Ramiaramanantsoa, T.; Rowe, J.; Whittaker, G.; Zawistowski, T.; Zocłońska, E.; Zwintz, K.

2016-04-01

We report on an analysis of high-precision, multi-colour photometric observations of the rapidly-oscillating Ap (roAp) star α Cir. These observations were obtained with the BRITE-Constellation, which is a coordinated mission of five nanosatellites that collects continuous millimagnitude-precision photometry of dozens of bright stars for up to 180 days at a time in two colours (≈Johnson B and R). BRITE stands for BRight Target Explorer. The object α Cir is the brightest roAp star and an ideal target for such investigations, facilitating the determination of oscillation frequencies with high resolution. This star is bright enough for complementary interferometry and time-resolved spectroscopy. Four BRITE satellites observed α Cir for146 d or 33 rotational cycles. Phasing the photometry according to the 4.4790 d rotational period reveals qualitatively different light variations in the two photometric bands. The phased red-band photometry is in good agreement with previously-published WIRE data, showing a light curve symmetric about phase 0.5 with a strong contribution from the first harmonic. The phased blue-lband data, in contrast, show an essentially sinusoidal variation. We model both light curves with Bayesian Photometric Imaging, which suggests the presence of two large-scale, photometrically bright (relative to the surrounding photosphere) spots. We also examine the high-frequency pulsation spectrum as encoded in the BRITE photometry. Our analysis establishes the stability of the main pulsation frequency over the last ≈20 yr, confirms the presence of frequency f7, which was not detected (or the mode not excited) prior to 2006, and excludes quadrupolar modes for the main pulsation frequency. Based on data collected by the BRITE-Constellation satellite mission, built, launched and operated thanks to support from the Austrian Aeronautics and Space Agency, the University of Vienna, the Canadian Space Agency (CSA), the Foundation for Polish Science & Technology (FNiTP MNiSW), and National Centre for Science (NCN).The light curves and the reduced data for α Circinus are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/588/A54 Member of the BRITE Executive Science Team (BEST).Member of the Photometry Tiger Team (PHOTT).

Exoplanet Caught on the Move

NASA Astrophysics Data System (ADS)

2010-06-01

For the first time, astronomers have been able to directly follow the motion of an exoplanet as it moves from one side of its host star to the other. The planet has the smallest orbit so far of all directly imaged exoplanets, lying almost as close to its parent star as Saturn is to the Sun. Scientists believe that it may have formed in a similar way to the giant planets in the Solar System. Because the star is so young, this discovery proves that gas giant planets can form within discs in only a few million years, a short time in cosmic terms. Only 12 million years old, or less than three-thousandths of the age of the Sun, Beta Pictoris is 75% more massive than our parent star. It is located about 60 light-years away towards the constellation of Pictor (the Painter) and is one of the best-known examples of a star surrounded by a dusty debris disc [1]. Earlier observations showed a warp of the disc, a secondary inclined disc and comets falling onto the star. "Those were indirect, but tell-tale signs that strongly suggested the presence of a massive planet, and our new observations now definitively prove this," says team leader Anne-Marie Lagrange. "Because the star is so young, our results prove that giant planets can form in discs in time-spans as short as a few million years." Recent observations have shown that discs around young stars disperse within a few million years, and that giant planet formation must occur faster than previously thought. Beta Pictoris is now clear proof that this is indeed possible. The team used the NAOS-CONICA instrument (or NACO [2]), mounted on one of the 8.2-metre Unit Telescopes of ESO's Very Large Telescope (VLT), to study the immediate surroundings of Beta Pictoris in 2003, 2008 and 2009. In 2003 a faint source inside the disc was seen (eso0842), but it was not possible to exclude the remote possibility that it was a background star. In new images taken in 2008 and spring 2009 the source had disappeared! The most recent observations, taken during autumn 2009, revealed the object on the other side of the disc after a period of hiding either behind or in front of the star (in which case it is hidden in the glare of the star). This confirmed that the source indeed was an exoplanet and that it was orbiting its host star. It also provided insights into the size of its orbit around the star. Images are available for approximately ten exoplanets, and the planet around Beta Pictoris (designated "Beta Pictoris b") has the smallest orbit known so far. It is located at a distance between 8 and 15 times the Earth-Sun separation - or 8-15 Astronomical Units - which is about the distance of Saturn from the Sun. "The short period of the planet will allow us to record the full orbit within maybe 15-20 years, and further studies of Beta Pictoris b will provide invaluable insights into the physics and chemistry of a young giant planet's atmosphere," says student researcher Mickael Bonnefoy. The planet has a mass of about nine Jupiter masses and the right mass and location to explain the observed warp in the inner parts of the disc. This discovery therefore bears some similarity to the prediction of the existence of Neptune by astronomers Adams and Le Verrier in the 19th century, based on observations of the orbit of Uranus. "Together with the planets found around the young, massive stars Fomalhaut and HR8799, the existence of Beta Pictoris b suggests that super-Jupiters could be frequent byproducts of planet formation around more massive stars," explains Gael Chauvin, a member of the team. Such planets disturb the discs around their stars, creating structures that should be readily observable with the Atacama Large Millimeter/submillimeter Array (ALMA), the revolutionary telescope being built by ESO together with international partners. A few other planetary candidates have been imaged, but they are all located further from their host star than Beta Pictoris b. If located in the Solar System, they all would lie close to or beyond the orbit of the furthest planet, Neptune. The formation processes of these distant planets are likely to be quite different from those in our Solar System and in Beta Pictoris. "The recent direct images of exoplanets - many made by the VLT - illustrate the diversity of planetary systems," says Lagrange. "Among those, Beta Pictoris b is the most promising case of a planet that could have formed in the same way as the giant planets in our Solar System." Notes [1] Debris discs are composed of dust resulting from collisions among larger bodies such as planetary embryos or asteroids. They are larger versions of the zodiacal dust band in our Solar System. The disc around Beta Pictoris was the first to be imaged and is now known to extend up to about 1000 times the distance between the Earth and the Sun. [2] NACO is an adaptive optics instrument attached to ESO's Very Large Telescope, located in Chile. Thanks to adaptive optics, astronomers can remove most of the blurring effect of the atmosphere and obtain very sharp images. More information This research was presented in a paper to appear this week in Science Express ("A Giant Planet Imaged in the disk of the Young Star Beta Pictoris," by A.-M. Lagrange et al.). The team is composed of A.-M. Lagrange, M. Bonnefoy, G. Chauvin, D. Ehrenreich, and D. Mouillet (Laboratoire d'Astrophysique de l'Observatoire de Grenoble, Université Joseph Fourier, CNRS, France), D. Apai (Space Telescope Science Institute, Baltimore, USA), A. Boccaletti, D. Gratadour, D. Rouan, and S. Lacour (LESIA, Observatoire de Paris-Meudon, France), and M. Kasper (ESO). ESO, the European Southern Observatory, is the foremost intergovernmental astronomy organisation in Europe and the world's most productive astronomical observatory. It is supported by 14 countries: Austria, Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. ESO carries out an ambitious programme focused on the design, construction and operation of powerful ground-based observing facilities enabling astronomers to make important scientific discoveries. ESO also plays a leading role in promoting and organising cooperation in astronomical research. ESO operates three unique world-class observing sites in Chile: La Silla, Paranal and Chajnantor. At Paranal, ESO operates the Very Large Telescope, the world's most advanced visible-light astronomical observatory and VISTA, the world's largest survey telescope. ESO is the European partner of a revolutionary astronomical telescope ALMA, the largest astronomical project in existence. ESO is currently planning a 42-metre European Extremely Large optical/near-infrared Telescope, the E-ELT, which will become "the world's biggest eye on the sky".

Spectroscopic and asteroseismic analysis of the remarkable main-sequence A star KIC 11145123

NASA Astrophysics Data System (ADS)

Takada-Hidai, Masahide; Kurtz, Donald W.; Shibahashi, Hiromoto; Murphy, Simon J.; Takata, Masao; Saio, Hideyuki; Sekii, Takashi

2017-10-01

A spectroscopic analysis was carried out to clarify the properties of KIC 11145123 - the first main-sequence star with a directly measured core-to-surface rotation profile - based on spectra observed with the High Dispersion Spectrograph (HDS) of the Subaru telescope. The atmospheric parameters (Teff = 7600 K, log g = 4.2, ξ = 3.1 km s-1 and [Fe/H] = -0.71 dex), the radial and rotation velocities, and elemental abundances were obtained by analysing line strengths and fitting line profiles, which were calculated with a 1D LTE model atmosphere. The main properties of KIC 11145123 are: (1) a low [Fe/H] = -0.71 ± 0.11 dex and a high radial velocity of -135.4 ± 0.2 km s-1. These are remarkable among late-A stars. Our best asteroseismic models with this low [Fe/H] have slightly high helium abundance and low masses of 1.4 M⊙. All of these results strongly suggest that KIC 11145123 is a Population II blue straggler; (2) the projected rotation velocity confirms the asteroseismically predicted slow rotation of the star; (3) comparisons of abundance patterns between KIC 11145123 and Am, Ap, and blue stragglers show that KIC 11145123 is neither an Am star nor an Ap star, but has abundances consistent with a blue straggler. We conclude that the remarkably long 100-d rotation period of this star is a consequence of it being a blue straggler, but both pathways for the formation of blue stragglers - merger and mass loss in a binary system - pose difficulties for our understanding of the exceedingly slow rotation. In particular, we show that there is no evidence of any secondary companion star, and we put stringent limits on the possible mass of any such purported companion through the phase modulation technique.

Near-IR Period-Luminosity Relations for variable stars in ω Centauri

NASA Astrophysics Data System (ADS)

Navarrete, C.; Catelan, M.; Contreras Ramos, R.; Gran, F.; Alonso-García, J.; Dékány, I.

2014-10-01

We report on an extensive time-series study of the globular cluster ω Centauri (NGC 5139), obtained in the framework of the VVV Templates project (Catelan et al. 2013, arXiv: 1310.1996). This cluster was chosen for this project due to its large variable star content. A total of 42 and 100 epochs of the cluster in J and K_{S}, respectively, were taken using VIRCAM@VISTA, and PSF photometry was performed to derive light curves for 270 pulsating stars (RRab, RRc, type II Cepheids and SX Phoenicis) with an unprecedented phase coverage in the near-IR. Period-Luminosity (PL) relations in both bands were derived using Fourier fitted magnitudes for RR Lyrae and Type II Cepheids, while weighted-average magnitudes were used for SX Phe stars. Using the PL relation for RRab stars derived by Dékány et al. (2013, ApJ, 776, 19L) in the VISTA K_{S} system, we determine a distance modulus of (m-M)_{0} = 13.78 ± 0.04 mag, in good agreement with Del Principe et al. (2006, ApJ, 652, 362). From Type II Cepheids we derived a value of (m-M)_{0} = 13.67 ± 0.07 mag, similar to what was found by Matsunaga et al. (2006, MNRAS, 370, 1979). For SX Phe stars, we use the derived periods and magnitudes to infer their pulsation modes, and we confirm that at least 12 of them are fundamental-mode pulsators (Olech et al. 2005, MNRAS, 363, 40).

FUV Detection of the Primary Star of eta Carinae

NASA Astrophysics Data System (ADS)

Davidson, K.; Smith, N.

2006-06-01

Using FUSE data, Iping et al (2005, ApJ 633, L37) report a direct detection of the elusive hot companion of eta Car. We argue, however, that much of the observed emission represents the primary star, with no proof that any of it comes from a secondary star. The hypothetical companion should dominate the ionizing radiation below 912 A, but this is not true for wavelengths around 1100 A observed with FUSE. Moreover, since a companion's UV would be partially reprocessed by the primary star's wind, any detection is likely to be ambiguous.The non-spherical primary wind allows production of strong UV radiation at low latitudes (Smith et al 2003, ApJ 586, 432), an effect that spherical models don't include. The N II 1085 feature, the relatively slow wind velocities seen by FUSE, and other details are characteristic of the primary wind, not the secondary. Zanella et al. (1984, A&A 137, 79) suggested that eta Car's far UV disappears during a spectroscopic event due to a shell ejection. The FUSE observations may be regarded as confirmation of that conjecture, which made no reference to a secondary star. The 2003 spectroscopic event was probably a mass ejection or a wind-disturbance episode, not merely an eclipse as assumed by Iping et al. A hot companion star seems likely to account for the ionizing UV and the X-ray variability, but the FUSE data do not confirm its existence.

Inotropic effects of diadenosine tetraphosphate in isolated canine cardiac preparations.

PubMed

Neumann, J; Meissner, A; Bokník, P; Gombosová, I; Knapp, J; Lüss, H; Müller, F U; Schlüter, H; Zidek, W; Rolf, N; Van Aken, H; Vahlensieck, U; Schmitz, W

1999-01-01

We studied the effects of diadenosine tetraphosphate (AP4A) on the force of contraction in canine preparations. The force of contraction was measured in isolated electrically driven (1 Hz) atrial and ventricular cardiac trabeculae from adult dogs. AP4A (100 microM) alone and after prestimulation with 10 nM isoproterenol reduced force of contraction in atrial preparations by approximately 24%. Moreover, AP4A (100 microM) alone and after prestimulation with 10 nM isoproterenol reduced the force of contraction in ventricular preparations by 29 and 29%, respectively. The negative inotropic effects of AP4A were abolished by the A1-adenosine receptor antagonist 1,3-dipropyl-cyclopentyl-xanthine (DPCPX). In summary, in canine myocardium, AP4A alone and after prestimulation with a beta-adrenoceptor agonist exerts negative inotropic effects, which are probably mediated via A1-adenosine receptors.

VizieR Online Data Catalog: Stellar activity and kinematics of FGK stars (Murgas+, 2013)

NASA Astrophysics Data System (ADS)

Murgas, F.; Jenkins, J. S.; Rojo, P.; Jones, H. R. A.; Pinfield, D. J.

2013-02-01

We present a compilation of stellar activity catalogs combined with galactic velocity information of 2529 F, G, and K stars. The stellar activity catalogs use in this work are: Jenkins et al. 2011 (Cat. J/A+A/531/A8); Gray et al. 2003 (Cat. J/AJ/126/2048), 2006 (Cat. J/AJ/132/161); Henry et al 1996 (Cat. J/A+A/111/439); Wright et al. 2004 (Cat. J/ApJS/152/261); Duncan et al. (1991ApJS...76..383D, Cat. III/159). The galactic velocities are taken from the Jenkins et al. 2011 (Cat. J/A+A/531/A8) and the Geneva-Copenhaguen Survey (GCS) Nordstrom et al. (2004A&A...418..989N, Cat. V/117). (1 data file).

VizieR Online Data Catalog: SDSS DR7 white dwarf catalog (Kleinman+, 2013)

NASA Astrophysics Data System (ADS)

Kleinman, S. J.; Kepler, S. O.; Koester, D.; Pelisoli, I.; Pecanha, V.; Nitta, A.; Costa, J. E. S.; Krzesinski, J.; Dufour, P.; Lachapelle, F.-R.; Bergeron, P.; Yip, C.-W.; Harris, H. C.; Eisenstein, D. J.; Althaus, L.; Corsico, A.

2013-01-01

Here, we report on the white dwarf catalog built from the SDSS DR7 (Cat. II/294). We have applied automated techniques supplemented by complete, consistent human identifications of each candidate white dwarf spectrum. We make use of the latest SDSS reductions and white dwarf model atmosphere improvements in our spectral fits, providing logg and Teff determinations for each identified clean DA and DB where we use the word "clean" to identify spectra that show only features of non-magnetic, nonmixed, DA or DB stars. Our catalog includes all white dwarf stars from the earlier Kleinman et al. (2004, Cat. J/ApJ/607/426) and Eisenstein et al. (2006, Cat. J/ApJS/167/40) catalogs, although occasionally with different identifications. (1 data file).

ASCA X-ray spectra of the active single stars Beta Ceti and pi(1) Ursae Majoris

NASA Technical Reports Server (NTRS)

Drake, S. A.; Singh, K. P.; White, N. E.; Simon, Theodore

1994-01-01

We present X-ray spectra obtaiined by ASCA of two single, active stars, the G dwarf pi(1) UMa, and the G9/K0 giant Beta Cet. The spectra of both stars require the presence of at least two plasma components with different temperatures, 0.3-0.4 keV and approximately 0.7 keV, in order for acceptable fits to be obtained. The spectral resolving power and signal-to-noise ratio of the solid state imaging spectrometer (SIS) spectra allow us to formally constrain the coronal abundances of a number of elements. In Beta Cet, we find Mg to be overabundant, while other elements such as O, Ne, and N are underabundant, relative to the solar photospheric values. From the lower signal-to-noise ratio SIS spectrum of pi(1) UMa, we find evidence for underabundances of O, Ne, and Fe. These results are discussed in the context of the present understanding of elemental abundances in solar and stellar coronae.

Dose- and time-dependent increase of lysosomal enzymes in embryonic cartilage in vitro after ionizing radiation

DOE Office of Scientific and Technical Information (OSTI.GOV)

Cornelissen, M.; de Ridder, L.

Radiation doses of 20, 50 or 100 Gy caused the same time related decrease for RNA and proteoglycan (PG) synthesis in embryonic cartilage in vitro (4 days culture). In this paper, participation of lysosomes in this radiation response is investigated. Therefore, we employ a cytochemical method using beta-glycerophosphate as substrate for acid phosphatase (AP) detection. Increase of AP was found 2 days after irradiation and increased during the whole culture period. The increase was more pronounced with a higher radiation dose. Stimulation of AP activity explains the observed radiation response of RNA and PG synthesis.

DOE Office of Scientific and Technical Information (OSTI.GOV)

Richards, Mercedes T.; Agafonov, Michail I.; Sharova, Olga I., E-mail: mrichards@astro.psu.edu, E-mail: agfn@nirfi.sci-nnov.ru, E-mail: shol@nirfi.sci-nnov.ru

Time-resolved H{alpha} spectra of magnetically active interacting binaries have been used to create three-dimensional (3D) Doppler tomograms by means of the Radioastronomical Approach. This is the first 3D reconstruction of {beta} Per, with RS Vul for comparison. These 3D tomograms have revealed evidence of the mass transfer process (gas stream, circumprimary emission, localized region, absorption zone), as well as loop prominences and coronal mass ejections (CMEs) in {beta} Per and RS Vul that could not be discovered from two-dimensional tomograms alone. The gas stream in both binaries may have been deflected beyond the central plane by the donor star's magneticmore » field. The stream was more elongated along the predicted trajectory in RS Vul than in {beta} Per, but not as pronounced as in U CrB (stream state). The loop prominence reached maximum V{sub z} velocities of {+-}155 km s{sup -1} in RS Vul compared to {+-}120 km s{sup -1} in {beta} Per, while the CME reached a maximum V{sub z} velocity of +150 km s{sup -1} in RS Vul and +100 km s{sup -1} in {beta} Per. The 3D tomograms show that the gas flows are not symmetric relative to the central plane and are not confined to that plane, a result confirmed by recent 15 GHz VLBI radio images of {beta} Per. Both the 3D H{alpha} tomography and the VLBI radio images support an earlier prediction of the superhump phenomenon in {beta} Per: that the gas between the stars is threaded with a magnetic field even though the hot B8V mass-gaining star is not known to have a magnetic field.« less

Angular Momentum Evolution in Young Low Mass Stars

NASA Astrophysics Data System (ADS)

Pinzón, G.; de La Reza, R.

2006-06-01

During the last decades, the study of rotation in young low mass stars has been one of the more active areas in the field of stellar evolution. Many theoretical efforts have been made to understand the angular momentum evolution and our picture now, reveals the main role of the stellar magnetic field in all pre-main sequence stage (Ghosh & Lamb 1979, ApJ, 234, 296; Cameron & Campbell 1993, A&A, 274, 309; Cameron & Campbell 1995, A&A, 298, 133; Kúker, Henning, & Rúdiger 2003, ApJ, 589, 397; Matt & Pudritz 2005, MNRAS, 356, 167). The mean rotation of most of the cool low mass stars remains roughly constant during the T Tauri stage. This can be explained by the disc locking scenario. This paradigm suggest that star start out as CTTS with periods of 4-14 days, perhaps locked to their disc, and that this disc is eventually lost mainly by accretion. At the current time, it is not clear that this is true for all low mass stars. Some authors have questioned its validity for stars less massive than 0.5 solar masses. Although the reality may eventually turn out to be considerably more complex, a simple consideration of the effects of and limits on disc locking of young low mass stars seems necessary.We have investigated the exchange of angular momentum between a low mass star and an accretion disc during the Hayashi Track (Pinzón, Kúker, & de la Reza 2005, in preparation) and also along the first 100Myr of stellar evolution. The model incorporates changes in the star's moment of inertia, magnetic field strength (Elstner & Rúdiger 2000, A&A, 358, 612), angular momentum loss by a magnetic wind and an exponential decrease of the accretion rate. The lifetime of the accretion disc is a free parameter in our model. The resulting rotation rates are in agreement with observed vsin and photometric periods for young stars belonging to co-moving groups and open young clusters.

Spectropolarimetry of Post-AGB Stars

NASA Astrophysics Data System (ADS)

Trammell, S. R.; Goodrich, R. W.; Dinerstein, H. L.

1992-12-01

We have used the technique of optical spectropolarimetry to investigate post-AGB stars, objects that represent the first stages of the transition from the AGB to a planetary nebula. Several of the observed objects display unpolarized emission lines superimposed on a highly polarized continuum. The continuum polarization provides evidence for the presence of an aspherical dust envelope early in the transition process. The observed objects were chosen from several samples: high latitude supergiants with IR excesses that are thought to be post-AGB stars (e.g. Bond et. al. 1984, PASP, 96, 176), their lower latitude counterparts (e.g. Hrivnak et. al. 1989, ApJ, 346, 265), post-AGB stars shown by Johnson & Jones (1991, AJ, 101, 1735) to have high broad band polarizations, and three highly polarized extreme carbon stars investigated by Cohen & Schmidt (1982, ApJ, 259, 693). GL 1403, an extreme carbon star, shows an abrupt position angle rotation at 6000 Angstroms, implying that at blue wavelengths we see a scattered stellar continuum, while the star itself is hidden from direct view. Longward of the position angle rotation, we begin to see the star directly. Menzies & Whitelock (1988, MNRAS, 233, 697) proposed that IRAS 20056+1834, an unreddened GO supergiant with very strong Na I emission lines and a large infrared excess, is a mass-losing star obscured from direct view, in which the photospheric light is seen in reflection. Our data support this interpretation; the Na I emission is unpolarized, indicating that it is produced in the shell, while the continuum is scattered and polarized (5-7%) by the aspherical shell of material. IRAS 20000+3239 also shows unpolarized Na I D emission and is probably similar to IRAS 20056+1834. IRC +10420 exhibits unpolarized Hα emission and GL 2699, an extreme carbon star, displays both polarized and unpolarized Hα as well as unpolarized low excitation forbidden [S II] and [O I] emission lines.

VizieR Online Data Catalog: Silicon depletion in the interstellar medium (Haris+, 2016)

NASA Astrophysics Data System (ADS)

Haris, U.; Parvathi, V. S.; Gudennavar, S. B.; Bubbly, S. G.; Murthy, J.; Sofia, U. J.

2018-03-01

Gudennavar et al. (2012, J/ApJS/199/8) compiled absorption line data for 3008 stars of which 131 sight lines included silicon column densities that were taken over 30 years of observations (Table 1). Most of the silicon lines (84) in our sample have come from van Steenberg & Shull (1988ApJS...67..225V) who used archival observations from the International Ultraviolet Explorer (IUE) to derive column densities to a number of different species. Most of the other observations (36) were made using the Goddard High Resolution Spectrograph (Spitzer & Fitzpatrick 1995ApJ...445..196S; Savage & Sembach 1996ARA&A..34..279S; Redfield & Linsky 2004ApJ...602..776R) or the Space Telescope Imaging Spectrograph (Sonnentrucker et al. 2003ApJ...596..350S; Gnacinski & Krogulec 2006AcA....56..373G; Miller et al. 2007ApJ...659..441M) with higher resolution and better signal-to-noise. (3 data files).

Cystinyl and pyroglutamyl-beta-naphthylamide hydrolyzing activities are modified coordinately between hypothalamus, liver and plasma depending on the thyroid status of adult male rats.

PubMed

Segarra, A B; Prieto, I; Martinez-Canamero, M; Vargas, F; De Gasparo, M; Vanderheyden, P; Zorad, S; Ramirez-Sanchez, M

2018-04-01

The hypothalamus determinates metabolic processes in liver through endocrine and autonomic control. Hypothalamic neuropeptides, such as thyrotropin releasing hormone or vasopressin, have been involved in liver metabolism. The thyroid status influences metabolic processes including liver metabolism in modulating those hypothalamic peptides whose functional status is regulated in part by aminopeptidase activities. In order to obtain data for a possible coordinated interaction between hypothalamus, plasma and liver, of some aminopeptidase activities that may partially reflect the hydrolysis of those peptides, pyroglutamyl- (pGluAP) and cystinyl- (CysAP) beta-naphthylamide hydrolyzing activities were determined fluorimetrically, both in their soluble and membrane-bound forms, in eu- hypo- and hyperthyroid adult male rats. Hyperthyroidism and hypothyroidism were induced with daily subcutaneous injections of tetraiodothyronine (300 μg/kg/day) or with 0.03% methimazole in drinking water for 6 weeks. Results demonstrated significant changes depending on the type of enzyme and the thyroid status. The most striking changes were observed for CysAP in liver where it was reduced in hypothyroidism and increased in hyperthyroidism. Significant intra- and inter-tissue correlations were observed. While there were positive inter-tissue correlations between liver, plasma and hypothalamus in eu-and hypothyroid rats, a negative correlation between hypothalamus and liver was observed in hyperthyroidism. These results suggest the influence of thyroid hormones and an interactive role for these activities in the control of liver metabolism. The present data also suggest a role for CysAP and pGluAP activities in liver function linked to their activities in hypothalamus.

Ca(2+)-stores mobilization by diadenosine tetraphosphate, Ap4A, through a putative P2Y purinoceptor in adrenal chromaffin cells.

PubMed Central

Castro, E.; Pintor, J.; Miras-Portugal, M. T.

1992-01-01

1. Diadenosine tetraphosphate (Ap4A) evoked a concentration-dependent increase in cytosolic [Ca2+] in resting chromaffin cells. The EC50 value for this action was 28.2 +/- 6.6 microM. This effect was also produced by diadenosine pentaphosphate (Ap5A) with an EC50 of 50 +/- 7 microM. 2. In contrast with this effect, pretreatment with Ap4A or Ap5A induced a 30% reduction in Ca2+ entry following 10 microM dimethylphenylpiperazinium. 3. The elevation in cytosolic [Ca2+] induced by Ap4A was persistent in approximately 100 nM external [Ca2+] and was sensitive to depletion of internal Ca2+ stores by a bradykinin prepulse or whole cell depletion in Ca2+. 4. The effect of Ap4A was mimicked and desensitized by the agonist adenosine 5'-O-(2-thiodiphosphate), and blocked by the P2Y-receptor antagonist, cibachrome blue. The P2X-receptor agonist alpha,beta-methylene adenosine 5'-triphosphate was inactive both by itself or in combination with Ap4A. This is compatible with a P2Y-purinoceptor-mediated action. PMID:1393282

Ca(2+)-stores mobilization by diadenosine tetraphosphate, Ap4A, through a putative P2Y purinoceptor in adrenal chromaffin cells.

PubMed

Castro, E; Pintor, J; Miras-Portugal, M T

1992-08-01

1. Diadenosine tetraphosphate (Ap4A) evoked a concentration-dependent increase in cytosolic [Ca2+] in resting chromaffin cells. The EC50 value for this action was 28.2 +/- 6.6 microM. This effect was also produced by diadenosine pentaphosphate (Ap5A) with an EC50 of 50 +/- 7 microM. 2. In contrast with this effect, pretreatment with Ap4A or Ap5A induced a 30% reduction in Ca2+ entry following 10 microM dimethylphenylpiperazinium. 3. The elevation in cytosolic [Ca2+] induced by Ap4A was persistent in approximately 100 nM external [Ca2+] and was sensitive to depletion of internal Ca2+ stores by a bradykinin prepulse or whole cell depletion in Ca2+. 4. The effect of Ap4A was mimicked and desensitized by the agonist adenosine 5'-O-(2-thiodiphosphate), and blocked by the P2Y-receptor antagonist, cibachrome blue. The P2X-receptor agonist alpha,beta-methylene adenosine 5'-triphosphate was inactive both by itself or in combination with Ap4A. This is compatible with a P2Y-purinoceptor-mediated action.

Physics of Cool Stars: Densities, Sizes, and Energetics

NASA Technical Reports Server (NTRS)

Dupree, Andrea K.

2001-01-01

The ORFEUS 1 (Orbiting and Retrievable Far and Extreme Ultraviolet Spectrometer) telescope obtained far ultraviolet spectra (lambda-lambda 912-1218) of luminous cool stars as a part of our observing program. Two classes of objects were measured: luminous single stars beta Dra (HD 159181) and two hybrid stars alpha Aqr (HD 209750) and alpha TrA (HD 150798) and two active binary systems: 44i Boo and UX Ari.

VizieR Online Data Catalog: Late-type targets in Taurus, Cha I, and Upper Sco (Todorov+, 2014)

NASA Astrophysics Data System (ADS)

Todorov, K. O.; Luhman, K. L.; Konopacky, Q. M.; McLeod, K. K.; Apai, D.; Ghez, A. M.; Pascucci, I.; Robberto, M.

2017-07-01

To characterize the multiplicity of low-mass stars and brown dwarfs in Taurus and Chamaeleon I, we combine the results from our survey with those from previous high-resolution images in these regions. The latter were collected with WFPC2 (Kraus et al. 2006ApJ...649..306K), Keck speckle imaging (Konopacky et al. 2007ApJ...663..394K), and Keck AO imaging (Kraus & Hillenbrand 2012, J/ApJ/757/141) in Taurus and with WFPC2 (Neuhauser et al. 2002A&A...384..999N), the Advanced Camera for Surveys on Hubble (Luhman 2007, J/ApJS/173/104), and AO at the Very Large Telescope (Ahmic et al. 2007ApJ...671.2074A; Lafreniere et al. 2008ApJ...683..844L) in Chamaeleon I. For comparison to these two regions, we also have compiled binary data measured for late-type members of the Upper Sco association ({tau}~11 Myr; Pecaut et al. 2012, J/ApJ/746/154) with WFPC2 and Keck AO (Kraus et al. 2005ApJ...633..452K; Biller et al. 2011ApJ...730...39B; Kraus & Hillenbrand 2012, J/ApJ/757/141). (1 data file).

VizieR Online Data Catalog: Spitzer photometry of ~1million stars in M31 & 15 gal. (Khan, 2017)

NASA Astrophysics Data System (ADS)

Khan, R.

2017-03-01

For M31, we used the IRAC 3.6, 4.5, 5.8, and 8um mosaics produced by Mould+ (2008, J/ApJ/687/230) and the MIPS 24um mosaic produced by Gordon+ (2006ApJ...638L..87G). For the other galaxies, we used the IRAC and MIPS mosaics produced by the Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt+ 2003PASP..115..928K) and the Local Volume Legacy Survey (LVL; Dale+ 2009, J/ApJ/703/517). We utilize the full mosaics available for each galaxy. (17 data files).

Branching Fractions and log(gf)s for Weak Lines of Co II connected to the Ground and Low Metastable Levels

NASA Astrophysics Data System (ADS)

Lawler, James Edward; Feigenson, Thomas; Sneden, Chris; Cowan, John J.

2018-01-01

New branching fraction (BF) measurements and log(gf)s of Highly Reliable Lines (HRLs) of Co II are reported. Our measurements test and confirm earlier work by Salih et al. [1985] and Mullman et al. [1998] and expand the earlier BF measurements to include more weak and very weak HRLs. HRLs are UV lines that connect to the population reservoir levels including the ground and low metastable levels of Co+. Such levels contain most of the cobalt in the photospheres of typical F, G, and K stars used in abundance studies. HRLs are essentially immune to departures from Local Thermodynamic Equilibrium (LTE) because they connect to the primary reservoir levels. Lightly-populated high-lying levels of the ion and essentially all levels of the neutral atom have some possibility of being pulled out of LTE through various reactions. Weak and very weak HRLs are needed to determine Co abundances in higher metallicity stars while dominant branches are useful in low metallicity stars of abundance surveys. A large set of HRLs with reliable log(gf)s is desired to avoid blending and saturation problems in photospheric studies. The relative abundance of Fe-peak elements changes as a function of metallicity [e.g. Henry et al. 2010, Sneden et al. 2016] but contributions to the trends from nuclear physics effects in early stars need to be cleanly separated from effect due to limitations of classic photospheric models based on One Dimensional (1D) and LTE approximations. The 1D/LTE approximations of classic photospheric models, which work in well in metal rich dwarf stars such as the Sun, are a source of some concern in Metal Poor (MP) giant stars due to much lower electron and atom pressures. Our new measurements on HRLS of Co II are applied to determine stellar abundances in MP stars.Henry, R. B. C., Cowan, J. J., & Sobeck, J, 2010, ApJ 709, 715Mullman, K. L., Cooper, J. C., & Lawler, J. E. 1998, ApJ, 495, 503Salih, S., Lawler, J. E., & Whaling, W. 1985, PhRvA, 31, 744Sneden et al. 2016, ApJ 817:53Supported by the Univ. of Wisconsin – Hilldale Foundation, NASA grant NNX16AE96G, and NSF grants AST-1516182 & AST1616040.

UTILIZING SYNTHETIC UV SPECTRA TO EXPLORE THE PHYSICAL BASIS FOR THE CLASSIFICATION OF LAMBDA BOÖTIS STARS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Cheng, Kwang-Ping; Johnson, Dustin M.; Tarbell, Erik S.

2016-04-15

Lambda Boo-type stars are a group of late B to early F-type Population I dwarfs that show mild to extreme deficiencies of iron-peak elements (up to 2 dex), but their C, N, O, and S abundances are near solar. This intriguing stellar class has recently regained the spotlight because of the directly imaged planets around a confirmed Lambda Boo star, HR 8799, and a suggested Lambda Boo star, Beta Pictoris. The discovery of a giant asteroid belt around Vega, another possible Lambda Boo star, also suggests hidden planets. The possible link between Lambda Boo stars and planet-bearing stars motivates usmore » to study Lambda Boo stars systematically. Since the peculiar nature of the prototype Lambda Boötis was first noticed in 1943, Lambda Boo candidates published in the literature have been selected using widely different criteria. In order to determine the origin of Lambda Boo stars’ unique abundance pattern and to better discriminate between theories explaining the Lambda Boo phenomenon, a consistent working definition of Lambda Boo stars is needed. We have re-evaluated all published Lambda Boo candidates and their available ultraviolet and visible spectra. In this paper, using observed and synthetic spectra, we explore the physical basis for the classification of Lambda Boo stars, and develop quantitative criteria that discriminate metal-poor stars from bona fide Lambda Boo stars. Based on these stricter Lambda Boo classification criteria, we conclude that neither Beta Pictoris nor Vega should be classified as Lambda Boo stars.« less

Einstein Observations of X-ray emission from A stars

NASA Astrophysics Data System (ADS)

Golub, L.; Harnden, F. R., Jr.; Maxson, C. W.; Rosner, R.; Vaiana, G. S.; Cash, W., Jr.; Snow, T. P., Jr.

1983-08-01

Results are reported from the combined CfA Stellar Survey of selected bright A stars and an Einstein Guest Observer program for Ap and Am stars. In an initial report of results from the CfA Stellar Surveys by Vaiana et al. (1981) it was noted that the spread in observed X-ray luminosities among the few A stars observed was quite large. The reasons for this large spread was studied by Pallavicini et al. (1981). It was found that the X-ray emission from normal stars is related very strongly to bolometric luminosity for early-type stars and to rotation rate for late-type stars. However, an exception to this rule has been the apparently anomalous behavior of A star X-ray emission, for which the large spread in luminosity showed no apparent correlation with either bolometric luminosity or stellar rotation rate. In the present study, it is shown that the level of emission from normal A stars agrees with the correlation observed for O and B stars.

Asteroseismology: Theory and phenomenology

NASA Technical Reports Server (NTRS)

Brown, Timothy M.

1994-01-01

Seismic studies of the Sun have succeeded in mapping the variation of sound speed with depth in the Sun, and variation of angular velocity with both depth and latitude. Many stars besides the Sun may also be amenable to asteroseismic analysis. Stars of roughly solar type should of course behave in ways similar to the sun, and stars of this sort form a large fraction of the potential targets for asteroseismology. But several other types of stars (delta scuti stars, roAP stars, and the pulsating white dwarfs) also have the desired pulsation characteristics. Pulsations in some of these stars are, for various reasons, much easier to observe than in the Sun-like stars. Virtually all unambiguous observations of multi-mode pulsators relate to these other categories of stars. Since oscillation mode frequencies are arguably the most precise measurement relating to a star that we can make, a few tens of such frequencies may still be of great importance to our understanding of the stellar structure and evolution.

Erratum: ``A Grid of Non-LTE Line-blanketed Model Atmospheres of O-Type Stars'' (ApJS, 146, 417 [2003])

NASA Astrophysics Data System (ADS)

Lanz, Thierry; Hubeny, Ivan

2003-07-01

We have constructed a comprehensive grid of 680 metal line-blanketed, non-LTE, plane-parallel, hydrostatic model atmospheres for the basic parameters appropriate to O-type stars. The OSTAR2002 grid considers 12 values of effective temperatures, 27,500K<=Teff<=55,000 K with 2500 K steps, eight surface gravities, 3.0<=logg<=4.75 with 0.25 dex steps, and 10 chemical compositions, from metal-rich relative to the Sun to metal-free. The lower limit of logg for a given effective temperature is set by an approximate location of the Eddington limit. The selected chemical compositions have been chosen to cover a number of typical environments of massive stars: the Galactic center, the Magellanic Clouds, blue compact dwarf galaxies like I Zw 18, and galaxies at high redshifts. The paper contains a description of the OSTAR2002 grid and some illustrative examples and comparisons. The complete OSTAR2002 grid is available at our Web site at ApJS, 146, 417 [2003]. Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771.

VizieR Online Data Catalog: Stars associated to Eagle Nebula (M16=NGC6611) (Guarcello+ 2010)

NASA Astrophysics Data System (ADS)

Guarcello, M. G.; Micela, G.; Peres, G.; Prisinzano, L.; Sciortino, S.

2010-08-01

This catalog contains coordinates and both optical and infrared photometry, plus usefull tags, of the candidate stars associated to the Eagle Nebula (M16), bost disk-less and disk-bearing, selected in Guarcello et al. 2010: "Chronology of star formation and disks evolution in the Eagle Nebula". The optical photometry in BVI bands comes from observations with WFI@ESO (Guarcello et al. 2007, Cat. J/A+A/462/245); JHK photometry have been obtained from 2MASS/PSC (Bonatto et al. 2006A&A...445..567B, Guarcello et al. 2007, Cat. J/A+A/462/245) and UKIDSS/GPS catalogs (Guarcello et al., 2010, in prep.) ; IRAC data are from GLIMPSE public survey (Indebetouw 2007ApJ...666..321I, Guarcello et al., 2009, Cat. J/A+A/496/453); X-ray data from three observations with Chandra/ACIS-I (Linsky et al., 2007, Cat. J/ApJ/654/347, Guarcello et al., 2007, J/A+A/462/245, Guarcello et al. 2010, in prep.). (1 data file).

Automated scanning of plastic nuclear track detectors using the Minnesota star scanner

NASA Technical Reports Server (NTRS)

Fink, P. J.; Waddington, C. J.

1986-01-01

The problems found in an attempt to adapt an automated scanner of astronomical plates, the Minnesota Automated Dual Plate Scanner (APS), to locating and measuring the etch pits produced by ionizing particles in plastic nuclear track detectors (CR-39) are described. A visual study of these pits was made to determine the errors introduced in determining positions and shapes. Measurements made under a low power microscope were compared with those from the APS.

Quantifying Stellar Mass Loss with High Angular Resolution Imaging

DTIC Science & Technology

2009-02-19

material – via massive winds, planetary nebulae and supernova explosions – seeding the interstellar medium with heavier elements. Subsequent...of Planetary Nebulae (Harpaz, ApJ, 498,293, (1998)), impacts the pre-explosion characteristic of SNII (Taylor, “The Stars”, Cambridge (1994)), and...A 464, 119) or may have an important role, such as Be Stars, W-R stars, and planetary nebulae . The Future of Interferometric O/IR Imaging. The

Spectra of solar proton ground level events using neutron monitor and neutron moderated detector recordings

NASA Technical Reports Server (NTRS)

Stoker, P. H.

1985-01-01

Recordings on relativistic solar flare protons observed at Sanae, Antarctic, show that the percentage increase in counting rates of the neutron moderated detector (4NMD) is larger than the percentage increase in counting rates of the 3NM64 neutron monitor. These relative increases are described by solar proton differential spectra j sub s(P) = AP(beta). The power beta is determined for each event and the hardnesses of the temporal variations of beta, found for the ground level events (GLE) of 7 May, 1978 and 22 November, 1977.

Fast radio bursts and their possible neutron star origins

NASA Astrophysics Data System (ADS)

Hessels, J. W. T.

2017-12-01

The discovery of the ‘Lorimer Burst’, a little over a decade ago, ignited renewed interest in searching for short-duration radio transients (Lorimer et al 2007 Science 318 777). This event is now considered to be the first established Fast Radio Burst (FRB), which is a class of millisecond-duration radio transients (Thornton et al 2013 Science 341 53). The large dispersive delays observed in FRBs distinguish them from the individual bright pulses from Galactic pulsars, and suggests that they originate deep in extragalactic space. Amazingly, FRBs are not rare: the implied event rate ranges up to many thousands of events per sky, per day (Champion et al 2016 MNRAS 460 L30). The fact that only two dozen FRBs have been discovered to date is a consequence of the limited sensitivity and field of view of current radio telescopes (Petroff et al 2016 PASA 33 e045). The precise localization of FRB 121102, the first and currently only FRB observed to repeat (Spitler et al 2014 ApJ 790 101; Spitler et al 2016 Nature 531 202; Scholz et al 2016 ApJ 833 177), has led to the unambiguous identification of its host galaxy and thus proven its extragalactic origin and large energy scale (Chatterjee et al 2017 Nature 541 58; Tendulkar et al 2017 ApJL 834 L7; Marcote et al 2017 ApJL 834 L8). It remains unclear, however, whether all FRBs are capable of repeating [many appear far less active (Petroff et al 2015 MNRAS 454 457)] or whether FRB 121102 implies that there are multiple sub-classes. Regardless, the repetitive nature of FRB 121102 and its localization to within a star-forming region in the host galaxy (Bassa et al 2017 ApJL 843 L8) imply that the bursts might originate from an exceptionally powerful neutron star - one necessarily quite unlike any we have observed in the Milky Way. In these proceedings, I give a very brief introduction to the FRB phenomenon and focus primarily on the insights that FRB 121102 has provided thus far.

DOE Office of Scientific and Technical Information (OSTI.GOV)

Railo, Antti; Nagy, Irina I.; Kilpelaeinen, Pekka

The Wnt family of glycoprotein growth factors controls a number of central cellular processes such as proliferation, differentiation and ageing. All the Wnt proteins analyzed so far either activate or inhibit the canonical {beta}-catenin signaling pathway that regulates transcription of the target genes. In addition, some of them activate noncanonical signaling pathways that involve components such as the JNK, heterotrimeric G proteins, protein kinase C, and calmodulin-dependent protein kinase II, although the precise signaling mechanisms are only just beginning to be revealed. We demonstrate here that Wnt-11 signaling is sufficient to inhibit not only the canonical {beta}-catenin mediated Wnt signalingmore » but also JNK/AP-1 and NF-{kappa}B signaling in the CHO cells, thus serving as a noncanonical Wnt ligand in this system. Inhibition of the JNK/AP-1 pathway is mediated in part by the MAPK kinase MKK4 and Akt. Moreover, protein kinase C is involved in the regulation of JNK/AP-1 by Wnt-11, but not of the NF-{kappa}B pathway. Consistent with the central role of Akt, JNK and NF-{kappa}B in cell survival and stress responses, Wnt-11 signaling promotes cell viability. Hence Wnt-11 is involved in coordination of key signaling pathways.« less

Isolation of Erwinia chrysanthemi kduD mutants altered in pectin degradation.

PubMed Central

Condemine, G; Hugouvieux-Cotte-Pattat, N; Robert-Baudouy, J

1986-01-01

Mutants of Erwinia chrysanthemi impaired in pectin degradation were isolated by chemical and Mu d(Ap lac) insertion mutagenesis. A mutation in the kduD gene coding for 2-keto-3-deoxygluconate oxidoreductase prevented the growth of the bacteria on polygalacturonate as the sole carbon source. Analysis of the kduD::Mu d(Ap lac) insertions indicated that kduD is either an isolated gene or the last gene of a polycistronic operon. Some of the Mu d(Ap lac) insertions were kduD-lac fusions in which beta-galactosidase synthesis reflected kduD gene expression. In all these fusions, beta-galactosidase activity was shown to be sensitive to catabolite repression by glucose and to be inducible by polygalacturonate, galacturonate, and other intermediates of polygalacturonate catabolism. Galacturonate-mediated induction was prevented by a mutation which blocked its metabolism to 2-keto-3-deoxygluconate. 2-Keto-3-deoxygluconate appeared to be the true inducer of kduD expression resulting from galacturonate degradation. 5-Keto-4-deoxyuronate or 2,5-diketo-3-deoxygluconate were the true inducers, originating from polygalacturonate cleavage. These three intermediates also appeared to induce pectate lyases, oligogalacturonate lyase, and 5-keto-4-deoxyuronate isomerase synthesis. PMID:3949717

Matrix proteins of Nipah and Hendra viruses interact with beta subunits of AP-3 complexes.

PubMed

Sun, Weina; McCrory, Thomas S; Khaw, Wei Young; Petzing, Stephanie; Myers, Terrell; Schmitt, Anthony P

2014-11-01

Paramyxoviruses and other negative-strand RNA viruses encode matrix proteins that coordinate the virus assembly process. The matrix proteins link the viral glycoproteins and the viral ribonucleoproteins at virus assembly sites and often recruit host machinery that facilitates the budding process. Using a co-affinity purification strategy, we have identified the beta subunit of the AP-3 adapter protein complex, AP3B1, as a binding partner for the M proteins of the zoonotic paramyxoviruses Nipah virus and Hendra virus. Binding function was localized to the serine-rich and acidic Hinge domain of AP3B1, and a 29-amino-acid Hinge-derived polypeptide was sufficient for M protein binding in coimmunoprecipitation assays. Virus-like particle (VLP) production assays were used to assess the relationship between AP3B1 binding and M protein function. We found that for both Nipah virus and Hendra virus, M protein expression in the absence of any other viral proteins led to the efficient production of VLPs in transfected cells, and this VLP production was potently inhibited upon overexpression of short M-binding polypeptides derived from the Hinge region of AP3B1. Both human and bat (Pteropus alecto) AP3B1-derived polypeptides were highly effective at inhibiting the production of VLPs. VLP production was also impaired through small interfering RNA (siRNA)-mediated depletion of AP3B1 from cells. These findings suggest that AP-3-directed trafficking processes are important for henipavirus particle production and identify a new host protein-virus protein binding interface that could become a useful target in future efforts to develop small molecule inhibitors to combat paramyxoviral infections. Henipaviruses cause deadly infections in humans, with a mortality rate of about 40%. Hendra virus outbreaks in Australia, all involving horses and some involving transmission to humans, have been a continuing problem. Nipah virus caused a large outbreak in Malaysia in 1998, killing 109 people, and smaller outbreaks have since occurred in Bangladesh and India. In this study, we have defined, for the first time, host factors that interact with henipavirus M proteins and contribute to viral particle assembly. We have also defined a new host protein-viral protein binding interface that can potentially be targeted for the inhibition of paramyxovirus infections. Copyright © 2014, American Society for Microbiology. All Rights Reserved.

Matrix Proteins of Nipah and Hendra Viruses Interact with Beta Subunits of AP-3 Complexes

PubMed Central

Sun, Weina; McCrory, Thomas S.; Khaw, Wei Young; Petzing, Stephanie; Myers, Terrell

2014-01-01

ABSTRACT Paramyxoviruses and other negative-strand RNA viruses encode matrix proteins that coordinate the virus assembly process. The matrix proteins link the viral glycoproteins and the viral ribonucleoproteins at virus assembly sites and often recruit host machinery that facilitates the budding process. Using a co-affinity purification strategy, we have identified the beta subunit of the AP-3 adapter protein complex, AP3B1, as a binding partner for the M proteins of the zoonotic paramyxoviruses Nipah virus and Hendra virus. Binding function was localized to the serine-rich and acidic Hinge domain of AP3B1, and a 29-amino-acid Hinge-derived polypeptide was sufficient for M protein binding in coimmunoprecipitation assays. Virus-like particle (VLP) production assays were used to assess the relationship between AP3B1 binding and M protein function. We found that for both Nipah virus and Hendra virus, M protein expression in the absence of any other viral proteins led to the efficient production of VLPs in transfected cells, and this VLP production was potently inhibited upon overexpression of short M-binding polypeptides derived from the Hinge region of AP3B1. Both human and bat (Pteropus alecto) AP3B1-derived polypeptides were highly effective at inhibiting the production of VLPs. VLP production was also impaired through small interfering RNA (siRNA)-mediated depletion of AP3B1 from cells. These findings suggest that AP-3-directed trafficking processes are important for henipavirus particle production and identify a new host protein-virus protein binding interface that could become a useful target in future efforts to develop small molecule inhibitors to combat paramyxoviral infections. IMPORTANCE Henipaviruses cause deadly infections in humans, with a mortality rate of about 40%. Hendra virus outbreaks in Australia, all involving horses and some involving transmission to humans, have been a continuing problem. Nipah virus caused a large outbreak in Malaysia in 1998, killing 109 people, and smaller outbreaks have since occurred in Bangladesh and India. In this study, we have defined, for the first time, host factors that interact with henipavirus M proteins and contribute to viral particle assembly. We have also defined a new host protein-viral protein binding interface that can potentially be targeted for the inhibition of paramyxovirus infections. PMID:25210190

The Beta Pictoris circumstellar disk. XV - Highly ionized species near Beta Pictoris

NASA Technical Reports Server (NTRS)

Deleuil, M.; Gry, C.; Lagrange-Henri, A.-M.; Vidal-Madjar, A.; Beust, H.; Ferlet, R.; Moos, H. W.; Livengood, T. A.; Ziskin, D.; Feldman, P. D.

1993-01-01

Temporal variations of the Fe II, Mg II, and Al III circumstellar lines towards Beta Pictoris have been detected and monitored since 1985. However, the unusual presence of Al III ions is still puzzling, since the UV stellar flux from an A5V star such as Beta Pic is insufficient to produce such an ion. In order to better define the origin of such a phenomenon, new observations have been carried out to detect faint signatures of other highly ionized species in the short UV wavelength range, where the stellar continuum flux is low. These observations reveal variations not only near the C IV doublet lines, but also in C I and Al II lines, two weakly ionized species, not clearly detectable until now. In the framework of an infalling body scenario, highly ionized species would be created in the tail, far from the comet head, by collisions with ambient gas surrounding the star, or a weak stellar wind. Spectral changes have also been detected near a CO molecular band location, which, if confirmed, would provide the first molecular signature around Beta Pictoris.

Excitation Mechanism of O I Lines in Herbig Ae/Be Stars

NASA Astrophysics Data System (ADS)

Mathew, Blesson; Manoj, P.; Narang, Mayank; Banerjee, D. P. K.; Nayak, Pratheeksha; Muneer, S.; Vig, S.; Pramod Kumar, S.; Paul, K. T.; Maheswar, G.

2018-04-01

We have investigated the role of a few prominent excitation mechanisms viz. collisional excitation, recombination, continuum fluorescence, and Lyman beta fluorescence on the O I line spectra in Herbig Ae/Be stars. The aim is to understand which of them is the central mechanism that explains the observed O I line strengths. The study is based on an analysis of the observed optical spectra of 62 Herbig Ae/Be stars and near-infrared spectra of 17 Herbig Ae/Be stars. The strong correlation observed between the line fluxes of O I λ8446 and O I λ11287, as well as a high positive correlation between the line strengths of O I λ8446 and Hα suggest that Lyman beta fluorescence is the dominant excitation mechanism for the formation of O I emission lines in Herbig Ae/Be stars. Furthermore, from an analysis of the emission line fluxes of O I λλ7774, 8446, and comparing the line ratios with those predicted by theoretical models, we assessed the contribution of collisional excitation in the formation of O I emission lines.

Vector space methods of photometric analysis - Applications to O stars and interstellar reddening

NASA Technical Reports Server (NTRS)

Massa, D.; Lillie, C. F.

1978-01-01

A multivariate vector-space formulation of photometry is developed which accounts for error propagation. An analysis of uvby and H-beta photometry of O stars is presented, with attention given to observational errors, reddening, general uvby photometry, early stars, and models of O stars. The number of observable parameters in O-star continua is investigated, the way these quantities compare with model-atmosphere predictions is considered, and an interstellar reddening law is derived. It is suggested that photospheric expansion affects the formation of the continuum in at least some O stars.

Diadenosine tetraphosphate hydrolase is part of the transcriptional regulation network in immunologically activated mast cells.

PubMed

Carmi-Levy, Irit; Yannay-Cohen, Nurit; Kay, Gillian; Razin, Ehud; Nechushtan, Hovav

2008-09-01

We previously discovered that microphthalmia transcription factor (MITF) and upstream stimulatory factor 2 (USF2) each forms a complex with its inhibitor histidine triad nucleotide-binding 1 (Hint-1) and with lysyl-tRNA synthetase (LysRS). Moreover, we showed that the dinucleotide diadenosine tetraphosphate (Ap(4)A), previously shown to be synthesized by LysRS, binds to Hint-1, and as a result the transcription factors are released from their suppression. Thus, transcriptional activity is regulated by Ap(4)A, suggesting that Ap(4)A is a second messenger in this context. For Ap(4)A to be unambiguously established as a second messenger, several criteria have to be fulfilled, including the presence of a metabolizing enzyme. Since several enzymes are able to hydrolyze Ap(4)A, we provided here evidence that the "Nudix" type 2 gene product, Ap(4)A hydrolase, is responsible for Ap(4)A degradation following the immunological activation of mast cells. The knockdown of Ap(4)A hydrolase modulated Ap(4)A accumulation, resulting in changes in the expression of MITF and USF2 target genes. Moreover, our observations demonstrated that the involvement of Ap(4)A hydrolase in gene regulation is not a phenomenon exclusive to mast cells but can also be found in cardiac cells activated with the beta-agonist isoproterenol. Thus, we have provided concrete evidence establishing Ap(4)A as a second messenger in the regulation of gene expression.

VizieR Online Data Catalog: Calibrator stars catalog for interferometers (Swihart+, 2017)

NASA Astrophysics Data System (ADS)

Swihart, S. J.; Garcia, E. V.; Stassun, K. G.; van Belle, G.; Mutterspaugh, M. W.; Elias, N.

2017-04-01

In order to obtain accurate stellar angular sizes, each star was fit with a model SED using the fitting routine sedFit, written by A. Boden (van Belle & von Braun, 2009, Cat. J/ApJ/694/1085; van Belle et al. 2016, Cat. J/AJ/152/16). We compiled a list of positions, spectral types and visual magnitudes for ~3000 bright (Vmag<6) stars in the northern hemisphere with declinations -15°<δ<82° using the SIMBAD database (Wenger et al., 2000A&AS..143....9W). We chose a brightness limit (Vmag<6) given that most visible light interferometers can obtain scientifically useful data on bright stars. We also removed any stars which appear in the JMMC bad calibrator list. (4 data files).

Influence of Coronal Abundance Variations

NASA Technical Reports Server (NTRS)

Scargle, Jeffrey D. (Technical Monitor); Kashyap, Vinay

2005-01-01

The PI of this project was Jeff Scargle of NASA/Ames. Co-I's were Alma Connors of Eureka Scientific/Wellesley, and myself. Part of the work was subcontracted to Eureka Scientific via SAO, with Vinay Kashyap as PI. This project was originally assigned grant number NCC2-1206, and was later changed to NCC2-1350 for administrative reasons. The goal of the project was to obtain, derive, and develop statistical and data analysis tools that would be of use in the analyses of high-resolution, high-sensitivity data that are becoming available with new instruments. This is envisioned as a cross-disciplinary effort with a number of "collaborators" including some at SA0 (Aneta Siemiginowska, Peter Freeman) and at the Harvard Statistics department (David van Dyk, Rostislav Protassov, Xiao-li Meng, Epaminondas Sourlas, et al). We have developed a new tool to reliably measure the metallicities of thermal plasma. It is unfeasible to obtain high-resolution grating spectra for most stars, and one must make the best possible determination based on lower-resolution, CCD-type spectra. It has been noticed that most analyses of such spectra have resulted in measured metallicities that were significantly lower than when compared with analyses of high- resolution grating data where available (see, e.g., Brickhouse et al., 2000, ApJ 530,387). Such results have led to the proposal of the existence of so-called Metal Abundance Deficient, or "MAD" stars (e.g., Drake, J.J., 1996, Cool Stars 9, ASP Conf.Ser. 109, 203). We however find that much of these analyses may be systematically underestimating the metallicities, and using a newly developed method to correctly treat the low-counts regime at the high-energy tail of the stellar spectra (van Dyk et al. 2001, ApJ 548,224), have found that the metallicities of these stars are generally comparable to their photospheric values. The results were reported at the AAS (Sourlas, Yu, van Dyk, Kashyap, and Drake, 2000, BAAS 196, v32, #54.02), and at the conference on Statistical Challenges in Modem Astronomy (Sourlas, van Dyk, Kashyap, Drake, and Pease, 2003, SCMA 111, Eds. E.D.Feigelson, G.J.Babu, New York:Springer, p489-490). We also described the limitations of one of the most egregiously misused and misapplied statistical tests in astrophysical literature, the F-test for verifying model components (Protassov, van Dyk, Connors, Kashyap, and Siemiginowska, 2002, ApJ, 571,545). Indeed, a search through the ApJ archives turned up 170 papers in the 5 previous years that used the F-test explicitly in some form or the other, and with the vast majority of them not using it correctly! Indeed, looking at just 4 issues of the ApJ in 2001, we found 13 instances of its use, of which nine were demonstrably incorrect. Clearly, it is difficult to understate the importance of this issue. We also worked on speeding up Bayes Blocks and Sparse Bayes Blocks algorithms to make them more tractable for large searches. We also supported staistics students and postdocs in both explicit physics- model-based (spectra with tens of thousands of atomic lines) and "model-free" -- i.e. non-parametric or semi-parametric -- algorithms. Work on using more of the latter is just beginning; while using multi-scale methods for Poisson imaging has come to hition. In fact, "An Image Restoration Technique with Error Estimates", by D. Esch, A. Connors, M. Karovska, and D. van Dyk, was published by ApJ (Esch et a1.2004, ApJ, 610, 1213). The code has been delivered to M. Karovska for CXC; and is available for beta-testing upon request. The other large project we worked on was on the self-consistent modeling of logN-logs curves in the Poisson limit. logN-logs curves are a fundamental tool in the study of source populations, luminosity functions, and cosmological parameters. However, their determination is hampered by statistical effects such as the Eddington bias, incompleteness due to detection efficiency, faint source flux fluctuations, etc. We have develed a new and powerful method using the full Poisson machinery that allows us to model the logN-logs distribution of X-ray sources in a self-consistent manner. Because we properly account for all the above statistical effects, our modeling is valid over the full range of the data, and not just for strong sources, as is normally done. Using a Bayesian approach and modeling the fluxes with known functional forms such as simple or broken power-laws, and conditioning the expected photon counts on the fluxes, the background contamination, effective area, detector vignetting, and detection probability, we can delve deeply into the low counts regime and extend the usefulness of medium sensitivity surveys such as ChAMP by orders of magnitude. The built-in flexibility of the algorithm also allows a simultaneous analysis of multiple datasets. We have applied this analysis to a set a Chandra observations (Sourlas, Kashyap, Zezas, van Dyk, 2004, HEAD #8, #16.32)

Comparison of sublingual tablets with nitroglycerin complexed with beta-cyclodextrin or titrated with crosspovidone--technological approach.

PubMed

Centkowska, Katarzyna; Sznitowska, Małgorzata

2008-01-01

Fast disintegrating sublingual tablets containing nitroglycerin either complexed with beta-cyclodextrin (NTG-CD) or titrated with crosspovidone (NTG-CP) were prepared using Starch 1500 or StarLac as disintegrants. Regarding disintegration time and stability of the active substance Starch 1500 was more appropriate for NTG-CD while for NTG-CP StarLac was suitable. Stability of NTG was better in NTG-CD tablets than in NTG-CP tablets, however, within 12 months of storage at 25 degrees C the loss of NTG in all formulations was still greater than 10%.

Morphology of Gas in the Galactic Center from Spectroscopy of H_3^+

NASA Astrophysics Data System (ADS)

Oka, Takeshi; Geballe, Thomas R.; Indriolo, Nick; Goto, Miwa

2012-06-01

Over the last several years our observations of the infrared spectrum of H_3^+ toward the Galactic center (GC) have established a high ionization rate (ζ > 2 × 10-15 s-1) and the existence of a vast amount of warm (T ˜250 K) and diffuse (n < 100 cm-3) gas with a high volume filling factor (f > 0.3) in the Central Molecular Zone (CMZ) of the GC, a region of radius ˜150 pc. These findings are gradually being assimilated into the astrophysics of the GC. Determining the morphology of this gas is difficult because the sightlines for study are limited by the uncontrollable locations of background stars suitable for spectroscopy of H_3^+. There are wide longitudinal gaps in the locations of those stars and the precise radial locations of the stars within the CMZ are uncertain. Nevertheless, the velocity profiles of the observed H_3^+ spectra indicate the presence of the Expanding Molecular Ring (EMR), a structure containing mostly diffuse gas expanding from the center with velocities of up to 180 km s-1 and bordering the CMZ. On the other hand, the 120 pc Molecular Ring, an inner t ring of cold dust and dense gas with radius ˜100 pc is not clearly seen in H_3^+. This is possibly because the sightlines that we have observed to date lie close to the Galactic plane and miss the ring, which goes above and below the Galactic plane. Oka, T., Geballe, T.R., Goto, M., Usuda, T., McCall, B.J. 2005, ApJ, 632, 882 Goto, Usuda, Nagata, Geballe, McCall, Indriolo, Suto, Henning, Morong, and Oka, 2008, ApJ, 688, 306. Geballe, T.R. and Oka, T. 2010, ApJ, 709, L70 Sofue, Y. 1995, PASJ, 47, 527 Molinari, S. et al. 2011, ApJ, 735, L33.

VizieR Online Data Catalog: The 4 brightest red giants in the UFD galaxy Ret 2 (Roederer+, 2016)

NASA Astrophysics Data System (ADS)

Roederer, I. U.; Mateo, M.; Bailey, J. I., III; Song, Y.; Bell, E. F.; Crane, J. D.; Loebman, S.; Nidever, D. L.; Olszewski, E. W.; Shectman, S. A.; Thompson, I. B.; Valluri, M.; Walker, M. G.

2018-03-01

There are only four stars brighter than the horizontal branch that are confirmed members of Ret 2 (Simon et al. 2015, J/ApJ/808/95; Walker et al. 2015, J/ApJ/808/108). We observed these four stars using one arm of the Michigan/Magellan Fiber System (M2FS) and MSpec double spectrograph (Bailey et al. 2012SPIE.8446E..5GB; Mateo et al. 2012SPIE.8446E..4YM) mounted on the Nasmyth platform at the 6.5 m Landon Clay Telescope (Magellan II) at Las Campanas Observatory, Chile. We observed four high-probability members of Ret 2 and one blank sky position simultaneously on 2015 November 14 and 16, with a total integration time of 6.67 hr. Both observations were taken in dark time. (4 data files).

Spectroscopic parallaxes of MAP region stars from UBVRI, DDO, and uvbyH-beta photometry. [Multichannel Astrometric Photometer for astronomical observation

NASA Technical Reports Server (NTRS)

Persinger, Tim; Castelaz, Michael W.

1990-01-01

This paper presents the results of spectral type and luminosity classification of reference stars in the Allegheny Observatory MAP parallax program, using broadband and intermediate-band photometry. In addition to the use of UBVRI and DDO photometric systems, the uvbyH-beta photometric system was included for classification of blue (B - V less than 0.6) reference stars. The stellar classifications made from the photometry are used to determine spectroscopic parallaxes. The spectroscopic parallaxes are used in turn to adjust the relative parallaxes measured with the MAP to absolute parallaxes. A new method for dereddening stars using more than one photometric system is presented. In the process of dereddening, visual extinctions, spectral types, and luminosity classes are determined, as well as a measure of the goodness of fit. The measure of goodness of fit quantifies confidence in the stellar classifications. It is found that the spectral types are reliable to within 2.5 spectral subclasses.

An Emission Measure Analysis of Stars Near the Transition Region Dividing Line

NASA Astrophysics Data System (ADS)

Linsky, Jeffery L.

We request high dispersion, short wavelength IUE spectra for three of the stars beta Gem (K0III), alpha Tau (K5III), epsilon Gem (G81b) and beta Cam (G0Ib) with exposure times of 16 hours or greater. These data will allow the measurement of line profiles, widths and Doppler shifts as well as density sensitive and opacity sensitive line ratios. Models of chromospheric and transition region structure will be calculated by emission measure techniques and model atmosphere computations for optically thick resonance lines such as MgII h and k, including partial redistribution radiation transfer. The chromospheric models will be used to investigate the energy balance of the atmosphere and the nature of the energy deposition processes. These results will be considered in relation to the evolutionary status of the stars, and will be compared with the atmospheric model properties of other stars previously studied by the authors and their collaborators.

The 90-day report for SL4 experiment S019: UV stellar astronomy

NASA Technical Reports Server (NTRS)

1974-01-01

The use of Experiment S019 to obtain moderate dispersion stellar spectra extending down to 1300A with sufficient spectral resolution to permit the study of ultraviolet (UV) line spectra and of spectral energy distributions of early-type stars is studied. Data obtained from this experiment should be of sufficient accuracy to permit detailed physical analysis of individual stars and nebulae, but an even more basic consideration is the expectation of obtaining spectra of a sufficient number of stars so that a statistically meaningful survey may be made of the UV spectra of a wide variety of star types. These should include all luminosity classes of spectral types O, B and A, as well as peculiar stars such as Wolf-Rayet stars and Ap or Am stars. An attempt was also made to obtain, in the no-prism mode, low dispersion UV spectra in a number of Milky Way star fields and in nearby galaxies.

[Achievements and problems of modern trials of antihypertensive drugs].

PubMed

Kobalava, Zh D; Kotovskaia, Iu V

2011-01-01

Most important value of lowering of substantially elevated arterial pressure (AP) for improvement of outcomes in patients with arterial hypertension (AH) was convincingly confirmed by large truly placebo controlled randomized clinical trials (RCT) with the use of mainly diuretics, and/or beta-adrenoblockers in the 60-80ths. Later comparative RCT confirmed equal antihypertensive efficacy of 5 main drug classes relative to AP level in brachial artery. In this review we discuss merit of auxiliary class-specific properties of antihypertensive agents potentially affecting prognosis besides AP lowering. We also discuss problems related to decline of significance of quantitative criteria of AH and consideration of AP level in general context of cardiovascular risk; problems of external validity of RCT; extrapolation of RCT results obtained in patients with complicated AH and very high cardiovascular risk on young patients with uncomplicated AH; significance of hard and surrogate end points.

Beta-blocking agents during electroconvulsive therapy: a review.

PubMed

Boere, E; Birkenhäger, T K; Groenland, T H N; van den Broek, W W

2014-07-01

Electroconvulsive therapy (ECT) is associated with at least transient episodes of hypertension and tachycardia. Beta-blocking agents may be indicated to prevent cardiovascular complications and may shorten seizure duration. This review evaluates studies that used beta-blocking agents during ECT to determine which agent has the most favourable outcomes on cardiovascular variables and seizure duration. A Medline database search was made using the combined keywords 'adrenergic beta-antagonists' and 'electroconvulsive therapy'. The search was restricted to double-blind randomized controlled trials and yielded 29 original studies. With the use of esmolol, significant attenuating effects were found on cardiovascular parameters in the first 5 min after stimulation; its shortening effects on seizure duration may be dose-related. With the use of labetalol, findings on cardiovascular effects were inconsistent during the first minutes after stimulation but were significant after 5 min and thereafter; seizure duration was scarcely studied. Landiolol attenuates heart rate but with inconsistent findings regarding arterial pressure (AP); seizure duration was mostly unaffected. Esmolol appears to be effective in reducing the cardiovascular response, although seizure duration may be affected with higher dosages. Landiolol can be considered a suitable alternative, but effects on AP need further investigation. Labetalol has been studied to a lesser extent and may have prolonged cardiovascular effects. The included studies varied in design, methodology, and the amount of exact data provided in the publications. Further study of beta-blocking agents in ECT is clearly necessary. © The Author [2014]. Published by Oxford University Press on behalf of the British Journal of Anaesthesia. All rights reserved. For Permissions, please email: journals.permissions@oup.com.

Polarized radiation diagnostics of stellar magnetic fields

NASA Astrophysics Data System (ADS)

Mathys, Gautier

The main techniques used to diagnose magnetic fields in stars from polarimetric observations are presented. First, a summary of the physics of spectral line formation in the presence of a magnetic field is given. Departures from the simple case of linear Zeeman effect are briefly considered: partial Paschen-Back effect, contribution of hyperfine structure, and combined Stark and Zeeman effects. Important approximate solutions of the equation of transfer of polarized light in spectral lines are introduced. The procedure for disk-integration of emergent Stokes profiles, which is central to stellar magnetic field studies, is described, with special attention to the treatment of stellar rotation. This formalism is used to discuss the determination of the mean longitudinal magnetic field (through the photographic technique and through Balmer line photopolarimetry). This is done within the specific framework of Ap stars, which, with their unique large-scale organized magnetic fields, are an ideal laboratory for studies of stellar magnetism. Special attention is paid to those Ap stars whose magnetically split line components are resolved in high-dispersion Stokes I spectra, and to the determination of their mean magnetic field modulus. Various techniques of exploitation of the information contained in polarized spectral line profiles are reviewed: the moment technique (in particular, the determination of the crossover and of the mean quadratic field), Zeeman-Doppler imaging, and least-squares deconvolution. The prospects that these methods open for linear polarization studies are sketched. The way in which linear polarization diagnostics complement their Stokes I and V counterparts is emphasized by consideration of the results of broad band linear polarization measurements. Illustrations of the use of various diagnostics to derive properties of the magnetic fields of Ap stars are given. This is used to show the interest of deriving more physically realistic models of the geometric structure of these fields. How this can possibly be achieved is briefly discussed. An overview of the current status of polarimetric studies of magnetic fields in non-degenerate stars of other types is presented. The final section is devoted to magnetic fields of white dwarfs. Current knowledge of magnetic fields of isolated white dwarfs is briefly reviewed. Diagnostic techniques are discussed, with particular emphasis on the variety of physical processes to be considered for understanding of spectral line formation over the broad range of magnetic field strengths encountered in these stars.

Probing conformational changes in the I-like domain and the cysteine-rich repeat of human beta 3 integrins following disulfide bond disruption by cysteine mutations: identification of cysteine 598 involved in alphaIIbbeta3 activation.

PubMed

Chen, P; Melchior, C; Brons, N H; Schlegel, N; Caen, J; Kieffer, N

2001-10-19

We have investigated receptor function and epitope expression of recombinant alpha(IIb)beta(3) mutated at Cys(177) or Cys(273) in the I-like domain as well as Cys(598), located in the fourth repeat of the membrane-proximal cysteine-rich region and mutated in a Glanzmann's thrombasthenia type II patient. The beta(3) mutants beta(3)C177A, beta(3)C273A, and beta(3)C598Y exhibited a decreased electrophoretic mobility in SDS-polyacrylamide gel electrophoresis under nonreducing conditions, confirming the disruption of the respective disulfide loops. Despite reduced surface expression, the alpha(IIb)beta(3)C177A, alpha(IIb)beta(3)C273A, and alpha(IIb)beta(3)C598Y receptors mediated cell adhesion to immobilized fibrinogen and translocated into focal adhesion plaques. The beta(3)C598Y mutation, but not the beta(3)C177A or beta(3)C273A mutations, induced spontaneous binding of the ligand mimetic monoclonal antibody PAC-1, while the beta(3)C177A and beta(3)C273A mutants exhibited reduced complex stability in the absence of Ca(2+). Epitope mapping of function-blocking monoclonal antibodies (mAbs) allowed the identification of two distinct subgroups; mAbs A2A9, pl2-46, 10E5, and P256 did not interact with alpha(IIb)beta(3)C273A and bound only weakly to alpha(IIb)beta(3)C177A, while mAbs AP2, LM609 and 7E3 bound normally to mutant alpha(IIb)beta(3)C273A, but interacted only weakly with mutant alpha(IIb)beta(3)C177A. Furthermore, a cryptic epitope recognized by mAb 4D10G3 and not exposed on wild type alpha(IIb)beta(3) became accessible only on mutant alpha(IIb)beta(3)C177A and was mapped to the 60-kDa chymotrypsin fragment of beta(3). Finally, the ligand-induced binding site (LIBS) epitopes AP5, D3, LIBS1, and LIBS2 were spontaneously expressed on all three mutants independent of RGDS or dithiothreitol treatment. Our results provide evidence that disruption of a single cysteine disulfide bond in the cysteine-rich repeat domain, but not in the I-like domain, activates integrin alpha(IIb)beta(3). In contrast, disruption of each of the disulfide bonds in the two long insertions of the I-like domain predicted to be in close contact with the alpha subunit beta-propeller domain affect the stability of the alpha(IIb)beta(3) heterodimer and inhibit complex-specific mAb binding without affecting the RGD binding capacity of the metal ion-dependent adhesion site-like domain.

Identifying Young, Nearby Stars

NASA Technical Reports Server (NTRS)

Webb, Rich; Song, Inseok; Zuckerman, Ben; Bessell, Mike

2001-01-01

Young stars have certain characteristics, e.g., high atmospheric abundance of lithium and chromospheric activity, fast rotation, distinctive space motion and strong X-ray flux compared to that of older main sequence stars. We have selected a list of candidate young (<100Myr) and nearby (<60pc) stars based on their space motion and/or strong X-ray flux. To determine space motion of a star, one needs to know its coordinates (RA, DEC), proper motion, distance, and radial velocity. The Hipparcos and Tycho catalogues provide all this information except radial velocities. We anticipate eventually searching approx. 1000 nearby stars for signs of extreme youth. Future studies of the young stars so identified will help clarify the formation of planetary systems for times between 10 and 100 million years. Certainly, the final output of this study will be a very useful resource, especially for adaptive optics and space based searches for Jupiter-mass planets and dusty proto-planetary disks. We have begun spectroscopic observations in January, 2001 with the 2.3 m telescope at Siding Spring Observatory (SSO) in New South Wales, Australia. These spectra will be used to determine radial velocities and other youth indicators such as Li 6708A absorption strength and Hydrogen Balmer line intensity. Additional observations of southern hemisphere stars from SSO are scheduled in April and northern hemisphere observations will take place in May and July at the Lick Observatory of the University of California. AT SSO, to date, we have observed about 100 stars with a high resolution spectrometer (echelle) and about 50 stars with a medium spectral resolution spectrometer (the "DBS"). About 20% of these stars turn out to be young stars. Among these, two especially noteworthy stars appear to be the closest T-Tauri stars ever identified. Interestingly, these stars share the same space motions as that of a very famous star with a dusty circumstellar disk--beta Pictoris. This new finding better constrains the age of beta Pictoris to be approx. 10 Myr.

VizieR Online Data Catalog: Rotation-Activity Correlations in K-M dwarfs II. (Houdebine+, 2017)

NASA Astrophysics Data System (ADS)

Houdebine, E. R.; Mullan, D. J.; Bercu, B.; Paletou, F.; Gebran, M.

2017-10-01

The spectra that we use for determining the CaII and Hα equivalent widths in the present study of dK4-dM4 stars came from three different echelle spectrographs; HARPS (High Accuracy Radial velocity Planet Search, ESO), SOPHIE (OHP), and FEROS (The Fiber-fed Extended Range Optical Spectrograph). The stars in our samples include all stars from all observing programs that have been carried out with HARPS and SOPHIE for stars belonging to the following spectral sub-types: dK4, dK6, dM2, and dM3. For dM4 stars, we compiled all measurements of vsini available in the literature (see Paper I; Houdebine+ 2016, J/ApJ/822/97). For the dK6 and dM3 samples, we also supplemented our own measurements with measurements available in the literature, notably for active stars (see Paper I). (7 data files).

The Origin and Evolution of the Galaxy Star Formation Rate-Stellar Mass Correlation

NASA Astrophysics Data System (ADS)

Gawiser, Eric; Iyer, Kartheik

2018-01-01

The existence of a tight correlation between galaxies’ star formation rates and stellar masses is far more surprising than usually noted. However, a simple analytical calculation illustrates that the evolution of the normalization of this correlation is driven primarily by the inverse age of the universe, and that the underlying correlation is one between galaxies’ instantaneous star formation rates and their average star formation rates since the Big Bang.Our new Dense Basis method of SED fitting (Iyer & Gawiser 2017, ApJ 838, 127) allows star formation histories (SFHs) to be reconstructed, along with uncertainties, for >10,000 galaxies in the CANDELS and 3D-HST catalogs at 0.5

Long-term outcomes in patients with schizophrenia treated with risperidone long-acting injection or oral antipsychotics in Spain: results from the electronic Schizophrenia Treatment Adherence Registry (e-STAR).

PubMed

Olivares, J M; Rodriguez-Morales, A; Diels, J; Povey, M; Jacobs, A; Zhao, Z; Lam, A; Villalobos Vega, J C; Cuéllar, J Alonso; de Castro, F J Alberca; Quintero, C Morillo-Velarde; Martíin, J F Román; Domínguez, P Tabares; Ojeda, J L Prados; Cortés, S Sanz; Cala, F I Mata; Marín, C Gutiérrez; Castro, L Moyano; Duaso, M A Haza; Albarracín, J Requena; Vergara, G Narbona; Benítez, A Fernández; Cleries, F Mayoral; Pérez-Brian, J M García-Herrera; Aragón, A Bordallo; Navarro, J C Rodríguez; Biedma, J A Algarra; de Pedro, R Bravo; González, J F Delgado; López, M E Jaén; Moreno, H Díaz; López, J A Soto; Rodríguez, E Ojeda; de Hoyos, C Martínez; Sacristán, M Pardilla; Martín, M D Molina; Ballesteros, E Martín; Rodríguez, P A Sopelana; Menéndez, L Fernández; Rivas, R Santos; del Pino Cuadrado, P; Lauffer, J Correas; Solano, J J Rodríguez; Martínez, J M Fernández; Solano, F García; Rodríguez, P García-Lamberde; Rodríguez, J A Romero; Cano, T Rodríguez; Fortacin, M Ducaju; Lobeiras, J M Blanco; Sampedro, J M Piñeiro; Bravo, A Pérez; Pellicer, A Fernández; López, M D Alonso; Liste, J Fraga; Fernández, M Riobo; Losada, A Casas; Mendez, R Vazquez-Noguerol; Romero, S Agra; Blanco, J J Blanco; Bonaselt, I Tortajada; Mahia, M C García; del Valle, E Ferrer Gómez; Yañez, P Quiroga; Camarasa, M Gelabert; Alonso, J A Barbado; Mendez, G Florez; Feliz, F Doce; Lamela, M A López; Piñero, M Vega; Alvarado, P Fuentes; Gómez, I López; Martín, P Fadon; Gómez, J L Santos; López, A García; Jiménez, A Rodríguez; Nafs, A Escudero; Barquero, N Casas; Ortiz, R Fernández-Villamor; Noguera, J L Velez; Carrasco, P Ruiz; Muñoz, J Martín; Palma, M Masegoza; Hortelano, C Marín; Bonome, L Sánchez; Sevilla, J Sánchez; Juan, J M Mongil San; Ramos, J M García; Muñoz, J L Vallejo; Guisasola, J Elorza; Vazquez, L Santamaria; Guerras, F Campo; Nebot, F J Arrufat; Fernández, F J Baron; Nicolau, A L Palomo; Subirats, R Catala; Kidias, M Messays; Navarro, V Fabregat; García, B Frades; del Rosal, F Mejias; de Vicente Muñoz, T; Ballester, J Año; Lieb, P Malabia; Martel, A Delgado; Bea, E Roca; Joaquim, I Grau; Enjuanes, F Boatas; Piñol, M Bañuelos; Carbonell, E Fontova I; Muñoz, R Martín; Giribets, C Argila; Sans, L Albages; Blanco, A Serrano; Felipe, M Arcega; Muñoz, P González; Villanueva, A Pons; Arroyo, M Bernardo; Borri, R Coronas; Fallada, S Miret; Merola, M Celma; Rodon, E Parellada; Palmes, J R Pigem; Martínez, E Pérez; Catala, J Matarredona; Coca, A Sandoval; Ferrandiz, F Pascual; Paya, E Ferrandiz; Caballero, G Iturri; Bonet, A Franco; Figueras, J Fluvia; Pagador, P Moreno; Garibo, M Medina; Camo, V Pérez; Carrillo, C Sanz; Valero, C Pelegrin; Rebollo, F J Caro; García Campayo, J; Sala Ayma, J M Sala; Roig, M Martínez; de Uña Mateos, M A; Bertolin, R García; García, A Martín; Mazo, F Jiménez; Velasco, J L Galvez; Pérez, L Santa Maria; Casado, C Jiménez; Barba, J J Mancheño; Diaz, M Conde; Rubio, J P Alcon; Mandoli, A Soler; Herrero, A Uson; Martínez, A Rodríguez; Serrano, P Salgado; Rodríguez, E Nieto; Montesinos, J Segui; Macia, J Ferragud; Mateos Marcos, A Mateos; Soto, J V Pérez-Fuster; Dumont, M Verdaguer; Pagan, J Parra; Martínez, V Balanza; Santiuste de Pablos, M; Delgado, C Espinosa; Quiles, M D Martínez; López, F J Manzanera; Navarro, P Pozo; Torres, A Micol; Ingles, F J Martínez; Arias-Camison, J M Salmeron; Manzano, J C López; Peña, R Villanueva; Guitarte, G Petersen; Fontecilla, H Blasco; Romero, J Barjau; Gil, R Sanz; Lozano, J Marín; Adanez, L Donaire; Zarranz Herrera-Oria, I; Jiménez, J Pérez; Vaz, F Carrato; García, O Sanz; Anton, C Contreras; Casula, R Reixach; Hernandez, M C Natividad; Escabias, F Teba; Torresano, J Rodríguez; Pérez-Villamil, A Huidobro; Estevez, L; Figuero, M Aragües; Muñoz de Morales, A; Calvin, J L Rodríguez; Criado, M Delgado; Rodríguez, V Molina; Ambrosolio, E Balbo; Madera, P M Holgado; Alfaro, G Ponce; Vidal, M M Rojas; Valtuille, A García; Ruiz, O; Cabornero, G Lucas; Echevarria Martínez de Bujo, M; Mallen, M J Maicas; Puigros, J Santandreu; Martorell, A Liñana; Forteza, A Clar; Arrebola, E Rodríguez; Rodríguez de la Torre, M; Saiz, C G Anton; Bardolet I Casas, C; Linde, E Rodríguez; De Arce Cordon, R; Molina, E M Padial; Carazo, F J Ruiz; Romero, J J Muro; Cano, D Vico; Dorado, M Soria; Velazquez, S Campos; Sánchez, A J Rodríguez; Leon, S Ocio; Sánchez, K Pachas; Benitez, M Henry; Zugarramurai, A Intxausti; Contreras, M A; De la Varga González, M; Marín, P Barreiro; Robina, F Gómez; García, M Sánchez; Pérez, F J Otero; Bros, P Cubero; Gómez, A Carrillo; de Dios Molina Martín, J; Perera, J L Carrasco; Averbach, M C; Perera, J L Carrasco; Palancares, E Goenaga; Gallego de Dios, M T; Rojo, C Fernández; Iglesias, S Sánchez; Merino, M I Rubio; Mestre, N Prieto; Urdaniz, A Pérez; Sánchez, J M Martínez; Seco, R Gordo; Muñoz, J Franco; Agut, M Mateos; Lozano, M L Blanco; Herguedas, F Martín; Pena, A Torcal; García, J Vicente; Martínez, A Varona; Sanz Granado, O Sanz; Fernández, M A Medina; Canseco, J M Moran; López, P A Megia; Martín, M A Franco; Barrio, J A Espina; Ubago, J Giner; Bennassar, M Roca; Díez, J M Olivares; Fleta, J L Hernandez; Fortes, F Porras; López, C Arango; Medina, O; Alvarez, D Figuera; Roca, J M Peña; Valladolid, G Rubio; Tavera, J A Furquet; García-Castrillon Sales, J A; Llordes, I Batalla; Melgarejo, C Anchuistegui; Cañas de la Paz, F; Callol, V Vallés; García, M Bousoño; García, J Bobes; Leal, F J Vaz; Corrales, E Cáceres; Iglesias, E Sánchez; Gómez, M A Carreiras; Serrano, G García; Chillarón, E G Román; Aguado, F J Samino; Castillo, J J Molina; González, A González; Vázquez, J Gallardo; Peralvarez, M Bolivar; Diaz, M Rios; Mesa, M Ybarzabal; Artiles, F J Acosta; Chao, M Ajoy; Mesa, M Ybarzabal; del Rosario Santana, P; Escudero, M A García; Berenguer, M Molla; Llacer, J M Bonete; Berna, J A Juan; Ortiz, J Barragán; Pardell, L Tost; Hernández-Alvarez de Sotomayor, C; Méndez, M R Cejas; Garate, R Cabrera; Múgica, B Díaz; González, M Caballero; Domingo, J Pujol; Navarro, C Sáez; Vera, G Selva; Cuquerella, M A; Monzo, J Lonjedo; Boada, P Cervera; Pérez, M F Martín; Parrado, E Carrasco; Sánchez, J J Yañez; Fernández, J Calvo

2009-06-01

The electronic Schizophrenia Treatment Adherence Registry (e-STAR) is a prospective, observational study of patients with schizophrenia designed to evaluate long-term treatment outcomes in routine clinical practice. Parameters were assessed at baseline and at 3 month intervals for 2 years in patients initiated on risperidone long-acting injection (RLAI) (n=1345) or a new oral antipsychotic (AP) (n=277; 35.7% and 36.5% on risperidone and olanzapine, respectively) in Spain. Hospitalization prior to therapy was assessed by a retrospective chart review. At 24 months, treatment retention (81.8% for RLAI versus 63.4% for oral APs, p<0.0001) and reduction in Clinical Global Impression Severity scores (-1.14 for RLAI versus -0.94 for APs, p=0.0165) were significantly higher with RLAI. Compared to the pre-switch period, RLAI patients had greater reductions in the number (reduction of 0.37 stays per patient versus 0.2, p<0.05) and days (18.74 versus 13.02, p<0.01) of hospitalizations at 24 months than oral AP patients. This 2 year, prospective, observational study showed that, compared to oral antipsychotics, RLAI was associated with better treatment retention, greater improvement in clinical symptoms and functioning, and greater reduction in hospital stays and days in hospital in patients with schizophrenia. Improved treatment adherence, increased efficacy and reduced hospitalization with RLAI offer the opportunity of substantial therapeutic improvement in schizophrenia.

Constituents of ophiuroidea. 1. Isolation and structure of three ganglioside molecular species from the brittle star Ophiocoma scolopendrina.

PubMed

Inagaki, M; Shibai, M; Isobe, R; Higuchi, R

2001-12-01

Three ganglioside molecular species, OSG-0 (1), OSG-1 (2), and OSG-2 (3) have been obtained from the polar lipid fraction of the chloroform/methanol extract of the brittle star Ophiocoma scolopendrina. The structures of these gangliosides have been determined on the basis of chemical and spectroscopic evidence as 1-O-[(N-glycolyl-alpha-D-neuraminosyl)-(2-->6)-beta-D-glucopyranosyl]-ceramide (1), 1-O-[8-O-sulfo-(N-acetyl-alpha-D-neuraminosyl)-(2-->6)-beta-D-glucopyranosyll-ceramide (2) and 1-O-[(N-glycolyl-alpha-D-neuraminosyl)-(2-->8)-(N-acetyl- and N-glycolyl-alpha-D-neuraminosyl)-(2-->6)-beta-D-glucopyranosyl]-ceramide (3). The ceramide moieties were composed of heterogeneous unsubstituted fatty acid, 2-hydroxy fatty acid and phytosphingosine units. Compounds 2 and 3 represent new ganglioside molecular species.

Modelling element distributions in the atmospheres of magnetic Ap stars

NASA Astrophysics Data System (ADS)

Alecian, G.; Stift, M. J.

2007-11-01

Context: In recent papers convincing evidence has been presented for chemical stratification in Ap star atmospheres, and surface abundance maps have been shown to correlate with the magnetic field direction. Radiatively driven diffusion, which is known to be sensitive to the magnetic field strength and direction, is among the processes responsible for these inhomogeneities. Aims: Here we explore the hypothesis that equilibrium stratifications - such that the diffusive particle flux is close to zero throughout the atmosphere - can, in a number of cases, explain the observed abundance maps and vertical distributions of the various elements. Methods: An iterative scheme adjusts the abundances in such a way as to achieve either zero particle flux or zero effective acceleration throughout the atmosphere, taking strength and direction of the magnetic field into account. Results: The investigation of equilibrium stratifications in stellar atmospheres with temperatures from 8500 to 12 000 K and fields up to 10 kG reveals considerable variations in the vertical distribution of the 5 elements studied (Mg, Si, Ca, Ti, Fe), often with zones of large over- or under-abundances and with indications of other competing processes (such as mass loss). Horizontal magnetic fields can be very efficient in helping the accumulation of elements in higher layers. Conclusions: A comparison between our calculations and the vertical abundance profiles and surface maps derived by magnetic Doppler imaging reveals that equilibrium stratifications are in a number of cases consistent with the main trends inferred from observed spectra. However, it is not clear whether such equilibrium solutions will ever be reached during the evolution of an Ap star.

The evidence for clumpy accretion in the Herbig Ae star HR 5999

NASA Technical Reports Server (NTRS)

Perez, M. R.; Grady, C. A.; The, P. S.

1993-01-01

Analysis of IUE high- and low-dispersion spectra of the young Herbig Ae star HR 5999 (HD 144668) covering 1978-1992 revealed dramatic changes in the Mg II h and k (2795.5, 2802.7 A) emission profiles, changes in the column density and distribution in radial velocity of accreting gas, and flux in the Ly(alpha), O I, and C IV emission lines, which are correlated with the UV excess luminosity. Variability in the spectral type inferred from the UV spectral energy distribution, ranging from A5 IV-III in high state to A7 III in the low state, was also observed. The trend of earlier inferred spectral type with decreasing wavelength and with increasing UV continuum flux has previously been noted as a signature of accretion disks in lower mass pre-main sequence stars (PMS) and in systems undergoing FU Orionis-type outbursts. Our data represent the first detection of similar phenomena in an intermediate mass (M greater than or equal to 2 solar mass) PMS star. Recent IUE spectra show gas accreting toward the star with velocities as high as plus 300 km/s, much as is seen toward beta Pic, and suggest that we also view this system through the debris disk. The absence of UV lines with the rotational broadening expected given the optical data (A7 IV, V sini=180 plus or minus 20 km/s for this system) also suggests that most of the UV light originates in the disk, even in the low continuum state. The dramatic variability in the column density of accreting gas, is consistent with clumpy accretion, such as has been observed toward beta Pic, is a hallmark of accretion onto young stars, and is not restricted to the clearing phase, since detectable amounts of accretion are present for stars with 0.5 Myr less than t(sub age) less than 2.8 Myr. The implications for models of beta Pic and similar systems are briefly discussed.

IUE observations of long period eclipsing binaries - A study of accretion onto non-degenerate stars

NASA Technical Reports Server (NTRS)

Plavec, M. J.

1980-01-01

IUE observations made in 1978-1979 recorded a whole class of interacting long-period binaries similar to beta Lyrae, which includes RX Cas, SX Cas, V 367 Cyg, W Cru, beta Lyr, and W Ser, called the W Serpentis stars. These mass-transferring binaries with relatively high mass transfer rate show two prominent features in the far ultraviolet: a continuum with a color temperature higher than the one observed in the optical region (about 12,000 K), and a strong emission line spectrum with the N V doublet at 1240 A, C IV doublet at 1550 A and lines of Si II, Si III, Si IV, C II, Fe III, AI III, etc. These phenomena are discussed on the assumption that they are due to accretion onto non-degenerate stars.

A map-based determination of the nature of Beta Delphini

NASA Technical Reports Server (NTRS)

Gatewood, George; Castelaz, Michael; Persinger, Timothy; Stein, John; Demarque, Pierre

1989-01-01

The Beta Delphini binary system presents a stringent test of the theory of stellar evolution. Improved parallax and component masses are found for its giant (F5 III and F5 IV) stars. A study of the evolutionary status of the system indicates it to be 1.9 Gyr (1.9 billion years) old and to have a metallicity of approximately 1.5 times that of the Sun. The perturbation due to the 26.6 yr orbital motion is clearly shown in this 2.2 yr study and allows the most precise determination of the relative masses of the component stars to date. The next few months present an unusual opportunity for orbital study as the system passes through periastron. Two of the reference stars are found to have distances of less than 100 parsecs.

T cell receptor (TCR) structure of autologous melanoma-reactive cytotoxic T lymphocyte (CTL) clones: tumor-infiltrating lymphocytes overexpress in vivo the TCR beta chain sequence used by an HLA-A2- restricted and melanocyte-lineage-specific CTL clone

PubMed Central

1993-01-01

HLA-A2+ melanomas express common melanoma-associated antigens (Ags) recognized in vitro by autologous cytotoxic T lymphocytes (CTL). However, it is not known whether tumor Ags can drive in vivo a selective accumulation/expansion of Ag-specific, tumor-infiltrating T lymphocytes (TIL). Therefore, to evaluate this possibility, 39 CTL clones isolated from several independent mixed lymphocyte tumor cultures (MLTC) of TIL and peripheral blood lymphocytes (PBL) of an HLA- A2+ melanoma patient and selected for T cell receptor (TCR)-dependent, HLA-restricted tumor lysis, were used for analysis of TCR alpha and beta chain structure by the cDNA polymerase chain reaction (PCR) technique with variable gene-specific primers followed by sequencing. Despite absence of oligoclonality in fresh TIL and PBL, as well as in T cells of day 28 MLTC (day of cloning), sequence analysis of TCR alpha and beta chains of TIL clones revealed a dominance of a major category of melanoma-specific, HLA-A2-restricted T cells expressing a V alpha 8.2/J alpha AP511/C alpha and V beta 2.1/D beta 1/J beta 1.1/C beta 1 TCR. The same TCR was also found in 2 out of 14 PBL clones. The other PBL clones employed a V alpha 2.1 gene segment associated with either V beta 13.2, 14, or w22. Clones A81 (V alpha 2.1/J alpha IGRJ alpha 04/C alpha and V beta 14/D beta 1/J beta 1.2/C beta 1) and A21 (V alpha 8.2/J alpha AP511/C alpha and V beta 2.1/D beta 1/J beta 1.1/C beta 1), representative of the two most frequent TCR of PBL and TIL, respectively, expressed different lytic patterns, but both were HLA-A2 restricted and lysed only HLA-A2+ melanomas and normal melanocytes, thus indicating recognition of two distinct HLA-A2-associated and tissue-related Ags. Finally, by the inverse PCR technique, the specific TCR beta chain (V beta 2.1/D beta 1/J beta 1.1/C beta 1) expressed by the dominant TIL clone was found to represent 19 and 18.4% of all V beta 2 sequences expressed in the fresh tumor sample and in the purified TIL, respectively, but < 0.19% of V beta 2+ sequences expressed in PBL. These results are consistent with the hypothesis that a clonal expansion/accumulation of a melanocyte-lineage-specific and HLA-A2-restricted T cell clone occurred in vivo at the site of tumor growth. PMID:8376931

VizieR Online Data Catalog: HIP and TGAS stars reddening and extinction (Gontcharov+ 2018)

NASA Astrophysics Data System (ADS)

Gontcharov, G. A.; Mosenkov, A. V.

2018-01-01

These are the reddening, interstellar extinction and extinction-to-reddening ratio estimates interpolated for 730,496 Gaia DR1 TGAS and Hipparcos stars within 415 pc from the Sun based on the 3D reddening map of Gontcharov (J/PAZh/43/521) and 3D extinction-to-reddening (total-to-selective extinction) ratio Rv=Av/E(B-V) map of Gontcharov (J/PAZh/38/15). For 711,237 Gaia DR1 TGAS stars the rMoMW distances from Astraatmadja and Bailer-Jones (2016ApJ...833..119A, Cat. J/ApJ/833/119) are used. For 19,259 Hipparcos stars, not in Gaia DR1 TGAS, the distances as the inversion of Hipparcos (I/311) parallaxes are used. The E(B-V) are calculated from initial E(J-Ks) as E(B-V)=E(J-Ks)*(0.047X3-0.1X2-0.09X+1.74), where X=(BT-VT) (B_T and V_T Tycho-2 bands) following the extinction law. This refined relation supersedes E(B-V)=1.655E(J-Ks) in the original 3D reddening map of Gontcharov. The Rv are interpolated from the 3D map of Rv of Gontcharov (2012AstL...38...12G, 2012PAZh...38...15G, Cat. J/PAZh/38/15). The Av are the product of E(B-V) and Rv. (2 data files).

Validation of the BetaStar® Advanced for Beta-lactams Test Kit for the Screening of Bulk Tank and Tanker Truck Milks for the Presence of Beta-lactam Drug Residues.

PubMed

Denhartigh, Andrew; Reynolds, Lindsay; Palmer, Katherine; Klein, Frank; Rice, Jennifer; Rejman, John J

2018-05-18

A validation study was conducted for an immunochromatographic method (BetaStar ® Advanced for Beta-lactams) for the detection of beta-lactam residues in raw, commingled bovine milk. The assay detected amoxicillin, ampicillin, cloxacillin, penicillin, cephapirin, and ceftiofur below the U.S. Food and Drug Administration tolerance levels but above the maximum sensitivity thresholds established by the National Conference on Interstate Milk Shipments. The results of internal and independent laboratory dose-response studies employing spiked samples were in agreement. The test detected all six drugs at the approximate 90/95% sensitivity levels in milk from cows treated with each drug. Selectivity of the assay was 100%, as no false-positive results were obtained in testing 1148 control milk samples. Testing the estimated 90/95% sensitivity level for amoxicillin (8.5 ppb), ampicillin (6.9 ppb), cloxacillin (8.9 ppb), penicillin (4.2 ppb), and cephapirin (17.6 ppb), and at 100 ppb for each antibiotic, resulted in 94-100% positive tests for each of the beta-lactam drugs. The results of ruggedness experiments established the operating parameter tolerances for the assay. Cross-reactivity testing established that the assay detects other certain beta-lactam drugs, but it does not cross-react with any of 30 drugs belonging to seven different drug classes. Abnormally high bacterial or somatic cell counts in raw milk produced no assay interference.

Observing Infrared Emission Lines of Neutron-Capture Species in Planetary Nebulae: New Detections with IGRINS

NASA Astrophysics Data System (ADS)

Dinerstein, Harriet L.; Sterling, N. C.; Kaplan, Kyle F.; Bautista, Manuel A.

2015-08-01

As the former envelopes of evolved stars, planetary nebulae (PNe) present an opportunity to study slow neutron-capture reactions (the “s-process”) during the AGB. Such studies differ from those of AGB stars in two ways. First, PNe represent the end point of self-enrichment and dredge-up in the star and most of its mass return to the ISM, enabling us to infer the nucleosynthetic yield of a specific element. Second, some s-process products are observable in PNe but difficult or impossible to observe in cool stars. These include some species with nuclear charge Z in the 30’s for which the major synthesis sites are uncertain. Optical emission lines of trans-iron species have been observed in some PNe, but are faint and can suffer from blending with lines of more abundant elements (Péquignot & Baluteau 1994, A&A, 283, 593; Sharpee et al. 2007, ApJ, 659, 1265). Observing infrared transitions from low energy states has proven to be a fruitful alternate approach. We used K-band lines of Se (Z=34) and Kr (Z=36) to study the demographics of their abundances in a large sample of Milky Way PNe (Dinerstein 2001, ApJ, 550, L223; Sterling & Dinerstein 2008, ApJ, 174, 158; Sterling, Porter, & Dinerstein 2015, submitted). An L-band emission line of Zn identified by Dinerstein & Geballe (2001, ApJ, 562, 515) and further observed by Smith, Zijlstra, & Dinerstein 2014 (MNRAS, 441, 3161), can be used as a tracer of the Fe-group, enabling determinations of the key stellar population diagnostic ratio [alpha/Fe] in PNe (see poster by Dinerstein et al., Focus Meeting 4). Using IGRINS, a high spectral resolution H and K band spectrometer (Park & Jaffe et al. 2014, Proc SPIE, 9147), we have discovered several new lines not previously reported in any astronomical object. Our detection of an H-band line of Rb (Z=37) confirms previous claims of optical Rb detections and indicates enrichment by a factor of ~4 in the PN NGC 7027 (Sterling, Dinerstein, Kaplan, & Bautista, in preparation). We also detect lines that we tentatively identify as Ge (Z=32) and Cd (Z=48). This work was supported by NSF grants AST 0708429 and 1412928.

Chemical Compositions and Anomalies in Stellar Coronae ADP99

NASA Technical Reports Server (NTRS)

Oliversen, Ronald J. (Technical Monitor); Drake, Jeremy

2005-01-01

Recent progress includes a paper accepted by the ApJ on AB Dor and V471 Tau, and papers on xi UMa and on giant stars submitted but still under ApJ revision. Atomic data has been investigated for line ratio abundance diagnostics, and in particular to determine the contributions of radiative recombination to observed line fluxes. Effects have generally been found to be less than 10%. Further investigations have been in into the possibility of modelling some of the recent coronal abundance anomally results in terms of Alven wave-driven separation of neutrals and ions in the upper chromosphere. Papers being readied for publication include one on active binary stars, and one on the Ne/O ratio in stellar coronae. The Ne/O is found to be approximately constant in all stars examined, and suggests that the current local ISM ratio might be too low by a factor of two. In summary, the work to-date is making good progress in mapping abundance anomalies as a function of spectral type and activity level. We are also making good progress with modelling that we will be able to test with our observational results.

VizieR Online Data Catalog: Young star forming region NGC 2264 Spitzer sources (Rapson+, 2014)

NASA Astrophysics Data System (ADS)

Rapson, V. A.; Pipher, J. L.; Gutermuth, R. A.; Megeath, S. T.; Allen, T. S.; Myers, P. C.; Allen, L. E.

2017-05-01

We utilize 3.6-8.0 um images of Mon OB1 East obtained with the Spitzer Space Telescope Infrared Array Camera (IRAC; Fazio et al. 2004ApJS..154...10F), 24 um images obtained with the Multi-Band Imaging Photometer (MIPS; Rieke et al. 2004ApJS..154...25R), along with 1-2.5 um NIR data from the Two Micron All Sky Survey (2MASS; Skrutskie et al. 2006AJ....131.1163S, Cat. VII/233) to classify YSOs. These YSOs in Mon OB1 East are classified as either protostars or stars with circumstellar disks by their infrared excess emission above photospheric emission. Spitzer data were gathered as part of two Guaranteed Time Observation programs and one additional program with the goal of studying clustered and distributed star formation throughout Mon OB1 East and comparing the results with those of other molecular clouds. Mon OB1 East was observed by Spitzer in 2004, 2007, and 2008 as part of the Guaranteed Time Observation programs 37 (IRAC data; PI: G. Fazio) and 58 (MIPS data; PI: G. Rieke), as well as program 40006 (IRAC+MIPS data; PI: G. Fazio). (1 data file).

Observational Studies of the Clearing Phase in Proto-Planetary Disks Surrounding Intermediate Mass Stars

NASA Technical Reports Server (NTRS)

Grady, Carol A.

1999-01-01

A detailed study of circumstellar gas associated with young, intermediate-mass stars has demonstrated that, far from being unique or an infrequently occurring phenomenon, beta Pic-like infall activity is routinely observed in stars younger than 10-50 Myr when the observer's line of sight lies within 15 degrees of the disk mid-plane. Detailed studies of 2 Herbig Ae/Be stars, AB Aur and HD 163296 demonstrate that enhanced infall episodes last 20-60 hours, comparable to the duration of similar episodes in beta Pictoris. The infall activity is consistent with detection of the comae of swarms of star-grazing bodies of asteroidal to cometary composition. Episodic fluctuations in the infall activity are clearly present by approximately 6 Myr, and may indicate the presence of massive planets within the disk. This study has therefore, directly contributed to NASA's Origins of Planetary Systems theme by identifying under what conditions extra-solar planetesimals can be remotely sensed, indicating that such bodies appear to be routinely detectable among young stars in the 1-10 Myr range, and suggesting that temporal studies of spectroscopic variability may provide a means of identifying those systems harboring massive planets. This study has resulted in 2 refereed review papers, 13 other refereed papers, and 17 conference papers.

Nuclear Phosphatidylinositol-Phosphate Type I Kinase α-Coupled Star-PAP Polyadenylation Regulates Cell Invasion.

PubMed

A P, Sudheesh; Laishram, Rakesh S

2018-03-01

Star-PAP, a nuclear phosphatidylinositol (PI) signal-regulated poly(A) polymerase (PAP), couples with type I PI phosphate kinase α (PIPKIα) and controls gene expression. We show that Star-PAP and PIPKIα together regulate 3'-end processing and expression of pre-mRNAs encoding key anti-invasive factors ( KISS1R , CDH1 , NME1 , CDH13 , FEZ1 , and WIF1 ) in breast cancer. Consistently, the endogenous Star-PAP level is negatively correlated with the cellular invasiveness of breast cancer cells. While silencing Star-PAP or PIPKIα increases cellular invasiveness in low-invasiveness MCF7 cells, Star-PAP overexpression decreases invasiveness in highly invasive MDA-MB-231 cells in a cellular Star-PAP level-dependent manner. However, expression of the PIPKIα-noninteracting Star-PAP mutant or the phosphodeficient Star-PAP (S6A mutant) has no effect on cellular invasiveness. These results strongly indicate that PIPKIα interaction and Star-PAP S6 phosphorylation are required for Star-PAP-mediated regulation of cancer cell invasion and give specificity to target anti-invasive gene expression. Our study establishes Star-PAP-PIPKIα-mediated 3'-end processing as a key anti-invasive mechanism in breast cancer. Copyright © 2018 A.P. and Laishram.

VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2005)

NASA Astrophysics Data System (ADS)

Skiff, A. B.

2004-05-01

This file contains spectral classifications for stars collected from the literature, serving as a continuation of the compilations produced by the Jascheks, by Kennedy, and by Buscombe. The source of each spectral type is indicated by a standard 19-digit bibcode citation. These papers of course should be cited in publication, not this compilation. The stars are identified either by the name used in each publication or by a valid SIMBAD identifier. Some effort has been made to determine accurate (~1" or better) coordinates for equinox J2000, and these serve as a secondary identifier. Magnitudes are provided as an indication of brightness, but these data are not necessarily accurate, as they often derive from photographic photometry or rough estimates. The classifications include MK types as well as types not strictly on the MK system (white dwarfs, Wolf-Rayet, etc), and in addition simple HD-style temperature types. Luminosity classes in the early Mount Wilson style (e.g. 'd' for dwarf, 'g' for giant) and other similar schemes have been converted to modern notation. Since a citation is provided for each entry, the source paper should be consulted for details about classification schemes, spectral dispersion, and instrumentation used. The file includes only spectral types determined from spectra (viz. line and band strengths or ratios), omitting those determined from photometry (e.g. DDO, Vilnius) or inferred from broadband colors or bulk spectral energy distributions. System-defining primary MK standard stars are included from the last lists by Morgan and Keenan, and are flagged by a + sign in column 79. The early-type standards comprise the 1973 "dagger standards" (1973ARA&A..11...29M) and stars from the Morgan, Abt, and Tapscott atlas (1978rmsa.book.....M). Keenan made continual adjustments to the standards lists up to the time of his death. Thus the late-type standards comprise those marked as high-weight standards in the 1989 Perkins catalogue (1989ApJS...71..245K = III/150), plus the carbon- and S-type standards (1980ApJS...43..379K, 1996ApJS..105..419B), and class IIIb 'clump giants' (1999ApJ...518..859K). In addition, I have made use of the final types by Keenan up to January 2000 shown at the Ohio State Web site (http://www-astronomy.mps.ohio-state.edu/MKCool). Though the present file contains all the stars in these lists, only those marked as standards are flagged as such. Garrison's list of MK 'anchor points' might also be consulted in this regard (1994mpyp.conf....3G). The catalogue includes for the first time results from many large-scale objective-prism spectral surveys done at Case, Stockholm, Crimea, Abastumani, and elsewhere. The stars in these surveys were usually identified only on charts or by other indirect means, and have been overlooked heretofore because of the difficulty in recovering the stars. More complete results from these separate publications, including notes and identifications, have been made available to the CDS, and are kept at the Lowell Observatory ftp area (ftp://ftp.lowell.edu/pub/bas/starcats). Not all of these stars are present in SIMBAD. As a 'living catalogue', an attempt will be made to keep up with current literature, and to extend the indexing of citations back in time. (1 data file).

Antibodies to Phosphatidylserine/Prothrombin Complex in Antiphospholipid Syndrome: Analytical and Clinical Perspectives.

PubMed

Peterson, Lisa K; Willis, Rohan; Harris, E Nigel; Branch, Ware D; Tebo, Anne E

2016-01-01

Antiphospholipid syndrome (APS) is an autoimmune disorder characterized by thrombosis and/or pregnancy-related morbidity accompanied by persistently positive antiphospholipid antibodies (aPL). Current laboratory criteria for APS classification recommend testing for lupus anticoagulant as well as IgG and IgM anticardiolipin, and beta-2 glycoprotein I (anti-β2GPI) antibodies. However, there appears to be a subset of patients with classical APS manifestations who test negative for the recommended criteria aPL tests. While acknowledging that such patients may have clinical features that are not of an autoimmune etiology, experts also speculate that these "seronegative" patients may test negative for relevant autoantibodies as a result of a lack of harmonization and/or standardization. Alternatively, they may have aPL that target other antigens involved in the pathogenesis of APS. In the latter, autoantibodies that recognize a phosphatidylserine/prothrombin (PS/PT) complex have been reported to be associated with APS and may have diagnostic relevance. This review highlights analytical and clinical attributes associated with PS/PT antibodies, taking into consideration the performance characteristics of criteria aPL tests in APS with specific recommendations for harmonization and standardization efforts. © 2016 Elsevier Inc. All rights reserved.

VizieR Online Data Catalog: Carbon-enhanced metal-poor (CEMP) star abundances (Yoon+, 2016)

NASA Astrophysics Data System (ADS)

Yoon, J.; Beers, T. C.; Placco, V. M.; Rasmussen, K. C.; Carollo, D.; He, S.; Hansen, T. T.; Roederer, I. U.; Zeanah, J.

2017-03-01

We have endeavored to compile a list that is as complete as possible of carbon-enhanced metal-poor (CEMP); CEMP-s (and CEMP-r/s) and CEMP-no stars having [Fe/H]<-1.0 and [C/Fe]>=+0.7 with available high-resolution spectroscopic abundance information. We have only considered stars with claimed detections or lower limits for carbon, along with several critical elemental-abundance ratios, such as [Ba/Fe] and [Eu/Fe]. The great majority of our sample comes from the literature compilation of Placco+ (2014, J/ApJ/797/21). See section 2 for further details. (2 data files).

VizieR Online Data Catalog: ubvyH{beta} photometry in NGC 1817 & 1807 (Balaguer-Nunez+ 2004)

NASA Astrophysics Data System (ADS)

Balaguer-Nunez, L.; Jordi, C.; Galadi-Enriquez, D.; Masana, E.

2004-07-01

The catalogue of accurate uvby-H{beta} and J2000 coordinates for 7842 stars in an area of 65'x40' around NGC 1817. We mark the selection of probable members of NGC 1817, combining this photometric study with the previous astrometric analysis (Balaguer-Nunez et al. 2004, Cat. ). Also given is the cross-identification of stars in common with the astrometry (Balaguer-Nunez et al. 2004, Cat. ), WEBDA (http://obswww.unige.ch/WEBDA), Hipparcos (ESA, 1997, Cat. ), Tycho-2 (Hog et al., 2000, Cat. ) and USNO-A2 (Monet et al., 1998, Cat. ) catalogues. (2 data files).

Deblending Microlensing Events Using Astrometric Shifts

NASA Astrophysics Data System (ADS)

Goldberg, D. M.; Wozniak, P.; Paczynski, B.

1997-12-01

In this poster, we present the prospect that astrometric shifts can be used to identify blended microlensing events in crowded fields. Moreover, by measuring an astrometric shift, one can determine the position of the true lensed star with respect to the local field with very high precision. We first perform several simulations of microlensing searches in crowded fields and find that if we assume a dark lens, and that the lensed star obeys a power law luminosity function, n(L)~ L(-beta ) , over half the simulated events show a measurable astrometric shift. For simulations of 20000 stars on a 256x 256 Nyquist sampled CCD frame, we found that with beta =2, 58% of the events were significantly blended (F_{*}/Ftot <= 0.9), and of those, 73% had a large astrometric shift (>= 0.5 pixels). For beta =3, we found that 85% were significantly blended, and that 85% of those had a significant shift. Since we expect most blended events to show a significant shift, we look in the OGLE I database (Wozniak & Szymanski 1997), and find measurable and systematic shifts in over half the candidate microlensing events, including OGLE # 5, which was considered to be blended from photometric data.

VES263: an intermediate mass YSO candidate as a new eruptive variable

NASA Astrophysics Data System (ADS)

Giannini, T.; Antoniucci, S.; Lorenzetti, D.; Harutyunyan, A.; Licchelli, D.; Munari, U.

2018-05-01

In the framework of our EXor monitoring programme dubbed EXORCISM (EXOR OptiCal and Infrared Systematic Monitoring - Antoniucci et al. 2013 PPVI, Lorenzetti et al. 2007 ApJ 665, 1182; Lorenzetti et al. 2009 ApJ 693, 1056), we observed the object VES263 signalled by a recent GAIA alert (http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia18azl) as "an emission line star undergoing repeat outbursts" having detected an alerting magnitude of 11.66 wrt a historic magnitude of 12.16.

The Chara Array Angular Diameter of HR 8799 Favors Planetary Masses for Its Imaged Companions

DTIC Science & Technology

2012-12-10

because of the shallow convective zones in A-type stars ( Charbonneau 1991). Accretion at these rates will quickly establish abundance anomalies within a...few Myr, but these anomalies will likewise disappear in as little as 1 Myr once the accretion has terminated (Turcotte & Charbonneau 1993); the... Charbonneau , P. 1991, ApJ, 372, L33 Chen, C. H., Sargent, B. A., Bohac, C., et al. 2006, ApJS, 166, 351 Claret, A., & Bloemen, S. 2011, A&A, 529, A75 Cox, A. N

Kepler-432: A Red Giant Interacting with One of its Two Long-period Giant Planets

NASA Astrophysics Data System (ADS)

Quinn, Samuel N.; White, Timothy. R.; Latham, David W.; Chaplin, William J.; Handberg, Rasmus; Huber, Daniel; Kipping, David M.; Payne, Matthew J.; Jiang, Chen; Silva Aguirre, Victor; Stello, Dennis; Sliski, David H.; Ciardi, David R.; Buchhave, Lars A.; Bedding, Timothy R.; Davies, Guy R.; Hekker, Saskia; Kjeldsen, Hans; Kuszlewicz, James S.; Everett, Mark E.; Howell, Steve B.; Basu, Sarbani; Campante, Tiago L.; Christensen-Dalsgaard, Jørgen; Elsworth, Yvonne P.; Karoff, Christoffer; Kawaler, Steven D.; Lund, Mikkel N.; Lundkvist, Mia; Esquerdo, Gilbert A.; Calkins, Michael L.; Berlind, Perry

2015-04-01

We report the discovery of Kepler-432b, a giant planet ({{M}b}=5.41-0.18+0.32 {{M}Jup}, {{R}b}=1.145-0.039+0.036 {{R}Jup}) transiting an evolved star ({{M}\\star }=1.32-0.07+0.10 {{M}⊙ },{{R}\\star }=4.06-0.08+0.12 {{R}⊙ }) with an orbital period of {{P}b}=52.501129-0.000053+0.000067 days. Radial velocities (RVs) reveal that Kepler-432b orbits its parent star with an eccentricity of e=0.5134-0.0089+0.0098, which we also measure independently with asterodensity profiling (AP; e=0.507-0.114+0.039), thereby confirming the validity of AP on this particular evolved star. The well-determined planetary properties and unusually large mass also make this planet an important benchmark for theoretical models of super-Jupiter formation. Long-term RV monitoring detected the presence of a non-transiting outer planet (Kepler-432c; {{M}c}sin {{i}c}=2.43-0.24+0.22 {{M}Jup}, {{P}c}=406.2-2.5+3.9 days), and adaptive optics imaging revealed a nearby (0\\buildrel{\\prime\\prime}\\over{.} 87), faint companion (Kepler-432B) that is a physically bound M dwarf. The host star exhibits high signal-to-noise ratio asteroseismic oscillations, which enable precise measurements of the stellar mass, radius, and age. Analysis of the rotational splitting of the oscillation modes additionally reveals the stellar spin axis to be nearly edge-on, which suggests that the stellar spin is likely well aligned with the orbit of the transiting planet. Despite its long period, the obliquity of the 52.5 day orbit may have been shaped by star-planet interaction in a manner similar to hot Jupiter systems, and we present observational and theoretical evidence to support this scenario. Finally, as a short-period outlier among giant planets orbiting giant stars, study of Kepler-432b may help explain the distribution of massive planets orbiting giant stars interior to 1 AU.

Beta-hydroxybutyrate Concentrations in Dogs with Acute Pancreatitis and Without Diabetes Mellitus.

PubMed

Hurrell, F E; Drobatz, K J; Hess, R S

2016-05-01

β-hydroxybutyrate (BOHB) concentrations have not been quantified in dogs with acute pancreatitis (AP). The aim of this study was to investigate BOHB concentrations in dogs with AP. A total of 154 client-owned dogs without DM. Prospective clinical study. Dogs were enrolled into 1 of 3 groups: AP, sick without an AP diagnosis, or fasted. Dogs were diagnosed with AP (44) if they had vomiting or anorexia, and either ultrasonographic findings consistent with AP or increased pancreatic lipase. Sick dogs without AP (68) had vomiting or anorexia but a diagnosis of AP was either not suspected or was excluded based on ultrasonographic findings or a normal pancreatic lipase. Dogs without anorexia or vomiting that were fasted for over 10 hours for a procedure were also enrolled (42). BOHB was measured on whole blood with a portable ketone meter. The Kruskal-Wallis test was performed to compare BOHB in the 3 groups. Pair-wise comparisons were performed using the Mann-Whitney test and Bonferroni corrected P-values are reported. Median BOHB concentration was significantly higher in dogs with AP (0.3 mmol/L, range 0-2.9 mmol/L) compared to sick dogs without AP (0.20 mmol/L, range 0-0.9 mmol/L, P = .007) and fasted dogs (0.1 mmol/L, range 0-0.4 mmol/L, P = .0001). Median BOHB concentration was significantly higher in sick dogs without AP compared to fasted dogs (P = .0002). In dogs without DM, BOHB is significantly higher in dogs with AP compared to other dogs. The diagnostic utility of this finding remains to be investigated. Copyright © 2016 The Authors. Journal of Veterinary Internal Medicine published by Wiley Periodicals, Inc. on behalf of the American College of Veterinary Internal Medicine.

Epibatidine, an alkaloid from the poison frog Epipedobates tricolor, is a powerful ganglionic depolarizing agent.

PubMed

Fisher, M; Huangfu, D; Shen, T Y; Guyenet, P G

1994-08-01

Epibatidine, a newly discovered alkaloid from the skin of Dendrobatidae frogs, has structural similarities to nicotine. We examined the effects of epibatidine on cardiorespiratory function and ganglionic synaptic transmission. Superior cervical or splanchnic sympathetic nerve discharge (sSND) and phrenic nerve discharge (PND) were recorded along with arterial pressure (AP) in urethane-anesthetized, paralyzed and artificially ventilated rats. Epibatidine administered i.v. at low doses (0.5-2 micrograms/kg) produced a transient increase in AP and sSND, followed by a decrease and return to baseline; this low dose of epibatidine also produced a dose-dependent increase in PND. At high doses (cumulative dose of 8-16 micrograms/kg), epibatidine produced bradycardia, a profound depression in sSND and a transient elimination of PND. After i.v. administration of the ganglionic blocker chlorisondamine (5 mg/kg), AP was still increased by 1 microgram/kg epibatidine (+39 +/- 11 mm Hg). This pressor effect was not altered by pretreatment with the alpha-1 adrenergic antagonist phentolamine (+40 +/- 10 mm Hg); however, it was blocked by additional pretreatment with the vasopressin antagonist [beta-mercapto-beta,beta-cyclopentamethylenepropiony1, O-ET-Tyr2,Val4,Arg8]vasopressin (50 micrograms/kg i.v.; +2 +/- 0.4 mm Hg). Low doses of epibatidine (0.5-2 micrograms/kg) produced firing of postganglionic neurons in a decentralized ganglion preparation and potentiated synaptic transmission; at high doses (cumulative dose of 8-16 micrograms/kg), the alkaloid blocked ganglionic synaptic transmission. These results suggest that epibatidine is a potent agonist of ganglionic nicotinic receptors and that the alkaloid elicits cardiorespiratory effects similar to those of nicotine.

Case reports of the use of immunoadsorption or plasma exchange in high-risk pregnancies of women with antiphospholipid syndrome.

PubMed

Bortolati, Maria; Marson, Piero; Chiarelli, Silvia; Tison, Tiziana; Facchinetti, Myriam; Gervasi, Maria Teresa; De Silvestro, Giustina; Ruffatti, Amelia

2009-04-01

Conventional treatment of antiphospholipid syndrome (APS) pregnancies with aspirin and/or heparin is sometimes unable to counteract maternal and/or fetal complications. In this article we report the cases of two patients who were unresponsive to conventional treatment for APS during their first pregnancy, and who were treated in the following pregnancy with plasma exchange and immunoadsorption respectively, in addition to conventional therapy. Both patients had a history of thrombotic events, a previous pregnancy loss at the 11th week of gestation and the same antiphospholipid antibody profile (lupus anticoagulant activity and high titers of immunoglobulin G (IgG) anti-beta2 glycoprotein I and IgG anticardiolipin antibodies). Patient 1 was treated from the fourth week of her second pregnancy with weekly plasma exchange. Due to fetal growth restriction and oligohydramnios in the 26th week she delivered, by cesarean section, a healthy female infant weighing 730 g who survived. Patient 2 was treated from the seventh week of her second pregnancy with twice a week protein A immunoadsorption. The pregnancy proceeded normally until the 36th week, when, due to slight intrauterine growth restriction, she delivered a healthy baby girl weighing 2375 g by cesarean section. Anti-beta2 glycoprotein I antibody trends were similar during both types of treatment. On the basis of our findings obtained from only two cases it is impossible to define the best aphaeretic treatment of APS high risk pregnancies. Nevertheless, as a whole these data suggest better disease control using the immunoadsorption technique as compared to plasma exchange, despite their apparently similar anti-beta2 glycoprotein I antibody removal capabilities.

VizieR Online Data Catalog: Omega Cen candidates RAVE-selected (Fernandez-Trincado+, 2015)

NASA Astrophysics Data System (ADS)

Fernandez-Trincado, J. G.; Robin, A. C.; Vieira, K.; Moreno, E.; Bienayme, O.; Reyle, C.; Valenzuela, O.; Pichardo, B.; Robles-Valdez, F.; Martins, A. M. M.

2015-11-01

The sample was selected from the RAVE DR4 catalog (Kordopatis et al., 2013, Cat. III/272), which provides accurate radial velocities with typical errors of σRV~2km/s, and distances and individual abundances with errors of about 10-20%, determined for approximately 390000 relatively bright stars (9mag20 (algo_conv=0 was required, indicating that the pipeline converges, see Kordopatis et al., 2013, Cat. III/272). This cut allowed us to obtain precise radial velocity measurements, typically σRV<2km/s, in order to constraint the full space motion. The metallicity [Fe/H] distribution for giant stars within Omega Centauri spans more than a magnitude order, from -2.2dex<[Fe/H]<-0.7dex (Johnson & Pilachowski, 2010, Cat. J/ApJ/722/1373), therefore we allowed stars in our sample to be in this range of metallicity. (1 data file).

VizieR Online Data Catalog: HST photometry of stars in HD 97950 (Pang+, 2016)

NASA Astrophysics Data System (ADS)

Pang, X.; Pasquali, A.; Grebel, E. K.

2016-07-01

The HD97950 cluster and its immediate surroundings in the giant HII region NGC3603 were observed with the Hubble Space Telescope (HST). The ultraviolet (UV) data were taken with the High Resolution Channel (HRC) of the Advanced Camera for Surveys (ACS) in 2005 (GO 10602, PI: Jesus Maiz Apellaniz) through the F220W, F250W, F330W, and F435W filters. The HRC is characterized by a spatial resolution of 0.03"/pixel and a field of view of 29''*25''. The optical observations were carried out with the Wide Field and Planetary Camera 2 (WFPC2) in two epochs: 1997 (GO 6763, PI: Laurent Drissen) and 2007 (GO 11193, PI: Wolfgang Brandner) through the F555W, F675W, and F814W filters. The Planetary Camera (PC) chip was centered on the cluster (0.045"/pixel, 40''*40'') for both programs. Pang et al. 2013 (cat. J/ApJ/764/73) reduced the two-epoch WFPC2 data and identified more than 400 member stars on the PC chip via relative proper motions. Of these member stars, 142 are in common between the HRC and PC images and thus have UV and optical photometry available (see Table1). Among the HD97950 cluster member stars determined from relative proper motions (Pang et al. 2013, cat. J/ApJ/764/73, Table2), there are five main-sequence (MS) stars located in the cluster with projected distances of r<0.7pc from the center, for which there are also spectral types available from Table3 of Melena et al. (2008AJ....135..878M). The photometry of these five MS stars is presented in Table2. The individual color excesses and extinctions of the member main sequence stars are listed in Table3. (3 data files).

VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2014)

NASA Astrophysics Data System (ADS)

Skiff, B. A.

2014-10-01

This file contains spectral classifications for stars collected from the literature, serving as a continuation of the compilations produced by the Jascheks, by Kennedy, and by Buscombe. The source of each spectral type is indicated by a standard 19-digit bibcode citation. These papers of course should be cited in publication, not this compilation. The stars are identified either by the name used in each publication or by a valid SIMBAD identifier. Some effort has been made to determine accurate (~1" or better) coordinates for equinox J2000 (and epoch 2000 if possible), and these serve as a secondary identifier. To the extent possible with current astrometric sources, the components of double stars and stars with composite spectra are shown as separate entries. Magnitudes are provided as an indication of brightness, but these data are not necessarily accurate, as they often derive from photographic photometry or rough estimates. The file includes only spectral types determined from spectra (viz. line and band strengths or ratios), omitting those determined from photometry (e.g. DDO, Vilnius) or inferred from broadband colors or spectral energy distributions. The classifications include MK types as well as types not strictly on the MK system (white dwarfs, Wolf-Rayet, etc), and in addition simple HD-style temperature types. Luminosity classes in the early Mount Wilson style (e.g. 'd' for dwarf, 'g' for giant) and other similar schemes have been converted to modern notation. Since a citation is provided for each entry, the source paper should be consulted for details about classification schemes, spectral dispersion, and instrumentation used. System-defining primary MK standard stars are included from the last lists by Morgan and Keenan, and are flagged by a + sign in column 83. The early-type standards comprise the 1973 "dagger standards" (1973ARA&A..11...29M) and stars from the Morgan, Abt, and Tapscott atlas (1978rmsa.book.....M). Standards from Table I of the Morgan & Abt 'MKA' paper (1972AJ.....77...35M) not appearing in the two later lists are added. Keenan made continual adjustments to the standards lists up to the time of his death. Thus the late-type standards comprise those marked as high-weight standards in the 1989 Perkins catalogue (1989ApJS...71..245K = III/150); the revised S-type standards in collaboration with Boeshaar (1980ApJS...43..379K); plus the carbon standards and class IIIb 'clump giants' in collaboration with Barnbaum (1996ApJS..105..419B and 1999ApJ...518..859K). In addition, I have made use of the final types by Keenan up to January 2000 shown at the Ohio State Web site (http://www.astronomy.ohio-state.edu/MKCool), accessed in autumn 2003. Though the present file contains all the stars in these lists, only those marked as standards are flagged as such. Garrison's list of MK 'anchor points' might also be consulted in this regard (1994mpyp.conf....3G, and http://www.astro.utoronto.ca/~garrison/mkstds.html). The catalogue includes for the first time results from many large-scale objective-prism spectral surveys done at Case, Stockholm, Crimea, Abastumani, and elsewhere. The stars in these surveys were usually identified only on charts or by other indirect means, and have been overlooked heretofore because of the difficulty in recovering the stars. More complete results from these separate publications, including notes and identifications, have been made available to the CDS, and are kept at the Lowell Observatory ftp area (ftp://ftp.lowell.edu/pub/bas/starcats). Not all of these stars are present in SIMBAD. As a 'living catalogue', an attempt will be made to keep up with current literature, and to extend the indexing of citations back in time. (2 data files).

VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)

NASA Astrophysics Data System (ADS)

Skiff, B. A.

2014-10-01

This file contains spectral classifications for stars collected from the literature, serving as a continuation of the compilations produced by the Jascheks, by Kennedy, and by Buscombe. The source of each spectral type is indicated by a standard 19-digit bibcode citation. These papers of course should be cited in publication, not this compilation. The stars are identified either by the name used in each publication or by a valid SIMBAD identifier. Some effort has been made to determine accurate (~1" or better) coordinates for equinox J2000 (and epoch 2000 if possible), and these serve as a secondary identifier. To the extent possible with current astrometric sources, the components of double stars and stars with composite spectra are shown as separate entries. Magnitudes are provided as an indication of brightness, but these data are not necessarily accurate, as they often derive from photographic photometry or rough estimates. The file includes only spectral types determined from spectra (viz. line and band strengths or ratios), omitting those determined from photometry (e.g. DDO, Vilnius) or inferred from broadband colors or spectral energy distributions. The classifications include MK types as well as types not strictly on the MK system (white dwarfs, Wolf-Rayet, etc), and in addition simple HD-style temperature types. Luminosity classes in the early Mount Wilson style (e.g. 'd' for dwarf, 'g' for giant) and other similar schemes have been converted to modern notation. Since a citation is provided for each entry, the source paper should be consulted for details about classification schemes, spectral dispersion, and instrumentation used. System-defining primary MK standard stars are included from the last lists by Morgan and Keenan, and are flagged by a + sign in column 83. The early-type standards comprise the 1973 "dagger standards" (1973ARA&A..11...29M) and stars from the Morgan, Abt, and Tapscott atlas (1978rmsa.book.....M). Standards from Table I of the Morgan & Abt 'MKA' paper (1972AJ.....77...35M) not appearing in the two later lists are added. Keenan made continual adjustments to the standards lists up to the time of his death. Thus the late-type standards comprise those marked as high-weight standards in the 1989 Perkins catalogue (1989ApJS...71..245K = III/150); the revised S-type standards in collaboration with Boeshaar (1980ApJS...43..379K); plus the carbon standards and class IIIb 'clump giants' in collaboration with Barnbaum (1996ApJS..105..419B and 1999ApJ...518..859K). In addition, I have made use of the final types by Keenan up to January 2000 shown at the Ohio State Web site (http://www.astronomy.ohio-state.edu/MKCool), accessed in autumn 2003. Though the present file contains all the stars in these lists, only those marked as standards are flagged as such. Garrison's list of MK 'anchor points' might also be consulted in this regard (1994mpyp.conf....3G, and http://www.astro.utoronto.ca/~garrison/mkstds.html). The catalogue includes for the first time results from many large-scale objective-prism spectral surveys done at Case, Stockholm, Crimea, Abastumani, and elsewhere. The stars in these surveys were usually identified only on charts or by other indirect means, and have been overlooked heretofore because of the difficulty in recovering the stars. More complete results from these separate publications, including notes and identifications, have been made available to the CDS, and are kept at the Lowell Observatory ftp area (ftp://ftp.lowell.edu/pub/bas/starcats). Not all of these stars are present in SIMBAD. As a 'living catalogue', an attempt will be made to keep up with current literature, and to extend the indexing of citations back in time. (2 data files).

VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2010)

NASA Astrophysics Data System (ADS)

Skiff, B. A.

2009-02-01

This file contains spectral classifications for stars collected from the literature, serving as a continuation of the compilations produced by the Jascheks, by Kennedy, and by Buscombe. The source of each spectral type is indicated by a standard 19-digit bibcode citation. These papers of course should be cited in publication, not this compilation. The stars are identified either by the name used in each publication or by a valid SIMBAD identifier. Some effort has been made to determine accurate (~1" or better) coordinates for equinox J2000 (and epoch 2000 if possible), and these serve as a secondary identifier. To the extent possible with current astrometric sources, the components of double stars and stars with composite spectra are shown as separate entries. Magnitudes are provided as an indication of brightness, but these data are not necessarily accurate, as they often derive from photographic photometry or rough estimates. The file includes only spectral types determined from spectra (viz. line and band strengths or ratios), omitting those determined from photometry (e.g. DDO, Vilnius) or inferred from broadband colors or spectral energy distributions. The classifications include MK types as well as types not strictly on the MK system (white dwarfs, Wolf-Rayet, etc), and in addition simple HD-style temperature types. Luminosity classes in the early Mount Wilson style (e.g. 'd' for dwarf, 'g' for giant) and other similar schemes have been converted to modern notation. Since a citation is provided for each entry, the source paper should be consulted for details about classification schemes, spectral dispersion, and instrumentation used. System-defining primary MK standard stars are included from the last lists by Morgan and Keenan, and are flagged by a + sign in column 83. The early-type standards comprise the 1973 "dagger standards" (1973ARA&A..11...29M) and stars from the Morgan, Abt, and Tapscott atlas (1978rmsa.book.....M). Standards from Table I of the Morgan & Abt 'MKA' paper (1972AJ.....77...35M) not appearing in the two later lists are added. Keenan made continual adjustments to the standards lists up to the time of his death. Thus the late-type standards comprise those marked as high-weight standards in the 1989 Perkins catalogue (1989ApJS...71..245K = III/150); the revised S-type standards in collaboration with Boeshaar (1980ApJS...43..379K); plus the carbon standards and class IIIb 'clump giants' in collaboration with Barnbaum (1996ApJS..105..419B and 1999ApJ...518..859K). In addition, I have made use of the final types by Keenan up to January 2000 shown at the Ohio State Web site (http://www.astronomy.ohio-state.edu/MKCool), accessed in autumn 2003. Though the present file contains all the stars in these lists, only those marked as standards are flagged as such. Garrison's list of MK 'anchor points' might also be consulted in this regard (1994mpyp.conf....3G, and http://www.astro.utoronto.ca/~garrison/mkstds.html). The catalogue includes for the first time results from many large-scale objective-prism spectral surveys done at Case, Stockholm, Crimea, Abastumani, and elsewhere. The stars in these surveys were usually identified only on charts or by other indirect means, and have been overlooked heretofore because of the difficulty in recovering the stars. More complete results from these separate publications, including notes and identifications, have been made available to the CDS, and are kept at the Lowell Observatory ftp area (ftp://ftp.lowell.edu/pub/bas/starcats). Not all of these stars are present in SIMBAD. As a 'living catalogue', an attempt will be made to keep up with current literature, and to extend the indexing of citations back in time. (2 data files).

VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2012)

NASA Astrophysics Data System (ADS)

Skiff, B. A.

2010-11-01

This file contains spectral classifications for stars collected from the literature, serving as a continuation of the compilations produced by the Jascheks, by Kennedy, and by Buscombe. The source of each spectral type is indicated by a standard 19-digit bibcode citation. These papers of course should be cited in publication, not this compilation. The stars are identified either by the name used in each publication or by a valid SIMBAD identifier. Some effort has been made to determine accurate (~1" or better) coordinates for equinox J2000 (and epoch 2000 if possible), and these serve as a secondary identifier. To the extent possible with current astrometric sources, the components of double stars and stars with composite spectra are shown as separate entries. Magnitudes are provided as an indication of brightness, but these data are not necessarily accurate, as they often derive from photographic photometry or rough estimates. The file includes only spectral types determined from spectra (viz. line and band strengths or ratios), omitting those determined from photometry (e.g. DDO, Vilnius) or inferred from broadband colors or spectral energy distributions. The classifications include MK types as well as types not strictly on the MK system (white dwarfs, Wolf-Rayet, etc), and in addition simple HD-style temperature types. Luminosity classes in the early Mount Wilson style (e.g. 'd' for dwarf, 'g' for giant) and other similar schemes have been converted to modern notation. Since a citation is provided for each entry, the source paper should be consulted for details about classification schemes, spectral dispersion, and instrumentation used. System-defining primary MK standard stars are included from the last lists by Morgan and Keenan, and are flagged by a + sign in column 83. The early-type standards comprise the 1973 "dagger standards" (1973ARA&A..11...29M) and stars from the Morgan, Abt, and Tapscott atlas (1978rmsa.book.....M). Standards from Table I of the Morgan & Abt 'MKA' paper (1972AJ.....77...35M) not appearing in the two later lists are added. Keenan made continual adjustments to the standards lists up to the time of his death. Thus the late-type standards comprise those marked as high-weight standards in the 1989 Perkins catalogue (1989ApJS...71..245K = III/150); the revised S-type standards in collaboration with Boeshaar (1980ApJS...43..379K); plus the carbon standards and class IIIb 'clump giants' in collaboration with Barnbaum (1996ApJS..105..419B and 1999ApJ...518..859K). In addition, I have made use of the final types by Keenan up to January 2000 shown at the Ohio State Web site (http://www.astronomy.ohio-state.edu/MKCool), accessed in autumn 2003. Though the present file contains all the stars in these lists, only those marked as standards are flagged as such. Garrison's list of MK 'anchor points' might also be consulted in this regard (1994mpyp.conf....3G, and http://www.astro.utoronto.ca/~garrison/mkstds.html). The catalogue includes for the first time results from many large-scale objective-prism spectral surveys done at Case, Stockholm, Crimea, Abastumani, and elsewhere. The stars in these surveys were usually identified only on charts or by other indirect means, and have been overlooked heretofore because of the difficulty in recovering the stars. More complete results from these separate publications, including notes and identifications, have been made available to the CDS, and are kept at the Lowell Observatory ftp area (ftp://ftp.lowell.edu/pub/bas/starcats). Not all of these stars are present in SIMBAD. As a 'living catalogue', an attempt will be made to keep up with current literature, and to extend the indexing of citations back in time. (2 data files).

VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2013)

NASA Astrophysics Data System (ADS)

Skiff, B. A.

2013-05-01

This file contains spectral classifications for stars collected from the literature, serving as a continuation of the compilations produced by the Jascheks, by Kennedy, and by Buscombe. The source of each spectral type is indicated by a standard 19-digit bibcode citation. These papers of course should be cited in publication, not this compilation. The stars are identified either by the name used in each publication or by a valid SIMBAD identifier. Some effort has been made to determine accurate (~1" or better) coordinates for equinox J2000 (and epoch 2000 if possible), and these serve as a secondary identifier. To the extent possible with current astrometric sources, the components of double stars and stars with composite spectra are shown as separate entries. Magnitudes are provided as an indication of brightness, but these data are not necessarily accurate, as they often derive from photographic photometry or rough estimates. The file includes only spectral types determined from spectra (viz. line and band strengths or ratios), omitting those determined from photometry (e.g. DDO, Vilnius) or inferred from broadband colors or spectral energy distributions. The classifications include MK types as well as types not strictly on the MK system (white dwarfs, Wolf-Rayet, etc), and in addition simple HD-style temperature types. Luminosity classes in the early Mount Wilson style (e.g. 'd' for dwarf, 'g' for giant) and other similar schemes have been converted to modern notation. Since a citation is provided for each entry, the source paper should be consulted for details about classification schemes, spectral dispersion, and instrumentation used. System-defining primary MK standard stars are included from the last lists by Morgan and Keenan, and are flagged by a + sign in column 83. The early-type standards comprise the 1973 "dagger standards" (1973ARA&A..11...29M) and stars from the Morgan, Abt, and Tapscott atlas (1978rmsa.book.....M). Standards from Table I of the Morgan & Abt 'MKA' paper (1972AJ.....77...35M) not appearing in the two later lists are added. Keenan made continual adjustments to the standards lists up to the time of his death. Thus the late-type standards comprise those marked as high-weight standards in the 1989 Perkins catalogue (1989ApJS...71..245K = III/150); the revised S-type standards in collaboration with Boeshaar (1980ApJS...43..379K); plus the carbon standards and class IIIb 'clump giants' in collaboration with Barnbaum (1996ApJS..105..419B and 1999ApJ...518..859K). In addition, I have made use of the final types by Keenan up to January 2000 shown at the Ohio State Web site (http://www.astronomy.ohio-state.edu/MKCool), accessed in autumn 2003. Though the present file contains all the stars in these lists, only those marked as standards are flagged as such. Garrison's list of MK 'anchor points' might also be consulted in this regard (1994mpyp.conf....3G, and http://www.astro.utoronto.ca/~garrison/mkstds.html). The catalogue includes for the first time results from many large-scale objective-prism spectral surveys done at Case, Stockholm, Crimea, Abastumani, and elsewhere. The stars in these surveys were usually identified only on charts or by other indirect means, and have been overlooked heretofore because of the difficulty in recovering the stars. More complete results from these separate publications, including notes and identifications, have been made available to the CDS, and are kept at the Lowell Observatory ftp area (ftp://ftp.lowell.edu/pub/bas/starcats). Not all of these stars are present in SIMBAD. As a 'living catalogue', an attempt will be made to keep up with current literature, and to extend the indexing of citations back in time. (2 data files).

Ultraviolet spectrophotometry from Gemini 11 of stars in Orion

NASA Technical Reports Server (NTRS)

Morgan, T. H.; Spear, G. G.; Kondo, Y.; Henize, K. G.

1975-01-01

Ultraviolet spectrophotometry in the wavelength region 2600-3600 A is reported for the bright early-type stars beta, eta, gamma, delta, iota, epsilon, sigma, zeta, and kappa Ori. The results are in good agreement with other observations, and, with the possible exception of the supergiants, are in good agreement with recent line-blanketed model atmospheres. There is evidence that the supergiants possess a small ultraviolet deficiency shortward of 3000 A relative to main-sequence stars of similar spectral type. The most extreme example of this phenomenon is the star kappa Ori.

Mythical Maia, ultrashort and 53 PSC variables. Lecture 4

DOE Office of Scientific and Technical Information (OSTI.GOV)

Cox, A.N.

1983-03-14

Moving down the main sequence from the ..beta.. Cephei variables, we come to later B-type stars. The suspicion of variability for these stars goes back to Vogel in 1891 who studied the radial velocities of Vega. Since that time there have been numerous studies of Vega (Wisniewski and Johnson 1979, Fernie 1981) and other B and early A stars which hint at variability in both radial velocity and light. Since Struve (1955) discussed these stars 28 years ago, they have been called the Maia stars after the Pleiades star that he thought was the prototype. The uncertainty in their actualmore » variability has led Breger (1980) to call them the mythical Maia variables.« less

Observation of a possible optical burst of the double star Beta Camelopardalis

NASA Technical Reports Server (NTRS)

Wdowiak, T. J.; Clifton, K. S.

1985-01-01

An intensified SEC Vidicon observation of a brightening of the image of Beta Cam for a duration of about 0.25 sec at 0932 UT on December 4, 1969 is described. The observation was made during airborne observations of meteors over Canada between latitudes of 50 and 60 deg N.

Endocrine regulation of gonadotropin and growth hormone gene transcription in fish.

PubMed

Melamed, P; Rosenfeld, H; Elizur, A; Yaron, Z

1998-06-01

The pituitary of a number of teleosts contains two gonadotropins (GtHs) which are produced in distinct populations of cells; the beta subunit of the GtH I being found in close proximity to the somatotrophs, while the II beta cells are more peripheral. In several species the GtH beta subunits are expressed at varying levels throughout the reproductive cycle, the I beta dominating in early maturing fish, after which the II beta becomes predominant. This suggests differential control of the beta subunit synthesis which may be regulated by both hypothalamic hormones and gonadal steroids. At ovulation and spawning, changes also occur in the somatotrophs, which become markedly more active, while plasma growth hormone (GH) levels increase. In a number of species, GnRH elevates either the I beta or the II beta mRNA levels, depending on the reproductive state of the fish. In tilapia, the GnRH effect on the II beta appears to be mediated through both cAMP-PKA and PKC pathways. GnRH also stimulates GH release in both goldfish and tilapia, but it increases the GH transcript levels only in goldfish; both GnRH and direct activation of PKC are ineffective in altering GH mRNA in tilapia pituitary cells. Dopamine (DA) does not alter II beta transcript levels in cultured tilapia pituitary cells, but increases GH mRNA levels in both rainbow trout and tilapia, in a PKA-dependent manner. This effect appears to be through interactions with Pit-1 and also by stabilizing the mRNA. Somatostatin (SRIF) does not alter GH transcript levels in either tilapia or rainbow trout, although it may alter GH synthesis by modulation of translation. Gonadal steroids appear to have differential effects on the transcription of the beta subunits. In tilapia, testosterone (T) elevates I beta mRNA levels in cells from immature or early maturing fish (in low doses), but depresses them in cells from late maturing fish and is ineffective in cells from regressed fish. Similar results were seen in early recrudescing male coho salmon injected with T or E2. T or E2 administered in vivo has dramatic stimulatory effects on the II beta transcript levels in immature fish of a number of species, while less powerful effects are seen in vitro. A response is also seen in cells from early maturing rainbow trout or tilapia, or regressed tilapia, but not in cells from late maturing or spawning fish. These results are substantiated by the finding that the promoter of the salmon II beta gene contains several estrogen responsive elements (EREs) which react and interact differently when exposed to varying levels of E2. In addition, activator protein-1 (AP-1) and steroidogenic factor-1 (SF-1) response elements are also found in the salmon II beta promoter; the AP-1 site is located close to a half ERE, while the SF-1 acts synergistically with the E2 receptor. The mRNA levels of both AP-1 and SP-1 are elevated, at least in mammals, by GnRH, suggesting possible sites for cross-talk between GnRH and steroid activated pathways. Reports of the effects of T or E2 on GH transcription differ. No effect is seen in vitro in pituitaries of tilapia, juvenile rainbow trout or common carp, but T does increase the transcript levels in pituitaries of both immature and mature goldfish. Reasons for these discrepancies are unclear, but other systemic hormones may be more instrumental than the gonadal steroids in regulating GH transcription. These include T3 which increases both GH mRNA levels and de novo synthesis (in tilapia and common carp) and insulin-like growth factor-I (IGF-I) which reduces GH transcript levels as well as inhibiting GH release.

A novel double fine guide sensor design on space telescope

NASA Astrophysics Data System (ADS)

Zhang, Xu-xu; Yin, Da-yi

2018-02-01

To get high precision attitude for space telescope, a double marginal FOV (field of view) FGS (Fine Guide Sensor) is proposed. It is composed of two large area APS CMOS sensors and both share the same lens in main light of sight. More star vectors can be get by two FGS and be used for high precision attitude determination. To improve star identification speed, the vector cross product in inter-star angles for small marginal FOV different from traditional way is elaborated and parallel processing method is applied to pyramid algorithm. The star vectors from two sensors are then used to attitude fusion with traditional QUEST algorithm. The simulation results show that the system can get high accuracy three axis attitudes and the scheme is feasibility.

Some experiments related to L-star instability in rocket motors

NASA Technical Reports Server (NTRS)

Kumar, R. N.; Mcnamara, R. P.

1973-01-01

The role of solid phase heterogeneity on the low-pressure L-star instability of nonmetallized AP/PBAN propellants is explored. Four particle size distributions are employed in propellants that are otherwise identical. Over one hundred test firings were conducted in the 21/2 in. diameter L-star burner. Pressure time histories in the chamber and color movies of two firings constitute the raw data. An economical firing program was used which enables the interesting range of L-star values to be covered during a single firing (at a set mean pressure), through the variations in the depleting propellant volume. Time-independent combustion, Helmholtz mode, chuff mode, and the pressure-burst phenomena are revealed as the principal signatures. Of these, the Helmholtz mode is found to be the most ordered form of instability.

Stellar Activity and Outer Atmospheric Structure of Yellow Supergiants from HST STIS and GHRS Spectroscopy

NASA Astrophysics Data System (ADS)

Brown, A.; Ayres, T. R.; Harper, G. M.; Osten, R. A.; Linsky, J. L.; Dupree, A. K.; Jordan, C.

2000-05-01

Yellow supergiants with spectral types F-G show a complex pattern of outer atmospheric structure with stellar wind and activity indicators varying significantly for stars with similar positions in the H-R diagram. The efficiency of the processes driving their stellar winds and heating their atmospheres is critically dependent on the evolutionary position and surface gravity of each star. We present high-resolution ultraviolet HST/STIS and HST/GHRS spectra for a range of intermediate mass F and G supergiants, including Alpha Car (F0 Ib), Beta Cam (G0 Ib), Beta Dra (G2 Ib), and Epsilon Gem (G8 Ib), and compare the atmospheric properties of these stars with lower luminosity giants and bright giants. We provide a systematic overview of the supergiant atmospheric properties dealing particularly with activity levels, the presence of hot ``transition region'' plasma, signatures of wind outflow, and the role of overlying cool absorbing plasma that becomes increasingly prominent for the cooler stars like Epsilon Gem. This work is supported by HST grants for program GO-08280 and by NASA grant NAG5-3226.

A Catalog of Averaged Magnetic Curves

NASA Astrophysics Data System (ADS)

Bychkov, V. D.; Bychkova, L. V.; Madej, J.

2017-06-01

The second version of the catalog contains information about 275 stars of different types. Since the first catalog was created, the situation fundamentally changed primarily due to a significant increase of accuracy of magnetic field (MF) measurements. Up to now, global magnetic fields were discovered and measured in stars of many types and their behavior was partially studied. Magnetic behavior of Ap/Bp stars was studied most thoroughly. The catalog contains data on 182 such objects. The main goals for the construction of the catalog are: 1) to review and summarize our knowledge about magnetic behavior of stars of different types; 2) the whole data are uniformly presented and processed which will allow one to perform statistical analysis of the variability of (longitudinal) magnetic fields of stars; 3) the data are presented in the most convenient way for testing different theoretical models; 4) the catalog will be useful for development of observational programs.

VizieR Online Data Catalog: Abundances of bright metal-poor stars (Schlaufman+, 2014)

NASA Astrophysics Data System (ADS)

Schlaufman, K. C.; Casey, A. R.

2016-11-01

As input to our sample selection, we use the APASS DR6 Catalog, the 2MASS All-Sky Point Source Catalog, and the AllWISE Source Catalog (Henden+ 2012JAVSO..40..430H; Skrutskie+ 2006AJ....131.1163S; Wright+ 2010AJ....140.1868W; Mainzer+ 2011ApJ...731...53M). We followed up our metal-poor star candidates with the Mayall 4m/Echelle, Gemini South/GMOS-S, and Magellan/MIKE telescopes and spectrographs. We observed 98 stars with the Mayall 4m/Echelle on 2013 June 25-27. We observed 90 stars with Gemini South/GMOS-S in service mode from 2014 March to July (R~3700). We observed 416 stars with Magellan/MIKE on 2014 June 21-23 and July 8-10 (R~41000 in the blue and R~35000 in the red). (3 data files).

Detection of magnetic fields in chemically peculiar stars observed with the K2 space mission

NASA Astrophysics Data System (ADS)

Buysschaert, B.; Neiner, C.; Martin, A. J.; Aerts, C.; Bowman, D. M.; Oksala, M. E.; Van Reeth, T.

2018-05-01

We report the results of an observational study aimed at searching for magnetic pulsating hot stars suitable for magneto-asteroseismology. A sample of sixteen chemically peculiar stars was selected and analysed using both high-resolution spectropolarimetry with ESPaDOnS and K2 high-precision space photometry. For all stars, we derive the effective temperature, surface gravity, rotational and non-rotational line broadening from our spectropolarimetric data. High-quality K2 light curves were obtained for thirteen of the sixteen stars and revealed rotational modulation, providing accurate rotation periods. Two stars show evidence for roAp pulsations, and one star shows signatures of internal gravity waves or unresolved g-mode pulsations. We confirm the presence of a large-scale magnetic field for eleven of the studied stars, of which nine are first detections. Further, we report one marginal detection and four non-detections. Two of the stars with a non-detected magnetic field show rotational modulation due to surface abundance inhomogeneities in the K2 light curve, and we confirm that the other two are chemically peculiar. Thus, these five stars likely host a weak (undetected) large-scale magnetic field.

Tumor-targeting peptide conjugated pH-responsive micelles as a potential drug carrier for cancer therapy.

PubMed

Wu, Xiang Lan; Kim, Jong Ho; Koo, Heebeom; Bae, Sang Mun; Shin, Hyeri; Kim, Min Sang; Lee, Byung-Heon; Park, Rang-Woon; Kim, In-San; Choi, Kuiwon; Kwon, Ick Chan; Kim, Kwangmeyung; Lee, Doo Sung

2010-02-17

Herein, we prepared tumor-targeting peptide (AP peptide; CRKRLDRN) conjugated pH-responsive polymeric micelles (pH-PMs) in cancer therapy by active and pH-responsive tumor targeting delivery systems, simultaneously. The active tumor targeting and tumoral pH-responsive polymeric micelles were prepared by mixing AP peptide conjugated PEG-poly(d,l-lactic acid) block copolymer (AP-PEG-PLA) into the pH-responsive micelles of methyl ether poly(ethylene glycol) (MPEG)-poly(beta-amino ester) (PAE) block copolymer (MPEG-PAE). These mixed amphiphilic block copolymers were self-assembled to form stable AP peptide-conjugated and pH-responsive AP-PEG-PLA/MPEG-PAE micelles (AP-pH-PMs) with an average size of 150 nm. The AP-pH-PMs containing 10 wt % of AP-PEG-PLA showed a sharp pH-dependent micellization/demicellization transition at the tumoral acid pH. Also, they presented the pH-dependent drug release profile at the acidic pH of 6.4. The fluorescence dye, TRITC, encapsulated AP-pH-PMs (TRITC-AP-pH-PMs) presented the higher tumor-specific targeting ability in vitro cancer cell culture system and in vivo tumor-bearing mice, compared to control pH-responsive micelles of MPEG-PAE. For the cancer therapy, the anticancer drug, doxorubicin (DOX), was efficiently encapsulated into the AP-pH-PMs (DOX-AP-pH-PMs) with a higher loading efficiency. DOX-AP-pH-PMs efficiently deliver anticancer drugs in MDA-MB231 human breast tumor-bearing mice, resulted in excellent anticancer therapeutic efficacy, compared to free DOX and DOX encapsulated MEG-PAE micelles, indicating the excellent tumor targeting ability of AP-pH-PMs. Therefore, these tumor-targeting peptide-conjugated and pH-responsive polymeric micelles have great potential application in cancer therapy.

Structural characterization of the N-terminal mineral modification domains from the molluscan crystal-modulating biomineralization proteins, AP7 and AP24.

PubMed

Wustman, Brandon A; Morse, Daniel E; Evans, John Spencer

2004-08-05

The AP7 and AP24 proteins represent a class of mineral-interaction polypeptides that are found in the aragonite-containing nacre layer of mollusk shell (H. rufescens). These proteins have been shown to preferentially interfere with calcium carbonate mineral growth in vitro. It is believed that both proteins play an important role in aragonite polymorph selection in the mollusk shell. Previously, we demonstrated the 1-30 amino acid (AA) N-terminal sequences of AP7 and AP24 represent mineral interaction/modification domains in both proteins, as evidenced by their ability to frustrate calcium carbonate crystal growth at step edge regions. In this present report, using free N-terminal, C(alpha)-amide "capped" synthetic polypeptides representing the 1-30 AA regions of AP7 (AP7-1 polypeptide) and AP24 (AP24-1 polypeptide) and NMR spectroscopy, we confirm that both N-terminal sequences possess putative Ca (II) interaction polyanionic sequence regions (2 x -DD- in AP7-1, -DDDED- in AP24-1) that are random coil-like in structure. However, with regard to the remaining sequences regions, each polypeptide features unique structural differences. AP7-1 possesses an extended beta-strand or polyproline type II-like structure within the A11-M10, S12-V13, and S28-I27 sequence regions, with the remaining sequence regions adopting a random-coil-like structure, a trait common to other polyelectrolyte mineral-associated polypeptide sequences. Conversely, AP24-1 possesses random coil-like structure within A1-S9 and Q14-N16 sequence regions, and evidence for turn-like, bend, or loop conformation within the G10-N13, Q17-N24, and M29-F30 sequence regions, similar to the structures identified within the putative elastomeric proteins Lustrin A and sea urchin spicule matrix proteins. The similarities and differences in AP7 and AP24 N-terminal domain structure are discussed with regard to joint AP7-AP24 protein modification of calcium carbonate growth. Copyright 2004 Wiley Periodicals, Inc.

CTF (Subchannel) Calculations and Validation L3:VVI.H2L.P15.01

DOE Office of Scientific and Technical Information (OSTI.GOV)

Gordon, Natalie

The goal of the Verification and Validation Implementation (VVI) High to Low (Hi2Lo) process is utilizing a validated model in a high resolution code to generate synthetic data for improvement of the same model in a lower resolution code. This process is useful in circumstances where experimental data does not exist or it is not sufficient in quantity or resolution. Data from the high-fidelity code is treated as calibration data (with appropriate uncertainties and error bounds) which can be used to train parameters that affect solution accuracy in the lower-fidelity code model, thereby reducing uncertainty. This milestone presents a demonstrationmore » of the Hi2Lo process derived in the VVI focus area. The majority of the work performed herein describes the steps of the low-fidelity code used in the process with references to the work detailed in the companion high-fidelity code milestone (Reference 1). The CASL low-fidelity code used to perform this work was Cobra Thermal Fluid (CTF) and the high-fidelity code was STAR-CCM+ (STAR). The master branch version of CTF (pulled May 5, 2017 – Reference 2) was utilized for all CTF analyses performed as part of this milestone. The statistical and VVUQ components of the Hi2Lo framework were performed using Dakota version 6.6 (release date May 15, 2017 – Reference 3). Experimental data from Westinghouse Electric Company (WEC – Reference 4) was used throughout the demonstrated process to compare with the high-fidelity STAR results. A CTF parameter called Beta was chosen as the calibration parameter for this work. By default, Beta is defined as a constant mixing coefficient in CTF and is essentially a tuning parameter for mixing between subchannels. Since CTF does not have turbulence models like STAR, Beta is the parameter that performs the most similar function to the turbulence models in STAR. The purpose of the work performed in this milestone is to tune Beta to an optimal value that brings the CTF results closer to those measured in the WEC experiments.« less

VizieR Online Data Catalog: Very metal-poor stars in the Milky Way's halo (Carollo+, 2014)

NASA Astrophysics Data System (ADS)

Carollo, D.; Freeman, K.; Beers, T. C.; Placco, V. M.; Tumlinson, J.; Martell, S. L.

2017-07-01

The Aoki et al. (2013, J/AJ/145/13) sample comprises 137 stars observed at high spectral resolution (R~30000), in the course of four observing runs between 2008 March and October, using the High Dispersion Spectrograph (Noguchi et al. 2002PASJ...54..855N) at the Subaru Telescope. We also include 190 stars from the Yong et al. (2013, J/ApJ/762/26) sample - the 38 stars from their "program sample," and 152 stars in their literature compilation. High-resolution spectra (22000

130. Post1911. Photograph labeled, 'SEASON 1913. CAPTAIN, 1st MATE, SUPT ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

130. Post-1911. Photograph labeled, 'SEASON 1913. CAPTAIN, 1st MATE, SUPT AND STOREKEEPER, A.P. ASS'N CANNERY, SHIP STAR OF ALASKA.' View forward from mizzenmast, post side. - Ship BALCLUTHA, 2905 Hyde Street Pier, San Francisco, San Francisco County, CA

Apple Polysaccharide inhibits microbial dysbiosis and chronic inflammation and modulates gut permeability in HFD-fed rats.

PubMed

Wang, Sheng; Li, Qian; Zang, Yue; Zhao, Yang; Liu, Nan; Wang, Yifei; Xu, Xiaotao; Liu, Li; Mei, Qibing

2017-06-01

The saying "An apple a day keeps the doctor away" has been known for over 150 years, and numerous studies have shown that apple consumption is closely associated with reduced risks of chronic diseases. It has been well accepted that dysbiosis is the reflection of various chronic diseases. Therefore, this study investigates the effects of apple polysaccharides (AP) on gut dysbiosis. High-fat diet (HFD) fed rats were treated for 14 weeks with AP. The microbiota composition, microbiota-generated short chain fatty acids (SCFAs), gut permeability and chronic inflammation were analyzed. AP treatment showed higher abundance of Bacteroidetes and Lactobacillus while lower Firmicutes and Fusobacteium. AP significantly increased total SCFAs level that contributed by acetic acid and isobutyric acid. Moreover, AP dramatically alleviated dysbiosis-associated gut permeability and chronic inflammation with decreased plasma LBP, up-regulation of Occludin, down-regulation of tumor necrosis factor a (TNF-a), monocyte chemotactic protein 1 (MCP-1), chemokine ligand 1 (CXCL-1) and interleukin 1 beta (IL-1β). The potential mechanism is due to the fact that AP reduces gut permeability, which involves the induction of autophagy in goblet cells. Therefore, AP exerts health benefits through inhibiting gut dysbiosis and chronic inflammation and modulating gut permeability in HFD-induced dysbiosis rats. Copyright © 2017 Elsevier B.V. All rights reserved.

Time-Series Monitoring of Open Star Clusters

NASA Astrophysics Data System (ADS)

Hojaev, A. S.; Semakov, D. G.

2006-08-01

Star clusters especially a compact ones (with diameter of few to ten arcmin) are suitable targets to search of light variability for orchestera of stars by means of ordinary Casegrain telescope plus CCD system. A special patroling with short time-fixed exposures and mmag accuracy could be used also to study of stellar oscillation for group of stars simultaneously. The last can be carried out both separately from one site and within international campaigns. Detection and study of optical variability of X-ray sources including X-ray binaries with compact objects might be as a result of a long-term monitoring of such clusters as well. We present the program of open star clusters monitoring with Zeiss 1 meter RCC telescope of Maidanak observatory has been recently automated. In combination with quite good seeing at this observatory (see, e.g., Sarazin, M. 1999, URL http://www.eso.org/gen-fac/pubs/astclim/) the automatic telescope equipped with large-format (2KX2K) CCD camera AP-10 available will allow to collect homogenious time-series for analysis. We already started this program in 2001 and had a set of patrol observations with Zeiss 0.6 meter telescope and AP-10 camera in 2003. 7 compact open clusters in the Milky Way (NGC 7801, King1, King 13, King18, King20, Berkeley 55, IC 4996) have been monitored for stellar variability and some results of photometry will be presented. A few interesting variables were discovered and dozens were suspected for variability to the moment in these clusters for the first time. We have made steps to join the Whole-Earth Telescope effort in its future campaigns.

Abundances in 54 Chemical Elements in Przybylski's Star: HD 101065

NASA Astrophysics Data System (ADS)

Cowley, Charles R.; et al.

We report abundances from carbon through uranium, based on ESO observations: SN >= 200, resolution 80,000. Light elements, through the iron group scatter with respect to the standard abundance distribution (SAD). Carbon and oxygen are mildly depleted, as are iron and nickel, while titanium and cobalt are enhanced. Calcium is depleted, but silicon, sulfur, and scandium are solar. The heavier elements including some 4d and REE's are generally enhanced by 3 to 4 dex. This is not extreme for an Ap star. The truly bizarre appearance of the spectrum is an an ionization phenomena. Some hotter Ap stars have comparable lanthanide abundances, but their second spectra are weaker due to double ionization. Our adopted model has a Te of 6600K, and log(g) = 4.2. Because of the high line opacity, the photospheric pressure is low, and convection is ineffective. Chemical separation has distorted the third r-process peak only slightly. The overall coherence of the heavier elements is remarkable. Additional information is available from http://www.astro.lsa.umich.edu/users/cowley/przyb.html. This abstract is based on a paper submitted to MNRAS, by CRC, and coauthors: T. A. Ryabchikova (Moscow & Vienna), F. Kupka (Vienna), D. Bord (Michigan), G. Mathys (ESO), and W. P. Bidelman (Case-Western Reserve).

Detection of Terrestrial Planets Using Transit Photometry

NASA Astrophysics Data System (ADS)

Koch, D.; Witteborn, F.; Jenkins, J.; Dunham, E.; Borucki, W.

2000-12-01

Transit photometry detection of planets offers many advantages: an ability to detect terrestrial-size planets, direct determination of the planet's size, applicability to all main-sequence stars, and a periodic signature (differential brightness change) being independent of stellar distance or planetary orbital semi-major axis. Ground and space based photometry have already been successful in detecting transits of the giant planet HD209458b (Charbonneau, et al. 2000, Castellano et al. 2000 and references therein). However, photometry 100 times better is required to detect terrestrial planets. We present results of measurements of an end-to-end photometric system incorporating all of the important confounding noise features of both the sky and a spacebased photometer including spacecraft jitter. In addition to demonstrating an instrumental noise of less than 10 ppm per transit (an Earth transit of a solar-like star is 80 ppm), the brightnesses of individual stars were dimmed to simulate Earth-size transit signals. These "transits" were reliably detected as part of the tests. Funding for this work was provided by NASA's Discovery and Origins programs and by NASA Ames. Charbonneau, D.; Brown, T.M.; Latham, D.W.; Mayor, M., ApJ, 529, L45, 2000. Castellano, T., Jenkins, J., Trilling, D. E., Doyle, L., and Koch, D., ApJ Let. 532, L51-L53 (2000)

(beta)-catenin mediates the specification of endoderm cells in ascidian embryos.

PubMed

Imai, K; Takada, N; Satoh, N; Satou, Y

2000-07-01

In the present study, we addressed the role of (beta)-catenin in the specification of embryonic cells of the ascidians Ciona intestinalis and C. savignyi and obtained the following results: (1) During cleavages, (beta)-catenin accumulated in the nuclei of vegetal blastomeres, suggesting that it plays a role in the specification of endoderm. (2) Mis- and/or overexpression of (beta)-catenin induced the development of an endoderm-specific alkaline phosphatase (AP) in presumptive notochord cells and epidermis cells without affecting differentiation of primary lineage muscle cells. (3) Downregulation of (beta)-catenin induced by the overexpression of cadherin resulted in the suppression of endoderm cell differentiation. This suppression was compensated for by the differentiation of extra epidermis cells. (4) Specification of notochord cells did not take place in the absence of endoderm differentiation. Both the overexpression of (beta)-catenin in presumptive notochord cells and the downregulation of (beta)-catenin in presumptive endoderm cells led to the suppression of Brachyury gene expression, resulting in the failure of notochord specification. These results suggest that the accumulation of (beta)-catenin in the nuclei of endoderm progenitor cells is the first step in the process of ascidian endoderm specification.

In cellulo examination of a beta-alpha hybrid construct of beta-hexosaminidase A subunits, reported to interact with the GM2 activator protein and hydrolyze GM2 ganglioside.

PubMed

Sinici, Incilay; Yonekawa, Sayuri; Tkachyova, Ilona; Gray, Steven J; Samulski, R Jude; Wakarchuk, Warren; Mark, Brian L; Mahuran, Don J

2013-01-01

The hydrolysis in lysosomes of GM2 ganglioside to GM3 ganglioside requires the correct synthesis, intracellular assembly and transport of three separate gene products; i.e., the alpha and beta subunits of heterodimeric beta-hexosaminidase A, E.C. # 3.2.1.52 (encoded by the HEXA and HEXB genes, respectively), and the GM2-activator protein (GM2AP, encoded by the GM2A gene). Mutations in any one of these genes can result in one of three neurodegenerative diseases collectively known as GM2 gangliosidosis (HEXA, Tay-Sachs disease, MIM # 272800; HEXB, Sandhoff disease, MIM # 268800; and GM2A, AB-variant form, MIM # 272750). Elements of both of the hexosaminidase A subunits are needed to productively interact with the GM2 ganglioside-GM2AP complex in the lysosome. Some of these elements have been predicted from the crystal structures of hexosaminidase and the activator. Recently a hybrid of the two subunits has been constructed and reported to be capable of forming homodimers that can perform this reaction in vivo, which could greatly simplify vector-mediated gene transfer approaches for Tay-Sachs or Sandhoff diseases. A cDNA encoding a hybrid hexosaminidase subunit capable of dimerizing and hydrolyzing GM2 ganglioside could be incorporated into a single vector, whereas packaging both subunits of hexosaminidase A into vectors, such as adeno-associated virus, would be impractical due to size constraints. In this report we examine the previously published hybrid construct (H1) and a new more extensive hybrid (H2), with our documented in cellulo (live cell- based) assay utilizing a fluorescent GM2 ganglioside derivative. Unfortunately when Tay-Sachs cells were transfected with either the H1 or H2 hybrid construct and then were fed the GM2 derivative, no significant increase in its turnover was detected. In vitro assays with the isolated H1 or H2 homodimers confirmed that neither was capable of human GM2AP-dependent hydrolysis of GM2 ganglioside.

In Cellulo Examination of a Beta-Alpha Hybrid Construct of Beta-Hexosaminidase A Subunits, Reported to Interact with the GM2 Activator Protein and Hydrolyze GM2 Ganglioside

PubMed Central

Sinici, Incilay; Yonekawa, Sayuri; Tkachyova, Ilona; Gray, Steven J.; Samulski, R. Jude; Wakarchuk, Warren; Mark, Brian L.; Mahuran, Don J.

2013-01-01

The hydrolysis in lysosomes of GM2 ganglioside to GM3 ganglioside requires the correct synthesis, intracellular assembly and transport of three separate gene products; i.e., the alpha and beta subunits of heterodimeric beta-hexosaminidase A, E.C. # 3.2.1.52 (encoded by the HEXA and HEXB genes, respectively), and the GM2-activator protein (GM2AP, encoded by the GM2A gene). Mutations in any one of these genes can result in one of three neurodegenerative diseases collectively known as GM2 gangliosidosis (HEXA, Tay-Sachs disease, MIM # 272800; HEXB, Sandhoff disease, MIM # 268800; and GM2A, AB-variant form, MIM # 272750). Elements of both of the hexosaminidase A subunits are needed to productively interact with the GM2 ganglioside-GM2AP complex in the lysosome. Some of these elements have been predicted from the crystal structures of hexosaminidase and the activator. Recently a hybrid of the two subunits has been constructed and reported to be capable of forming homodimers that can perform this reaction in vivo, which could greatly simplify vector-mediated gene transfer approaches for Tay-Sachs or Sandhoff diseases. A cDNA encoding a hybrid hexosaminidase subunit capable of dimerizing and hydrolyzing GM2 ganglioside could be incorporated into a single vector, whereas packaging both subunits of hexosaminidase A into vectors, such as adeno-associated virus, would be impractical due to size constraints. In this report we examine the previously published hybrid construct (H1) and a new more extensive hybrid (H2), with our documented in cellulo (live cell- based) assay utilizing a fluorescent GM2 ganglioside derivative. Unfortunately when Tay-Sachs cells were transfected with either the H1 or H2 hybrid construct and then were fed the GM2 derivative, no significant increase in its turnover was detected. In vitro assays with the isolated H1 or H2 homodimers confirmed that neither was capable of human GM2AP-dependent hydrolysis of GM2 ganglioside. PMID:23483939

Magnetic fields in non-convective regions of stars.

PubMed

Braithwaite, Jonathan; Spruit, Henk C

2017-02-01

We review the current state of knowledge of magnetic fields inside stars, concentrating on recent developments concerning magnetic fields in stably stratified (zones of) stars, leaving out convective dynamo theories and observations of convective envelopes. We include the observational properties of A, B and O-type main-sequence stars, which have radiative envelopes, and the fossil field model which is normally invoked to explain the strong fields sometimes seen in these stars. Observations seem to show that Ap-type stable fields are excluded in stars with convective envelopes. Most stars contain both radiative and convective zones, and there are potentially important effects arising from the interaction of magnetic fields at the boundaries between them; the solar cycle being one of the better known examples. Related to this, we discuss whether the Sun could harbour a magnetic field in its core. Recent developments regarding the various convective and radiative layers near the surfaces of early-type stars and their observational effects are examined. We look at possible dynamo mechanisms that run on differential rotation rather than convection. Finally, we turn to neutron stars with a discussion of the possible origins for their magnetic fields.

Magnetic fields in non-convective regions of stars

PubMed Central

Braithwaite, Jonathan

2017-01-01

We review the current state of knowledge of magnetic fields inside stars, concentrating on recent developments concerning magnetic fields in stably stratified (zones of) stars, leaving out convective dynamo theories and observations of convective envelopes. We include the observational properties of A, B and O-type main-sequence stars, which have radiative envelopes, and the fossil field model which is normally invoked to explain the strong fields sometimes seen in these stars. Observations seem to show that Ap-type stable fields are excluded in stars with convective envelopes. Most stars contain both radiative and convective zones, and there are potentially important effects arising from the interaction of magnetic fields at the boundaries between them; the solar cycle being one of the better known examples. Related to this, we discuss whether the Sun could harbour a magnetic field in its core. Recent developments regarding the various convective and radiative layers near the surfaces of early-type stars and their observational effects are examined. We look at possible dynamo mechanisms that run on differential rotation rather than convection. Finally, we turn to neutron stars with a discussion of the possible origins for their magnetic fields. PMID:28386410

Inhibitory function of adapter-related protein complex 2 alpha 1 subunit in the process of nuclear translocation of human immunodeficiency virus type 1 genome

DOE Office of Scientific and Technical Information (OSTI.GOV)

Kitagawa, Yukiko; Department of Oral and Maxillofacial Surgery II, Osaka University, Osaka 565-0871; Kameoka, Masanori

2008-03-30

The transfection of human cells with siRNA against adapter-related protein complex 2 alpha 1 subunit (AP2{alpha}) was revealed to significantly up-regulate the replication of human immunodeficiency virus type 1 (HIV-1). This effect was confirmed by cell infection with vesicular stomatitis virus G protein-pseudotyped HIV-1 as well as CXCR4-tropic and CCR5-tropic HIV-1. Viral adsorption, viral entry and reverse transcription processes were not affected by cell transfection with siRNA against AP2{alpha}. In contrast, viral nuclear translocation as well as the integration process was significantly up-regulated in cells transfected with siRNA against AP2{alpha}. Confocal fluorescence microscopy revealed that a subpopulation of AP2{alpha} wasmore » not only localized in the cytoplasm but was also partly co-localized with lamin B, importin {beta} and Nup153, implying that AP2{alpha} negatively regulates HIV-1 replication in the process of nuclear translocation of viral DNA in the cytoplasm or the perinuclear region. We propose that AP2{alpha} may be a novel target for disrupting HIV-1 replication in the early stage of the viral life cycle.« less

The structure, energy balance, and winds of cool stars

NASA Technical Reports Server (NTRS)

Linsky, J. L.

1982-01-01

The phenomena associated with magnetic fields in the Sun are summarized and it is shown that similar phenomena occur in cool stars. High dispersion spectra are providing unique information concerning densities, atmospheric extension, and emission line widths. A recent unanticipated discovery is that the transition lines are redshifted (an antiwind) in beta Dra (G2 Ib) and perhaps other stars. This is interpreted as indicating downflows in closed magnetic flux tubes as are seen in the solar flux tubes above sunspots. The G and K giants and supergiants are classified as active stars, quiet stars, or hybrid stars depending on whether their atmospheres are dominated by closed magnetic flux tubes, open field geometries, or a predominately open geometry with a few closed flux tubes embedded.

The dwarf spheroidal galaxy in Draco. I - New BV photometry. II - Galactic foreground reddening

NASA Technical Reports Server (NTRS)

Stetson, P. B.

1979-01-01

BV photoelectric photometry for 39 stars and BV photographic photometry for 514 stars in the field of the Draco dwarf spheroidal galaxy are presented. The color-magnitude diagram for 512 of these field stars is found to display a well-defined red horizontal branch as well as a red giant branch whose observed width is comparable to the accidental photometric error. The results also indicate that a more diffuse sequence of stars lies about 0.1 mag to the blue of the giant branch and that an upper horizontal branch of more massive core helium-burning stars may also be present. The foreground reddening toward Draco is then determined by narrow-band uvby-beta photometry of galactic B-A-F stars.

Characterization of proflavine metabolites in rainbow trout.

PubMed

Yu, Z; Hayton, W L; Chan, K K

1997-04-01

Proflavine (3,6-diaminoacridine) has potential for use as an antiinfective in fish, and its metabolism by rainbow trout was therefore studied. Fourteen hours after intraarterial bolus administration of 10 mg/kg of proflavine, three metabolites were found in liver and bile, and one metabolite was found in plasma using reversed-phase HPLC with UV detection at 262 nm. Treatment with hydrochloric acid converted the three metabolites to proflavine, which suggested that the metabolites were proflavine conjugates. Treatment with beta-glucuronidase and saccharic acid 1,4-lactone, a specific beta-glucuronidase inhibitor, revealed that two metabolites were proflavine glucuronides. For determination of UV-VIS absorption and mass spectra, HPLC-purified metabolites were isolated from liver. Data from these experiments suggested that the proflavine metabolites were 3-N-glucuronosyl proflavine (PG), 3-N-glucuronosyl,6-N-acetyl proflavine (APG), and 3-N-acetylproflavine (AP). The identities of the metabolites were verified by chemical synthesis. When synthetic PG and AP were compared with the two metabolites isolated from trout, they had the same molecular weight as determined by matrix-assisted, laser desorption ionization, time-of-flight MS. In addition, they coeluted on HPLC under different mobile phase conditions. Finally, the in vitro incubation with liver subcellular preparations confirmed this characterization and provided the evidence that APG can be formed by glucuronidation of AP or acetylation of PG.

Inotropic effects of diadenosine tetraphosphate (AP4A) in human and animal cardiac preparations.

PubMed

Vahlensieck, U; Bokník, P; Gombosová, I; Huke, S; Knapp, J; Linck, B; Lüss, H; Müller, F U; Neumann, J; Deng, M C; Scheld, H H; Jankowski, H; Schlüter, H; Zidek, W; Zimmermann, N; Schmitz, W

1999-02-01

Diadenosine tetraphosphate (AP4A) is an endogenous compound and exerts diverse physiological effects in animal systems. However, the effects of AP4A on inotropy in ventricular cardiac preparations have not yet been studied. The effects of AP4A on force of contraction (FOC) were studied in isolated electrically driven guinea pig and human cardiac preparations. Furthermore, the effects of AP4A on L-type calcium current and [Ca]i were studied in isolated guinea pig ventricular myocytes. In guinea pig left atria, AP4A (0.1-100 microM) reduced FOC maximally by 36.5 +/- 4.3%. In guinea pig papillary muscles, AP4A (100 microM) alone was ineffective, but reduced isoproterenol-stimulated FOC maximally by 29.3 +/- 3.4%. The negative inotropic effects of AP4A in atria and papillary muscles were abolished by the A1-adenosine receptor antagonist 1, 3-dipropyl-cyclopentylxanthine. In guinea pig ventricular myocytes, AP4A (100 microM) attenuated isoproterenol-stimulated L-type calcium current and [Ca]i. In human atrial and ventricular preparations, AP4A (100 microM) alone increased FOC to 158.3 +/- 12.4% and 167.5 +/- 25.1%, respectively. These positive inotropic effects were abolished by the P2-purinoceptor antagonist suramin. On the other hand, AP4A (100 microM) reduced FOC by 27.2 +/- 7.4% in isoproterenol-stimulated human ventricular trabeculae. The latter effect was abolished by 1,3-dipropyl-cyclopentylxanthine. In summary, after beta adrenergic stimulation AP4A exerts negative inotropic effects in animal and human ventricular preparations via stimulation of A1-adenosine receptors. In contrast, AP4A alone can exert positive inotropic effects via P2-purinoceptors in human ventricular myocardium. Thus, P2-purinoceptor stimulation might be a new positive inotropic principle in the human myocardium.

P alpha-chiral phosphorothioate analogues of bis(5'-adenosyl)tetraphosphate (Ap4A); their enzymatic synthesis and degradation.

PubMed Central

Lazewska, D; Guranowski, A

1990-01-01

Synthesis of Sp and Rp diastereomers of Ap4A alpha S has been characterized in two enzymatic systems, the lysyl-tRNA synthetase from Escherichia coli and the Ap4A alpha, beta-phosphorylase from Saccharomyces cerevisiae. The synthetase was able to use both (Sp)ATP alpha S and (Rp)ATP alpha S as acceptors of adenylate thus yielding corresponding monothioanalogues of Ap4A,(Sp) Ap4A alpha S and (Rp)Ap4A alpha S. No dithiophosphate analogue was formed. Relative synthetase velocities of the formation of Ap4A,(Sp) Ap4A alpha S and (Rp)Ap4A alpha S were 1:0.38:0.15, and the computed Km values for (Sp)ATP alpha S and (Rp)ATP alpha S were 0.48 and 1.34 mM, respectively. The yeast Ap4A phosphorylase synthesized (Sp)Ap4A alpha S and (Rp)Ap4A alpha S using adenosine 5'-phosphosulfate (APS) as source of adenylate. The adenylate was accepted by corresponding thioanalogues of ATP. In that system, relative velocities of Ap4A, (Sp)Ap4A alpha S and (Rp)Ap4A alpha S formation were 1:0.15:0.60. The two isomeric phosphorothioate analogues of Ap4A were tested as substrates for the following specific Ap4A-degrading enzymes: (asymmetrical) Ap4A hydrolase (EC 3.6.1.17) from yellow lupin (Lupinus luteus) seeds hydrolyzed each of the analogues to AMP and the corresponding isomer of ATP alpha S; (symmetrical) Ap4A hydrolase (EC 3.6.1.41) from E. coli produced ADP and the corresponding diastereomer of ADP alpha S; and Ap4A phosphorylase (EC 2.7.7.53) from S. cerevisiae cleaved the Rp isomer only at the unmodified end yielding ADP and (Rp)ATP alpha S whereas the Sp isomer was degraded non-specifically yielding a mixture of ADP, (Sp)ADP alpha S, ATP and (Sp)ATP alpha S. For all the Ap4A-degrading enzymes, the Rp isomer of Ap4A alpha S appeared to be a better substrate than its Sp counterpart; stereoselectivity of the three enzymes for the Ap4A alpha S diastereomers is 51, 6 and 2.5, respectively. Basic kinetic parameters of the degradation reactions are presented and structural requirements of the Ap4A-metabolizing enzymes with respect to the potential substrates modified at the Ap4A-P alpha are discussed. PMID:2172926

Neuropsychological correlates of transcription factor AP-2Beta, and its interaction with COMT and MAOA in healthy females.

PubMed

Schabram, Ina; Eggermann, Thomas; Siegel, Steven J; Gründer, Gerhard; Zerres, Klaus; Vernaleken, Ingo

2013-01-01

The transcription factor AP-2β has been shown to impact clinical and neuropsychological properties. Apparently, it regulates the transcription of genes that code for molecules which are part of the catecholaminergic transmission system. This investigation focuses on possible effects of the transcription factor AP-2β intron 2 polymorphism on cognitive performance parameters. This hypothesis-driven investigation examined the effects and interactions of the transcription factor AP-2β intron 2 polymorphism, the Val158Met catechol-O-methyltransferase (COMT) polymorphism, and the variable number of tandem repeat polymorphism of monoamine oxidase A (MAOA) on cognitive performance parameters within a group of 200 healthy women (age: mean ± SD, 23.93 ± 3.33 years). The AP-2β polymorphism significantly influenced cognitive performance (in particular, the Trail Making Test part B), whereas the MAOA and COMT polymorphisms did not. However, there was an interaction effect of the AP-2β × MAOA × COMT genotypes on the decision bias β of the degraded-stimulus version of the continuous performance task. Only the Val158Met COMT polymorphism showed an influence on personality questionnaires (openness and self-transcendence; NEO Five-Factor Inventory, Temperament and Character Inventory). The transcription factor AP-2β intron 2 polymorphism had more influence on cognition than the MAOA and COMT polymorphisms. Possibly, the AP-2β genotype might influence cognition through pathways other than those that regulate MAOA and COMT transcription. Interactions of transcription factor AP-2β, COMT, and MAOA polymorphisms suggest higher leverage effects of transcription factor AP-2β in subjects with high dopamine availability. Copyright © 2013 S. Karger AG, Basel.

Involvement of activator protein 1 complexes in the epithelium-specific activation of the laminin gamma2-chain gene promoter by hepatocyte growth factor (scatter factor).

PubMed Central

Olsen, J; Lefebvre, O; Fritsch, C; Troelsen, J T; Orian-Rousseau, V; Kedinger, M; Simon-Assmann, P

2000-01-01

Laminin-5 is a trimer of laminin alpha3, beta3 and gamma2 chains that is found in the intestinal basement membrane. Deposition of the laminin gamma2 chain at the basement membrane is of great interest because it undergoes a developmental shift in its cellular expression. Here we study the regulatory elements that control basal and cytokine-activated transcriptional expression of the LAMC2 gene, which encodes the laminin gamma2 chain. By using transient transfection experiments we demonstrated the presence of constitutive and cytokine-responsive cis-elements. Comparison of the transcriptional activity of the LAMC2 promoter in the epithelial HT29mtx cells with that in small-intestinal fibroblastic cells (C20 cells) led us to conclude that two regions with constitutive epithelium-specific activity are present between positions -1.2 and -0.12 kb. This was further validated by transfections of primary foetal intestinal endoderm and mesenchyme. A 2.5 kb portion of the LAMC2 5' flanking region was equally responsive to PMA and hepatocyte growth factor (HGF), whereas it was less responsive to transforming growth factor beta1. A minimal promoter limited to the initial 120 bp upstream of the transcriptional start site maintained inducibility by PMA and HGF. This short promoter fragment contains two activator protein 1 (AP-1) elements and the 5'-most of these is a composite AP-1/Sp1 element. The 5'AP-1 element is crucial to the HGF-mediated activity of the promoter; analysis of interacting nuclear proteins demonstrated that AP-1 proteins containing JunD mediate the response to HGF. PMID:10749670

Race-Specific Associations of Myeloperoxidase with Atherosclerosis in a Population-Based Sample: The Dallas Heart Study

PubMed Central

Chen, Lu; Rohatgi, Anand; Ayers, Colby R.; Das, Sandeep R.; Khera, Amit; Berry, Jarett D.; McGuire, Darren K.; de Lemos, James A.

2011-01-01

Objective Myeloperoxidase (MPO) is a leukocyte-derived enzyme that appears to be directly involved in atherosclerosis development. We evaluated the association of circulating MPO with coronary and aortic atherosclerosis in a large, multiethnic population. Methods and Results Plasma levels of MPO were measured in 3294 subjects participating in the Dallas Heart Study, a probability-based population sample. Coronary artery calcification (CAC) was measured by EBCT, and abdominal aorta plaque prevalence (AP) and burden (APB), as well as abdominal aorta wall thickness (AWT) were determined by MRI. Associations between MPO and atherosclerosis phenotypes were assessed in multivariable analyses adjusting for traditional atherosclerosis risk factors. MPO levels in the 4th compared with 1st quartile independently associated with prevalent AP (OR 1.41, 95% CI 1.08–1.84), APB (beta coefficient 0.23, p=0.02), and AWT (beta coefficient 0.04, p=0.03), but not with prevalent CAC (OR 0.84, 95% CI 0.61–1.17). MPO remained associated with aortic atherosclerosis phenotypes but not coronary calcification after adjustment for other inflammatory biomarkers. A significant interaction was observed between race/ethnicity, MPO and AP (pinteraction=0.038), such that MPO levels in the 4th vs 1st quartile associated with prevalent AP in African Americans, (OR 1.81, 95% CI 1.23–2.65) but not in White or Hispanic participants (OR 0.99, 95% CI 0.68–1.44). Conclusion Higher levels of MPO associated with aortic but not coronary atherosclerosis, with significant associations limited to African American participants. These findings suggest that MPO might be a novel risk factor contributing to racial disparities in peripheral vascular disease. PMID:21917261

VizieR Online Data Catalog: IN-SYNC. III. Radial velocities of IC348 stars (Cottaar+, 2015)

NASA Astrophysics Data System (ADS)

Cottaar, M.; Covey, K. R.; Foster, J. B.; Meyer, M. R.; Tan, J. C.; Nidever, D. L.; Drew Chojnowski, S.; da Rio, N.; Flaherty, K. M.; Frinchaboy, P. M.; Majewski, S.; Skrutskie, M. F.; Wilson, J. C.; Zasowski, G.

2015-11-01

Cottaar et al. (Paper I, 2014, J/ApJ/794/125) describes the analysis of the high-resolution near-infrared spectra obtained by the APOGEE multi-object spectrograph from stars in IC 348, NGC 1333, NGC 2264, and Orion A as part of the INfrared Spectroscopy of Young Nebulous Clusters (IN-SYNC) ancillary program. Using radial velocities determined from APOGEE spectra of 380 likely cluster members, we have measured the radial velocity distribution of the young (2-6Myr) cluster IC 348. (2 data files).

Aircraft Avionics Suitable for Advanced Approach Applications. Volume 1. Aircraft Fleet Equipage.

DTIC Science & Technology

1986-07-01

have much greater display flexibility based on the menu selected by the crew and must be treated separately. Figures 2-1 through 2-10 present the...610, AD-611, ANS-31 Auto Pilot - 32* - AP-105 Flight Director - 30* - FD-108 IFC - 68 - SPZ 200, STARS/SPI 400/500, KFC -300, FCS-80 Radar 30 70 - RDR...SPZ 200A/STARS/SI, KFC -300, CENTURY IV Radar 24 76 - WXR-300, RDR-130, Primus, RDR-160, RDR-150, RDR-1300, AVQ-55, RDR-140, RDR-1200, AVQ-21, KWX-50

Local Interstellar Medium Properties and Deuterium Abundances for the Lines of Sight Toward HR 1099, 31 Comae, beta Ceti, and beta Cassiopeiae

NASA Technical Reports Server (NTRS)

Piskunov, Nikolai; Wood, Brian E.; Linsky, Jeffrey L.; Dempsey, Robert C.; Ayres, Thomas R.

1997-01-01

We analyze Goddard High-Resolution Spectrograph data to infer the properties of local interstellar gas and the Deuterium/Hydrogen (D/H) ratio for lines of sight toward four nearby late-type stars-HR 1099, 31 Comae, beta Ceti, and beta Cassiopeiae. The data consist of spectra of the hydrogen and deuterium Lyman-(alpha) lines, and echelle spectra of the Mg IIh and k lines toward all stars except beta Cas. Spectra of the RS CVn-type spectroscopic binary system HR 1099 were obtained near opposite quadratures to determine the intrinsic stellar emission line profile and the interstellar absorption separately. Multiple-velocity components were found toward HR 1099 and beta Cet. The spectra of 31 Com and beta Cet are particularly interesting because they sample lines of sight toward the north and south Galactic poles, respectively, for which H I and D I column densities were not previously available. The north Galactic pole appears to be a region of low hydrogen density like the 'interstellar tunnel' toward epsilon CMa. The temperature and turbulent velocities of the Local InterStellar Medium (LISM) that we measure for the lines of sight toward HR 1099, 31 Com, beta Cet, and beta Cas are similar to previously measured values (T approx.7000 K and xi = 1.0-1.6 km/s). The deuterium/hydrogen ratios found for these lines of sight are also consistent with previous measurements of other short lines of sight, which suggest D/H approx. 1.6 x 10(sup -5). In contrast, the Mg abundance measured for the beta Cet line of sight (implying a logarithmic depletion of D(Mg) = +0.30 +/- 0.15) is about 5 times larger than the Mg abundance previously observed toward alpha Cen, and about 20 times larger than all other previous measurements for the LISM. These results demonstrate that metal abundances in the LISM vary greatly over distances of only a few parsecs.

CRITICAL EVALUATION OF MAGNETIC FIELD DETECTIONS REPORTED FOR PULSATING B-TYPE STARS IN LIGHT OF ESPaDOnS, NARVAL, AND REANALYZED FORS1/2 OBSERVATIONS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Shultz, M.; Wade, G. A.; Grunhut, J.

2012-05-01

Recent spectropolarimetric studies of seven slowly pulsating B (SPB) and {beta} Cep stars have suggested that photospheric magnetic fields are more common in B-type pulsators than in the general population of B stars, suggesting a significant connection between magnetic and pulsational phenomena. We present an analysis of new and previously published spectropolarimetric observations of these stars. New Stokes V observations obtained with the high-resolution ESPaDOnS and Narval instruments confirm the presence of a magnetic field in one of the stars ({epsilon} Lup), but find no evidence of magnetism in five others. A re-analysis of the published longitudinal field measurements obtainedmore » with the low-resolution FORS1/2 spectropolarimeters finds that the measurements of all stars show more scatter from zero than can be attributed to Gaussian noise, suggesting the presence of a signal and/or systematic underestimation of error bars. Re-reduction and re-measurement of the FORS1/2 spectra from the ESO archive demonstrates that small changes in reduction procedure lead to substantial changes in the inferred longitudinal field, and substantially reduces the number of field detections at the 3{sigma} level. Furthermore, we find that the published periods are not unique solutions to the time series of either the original or the revised FORS1/2 data. We conclude that the reported field detections, proposed periods, and field geometry models for {alpha} Pyx, 15 CMa, 33 Eri, and V1449 Aql are artifacts of the data analysis and reduction procedures, and that magnetic fields at the reported strength are no more common in SPB/{beta} Cep stars than in the general population of B stars.« less

Beta-Decay Rates for Exotic Nuclei and R-Process Nucleosynthesis

NASA Astrophysics Data System (ADS)

Suzuki, Toshio; Yoshida, Takashi; Wanajo, Shinya; Kajino, Toshitaka; Otsuka, Takaharu

Beta-decay rates for exotic nuclei at N = 126 relevant to r-process nucleosynthesis are studied by shell-model calculations. The half-lives obtained are used to study r-process nucleosynthesis in core-collapse supernova explosions and binary neutron star mergers. The element abundances are obtained up to the third peak as well as beyond the peak region up to uranium.

Observations of H-beta and He II lambda 4686 lines in the spectra of flares of UV Cet-type stars

NASA Astrophysics Data System (ADS)

Chugainov, P. F.; Petrov, P. P.; Scherbakov, A. G.

The main results of 45.4 hours of continuous spectroscopic and photoelectric B-band observations of AD Leo, DT Virgo, and YZ CMi are discussed. In two AD Leo flares and two YZ CMi flares, an increase of the central intensity of H-beta was observed 10-20 min before the maximum B-band brightness. The spectra of one AD Leo flare and one YZ CMi flare definitely indicate the formation of broad wings of H-beta occurring mainly during flare maximum. These flares surpass the other four in total optical energy. The Stark effect seems to be the most appropriate explanation for the origin of the wings. The upper limit of the equivalent widths of the He II wavelength 4686 line was higher than that in the quiet state. The equivalent width values cannot be explained by the cascade recombination mechanism if the ratio of optical and X-ray luminosities is nearly the same for all flares of UV Cet-type stars.

Astronomical Observations by Speckle Interferometry.

DTIC Science & Technology

1986-06-12

commonly -been noted [Heintz (101)] that it was Karl *, Schwarzchild who iui 1895 [ Schwarzschild (190)] made the first measure- ments of binary stars...J. Lett 163. Michelson, A A, Pease. F. G. 1921. Ap. 280: L23 J. 53: 249 190. Schwarzschild . K. 1896. Astron. Nadir. 164. Morgan. B. L., lieddoes. 1

Functional cooperation between GATA factors and cJUN on the star promoter in MA-10 Leydig cells.

PubMed

Martin, Luc J; Bergeron, Francis; Viger, Robert S; Tremblay, Jacques J

2012-01-01

Steroid hormone biosynthesis requires the steroidogenic acute regulatory protein (STAR). STAR is part of a protein complex that transports cholesterol through the mitochondrial membrane where steroidogenesis begins. Several transcription factors participate to direct the proper spatiotemporal and hormonal regulation of the Star gene in Leydig cells. Mechanistically, this is believed to involve the functional interplay between many of these factors. Here we report a novel transcriptional cooperation between GATA factors and cJUN on the mouse Star and human STAR promoters in MA-10 Leydig cells. This cooperation was observed with different GATA members (GATA1, 4, and 6), whereas only cJUN could cooperate with GATA factors. GATA/cJUN transcriptional cooperation on the Star promoter is mediated via closely juxtaposed GATA and AP-1 binding motifs. Mutation of all functional GATA and cJUN elements abolished GATA/cJUN cooperation, which is in agreement with previous data reporting a direct interaction between GATA4 and cJUN in a heterologous system. These data add valuable new insights that further define the molecular mechanisms that govern Star transcription in steroidogenic cells of the testis.

ChromaStarPy: A Stellar Atmosphere and Spectrum Modeling and Visualization Lab in Python

NASA Astrophysics Data System (ADS)

Short, C. Ian; Bayer, Jason H. T.; Burns, Lindsey M.

2018-02-01

We announce ChromaStarPy, an integrated general stellar atmospheric modeling and spectrum synthesis code written entirely in python V. 3. ChromaStarPy is a direct port of the ChromaStarServer (CSServ) Java modeling code described in earlier papers in this series, and many of the associated JavaScript (JS) post-processing procedures have been ported and incorporated into CSPy so that students have access to ready-made data products. A python integrated development environment (IDE) allows a student in a more advanced course to experiment with the code and to graphically visualize intermediate and final results, ad hoc, as they are running it. CSPy allows students and researchers to compare modeled to observed spectra in the same IDE in which they are processing observational data, while having complete control over the stellar parameters affecting the synthetic spectra. We also take the opportunity to describe improvements that have been made to the related codes, ChromaStar (CS), CSServ, and ChromaStarDB (CSDB), that, where relevant, have also been incorporated into CSPy. The application may be found at the home page of the OpenStars project: http://www.ap.smu.ca/OpenStars/.

Submillimeter studies of main-sequence stars

NASA Technical Reports Server (NTRS)

Zuckerman, B.; Becklin, E. E.

1993-01-01

JCMT maps of the 800-micron emission from Vega, Fomalhaut, and Beta Pictoris are interpreted to indicate that they are not ringed by large reservoirs of distant orbiting dust particles that are too cold to have been detected by IRAS. A search for 800-micron emission from stars in the Pleiades and Ursa Majoris open clusters is reported. In comparison with the mass of dust particles near T Tauri and Herbig Ae stars, the JCMT data indicate a decline in dust mass during the initial 3 x 10 exp 8 yr that a star spends on the main sequence that is at least as rapid as (time) exp -2. It is estimated that in the Kuiper belt the ratio of total mass carried by small particles to that carried by comets is orders of magnitude smaller than this ratio is 1 AU from the sun. If 800-micron opacities calculated by Pollack et al. (1993) are correct, then the particles with radii less than 100 microns that dominate the FIR fluxes measured by IRAS cannot entirely account for the measured 800-micron fluxes at Vega, Beta Pic, and Fomalhaut; larger particles must be present as well.

CMOS VLSI Active-Pixel Sensor for Tracking

NASA Technical Reports Server (NTRS)

Pain, Bedabrata; Sun, Chao; Yang, Guang; Heynssens, Julie

2004-01-01

An architecture for a proposed active-pixel sensor (APS) and a design to implement the architecture in a complementary metal oxide semiconductor (CMOS) very-large-scale integrated (VLSI) circuit provide for some advanced features that are expected to be especially desirable for tracking pointlike features of stars. The architecture would also make this APS suitable for robotic- vision and general pointing and tracking applications. CMOS imagers in general are well suited for pointing and tracking because they can be configured for random access to selected pixels and to provide readout from windows of interest within their fields of view. However, until now, the architectures of CMOS imagers have not supported multiwindow operation or low-noise data collection. Moreover, smearing and motion artifacts in collected images have made prior CMOS imagers unsuitable for tracking applications. The proposed CMOS imager (see figure) would include an array of 1,024 by 1,024 pixels containing high-performance photodiode-based APS circuitry. The pixel pitch would be 9 m. The operations of the pixel circuits would be sequenced and otherwise controlled by an on-chip timing and control block, which would enable the collection of image data, during a single frame period, from either the full frame (that is, all 1,024 1,024 pixels) or from within as many as 8 different arbitrarily placed windows as large as 8 by 8 pixels each. A typical prior CMOS APS operates in a row-at-a-time ( grolling-shutter h) readout mode, which gives rise to exposure skew. In contrast, the proposed APS would operate in a sample-first/readlater mode, suppressing rolling-shutter effects. In this mode, the analog readout signals from the pixels corresponding to the windows of the interest (which windows, in the star-tracking application, would presumably contain guide stars) would be sampled rapidly by routing them through a programmable diagonal switch array to an on-chip parallel analog memory array. The diagonal-switch and memory addresses would be generated by the on-chip controller. The memory array would be large enough to hold differential signals acquired from all 8 windows during a frame period. Following the rapid sampling from all the windows, the contents of the memory array would be read out sequentially by use of a capacitive transimpedance amplifier (CTIA) at a maximum data rate of 10 MHz. This data rate is compatible with an update rate of almost 10 Hz, even in full-frame operation

Molecular Gas Clumps from the Destruction of Icy Bodies in the beta Pictoris Debris Disk

NASA Technical Reports Server (NTRS)

Dent, W. R. F.; Wyatt, M. C.; Roberge, A.; Augereau, J. -C.; Casassus, S.; Corder, S.; Greaves, J. S.; DeGregorio-Monsalvo, I.; Hales, A.; Jackson, A. P.;

Cross-talk between Smad and p38 MAPK signalling in transforming growth factor {beta} signal transduction in human glioblastoma cells

DOE Office of Scientific and Technical Information (OSTI.GOV)

Dziembowska, Magdalena; Danilkiewicz, Malgorzata; Wesolowska, Aleksandra

2007-03-23

Transforming growth factor-beta (TGF-{beta}) is a multifunctional cytokine involved in the regulation of cell proliferation, differentiation, and survival. Malignant tumour cells often do not respond to TGF-{beta} by growth inhibition, but retain responsiveness to cytokine in regulating extracellular matrix deposition, cell adhesion, and migration. We demonstrated that TGF-{beta}1 does not affect viability or proliferation of human glioblastoma T98G, but increases transcriptional responses exemplified by induction of MMP-9 expression. TGF-{beta} receptors were functional in T98G glioblastoma cells leading to SMAD3/SMAD4 nuclear translocation and activation of SMAD-dependent promoter. In parallel, a selective activation of p38 MAPK, and phosphorylation of its substrates: ATF2more » and c-Jun proteins were followed by a transient activation of AP-1 transcription factor. Surprisingly, an inhibition of p38 MAPK with a specific inhibitor, SB202190, abolished TGF-inducible activation of Smad-dependent promoter and decreased Smad2 phosphorylation. It suggests an unexpected interaction between Smad and p38 MAPK pathways in TGF-{beta}1-induced signalling.« less

Kinetic mechanism of ATP-sulphurylase from rat chondrosarcoma.

PubMed Central

Lyle, S; Geller, D H; Ng, K; Westley, J; Schwartz, N B

1994-01-01

ATP-sulphurylase catalyses the production of adenosine 5'-phosphosulphate (APS) from ATP and free sulphate with the release of PPi. APS kinase phosphorylates the APS intermediate to produce adenosine 3'-phosphate 5'-phosphosulphate (PAPS). The kinetic mechanism of rat chondrosarcoma ATP-sulphurylase was investigated by steady-state methods in the physiologically forward direction as well as the reverse direction. The sulphurylase activity was coupled to APS kinase activity in order to overcome the thermodynamic constraints of the sulphurylase reaction in the forward direction. Double-reciprocal initial-velocity plots for the forward sulphurylase intersect to the left of the ordinate for this reaction. KmATP and Kmsulphate were found to be 200 and 97 microM respectively. Chlorate, a competitive inhibitor with respect to sulphate, showed uncompetitive inhibition with respect to ATP with an apparent Ki of 1.97 mM. Steady-state data from experiments in the physiologically reverse direction also yielded double-reciprocal initial-velocity patterns that intersect to the left of the ordinate axis, with a KmAPS of 39 microM and a Kmpyrophosphate of 18 microM. The results of steady-state experiments in which Mg2+ was varied indicated that the true substrate is the MgPPi complex. An analogue of APS, adenosine 5'-[beta-methylene]phosphosulphate, was a linear inhibitor competitive with APS and non-competitive with respect to MgPPi. The simplest formal mechanism that agrees with all the data is an ordered steady-state single displacement with MgATP as the leading substrate in the forward direction and APS as the leading substrate in the reverse direction. PMID:8042976

GrayStarServer: Server-side Spectrum Synthesis with a Browser-based Client-side User Interface

NASA Astrophysics Data System (ADS)

Short, C. Ian

2016-10-01

We present GrayStarServer (GSS), a stellar atmospheric modeling and spectrum synthesis code of pedagogical accuracy that is accessible in any web browser on commonplace computational devices and that runs on a timescale of a few seconds. The addition of spectrum synthesis annotated with line identifications extends the functionality and pedagogical applicability of GSS beyond that of its predecessor, GrayStar3 (GS3). The spectrum synthesis is based on a line list acquired from the NIST atomic spectra database, and the GSS post-processing and user interface client allows the user to inspect the plain text ASCII version of the line list, as well as to apply macroscopic broadening. Unlike GS3, GSS carries out the physical modeling on the server side in Java, and communicates with the JavaScript and HTML client via an asynchronous HTTP request. We also describe other improvements beyond GS3 such as a more physical treatment of background opacity and atmospheric physics, the comparison of key results with those of the Phoenix code, and the use of the HTML < {canvas}> element for higher quality plotting and rendering of results. We also present LineListServer, a Java code for converting custom ASCII line lists in NIST format to the byte data type file format required by GSS so that users can prepare their own custom line lists. We propose a standard for marking up and packaging model atmosphere and spectrum synthesis output for data transmission and storage that will facilitate a web-based approach to stellar atmospheric modeling and spectrum synthesis. We describe some pedagogical demonstrations and exercises enabled by easily accessible, on-demand, responsive spectrum synthesis. GSS may serve as a research support tool by providing quick spectroscopic reconnaissance. GSS may be found at www.ap.smu.ca/~ishort/OpenStars/GrayStarServer/grayStarServer.html, and source tarballs for local installations of both GSS and LineListServer may be found at www.ap.smu.ca/~ishort/OpenStars/.

PKC412 (CGP41251) modulates the proliferation and lipopolysaccharide-induced inflammatory responses of RAW 264.7 macrophages

DOE Office of Scientific and Technical Information (OSTI.GOV)

Miyatake, Katsutoshi; Institute for Genome Research, The University of Tokushima, Tokushima; Inoue, Hiroshi

2007-08-17

PKC412 (CGP41251) is a multitarget protein kinase inhibitor with anti-tumor activities. Here, we investigated the effects of PKC412 on macrophages. PKC412 inhibited the proliferation of murine RAW 264.7 macrophages through induction of G2/M cell cycle arrest and apoptosis. At non-toxic drug concentrations, PKC412 significantly suppressed the lipopolysaccharide (LPS)-induced release of TNF-{alpha} and nitric oxide, while instead enhancing IL-6 secretion. PKC412 attenuated LPS-induced phosphorylations of MKK4 and JNK, as well as AP-1 DNA binding activities. Furthermore, PKC412 suppressed LPS-induced Akt and GSK-3{beta} phosphorylations. These results suggest that the anti-proliferative and immunomodulatory effects of PKC412 are, at least in part, mediated throughmore » its interference with the MKK4/JNK/AP-1 and/or Akt/GSK-3{beta} pathways. Since macrophages contribute significantly to the development of both acute and chronic inflammation, PKC412 may have therapeutic potential and applications in treating inflammatory and/or autoimmune diseases.« less

[The complement system as a main actor in the pathogenesis of obstetric antiphospholipid syndrome].

PubMed

Alijotas-Reig, Jaume

2010-01-23

Pregnancy losses are the main obstetrical complications of the obstetric antiphospholipid syndrome (obstetric-APS). Classically, they have been strongly attributed to thrombosis and further placental infarcts. But in some cases is not possible to show evidence of decidual thrombosis or placental vasculopathy, and sometimes inflammatory signs are present. Besides, the prevalence of systemic thrombosis is low in obstetric APS patients. Some cases have low plasma C4/C3 levels. Animal models show a local inflammatory mechanism. The beta2-glycoprotein-I/anti-beta2-glycoprotein-I complexes activate both, classical and alternative complement pathways. Complement proteins may injure trophoblast cells, recruiting and activating monocytes and neutrophils. Free radicals and proteolytic enzymes could also attack trophoblastic cells. In addition, an amplifier loop between the tissue factor, inflammatory cells and complement proteins could exist. Overall, these diverse mechanisms may explain both, inflammatory and thrombophilic placental alterations. In the end, the role played in this binomial by certain pro-inflammatory cytokines, mainly TNF-alpha, remains to clarify. Copyright 2009 Elsevier España, S.L. All rights reserved.

Analysis of Voyager spectra of the beta Cephei star nu Eridani

NASA Technical Reports Server (NTRS)

Porri, A.; Stalio, R.; Ali, B.; Polidan, R. S.; Morossi, C.

1994-01-01

Voyager 500-1700 A spectrophotometric observations of the beta Cephei star nu Eri are presented and discussed. The Voyager observations were obtained in 1981 and cover six pulsation cycles of the star. These data are supplemented with a set of nine International Ultraviolet Explorer (IUE) SWP high-resolution observations covering one, earlier epoch, pulsation cycle. Light curves are derived from the Voyager data at 1055 and 1425 A. These light curves are found to be consistent in both shape and period with published optical curves. The 1055 A light curve also exhibits a phenomenon not seen in the optical curves: a small but highly significant systematic increase in the flux of the maximum light phases while maintaining a constant minimum light level over the interval of observation. Substantially larger errors in the longer wavelength data preclude discussion of this phenomenon in the 1425 A light curve. Examination of the far-UV continuum in nu Eri during this period shows that the color temperature is lower for the brighter maxima. Analysis of the far-UV continuum at maximum and minimum light yields an effective temperature difference between these two phases of 2200 + or - 750 K. Spectroscopically, three prominent features are seen in the Voyager data: a feature at 985 A mostly due to a blend of C III 977 A, H I Ly gamma 972 A, and N III 990 A; a feature at 1030 A due to H I Ly beta 1026 A and C II 1037 A; and the Si IV resonance doublet near 1400 A. A comparison of the 912-1700 A spectral region in nu Eri with a set of standard, i.e., nonpulsating stars, shows that nu Eri closely resembles the standard both in continuum shape and spectral line strengths with the possible exception of a slight flux excess between 912 and 975 A. The equivalent width of the 985 A feature is shown to vary in strength over the pulsation cycle in antiphase with the light curve and variations seen in the C IV 1548-1551 lines from the IUE data. This behavior of the 985 A feature is most likely caused by variations in the strength of the Ly gamma component of the blend. Comparisons are also made between nu Eri and the only other beta Cephei star studied in the far-UV, BW Vul, with the most notable differences between the two stars being the much larger delta(T(sub eff)) for BW Vul and the almost total absence of abnormalities in observed spectrum of nu Eri.

The evolution of stable magnetic fields in stars: an analytical approach

NASA Astrophysics Data System (ADS)

Mestel, Leon; Moss, David

2010-07-01

The absence of a rigorous proof of the existence of dynamically stable, large-scale magnetic fields in radiative stars has been for many years a missing element in the fossil field theory for the magnetic Ap/Bp stars. Recent numerical simulations, by Braithwaite & Spruit and Braithwaite & Nordlund, have largely filled this gap, demonstrating convincingly that coherent global scale fields can survive for times of the order of the main-sequence lifetimes of A stars. These dynamically stable configurations take the form of magnetic tori, with linked poloidal and toroidal fields, that slowly rise towards the stellar surface. This paper studies a simple analytical model of such a torus, designed to elucidate the physical processes that govern its evolution. It is found that one-dimensional numerical calculations reproduce some key features of the numerical simulations, with radiative heat transfer, Archimedes' principle, Lorentz force and Ohmic decay all playing significant roles.

Heart Failure with Preserved Ejection Fraction: Comparison of Patients With and Without Angina Pectoris (From the Duke Databank for Cardiovascular Disease)

PubMed Central

Mentz, Robert J.; Broderick, Samuel; Shaw, Linda K.; Fiuzat, Mona; O'Connor, Christopher M.

2013-01-01

Objectives We aimed to investigate the characteristics and outcomes of patients with heart failure with preserved ejection fraction (HFpEF) and angina pectoris (AP). Background AP is a predictor of adverse events in patients with heart failure with reduced EF. The implications of AP in HFpEF are unknown. Methods We analyzed HFpEF patients (EF≥50%) who underwent coronary angiography at Duke University Medical Center from 2000–2010 with and without AP in the previous 6 weeks. Time to first event was examined using Kaplan-Meier methods for the primary endpoint of death/myocardial infarction (MI)/revascularization/stroke (i.e., MACE) and secondary endpoints of death/MI/revascularization, death/MI/stroke, death/MI, death and cardiovascular death/cardiovascular hospitalization. Results In the Duke Databank, 3517 patients met criteria for inclusion and 1402 (40%) had AP. Those with AP were older with more comorbidities, and prior revascularization vs. non-AP patients. AP patients more often received beta-blockers, ACE-inhibitors, nitrates, and statins (all P<0.05). In unadjusted analysis, AP patients had increased MACE and death/MI/revascularization (both P <0.001), lower rates of death and death/MI (both P<0.05), and similar rates of death/MI/stroke and cardiovascular death/cardiovascular hospitalization (both P>0.1). After multivariable adjustment, those with AP remained at increased risk for MACE (Hazard Ratio [HR] 1.30; 95% Confidence Interval [CI], 1.17–1.45) and death/MI/revascularization (HR 1.29; 95% CI, 1.15–1.43), but were at similar risk for other endpoints (P>0.06). Conclusions AP in HFpEF patients with a history of coronary artery disease is common despite medical therapy and is independently associated with increased MACE due to revascularization with similar risk of death, MI, and hospitalization. PMID:24161322

[Effects of astragalus polysaccharides-chitosan/polylactic acid composite material on biological behavior of canine bone marrow stromal cells cultured in vitro].

PubMed

Xu, Chun-Jiao; Jian, Xin-Chun; Peng, Jie-Ying; Guo, Feng; Huang, Bai-Ying; Xiong, Cheng-Dong; Pan, Gao-Feng

2005-06-01

To observe the biological behavior of canine bone marrow stromal cells (BMSCs) cultured in vitro with the astragalus polysaccharides-chitosan/polylactic acid (AP-C/PLA) and with the chitosan/polylactic acid (C/PLA) and to find a suitable compound material for periodontal tissue engineering. BMSCs (induced 14 days by 50 mg/L vitamine C, 10(-8) mol/L dexamethasone, 10 mmol/L beta-sodium glycerylphosphate) were cultured on AP-C/PLA or C/PLA for 5 days respectively. The BMSCs attachment and the morphology were observed with scanning electronic microscope and the combining rates were counted. Type I collagen synthesis was examined with immunohistochemistry staining and the content of osteocalin was determined with radio-immunological method. Combining rates, type I collagen synthesis, and the content of osteocalin of BMSCs on AP-C/PLA were significantly higher than those on C/PLA. AP-C/PLA may promote the BMSC proliferation, differentiation and extracellular matrix synthesis, and it can be used as a good scaffold material for bone tissue engineering.

VizieR Online Data Catalog: M31 PHAT star clusters ages and masses (Fouesneau+, 2014)

NASA Astrophysics Data System (ADS)

Fouesneau, M.; Johnson, L. C.; Weisz, D. R.; Dalcanton, J. J.; Bell, E. F.; Bianchi, L.; Caldwell, N.; Gouliermis, D. A.; Guhathakurta, P.; Kalirai, J.; Larsen, S. S.; Rix, H.-W.; Seth, A. C.; Skillman, E. D.; Williams, B. F.

2017-07-01

For this paper, we use the list of 601 high-probability cluster candidates from the Johnson et al. (2012, J/ApJ/752/95) Year 1 catalog, which contains integrated photometry through six broadband filters from the UV to the near-infrared: F275W (UV), F336W (U), F475W (g), F814W (I), F110W (J), F160W (H). Clusters were detected by eye, primarily based on the F475W images, and visually classified based on their sizes, shapes, and concentrations as explained in Johnson et al. (2012, J/ApJ/752/95). (1 data file).

VizieR Online Data Catalog: Stellar parameters and abundances for M30 (Gruyters+, 2016)

NASA Astrophysics Data System (ADS)

Gruyters, P.; Lind, K.; Richard, F.; Grundahl, O.; Asplund, M.; Casagrande, L.; Charbonnel, C.; Milone, A.; Primas, F.; Korn, A. J.

2016-03-01

Coordinates, photometry and derived effective temperatures for the 144 observed stars in M30. Effective temperatures where derived using three different temperature scales: a scale based on a Victoria isochrone (Vandenberg et al., 2014ApJ...794...72V), a scale based on the Alonso relations (Alonso, 1996A&A...313..873A, 1999A&AS..140..261A) and a scale based on the Ramirez (2005ApJ...626..465R) and Casagrande (2010A&A...512A..54C, Cat. J/A+A/512/A54) relations. Additionally, the derived Hα temperatures are given. (2 data files).

Cool circumstellar matter around nearby main-sequence stars

NASA Technical Reports Server (NTRS)

Walker, H. J.; Wolstencroft, R. D.

1988-01-01

Stars are presented which have characteristics similar to Vega and other main-sequence stars with cool dust disks, based on the IRAS Point Source Catalog fluxes. The objects are selected to have a 60-micron/100-micron ratio similar to Vega, Beta Pic, Alpha PsA, and Epsilon Eri, and they are also required to show evidence of extension in the IRAS Working Survey Database. The fluxes are modeled using a blackbody energy distribution. The temperatures derived range from 50 to 650 K. The diameters of the dust disks observed by IRAS are estimated.

Synthetic filter photometry and evolutionary status of two Be stars in the association Per OB1

NASA Technical Reports Server (NTRS)

Torres, Ana V.

1987-01-01

Stromgren and H-beta colors have been determined from spectrophotometric observations for two Be stars without published photometry in the association Per OB1: HD 12856 (B0 pe) and HD 13890 (B1 III:pe). Stellar parameters and improved spectral types are then derived from the color indices using the calibrations of Jakobsen (1986), and independently from the BCD classification method. The intrinsic properties of HD 12856 and HD 13890 are compared with those of normal B stars and are used to estimate their evolutionary status.

VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2008)

NASA Astrophysics Data System (ADS)

Skiff, B. A.

2007-01-01

This file contains spectral classifications for stars collected from the literature, serving as a continuation of the compilations produced by the Jascheks, by Kennedy, and by Buscombe. The source of each spectral type is indicated by a standard 19-digit bibcode citation. These papers of course should be cited in publication, not this compilation. The stars are identified either by the name used in each publication or by a valid SIMBAD identifier. Some effort has been made to determine accurate (~1" or better) coordinates for equinox J2000 (and epoch 2000 if possible), and these serve as a secondary identifier. To the extent possible with current astrometric sources, the components of double stars and stars with composite spectra are shown as separate entries. Magnitudes are provided as an indication of brightness, but these data are not necessarily accurate, as they often derive from photographic photometry or rough estimates. The file includes only spectral types determined from spectra (viz. line and band strengths or ratios), omitting those determined from photometry (e.g. DDO, Vilnius) or inferred from broadband colors or spectral energy distributions. The classifications include MK types as well as types not strictly on the MK system (white dwarfs, Wolf-Rayet, etc), and in addition simple HD-style temperature types. Luminosity classes in the early Mount Wilson style (e.g. 'd' for dwarf, 'g' for giant) and other similar schemes have been converted to modern notation. Since a citation is provided for each entry, the source paper should be consulted for details about classification schemes, spectral dispersion, and instrumentation used. System-defining primary MK standard stars are included from the last lists by Morgan and Keenan, and are flagged by a + sign in column 79. The early-type standards comprise the 1973 "dagger standards" (1973ARA&A..11...29M) and stars from the Morgan, Abt, and Tapscott atlas (1978rmsa.book.....M). Standards from Table I of the Morgan & Abt 'MKA' paper (1972AJ.....77...35M) not appearing in the two later lists are added. Keenan made continual adjustments to the standards lists up to the time of his death. Thus the late-type standards comprise those marked as high-weight standards in the 1989 Perkins catalogue (1989ApJS...71..245K = III/150); the revised S-type standards in collaboration with Boeshaar (1980ApJS...43..379K); plus the carbon standards and class IIIb 'clump giants' in collaboration with Barnbaum (1996ApJS..105..419B and 1999ApJ...518..859K). In addition, I have made use of the final types by Keenan up to January 2000 shown at the Ohio State Web site (http://www-astronomy.mps.ohio-state.edu/MKCool), accessed in autumn 2003. Though the present file contains all the stars in these lists, only those marked as standards are flagged as such. Garrison's list of MK 'anchor points' might also be consulted in this regard (1994mpyp.conf....3G, and http://www.astro.utoronto.ca/~garrison/mkstds.html). The catalogue includes for the first time results from many large-scale objective-prism spectral surveys done at Case, Stockholm, Crimea, Abastumani, and elsewhere. The stars in these surveys were usually identified only on charts or by other indirect means, and have been overlooked heretofore because of the difficulty in recovering the stars. More complete results from these separate publications, including notes and identifications, have been made available to the CDS, and are kept at the Lowell Observatory ftp area (ftp://ftp.lowell.edu/pub/bas/starcats). Not all of these stars are present in SIMBAD. As a 'living catalogue', an attempt will be made to keep up with current literature, and to extend the indexing of citations back in time. The sky coverage of the catalogue as of 2008 Aug 8 is shown in equatorial and galactic coordinates on these figures prepared by Chris Watson (AAVSO): ftp://ftp.lowell.edu/pub/bas/starcats/mktypes_equ.gif (113Kb) ftp://ftp.lowell.edu/pub/bas/starcats/mktypes_gal.gif (107Kb) (2 data files).

VizieR Online Data Catalog: He abundances in M30 and NGC 6397 (Mucciarelli+, 2014)

NASA Astrophysics Data System (ADS)

Mucciarelli, A.; Lovisi, L.; Lanzoni, B.; Ferraro, F. R.

2017-06-01

In this work we analyzed a set of high-resolution spectra acquired with the multi-object spectrograph FLAMES in the MEDUSA/GIRAFFE mode at the Very Large Telescope of the European Southern Observatory (ESO). The spectra are part of a data set secured within a project aimed at studying the general properties of blue straggler stars (Ferraro et al. 2006ApJ...647L..53F, 2009Natur.462.1028F, 2012Natur.492..393F; Lovisi et al. 2012, J/ApJ/754/91; 2013, J/ApJ/772/148). The employed GIRAFFE grating is HR5A (4340-4587 Å, with a spectral resolution of ~18000), suitable to sample the He I line at 4471.5 Å. Spectra have been reduced with the standard ESO FLAMES pipeline. Six exposures of 45 minutes each have been secured in each cluster. (1 data file).

VizieR Online Data Catalog: Keck/MOSFIRE spectroscopy of ZFOURGE galaxies (Tran+, 2017)

NASA Astrophysics Data System (ADS)

Tran, K.-V. H.; Alcorn, L. Y.; Kacprzak, G. G.; Nanayakkara, T.; Straatman, C.; Yuan, T.; Cowley, M.; Dave, R.; Glazebrook, K.; Kewley, L. J.; Labbe, I.; Martizzi, D.; Papovich, C.; Quadri, R.; Spitler, L. R.; Tomczak, A.

2017-06-01

Here we combine Hα emission from our ZFIRE survey (Nanayakkara+ 2016, J/ApJ/828/21) with galaxy properties from the ZFOURGE survey (Straatman+ 2016, J/ApJ/830/51) and IR luminosities from Spitzer to track how galaxies grow at z~2. ZFIRE is a near-IR spectroscopic survey with MOSFIRE on Keck I where targets are selected from ZFOURGE, an imaging survey that combines deep near-IR observations taken with the FourStar Imager at the Magellan Observatory with public multi-wavelength observations, e.g., Hubble Space Telescope (HST) imaging from CANDELS (Grogin+ 2011ApJS..197...35G). The Keck/MOSFIRE spectroscopy was obtained on observing runs in 2013 December and 2014 February. A total of eight slit masks were observed in the K-band (1.93-2.38um). We also observed two masks in the H-band covering 1.46-1.81um. (1 data file).

Copernicus observations of the Ap star Epsilon Ursae Majoris

NASA Technical Reports Server (NTRS)

Mallama, A. D.; Molnar, M. R.

1977-01-01

Spectral scans of the Ap star Epsilon UMa made with the Copernicus satellite show strong line blanketing from profuse Cr II and Fe II lines. In the spectral region covering 1900 to 3000 A, about 500 lines are present which suppress the apparent continuum by at least 15-30%. An accurate line-identification list is compiled showing Eu II present in addition to Mn II and Ni II. The identification of Eu II, however, rests on very stringent identification limits for Fe II. If these are relaxed, the existence of Eu II is dubious. There are no broad features in this spectral region which would suggest strong photoionization discontinuities by metals, but one feature near 2137 A might contain the photoionization edge due to Cr I 5S lying 0.94 eV above the ground level. However, a significant correlation between the line-blanketing strength and the amplitude of the OAO-2 ultraviolet light curves was found such that both monotonically increase in the same proportion toward shorter wavelengths. This gives additional strength to the suggestion that variations in the metal line-blanketing cause the observed photometric variations.

VizieR Online Data Catalog: Kepler pipeline transit signal recovery. III. (Christiansen+, 2016)

NASA Astrophysics Data System (ADS)

Christiansen, J. L.; Clarke, B. D.; Burke, C. J.; Jenkins, J. M.; Bryson, S. T.; Coughlin, J. L.; Mullally, F.; Thompson, S. E.; Twicken, J. D.; Batalha, N. M.; Haas, M. R.; Catanzarite, J.; Campbell, J. R.; Uddin, A. K.; Zamudio, K.; Smith, J. C.; Henze, C. E.

2018-03-01

Here we describe the third transit injection experiment, which tests the entire Kepler observing baseline (Q1-Q17) for the first time across all 84 CCD channels. It was performed to measure the sensitivity of the Kepler pipeline used to generate the Q1-Q17 Data Release 24 (DR24) catalog of Kepler Objects of Interest (Coughlin et al. 2016, J/ApJS/224/12) available at the NASA Exoplanet Archive (Akeson et al. 2013PASP..125..989A). The average detection efficiency describes the likelihood that the Kepler pipeline would successfully recover a given transit signal. To measure this property we perform a Monte Carlo experiment where we inject the signatures of simulated transiting planets around 198154 target stars, one per star, across the focal plane starting with the Q1-Q17 DR24 calibrated pixels. The simulated transits are generated using the Mandel & Agol (2002ApJ...580L.171M) model. Of the injections, 159013 resulted in three or more injected transits (the minimum required for detection by the pipeline) and were used for the subsequent analysis. (1 data file).

Biological actions of curcumin on articular chondrocytes.

PubMed

Henrotin, Y; Clutterbuck, A L; Allaway, D; Lodwig, E M; Harris, P; Mathy-Hartert, M; Shakibaei, M; Mobasheri, A

2010-02-01

Curcumin (diferuloylmethane) is the principal biochemical component of the spice turmeric and has been shown to possess potent anti-catabolic, anti-inflammatory and antioxidant, properties. This article aims to provide a summary of the actions of curcumin on articular chondrocytes from the available literature with the use of a text-mining tool. We highlight both the potential benefits and drawbacks of using this chemopreventive agent for treating osteoarthritis (OA). We also explore the recent literature on the molecular mechanisms of curcumin mediated alterations in gene expression mediated via activator protein 1 (AP-1)/nuclear factor-kappa B (NF-kappaB) signalling in chondrocytes, osteoblasts and synovial fibroblasts. A computer-aided search of the PubMed/Medline database aided by a text-mining tool to interrogate the ResNet Mammalian database 6.0. Recent work has shown that curcumin protects human chondrocytes from the catabolic actions of interleukin-1 beta (IL-1beta) including matrix metalloproteinase (MMP)-3 up-regulation, inhibition of collagen type II and down-regulation of beta1-integrin expression. Curcumin blocks IL-1beta-induced proteoglycan degradation, AP-1/NF-kappaB signalling, chondrocyte apoptosis and activation of caspase-3. The available data from published in vitro and in vivo studies suggest that curcumin may be a beneficial complementary treatment for OA in humans and companion animals. Nevertheless, before initiating extensive clinical trials, more basic research is required to improve its solubility, absorption and bioavailability and gain additional information about its safety and efficacy in different species. Once these obstacles have been overcome, curcumin and structurally related biochemicals may become safer and more suitable nutraceutical alternatives to the non-steroidal anti-inflammatory drugs that are currently used for the treatment of OA. Copyright 2009 Osteoarthritis Research Society International. All rights reserved.

Superoxide anion stress attenuates the contractile response of the Guinea pig vas deferens to ATP and diadenosine tetraphosphate. Possible effect on calcium dysregulation.

PubMed

Al-Rawi, Mahmood B; Aleisa, Abdulaziz M; Khattab, Mahmoud M

2008-01-01

Induction of endogenous superoxide anion stress by the use of the superoxide dismutase inhibitor diethylthiocarbamate (DETCA; 10 mmol/l) produced a potent inhibition of the ATP (0.3-10 mmol/l) and diadenosine tetraphosphate (AP(4)A) contractile activity in the isolated vas deferens by 29-92 and 24-90%, respectively. Pyrogallol (0.1 mmol/l), the exogenous superoxide anion generator, produced a significant inhibition on the contractile activity of the vas deferens induced by ATP and AP(4)A by 33-89 and 25-82%, respectively. DETCA (10 mmol/l) and pyrogallol (0.1 mmol/l) attenuated the contractile response of isolated guinea pig vas deferens strips to the selective P2X agonist alpha,beta-methyleneATP (alpha,beta-meATP; 50 micromol/l) by 25 and 47%, respectively. In Ca(2+)-free high-K(+) (80 mmol/l) Krebs solution, pyrogallol and DETCA produced inhibition of the contractile response to alpha,beta-meATP (50 micromol/l) in similar way to that in normal Krebs solution. The further addition of CaCl(2) (1 mmol/l) abolished the inhibitory effects exerted by pyrogallol and DETCA. The control contractile response to alpha,beta-meATP (50 micromol/l) was not affected in Ca(2+)-free high-K(+) (80 mmol/l) Krebs solution. It may be concluded that superoxide anion stress produces a significant inhibitory effect on both mono- and di-nucleotide purinergic contraction of the vas deferens. Superoxide anion appears to interrupt the P2X(1)-mediated transduction cascade at some step(s) of intracellular calcium handling. Copyright 2008 S. Karger AG, Basel.

Magnetic Doppler imaging of the chemically peculiar star HD 125248

NASA Astrophysics Data System (ADS)

Rusomarov, N.; Kochukhov, O.; Ryabchikova, T.; Ilyin, I.

2016-04-01

Context. Intermediate-mass, chemically peculiar stars with strong magnetic fields provide an excellent opportunity to study the topology of their surface magnetic fields and the interplay between magnetic geometries and abundance inhomogeneities in the atmospheres of these stars. Aims: We reconstruct detailed maps of the surface magnetic field and abundance distributions for the magnetic Ap star HD 125248. Methods: We performed the analysis based on phase-resolved, four Stokes parameter spectropolarimetric observations obtained with the HARPSpol instrument. These data were interpreted with the help of magnetic Doppler imaging techniques and model atmospheres taking the effects of strong magnetic fields and nonsolar chemical composition into account. Results: We improved the atmospheric parameters of the star, Teff = 9850 ± 250 K and log g = 4.05 ± 0.10. We performed detailed abundance analysis, which confirmed that HD 125248 has abundances typical of other Ap stars, and discovered significant vertical stratification effects for the Fe II and Cr II ions. We computed LSD Stokes profiles using several line masks corresponding to Fe-peak and rare earth elements, and studied their behavior with rotational phase. Combining previous longitudinal field measurements with our own observations, we improved the rotational period of the star Prot = 9.29558 ± 0.00006 d. Magnetic Doppler imaging of HD 125248 showed that its magnetic field is mostly poloidal and quasi-dipolar with two large spots of different polarity and field strength. The chemical maps of Fe, Cr, Ce, Nd, Gd, and Ti show abundance contrasts of 0.9-3.5 dex. Among these elements, the Fe abundance map does not show high-contrast features. Cr is overabundant around the negative magnetic pole and has 3.5 dex abundance range. The rare earth elements and Ti are overabundant near the positive magnetic pole. Conclusions: The magnetic field of HD 125248 has strong deviations from the classical oblique dipole field geometry. A comparison of the magnetic field topology of HD 125248 with the results derived for other stars using four Stokes magnetic Doppler imaging suggests evidence that the field topology becomes simpler with increasing age. The abundance maps show weak correlation with magnetic field geometry, but they do not agree with the theoretical atomic diffusion calculations, which predict element accumulation in the horizontal field regions. Based on observations collected at the European Southern Observatory, Chile (ESO programs 088.D-0066, 090.D-0256).

A Calibrated H-alpha Index to Monitor Emission Line Objects

NASA Astrophysics Data System (ADS)

Hintz, Eric G.; Joner, M. D.

2013-06-01

Over an 8 year period we have developed a calibrated H-alpha index, similar to the more traditional H-beta index, based on spectrophotometric observations (Joner & Hintz, 2013) from the DAO 1.2-m Telescope. While developing the calibration for this filter set we also obtained spectra of a number of emission line systems such as high mass x-ray binaries (HMXB), Be stars, and young stellar objects. From this work we find that the main sequence stars fill a very tight relation in the H-alpha/H-beta plane and that the emission line objects are easily detected. We will present the overall location of these emission line objects. We will also present the changes experiences by these objects over the course of the years of the project.

Ultraviolet photometry from the Orbiting Astronomical Observatory. XXVIII - Ultraviolet light curves for Alpha Lupi and BW Vulpeculae

NASA Technical Reports Server (NTRS)

Lesh, J. R.

1978-01-01

Photometric data from the Wisconsin Experiment Package on OAO-2 have been used to construct light curves at three ultraviolet wavelengths for Alpha Lup and at seven wavelengths for BW Vul. Both stars are well-known variables of the Beta Cephei (Beta Canis Majoris) type. The light curves for Alpha Lup are in good agreement with the radial-velocity period. A temperature variation of 400-500 K is derived. The BW Vul light curves confirm recent ephemerides based on a secularly varying period and show a stillstand near light maximum at some wavelengths. Both stars exhibit increasing light amplitude at the shortest ultraviolet wavelengths. There is little evidence for cycle-to-cycle variations on a time scale of the order of 1 day.

The magnetic early B-type stars I: magnetometry and rotation

NASA Astrophysics Data System (ADS)

Shultz, M. E.; Wade, G. A.; Rivinius, Th; Neiner, C.; Alecian, E.; Bohlender, D.; Monin, D.; Sikora, J.; MiMeS Collaboration; BinaMIcS Collaboration

2018-04-01

The rotational and magnetic properties of many magnetic hot stars are poorly characterized, therefore the Magnetism in Massive Stars and Binarity and Magnetic Interactions in various classes of Stars collaborations have collected extensive high-dispersion spectropolarimetric data sets of these targets. We present longitudinal magnetic field measurements for 52 early B-type stars (B5-B0), with which we attempt to determine their rotational periods Prot. Supplemented with high-resolution spectroscopy, low-resolution Dominion Astrophysical Observatory circular spectropolarimetry, and archival Hipparcos photometry, we determined Prot for 10 stars, leaving only five stars for which Prot could not be determined. Rotational ephemerides for 14 stars were refined via comparison of new to historical magnetic measurements. The distribution of Prot is very similar to that observed for the cooler Ap/Bp stars. We also measured v sin i and vmac for all stars. Comparison to non-magnetic stars shows that v sin i is much lower for magnetic stars, an expected consequence of magnetic braking. We also find evidence that vmac is lower for magnetic stars. Least-squares deconvolution profiles extracted using single-element masks revealed widespread, systematic discrepancies in between different elements: this effect is apparent only for chemically peculiar stars, suggesting it is a consequence of chemical spots. Sinusoidal fits to H line measurements (which should be minimally affected by chemical spots), yielded evidence of surface magnetic fields more complex than simple dipoles in six stars for which this has not previously been reported; however, in all six cases, the second- and third-order amplitudes are small relative to the first-order (dipolar) amplitudes.

The Copernicus ultraviolet spectral atlas of Beta Orionis

NASA Technical Reports Server (NTRS)

Rogerson, J. B., Jr.; Upson, W. L., II

1982-01-01

An ultraviolet spectral atlas is presented for the B8 Ia star Beta Orionis, which has been scanned from 999 to 1561 A by the Princeton spectrometer aboard the Copernicus satellite. From 999 to 1420 A the observations have a nominal resolution of 0.05 A. At the longer wavelengths the resolution is 0.1 A. The atlas is presented in graphs. Lines identified in the spectrum are also listed.

Cometary Dust in the Debris of HD 31648 and HD163296: Two "Baby" Beta pictoris Stars

NASA Technical Reports Server (NTRS)

Sitko, Michael L.; Grady, Carol A.; Lynch, David K.; Russell, Ray W.; Hanner, Martha S.

1999-01-01

The debris disks surrounding the pre-main-sequence stars HD 31648 and HD 163296 were observed spectroscopically between 3 and 14 microns. Both stars possess a silicate emission feature at 10 Am that resembles that of the star P Pictoris and those observed in solar system comets. The structure of the band is consistent with a mixture of olivine and pyroxene material, plus an underlying continuum of unspecified origin. The similarity in both size and structure of the silicate band suggests that the material in these systems had a processing history similar to that in our own solar system prior to the time that the grains were incorporated into comets.

Numerical Simulation of the Global Star Formation Pattern in the LMC

NASA Astrophysics Data System (ADS)

Gardiner, L. T.; Turfus, C.

Dottori et al. (1996, ApJ 461, 742) have recently presented evidence for the idea that the observed distribution of young star clusters in the Large Magellanic Cloud (LMC) has resulted from the gravitational perturbation induced by a bar potential offset from the LMC disk center. We have constructed a dynamical model of the LMC to examine the effects of such an off-center perturbation on the global distribution of the gas and star formation activity. We have used a newly developed hybrid N-body/cellular automaton scheme for modeling star formation in galaxies which incorporates the dual mechanisms of gravitational instability and self-propagating star formation, combined with feedback of kinetic energy from star-forming regions into the interstellar medium. We find that a weak rotating bar perturbation, whose center is displaced by 0.6 kpc from the disk center, gives rise to an asymmetric spiral structure which mimics the chains of recent star formation observed in the LMC as well as delineating activity in the bar region. Large gas concentrations are produced where the spiral arms merge in the northern part of the galaxy, and such structures may have observed counterparts in giant star-forming complexes such as Constellation III in the NE part of the LMC.

VizieR Online Data Catalog: Low-resolution near-infrared stellar spectra from CIBER (Kim+, 2017)

NASA Astrophysics Data System (ADS)

Kim, M. G.; Lee, H. M.; Arai, T.; Bock, J.; Cooray, A.; Jeong, W.-S.; Kim, S. J.; Korngut, P.; Lanz, A.; Lee, D. H.; Lee, M. G.; Matsumoto, T.; Matsuura, S.; Nam, U. W.; Onishi, Y.; Shirahata, M.; Smidt, J.; Tsumura, K.; Yamamura, I.; Zemcov, M.

2017-06-01

We present flux-calibrated near-infrared spectra of 105 stars from 0.8{<=}λ{<=}1.8μm with spectral resolution 15{<=}λ/Δλ{<=}30 over the range. The Low-Resolution Spectrometer (LRS) is one of the four optical instruments of the Cosmic Infrared Background Experiment (CIBER) payload; the others are a narrowband spectrometer and two wide-field imagers. The LRS is a prism-dispersed spectrometer with five rectangular 5.35°*2.8' slits imaging a 5.8°*5.8° field of view. The detector has 256*256 pixels at a pixel scale of 1.36'*1.36'. CIBER has flown four times (2009 February, 2010 July, 2012 March, and 2013 June) with apogees and total exposure times of over 325km and ~240s, respectively, in the first three flights and of 550km and 335s in the final, non-recovered flight. Due to spurious signal contamination from thermal emission from the shock-heated rocket skin, we do not use the first flight data in this work. The star spectral types are determined by fitting known spectral templates to the measured LRS spectra. We use the Infrared Telescope Facility (IRTF) and Pickles 1998 (Cat. J/PASP/110/863) templates for the SED fitting. The SpeX instrument installed on the IRTF observed stars using a medium-resolution spectrograph (R=2000). The template library contains spectra for 210 cool stars (F to M type) with wavelength coverage from 0.8 to 2.5μm (Cushing 2005ApJ...623.1115C; Rayner 2009ApJS..185..289R). The Pickles library is a synthetic spectral library that combines spectral data from various observations to achieve wavelength coverage from the UV (0.115μm) to the near-infrared (2.5μm). It contains 131 spectral templates for all star types (i.e., O to M type) with a uniform sampling interval of 5Å. (6 data files).

Correlation of beta-catenin localization with cyclooxygenase-2 expression and CpG island methylator phenotype (CIMP) in colorectal cancer.

PubMed

Kawasaki, Takako; Nosho, Katsuhiko; Ohnishi, Mutsuko; Suemoto, Yuko; Kirkner, Gregory J; Dehari, Reiko; Meyerhardt, Jeffrey A; Fuchs, Charles S; Ogino, Shuji

2007-07-01

The WNT/beta-catenin (CTNNB1) pathway is commonly activated in the carcinogenic process. Cross-talks between the WNT and cyclooxygenase-2 (COX-2 or PTGS2)/prostaglandin pathways have been suggested. The relationship between beta-catenin activation and microsatellite instability (MSI) in colorectal cancer has been controversial. The CpG island methylator phenotype (CIMP or CIMP-high) with widespread promoter methylation is a distinct epigenetic phenotype in colorectal cancer, which is associated with MSI-high. However, no study has examined the relationship between beta-catenin activation and CIMP status. Using 832 population-based colorectal cancer specimens, we assessed beta-catenin localization by immunohistochemistry. We quantified DNA methylation in eight CIMP-specific promoters [CACNA1G, CDKN2A(p16), CRABP1, IGF2, MLH1, NEUROG1, RUNX3, and SOCS1] by real-time polymerase chain reaction (MethyLight). MSI-high, CIMP-high, and BRAF mutation were associated inversely with cytoplasmic and nuclear beta-catenin expressions (i.e., beta-catenin activation) and associated positively with membrane expression. The inverse relation between beta-catenin activation and CIMP was independent of MSI. COX-2 overexpression correlated with cytoplasmic beta-catenin expression (even after tumors were stratified by CIMP status), but did not correlate significantly with nuclear or membrane expression. In conclusion, beta-catenin activation is inversely associated with CIMP-high independent of MSI status. Cytoplasmic beta-catenin is associated with COX-2 overexpression, supporting the role of cytoplasmic beta-catenin in stabilizing PTGS2 (COX-2) mRNA.

Astrophysical interpretation of the anisotropies in the unresolved gamma-ray background

NASA Astrophysics Data System (ADS)

Ando, Shin'ichiro; Fornasa, Mattia; Fornengo, Nicolao; Regis, Marco; Zechlin, Hannes-S.

2017-06-01

Recently, a new measurement of the auto- and cross-correlation angular power spectrum (APS) of the isotropic gamma-ray background was performed, based on 81 months of data of the Fermi Large-Area Telescope (LAT). Here, we fit, for the first time, the new APS data with a model describing the emission of unresolved blazars. These sources are expected to dominate the anisotropy signal. The model we employ in our analysis reproduces well the blazars resolved by Fermi LAT. When considering the APS obtained by masking the sources listed in the 3FGL catalog, we find that unresolved blazars underproduce the measured APS below ˜1 GeV . Contrary to past results, this suggests the presence of a new contribution to the low-energy APS, with a significance of, at least, 5 σ . The excess can be ascribed to a new class of faint gamma-ray emitters. If we consider the APS obtained by masking the sources in the 2FGL catalog, there is no underproduction of the APS below 1 GeV, but the new source class is still preferred over the blazars-only scenario (with a significance larger than 10 σ ). The properties of the new source class and the level of anisotropies induced in the isotropic gamma-ray background are the same, independent of the APS data used. In particular, the new gamma-ray emitters must have a soft energy spectrum, with a spectral index ranging, approximately, from 2.7 to 3.2. This complicates their interpretation in terms of known sources, since, normally, star-forming and radio galaxies are observed with a harder spectrum. The new source class identified here is also expected to contribute significantly to the intensity of the isotropic gamma-ray background.

New Frontiers in Binary Stars: Science at High Angular Resolution

DTIC Science & Technology

2008-01-01

been obtained (e.g., Horch et al. 2006), even a moderate improvement in ground-based interferometric sensitivities (V∼9 mag) could, within the decade...512, 864 Hillenbrand, L. A. & White, R. J. 2004, ApJ, 604, 741 Horch , E. P., et al. 2006, AJ, 132, 836 Hummel, C. A., et al. 2001, AJ, 121, 1623

VizieR Online Data Catalog: IN-SYNC. II. Candidate young stars in NGC 1333 (Foster+, 2015)

NASA Astrophysics Data System (ADS)

Foster, J. B.; Cottaar, M.; Covey, K. R.; Arce, H. G.; Meyer, M. R.; Nidever, D. L.; Stassun, K. G.; Tan, J. C.; Chojnowski, S. D.; da Rio, N.; Flaherty, K. M.; Rebull, L.; Frinchaboy, P. M.; Majewski, S. R.; Skrutskie, M.; Wilson, J. C.; Zasowski, G.

2015-06-01

Spectra were obtained using the APOGEE multiobject spectrograph (1.51-1.69um with R~22500). The details of the data reduction and spectral fitting are presented in Paper I (INfrared Spectra of Young Nebulous Clusters (IN-SYNC); Cottaar et al. (2014, J/ApJ/794/125). (3 data files).

VizieR Online Data Catalog: Cl0939+4713 Hα z~0.4 star-forming galaxies (Sobral+ 2016)

NASA Astrophysics Data System (ADS)

Sobral, D.; Stroe, A.; Koyama, Y.; Darvish, B.; Calhau, J.; Afonso, A.; Kodama, T.; Nakata, F.

2017-06-01

We followed up 214 candidate Hα line emitters from Koyama et al. (2011ApJ...734...66K) using AF2 on the WHT in La Palma (program ID: W14BN020) on the second half of four nights during 2015 January 22-25. (1 data file).

Apparatus Notes

ERIC Educational Resources Information Center

Eaton, Bruce G., Ed.

1976-01-01

Includes five brief articles on: solar-heating demonstration equipment, mercury or sodium vapor lamp spectroscopy, an apparatus for simulating variable stars, a voltage-to-frequency converter, and an introductory absorption experiment for low-energy beta particles. (MLH)

Submillimeter Imaging of Dust Around Main Sequence Stars

NASA Technical Reports Server (NTRS)

Jewitt, David

1998-01-01

This grant was to image circumstellar dust disks surrounding main-sequence stars. The delivery of the SCUBA detector we had planned to use for this work was delayed repeatedly, leading us to undertake a majority of the observations with the UKT14 submillimeter detector at the JCMT (James Clerk Maxwell Telescope) and optical imagers and a coronagraph at the University of Hawaii 2.2-m telescope. Major findings under this grant include: (1) We discovered 5 asymmetries in the beta Pictoris regenerated dust disk. The discovery of these asymmetries was a surprise, since smearing due to Keplerian shear should eliminate most such features on timescales of a few thousand years. One exception is the "wing tilt" asymmetry, which we interpret as due to the scattering phase function of dust disk particles. From the wing tilt and a model of the phase function, we find a disk plane inclination to the line of sight of < 5 degrees. Other asymmetries (e.g. the butterfly asymmetry) suggest a disk that has been recently disturbed. We searched for possible nearby perturbers but found no clear candidates. Low mass stars (M dwarfs) and brown dwarfs would have fallen beneath the sensitivity threshhold of our survey, however. (2) We calculated a set of disk models to assess the detectability of dust disks around stars as a function of (a) distance, (b) disk, inclination (c) dust optical depth/mass, and (d) imaging resolution. These models guided our observational strategy on Mauna Kea. (3) We performed a coronagraphic survey of approx. 100 main-sequence stars in search of additional examples of circumstellar disks. The best new candidate disk, around the 5 M(sun) star BD+31deg.643, is distinguished by its large extent (few x 10( exp 3) AU). This disk, if real, cannot be rotationally supported. We suggest that the dust particles are ejected from a smaller, unseen disk (Kuiper Belt?) by strong radiation pressure forces due to the high luminosity central star. (4) SCUBA images of circumstellar dust disks were obtained at 850 gm in 1997/8. These images show extended, asymmetric emission, but have a signal-to-noise ratio too low to permit disk mapping to large projected distances. Our images of beta Pic, in particular, are in agreement with those obtained by Holland et al., and appear to confirm the blob-structure reported first by these authors. We have not yet been able to confirm that the structure is intrinsic to the disk, since beta Pic is at -50 degree declination, and suitable observing opportunities from northern latitudes are comparatively rare (even at the +20 degree latitude of JCMT). It is possible, for instance, that the main 850 micro-m blob is merely a galaxy or other high-z source projected onto the beta Pic mid-plane.

Title: Detection of a 31.6 s pulse period for the supernova impostor SN 2010da in NGC 300, observed in ULX state

NASA Astrophysics Data System (ADS)

Carpano, S.; Haberl, F.; Maitra, C.

2018-01-01

The supernova impostor SN 2010da located in NGC 300, later identified as a likely Supergiant B[e] High-mass X-ray binary (Lau et al. 2016, ApJ, 830, 142 and Villar et al. 2016, ApJ, 830, 11), was observed in outburst during two long (139 and 82 ks) XMM-Newton observations performed on 2016 December 17 to 20. We report the discovery of a strong periodic modulation in the X-ray flux with a pulse period of 31.6 s and a very rapid spin-up, and confirm therefore that the compact object is a neutron star.

Deep Stromvil Photometry for Star Formation in the Head of the Pelican Nebula

NASA Astrophysics Data System (ADS)

Boyle, Richard P.; J., S.; Stott, J.; J., S.; Janusz, R.; J., S.; Straizys, V.

2010-01-01

The North America and Pelican Nebulae, and specifically the dark cloud L935 contain regions of active star formation (Herbig, G. H. 1958, ApJ, 128,259). Previously we reported on Vatican telescope observations by Stromvil intermediate-band filters in a 12-arcmin field in the "Gulf of Mexico" region of L935. There we classify A, F, and G-type stars. However, the many faint K and M-type dwarf stars remain somewhat ambiguous in calibration and classification. But attaining reasonable progress, we turn to another part of L935 located near the Pelican head. This area includes the "bright rim" which is formed by dust and gas condensed by the light pressure of an unseen O-type star hidden behind the dense dark cloud. Straizys and Laugalys (2008 Baltic Astronomy, 17, 143 ) have identified this star to be one of the 2MASS objects with Av=23 mag. A few concentrations of faint stars, V 13 to 14 mag. are immersed in this dark region. Among these stars are a few known emission-line objects (T-Tauri or post T-Tauri stars). A half degree nearby are some photometric Vilnius standards we use to calibrate our new field. We call on 2MASS data for correlative information. Also the Stromvil photometry offers candidate stars for spectral observations. The aim of this study in the Vilnius and Stromvil photometric systems is to classify stars down to V = 18 mag., to confirm the existence of the young star clusters, and to determine the distance of the cloud covering the suspected hidden ionizing star.

Dust disks around Vega-type stars

NASA Astrophysics Data System (ADS)

Chini, R.; Kruegel, E.; Kreysa, E.; Shustov, B.; Tutukov, A.

1991-12-01

This study presents 1300-micron observations of the circumstellar dust around Vega-type stars. A comparison of the new data (24-arcsec HPBW) for Alpha PsA, Tau-1 Eri and Epsilon Eri with previous measurements made at an angular resolution of 11-arcsec shows that the dust emission is extended. From measurements at different positions it is concluded that the circumstellar dust around Beta Pic does not exceed the size of the optical disk of 500 AU. A model for Beta Pic that fits optical as well as IR data is discussed. Finally, a scenario for the evolution of circumstellar grains is suggested where, on one side, the Poynting-Robertson effect removes the small particles and, on the other side, collisions lead to the formation of larger bodies. Time-dependent IR spectra in reasonable agreement with observations are presented.

UV habitable zones around M stars

NASA Astrophysics Data System (ADS)

Buccino, Andrea P.; Lemarchand, Guillermo A.; Mauas, Pablo J. D.

2007-12-01

During the last decade there was a change in paradigm, which led to consider that terrestrial-type planets within liquid-water habitable zones (LW-HZ) around M stars can also be suitable places for the emergence and evolution of life. Since many dMe stars emit large amount of UV radiation during flares, in this work we analyze the UV constrains for living systems on Earth-like planets around dM stars. We apply our model of UV habitable zone (UV-HZ; Buccino, A.P., Lemarchand, G.A., Mauas, P.J.D., 2006. Icarus 183, 491-503) to the three planetary systems around dM stars (HIP 74995, HIP 109388 and HIP 113020) observed by IUE and to two M-flare stars (AD Leo and EV Lac). In particular, HIP 74995 hosts a terrestrial planet in the LW-HZ, which is the exoplanet that most resembles our own Earth. We show, in general, that during the quiescent state there would not be enough UV radiation within the LW-HZ to trigger the biogenic processes and that this energy could be provided by flares of moderate intensity, while strong flares do not necessarily rule-out the possibility of life-bearing planets.

VizieR Online Data Catalog: Stellar encounters with long-period comets (Feng+, 2015)

NASA Astrophysics Data System (ADS)

Feng, F.; Bailer-Jones, C. A. L.

2016-07-01

We have conducted simulations of the perturbation of the Oort cloud in order to estimate the significance of known encounters in generating long-period comets. We collected the data of stellar encounters from three sources: (Bailer-Jones, 2015, Cat. J/A+A/575/A35, hereafter BJ15), Dybczynski & Berski (2015MNRAS.449.2459D), and Mamajek et al. (2015ApJ...800L..17M). Following BJ15, we use the term 'object' to refer to each encountering star in our catalogue. A specific star may appear more than once but with different data, thus leading to a different object. (1 data file).

The likely optical counterpart of X-ray transient KS 1731-260

NASA Astrophysics Data System (ADS)

Wijnands, Rudy; Groot, Paul J.; Miller, Jon J.; Markwardt, Craig; Lewin, Walter H. G.; van der Klis, Michiel

2001-07-01

During our 27 March 2001 Chandra observation of the neutron star X-ray transient KS 1731-260, two X-ray sources were detected (Wijnands et al. 2001, ApJL submitted, astro-ph/0107380). One of those sources is very likely a star in the USNO A2.0 optical catalog (Monet et al. 1998, USNO-SA2.0, U.S. Naval Observatory, Washington DC) and in the Two Micron All Sky Survey (2MASS) point source catalog with a position (from 2MASS) of R.A = 17h34m12.70s, Dec. -26d05m48.4s (+/- 0.2 arcseconds).

TGF-beta induces connexin43 gene expression in normal murine mammary gland epithelial cells via activation of p38 and PI3K/AKT signaling pathways.

PubMed

Tacheau, Charlotte; Fontaine, Juliette; Loy, Jennifer; Mauviel, Alain; Verrecchia, Franck

2008-12-01

One of the shared physiological roles between TGF-beta and connexin family members is to inhibit epithelial cell cycle progression and consequently, to provide protection against malignant transformation. Herein, we demonstrated that TGF-beta1 induces the expression of connexin43 (Cx43) in normal murine mammary gland (NMuMG) cell lines at the protein and mRNA levels, and transcriptionally. Using overexpression of a truncated dominant-negative form of Cx43, we determined that the modulation of gap junctional communication by TGF-beta1 plays a key role in the control of NMuMG cells proliferation by TGF-beta1. In addition, using overexpression of truncated dominant-negative forms of either Smad2 or Smad3, and MDA-MB-468 human breast carcinoma cells deficient for Smad4, we determined that the Smad cascade is not implicated in TGF-beta1 effect on Cx43 expression. Using specific pharmacologic inhibitors for JNK, ERK, p38, and PI3K/AKT signaling pathways, we demonstrated the cooperative role of p38 and PI3K/AKT signaling in TGF-beta1-induced Cx43 expression and gap junctional communication. Furthermore, transfection of a c-jun antisense expression vector significantly prevented TGF-beta1-induced Cx43 gene expression demonstrating the involvement of c-Jun/AP-1 pathway together with p38 and PI3K/AKT pathways in mediating TGF-beta1-induced Cx43 gene expression.

Heart failure with preserved ejection fraction: comparison of patients with and without angina pectoris (from the Duke Databank for Cardiovascular Disease).

PubMed

Mentz, Robert J; Broderick, Samuel; Shaw, Linda K; Fiuzat, Mona; O'Connor, Christopher M

2014-01-28

This study investigated the characteristics and outcomes of patients with heart failure with preserved ejection fraction (HFpEF) and angina pectoris (AP). AP is a predictor of adverse events in patients with heart failure with reduced EF. The implications of AP in HFpEF are unknown. We analyzed HFpEF patients (EF ≥50%) who underwent coronary angiography at Duke University Medical Center from 2000 through 2010 with and without AP in the previous 6 weeks. Time to first event was examined using Kaplan-Meier methods for the primary endpoint of death/myocardial infarction (MI)/revascularization/stroke (i.e., major adverse cardiac events [MACE]) and secondary endpoints of death/MI/revascularization, death/MI/stroke, death/MI, death, and cardiovascular death/cardiovascular hospitalization. In the Duke Databank, 3,517 patients met criteria for inclusion and 1,402 (40%) had AP. Those with AP were older with more comorbidities and prior revascularization compared with non-AP patients. AP patients more often received beta-blockers, angiotensin-converting enzyme inhibitors, nitrates, and statins (all p < 0.05). In unadjusted analysis, AP patients had increased MACE and death/MI/revascularization (both p < 0.001), lower rates of death and death/MI (both p < 0.05), and similar rates of death/MI/stroke and cardiovascular death/cardiovascular hospitalization (both p > 0.1). After multivariable adjustment, those with AP remained at increased risk for MACE (hazard ratio [HR]: 1.30, 95% confidence interval [CI]: 1.17 to 1.45) and death/MI/revascularization (HR: 1.29, 95% CI: 1.15 to 1.43), but they were at similar risk for other endpoints (p > 0.06). AP in HFpEF patients with a history of coronary artery disease is common despite medical therapy and is independently associated with increased MACE due to revascularization with similar risk of death, MI, and hospitalization. Copyright © 2014 American College of Cardiology Foundation. Published by Elsevier Inc. All rights reserved.

Chandra/ACIS Spectra of the 30 Doradus Star Forming Region

NASA Astrophysics Data System (ADS)

Townsley, L.; Broos, P.; Feigelson, E.; Burrows, D.; Chu, Y.-H.; Garmire, G.; Griffiths, R.; Maeda, Y.; Tsuboi, Y.

2000-12-01

We present the first high-spatial-resolution X-ray spectra of constituents of the 30 Doradus star-forming region in the Large Magellanic Cloud, obtained with the Advanced CCD Imaging Spectrometer (ACIS) aboard the Chandra X-ray Observatory. Our continuing efforts to remove the spectral effects of CCD charge transfer inefficiency (CTI) due to radiation damage are described. The central cluster of young high-mass stars, R136, is resolved at the arcsecond level by ACIS, allowing spectral analysis of several constituents. Other Wolf-Rayet stars and multiple systems (e.g. R139, R140) are also detected. Spatially-resolved spectra are presented for N157B, the plerion SNR recently shown by X-ray observations to contain a 16-msec pulsar (Marshall et al., ApJ 499, L179). The spectrally soft superbubble structures seen by ROSAT are visible in the Chandra image; a composite spectrum, improved with CTI correction, is presented. Support for this effort was provided by NASA contract NAS8-38252 to Gordon Garmire, the ACIS Principal Investigator.

Hydra multiple head star sensor and its in-flight self-calibration of optical heads alignment

NASA Astrophysics Data System (ADS)

Majewski, L.; Blarre, L.; Perrimon, N.; Kocher, Y.; Martinez, P. E.; Dussy, S.

2017-11-01

HYDRA is EADS SODERN new product line of APS-based autonomous star trackers. The baseline is a multiple head sensor made of three separated optical heads and one electronic unit. Actually the concept which was chosen offers more than three single-head star trackers working independently. Since HYDRA merges all fields of view the result is a more accurate, more robust and completely autonomous multiple-head sensor, releasing the AOCS from the need to manage the outputs of independent single-head star trackers. Specific to the multiple head architecture and the underlying data fusion, is the calibration of the relative alignments between the sensor optical heads. The performance of the sensor is related to its estimation of such alignments. HYDRA design is first reminded in this paper along with simplification it can bring at system level (AOCS). Then self-calibration of optical heads alignment is highlighted through descriptions and simulation results, thus demonstrating the performances of a key part of HYDRA multiple-head concept.

Resolving Supercritical Orion Cores

NASA Astrophysics Data System (ADS)

Li, Di; Chapman, N.; Goldsmith, P.; Velusamy, T.

2009-01-01

The theoretical framework for high mass star formation (HMSF) is unclear. Observations reveal a seeming dichotomy between high- and low-mass star formation, with HMSF occurring only in Giant Molecular Clouds (GMC), mostly in clusters, and with higher star formation efficiencies than low-mass star formation. One crucial constraint to any theoretical model is the dynamical state of massive cores, in particular, whether a massive core is in supercritical collapse. Based on the mass-size relation of dust emission, we select likely unstable targets from a sample of massive cores (Li et al. 2007 ApJ 655, 351) in the nearest GMC, Orion. We have obtained N2H+ (1-0) maps using CARMA with resolution ( 2.5", 0.006 pc) significantly better than existing observations. We present observational and modeling results for ORI22. By revealing the dynamic structure down to Jeans scale, CARMA data confirms the dominance of gravity over turbulence in this cores. This work was performed by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.

Molecular and functional characterization of clathrin- and AP-2-binding determinants within a disordered domain of auxilin.

PubMed

Scheele, Urte; Alves, Jurgen; Frank, Ronald; Duwel, Michael; Kalthoff, Christoph; Ungewickell, Ernst

2003-07-11

Uncoating of clathrin-coated vesicles requires the J-domain protein auxilin for targeting hsc70 to the clathrin coats and for stimulating the hsc70 ATPase activity. This results in the release of hsc70-complexed clathrin triskelia and concomitant dissociation of the coat. To understand the complex role of auxilin in uncoating and clathrin assembly in more detail, we analyzed the molecular organization of its clathrin-binding domain (amino acids 547-813). CD spectroscopy of auxilin fragments revealed that the clathrin-binding domain is almost completely disordered in solution. By systematic mapping using synthetic peptides and by site-directed mutagenesis, we identified short peptide sequences involved in clathrin heavy chain and AP-2 binding and evaluated their significance for the function of auxilin. Some of the binding determinants, including those containing sequences 674DPF and 636WDW, showed dual specificity for both clathrin and AP-2. In contrast, the two DLL motifs within the clathrin-binding domain were exclusively involved in clathrin binding. Surprisingly, they interacted not only with the N-terminal domain of the heavy chain, but also with the distal domain. Moreover, both DLL peptides proved to be essential for clathrin assembly and uncoating. In addition, we found that the motif 726NWQ is required for efficient clathrin assembly activity. Auxilin shares a number of protein-protein interaction motifs with other endocytic proteins, including AP180. We demonstrate that AP180 and auxilin compete for binding to the alpha-ear domain of AP-2. Like AP180, auxilin also directly interacts with the ear domain of beta-adaptin. On the basis of our data, we propose a refined model for the uncoating mechanism of clathrin-coated vesicles.

Copernicus spectra of beta Lyrae. [in far UV

NASA Technical Reports Server (NTRS)

Hack, M.; Hutchings, J. B.; Kondo, Y.; Mccluskey, G. E.; Plavec, M.; Polidan, R. S.

1974-01-01

The observations reported were made in August and September 1973. The principal data were scans in the low resolution mode at phases nearly coincident with the two light minima. Shorter scans were obtained at the two quadrature phases. The data show that the secondary component of beta Lyrae is a hotter object than the visible B8 star. The velocity amplitude of the lines suggests that the secondary is the more massive object, by a factor of several times.

ACS Imaging of beta Pic: Searching for the origin of rings and asymmetry in planetesimal disks

NASA Astrophysics Data System (ADS)

Kalas, Paul

2003-07-01

The emerging picture for planetesimal disks around main sequence stars is that their radial and azimuthal symmetries are significantly deformed by the dynamical effects of either planets interior to the disk, or stellar objects exterior to the disk. The cause of these structures, such as the 50 AU cutoff of our Kuiper Belt, remains mysterious. Structure in the beta Pic planetesimal disk could be due to dynamics controlled by an extrasolar planet, or by the tidal influence of a more massive object exterior to the disk. The hypothesis of an extrasolar planet causing the vertical deformation in the disk predicts a blue color to the disk perpendicular to the disk midplane. The hypothesis that a stellar perturber deforms the disk predicts a globally uniform color and the existence of ring-like structure beyond 800 AU radius. We propose to obtain deep, multi-color images of the beta Pic disk ansae in the region 15"-220" {200-4000 AU} radius with the ACS WFC. The unparalleled stability of the HST PSF means that these data are uniquely capable of delivering the color sensitivity that can distinguish between the two theories of beta Pic's disk structure. Ascertaining the cause of such structure provide a meaningful context for understanding the dynamical history of our early solar system, as well as other planetesimal systems imaged around main sequence stars.

Evidence for Black Hole Event Horizons?, or Luminosities of Black Hole and Neutron Star Transients

NASA Astrophysics Data System (ADS)

Garcia, M.; McClintock, J.; Narayan, R.

1996-12-01

Recently, models for Advection Dominated Accretion Flow (ADAF) have been shown to explain many of the quiescent properties of the X-ray and optical emission from black hole soft X-ray transients (BH SXT) (Narayan, McClintock and Yi 1996 ApJ 457, 821; Narayan, Barret and McClintock 1996, submitted to ApJ). One novel feature of the ADAF model is that the black hole event horizon plays a key role in the energetics of the flow, in that it absorbs the majority of the energy in the accretion flow. An ADAF flow around a neutron star (NS) SXT instead will release all of its accretion energy upon impacting on the NS surface (Yi et al 1996, submitted to A&A). Therefore one expects that NS SXT will be substantially more luminous than BH SXT in quiescence. We present results on 5 NS SXT and 4 BH SXT that appear to bear out this expectation. In the context of the ADAF model, the larger dynamic range in BH SXT outburst/quiescent luminosities can be seen as evidence for the existence of an event horizon in these BH.

VizieR Online Data Catalog: Pan-Pacific Planet Search (PPPS) I. 7 CMa (Wittenmyer+, 2011)

NASA Astrophysics Data System (ADS)

Wittenmyer, R. A.; Endl, M.; Wang, L.; Johnson, J. A.; Tinney, C. G.; O'Toole, S. J.

2013-05-01

The "Pan-Pacific Planet Search" (PPPS) originated as a Southern Hemisphere extension of the established Lick & Keck Observatory survey for planets orbiting Northern "retired A stars" (Johnson et al. 2006ApJ...652.1724J, 2007ApJ...665..785J, 2010PASP..122..905J). This program is using the 3.9m Anglo-Australian Telescope (AAT) to observe a metal-rich sample of Southern Hemisphere subgiants. Observations for the PPPS began at the AAT in 2009 February. Observing time is scheduled such that each target should receive 4-6 observations per year. PPPS Doppler measurements are made with the UCLES echelle spectrograph (at the 3.9m AAT) which achieves a resolution of 45000 with a 1 arcsec slit. We have observed 7 CMa on 21 epochs, and an iodine-free template observation was obtained on 2010 January 30. Since 7 CMa is an extremely bright star, exposure times ranged from 100 to 500s, with a resulting S/N of ~200-300/pixel each epoch. The data span a total of 917 days and have a mean internal velocity uncertainty of 6.5m/s. (2 data files).

The SEEDS Direct Imaging Survey for Planets and Scattered Dust Emission in Debris Disk Systems

NASA Technical Reports Server (NTRS)

Janson, Markus; Brandt, Timothy; Moro-Martin, Amaya; Usuda, Tomonori; Thalmann, Christian; Carson, Joseph C.; Goto, Miwa; Currie, Thayne; McElwain, M. W.; Itoh, Yoichi;

An Analysis of the Rapidly Rotating Bp star HD 133880

NASA Technical Reports Server (NTRS)

Bailey, J. D.; Grunhut, J.; Shultz, M.; Wade, G.; Landstreet, J. D.; Bohlender, D.; Lim, J.; Wong, K.; Drake, S.; Linsky, J.

2012-01-01

HD 133880 is a rapidly rotating chemically peculiar B-type (Bp) star (nu sin i approx = 103km/s) and is host to one of the strongest magnetic fields of any Ap/Bp star. A member of the Upper Centaurus Lupus association, it is a star with a well-determined age of 16 Myr. 12 new spectra, four of which are polarimetric, obtained from the FEROS, ESPaDOnS and HARPS instruments, provide sufficient material from which to re-evaluate the magnetic field and obtain a first approximation to the atmospheric abundance distributions of He, O, Mg, Si, Ti. Cr, Fe, Ni, Pr and Nd. An abundance analysis was carried out using ZEEMAN, a program which synthesizes spectral line profiles for stars with permeating magnetic fields. The magnetic field structure was characterized by a colinear multipole expansion from the observed variations of the longitudinal and surface fields with rotational phase. Both magnetic hemispheres are clearly visible during the stellar rotation, and thus a three-ring abundance distribution model encompassing both magnetic poles and magnetic equator with equal spans in colatitude was adopted. Using the new magnetic field measurements and optical photometry together with previously published data, we refine the period of HD 133880 to P = 0.877 476 +/- 0.000009 d. Our simple axisymmetric magnetic field model is based on a predominantly quadrupolar component that roughly describes the field variations. Using spectrum synthesis, we derived mean abundances for O, Mg, Si, Ti, Cr, Fe and Pr. All elements; except Mg, are overabundant compared to the Son. Mg appears to be approximately uniform over the stellar surface, while all other elements are more abundant in the negative magnetic hemisphere than in the positive magnetic hemisphere. In contrast to most Ap/Bp stars which show an underabundance in 0, in HD 133880 this element is clearly overabundant compared to the solar abundance ratio. In studying the Ha and Paschen lines in the optical spectra, we could not unambiguously detect information about the magnetosphere of HD 133880. However, radio emission data at both 3 and 6 cm suggest that the magnetospheric plasma is held in rigid rotation with the star by the magnetic field and further supported against collapse by the rapid rotation. Subtle differences in the shapes of the optically thick radio light curves at 3 and 6 cm suggest that the large-scale magnetic field is not fully axisymmetric at large distances from the star.

The 11 micron Silicon Carbide Feature in Carbon Star Shells

NASA Technical Reports Server (NTRS)

Speck, A. K.; Barlow, M. J.; Skinner, C. J.

1996-01-01

Silicon carbide (SiC) is known to form in circumstellar shells around carbon stars. SiC can come in two basic types - hexagonal alpha-SiC or cubic beta-SiC. Laboratory studies have shown that both types of SiC exhibit an emission feature in the 11-11.5 micron region, the size and shape of the feature varying with type, size and shape of the SiC grains. Such a feature can be seen in the spectra of carbon stars. Silicon carbide grains have also been found in meteorites. The aim of the current work is to identity the type(s) of SiC found in circumstellar shells and how they might relate to meteoritic SiC samples. We have used the CGS3 spectrometer at the 3.8 m UKIRT to obtain 7.5-13.5 micron spectra of 31 definite or proposed carbon stars. After flux-calibration, each spectrum was fitted using a chi(exp 2)-minimisation routine equipped with the published laboratory optical constants of six different samples of small SiC particles, together with the ability to fit the underlying continuum using a range of grain emissivity laws. It was found that the majority of observed SiC emission features could only be fitted by alpha-SiC grains. The lack of beta-SiC is surprising, as this is the form most commonly found in meteorites. Included in the sample were four sources, all of which have been proposed to be carbon stars, that appear to show the SiC feature in absorption.

FAMIAS User Manual

NASA Astrophysics Data System (ADS)

Zima, Wolfgang

2008-10-01

The excitation of pulsation modes in Beta Cephei and Slowly Pulsating B stars is known to be very sensitive to opacity changes in the stellar interior where T ~ 2 x 10E5 K. In this region differences in opacity up to ~ 50% can be induced by the choice between OPAL and OP opacity tables, and between two different metal mixtures (Grevesse & Noels 1993 and Asplund et al. 2005). We have extended the non-adiabatic computations presented in Miglio et al. (2007) towards models of higher mass and pulsation modes of degree l = 3, and we present here the instability domains in the HR- and log P-log Teff diagrams resulting from different choices of opacity tables, and for three different metallicities. FAMIAS (Frequency Analysis and Mode Identification for AsteroSeismology) is a collection of state-of-the-art software tools for the analysis of photometric and spectroscopic time series data. It is one of the deliverables of the Work Package NA5: Asteroseismology of the European Coordination Action in Helio-and Asteroseismology (HELAS). Two main sets of tools are incorporated in FAMIAS. The first set allows to search for periodicities in the data using Fourier and non-linear least-squares fitting algorithms. The other set allows to carry out a mode identification for the detected pulsation frequencies to determine their pulsational quantum numbers, the harmonic degree, m. The types of stars to which famias is applicable are main-sequence pulsators hotter than the Sun. This includes the Gamma Dor stars, Delta Sct stars, the slowly pulsating B stars and the Beta Cep stars - basically all pulsating main-sequence stars, for which empirical mode identification is required to successfully carry out asteroseismology. This user manual describes how to use the different features of FAMIAS and provides two tutorials that demonstrate the usage of FAMIAS for spectroscopic and photometric mode identification.

The chromospheres of late-type stars. I - Eridani as a test case of multiline modelling

NASA Technical Reports Server (NTRS)

Thatcher, John D.; Robinson, Richard D.; Rees, David E.

1991-01-01

A new model of the lower chromosphere of the dwarf K2 star Epsilon Eridani is derived by matching flux profiles of the Ca IR triplet lines 8498 and 8542 A H-alpha and H-beta lines and the Na D lines (all observed simultaneously at the AAT), and the Ca II K line. The coupled non-LTE equations of statistical equilibrium and radiative transfer are solved under the constraint of hydrostatic equilibrium using the Carlsson (1986) code. Within the framework of the model, the Na D lines are an important photospheric diagnostic, and the Ca IR triplet lines can be used to locate the temperature minimum. The computed H-alpha and H-beta depths are highly sensitive constraints on the transition zone gradients and base pressures allowing us to derive a pressure at the base of the transition zone of 0.9 dyn/cm.

Beta-Decay Rates for Exotic Nuclei and R-Process Nucleosynthesis up to Th and U

NASA Astrophysics Data System (ADS)

Suzuki, Toshio; Yoshida, Takashi; Shibagaki, Shota; Kajino, Toshitaka; Otsuka, Takaharu

Beta-decay rates for exotic nuclei with N = 126 relevant to r-process nucleosynthesis are studied up to Z = 78 by shell-model calculations. The half-lives for the waiting-point nuclei obtained, which are short compared to a standard FRDM, are used to study r-process nucleosynthesis in neutrino-driven winds and magneto-hydrodynamic jets of core-collapse supernova explosions as well as in binary neutron star mergers. The element abundances are obtained up to the third peak as well as beyond the peak region up to thorium and uranium. Thorium and uranium are found to be produced more with the shorter shell-model half-lives and their abundances come closer to the observed values in core-collapse supernova explosions, while in case of binary neutron star mergers they are produced as much as the observed values rather independent of the half-lives.

The 3 micron spectrum of the classical Be star Beta Monocerotis A

NASA Technical Reports Server (NTRS)

Sellgren, K.; Smith, R. G.

1992-01-01

A 3.1-3.7-micron spectrum of the classical Be star Beta Mon A is presented at a resolution of lambda/Delta-lambda of 700-800. The spectrum shows strong hydrogen recombination lines, including Pf-delta and a series of Humphreys lines from Hu 19 to Hu 28. The relative recombination line strengths suggest that Pf-delta has a large optical depth. The Humphreys lines have relative strengths consistent with case B and may be optically thin. The line widths observed are broader than the Balmer lines and similar in width to Fe II lines, consistent with a disk model in which optically thinner lines arise primarily from a faster rotating inner disk, while optically thicker lines come mainly from a slower rotating outer disk. The apparent lack of Stark broadening of the Humphreys lines is used to place an upper limit on the circumstellar electron density of about 10 exp 12/cu cm.

VizieR Online Data Catalog: California-Kepler Survey (CKS). III. Planet radii (Fulton+, 2017)

NASA Astrophysics Data System (ADS)

Fulton, B. J.; Petigura, E. A.; Howard, A. W.; Isaacson, H.; Marcy, G. W.; Cargile, P. A.; Hebb, L.; Weiss, L. M.; Johnson, J. A.; Morton, T. D.; Sinukoff, E.; Crossfield, I. J. M.; Hirsch, L. A.

2017-11-01

We adopt the stellar sample and the measured stellar parameters from the California-Kepler Survey (CKS) program (Petigura et al. 2017, Cat. J/AJ/154/107; Paper I). The measured values of Teff, logg, and [Fe/H] are based on a detailed spectroscopic characterization of Kepler Object of Interest (KOI) host stars using observations from Keck/HIRES. In Johnson et al. 2017 (Cat J/AJ/154/108; Paper II), we associated those stellar parameters from Paper I to Dartmouth isochrones (Dotter et al. 2008ApJS..178...89D) to derive improved stellar radii and masses, allowing us to recalculate planetary radii using the light-curve parameters from Mullally et al. 2015 (Cat. J/ApJS/217/31). (1 data file).

Interleukin-1beta contributes via nitric oxide to the upregulation and functional activity of the zinc transporter Zip14 (Slc39a14) in murine hepatocytes.

PubMed

Lichten, Louis A; Liuzzi, Juan P; Cousins, Robert J

2009-04-01

Zinc metabolism during chronic disease is dysregulated by inflammatory cytokines. Experiments with IL-6 knockout mice show that LPS regulates expression of the zinc transporter, Zip14, by a mechanism that is partially independent of IL-6. The LPS-induced model of sepsis may occur by a mechanism signaled by nitric oxide (NO) as a secondary messenger. To address the hypothesis that NO can modulate Zip14 expression, we treated primary hepatocytes from wild-type mice with the NO donor S-nitroso N-acetyl penicillamine (SNAP). After treatment with SNAP, steady-state Zip14 mRNA levels displayed a maximal increase after 8 h and a concomitant increase in the transcriptional activity of the gene. Chromatin immunoprecipitation documented the kinetics of activator protein (AP)-1 and RNA polymerase II association with the Zip14 promoter after NO exposure, indicating a role of AP-1 in transcription of Zip14. We then stimulated the primary murine hepatocytes with IL-1beta, an LPS-induced proinflammatory cytokine and a potent activator of inducible NO synthase (iNOS) and NO production. In support of our hypothesis, IL-1beta treatment led to a threefold increase in Zip14 mRNA and enhanced zinc transport, as measured with a zinc fluorophore, in wild-type but not iNOS-/- hepatocytes. These data suggest that signaling pathways activated by NO are factors in the upregulation of Zip14, which in turn mediates hepatic zinc accumulation and hypozincemia during inflammation and sepsis.

Ski acts as a co-repressor with Smad2 and Smad3 to regulate the response to type beta transforming growth factor.

PubMed

Xu, W; Angelis, K; Danielpour, D; Haddad, M M; Bischof, O; Campisi, J; Stavnezer, E; Medrano, E E

2000-05-23

The c-ski protooncogene encodes a transcription factor that binds DNA only in association with other proteins. To identify co-binding proteins, we performed a yeast two-hybrid screen. The results of the screen and subsequent co-immunoprecipitation studies identified Smad2 and Smad3, two transcriptional activators that mediate the type beta transforming growth factor (TGF-beta) response, as Ski-interacting proteins. In Ski-transformed cells, all of the Ski protein was found in Smad3-containing complexes that accumulated in the nucleus in the absence of added TGF-beta. DNA binding assays showed that Ski, Smad2, Smad3, and Smad4 form a complex with the Smad/Ski binding element GTCTAGAC (SBE). Ski repressed TGF-beta-induced expression of 3TP-Lux, the natural plasminogen activator inhibitor 1 promoter and of reporter genes driven by the SBE and the related CAGA element. In addition, Ski repressed a TGF-beta-inducible promoter containing AP-1 (TRE) elements activated by a combination of Smads, Fos, and/or Jun proteins. Ski also repressed synergistic activation of promoters by combinations of Smad proteins but failed to repress in the absence of Smad4. Thus, Ski acts in opposition to TGF-beta-induced transcriptional activation by functioning as a Smad-dependent co-repressor. The biological relevance of this transcriptional repression was established by showing that overexpression of Ski abolished TGF-beta-mediated growth inhibition in a prostate-derived epithelial cell line.

Imaging Forming Planetary Systems: The HST/STIS Legacy and Prospects for Future Missions

NASA Technical Reports Server (NTRS)

Grady, Carol; Woodgate, Bruce E.; Bowers, Charles; Weinberger, Alycia; Schneider, Glenn; Oegerle, William R. (Technical Monitor)

2002-01-01

The first indication that debris and protoplanetary disks associated with other, young planetary systems were sufficiently nearby to image came with the IRAS detection of infrared excesses around $\\beta$ Pic, Vega, Fomalhaut, and $\\epsilon$ Eri. Moving beyond analysis of the infrared excess to optical and near-IR imaging requires access to high Strehl ratio and high contrast imaging techniques, with the ability to efficiently reject the residual scattered and diffracted light from the star to reveal the fainter scattered light and circumstellar emission originating from the vicinity of the star. HST/STIS imaging studies have made use of incomplete Lyot coronagraphic imaging modes to reveal the warped, inner disk of $\\beta$ Pic, provide the highest spatial resolution images of young debris disk systems such as HR 4796A, have revealed the presence of azimuthally symmetric structure in HD 141569 and HD 163296, and have demonstrated that currently active, collimated outflows survive to higher stellar masses than previously expected, and through more of the star's pre-main sequence lifetime than anticipated. The HST/STIS coronagraphic imaging legacy will be discussed, together with the implications for future NIR and optical high contrast imaging capabilities.

Anatomy of a flaring proto-planetary disk around a young intermediate-mass star.

PubMed

Lagage, Pierre-Olivier; Doucet, Coralie; Pantin, Eric; Habart, Emilie; Duchêne, Gaspard; Ménard, François; Pinte, Christophe; Charnoz, Sébastien; Pel, Jan-Willem

2006-10-27

Although planets are being discovered around stars more massive than the Sun, information about the proto-planetary disks where such planets have built up is sparse. We have imaged mid-infrared emission from polycyclic aromatic hydrocarbons at the surface of the disk surrounding the young intermediate-mass star HD 97048 and characterized the disk. The disk is in an early stage of evolution, as indicated by its large content of dust and its hydrostatic flared geometry, indicative of the presence of a large amount of gas that is well mixed with dust and gravitationally stable. The disk is a precursor of debris disks found around more-evolved A stars such as beta-Pictoris and provides the rare opportunity to witness the conditions prevailing before (or during) planet formation.

Coronal Structures in Cool Stars: XMM-NEWTON Hybrid Stars and Coronal Evolution

NASA Technical Reports Server (NTRS)

Dupree, Andrea K.; Mushotzky, Richard (Technical Monitor)

2003-01-01

This program addresses the evolution of stellar coronas by comparing a solar-like corona in the supergiant Beta Dra (G2 Ib-IIa) to the corona in the allegedly more evolved state of a hybrid star, alpha TrA (K2 II-III). Because the hybrid star has a massive wind, it appears likely that the corona will be cooler and less dense as the magnetic loop structures are no longer closed. By analogy with solar coronal holes, when the topology of the magnetic field is configured with open magnetic structures, both the coronal temperature and density are lower than in atmospheres dominated by closed loops. The hybrid stars assume a pivotal role in the definition of coronal evolution, atmospheric heating processes and mechanisms to drive winds of cool stars. We are attempting to determine if this model of coronal evolution is correct by using XMM-NEWTON RGS spectra for the 2 targets we were allocated through the Guest Observer program.

A VLA radio-continuum survey of a sample of confirmed and marginal barium stars

NASA Technical Reports Server (NTRS)

Drake, Stephen A.; Simon, Theodore; Linsky, Jeffrey L.

1987-01-01

Results are reported from a 6-cm VLA survey of five confirmed Ba II stars and eight mild Ba II stars, undertaken to search for evidence of gyrosynchrotron emission or thermal emission from the primary star's wind that is enhanced or photoionized by a white dwarf companion. Of these 13 stars, only Beta UMi was detected as a possible radio source at a flux level of 0.11 mJy (3sigma). The 6-cm radio luminosities (L6) of the other stars are as small as log L6 less than or equal to 14.0 and are an order of magnitude or more lower than the average levels found in RS CVn systems, but are consistent with the L6 upper limits previously found for stars of spectral type similar to the Ba II stars and normal elemental abundances. The upper limit to the radio luminosity for the possible mild Ba II star 56 Peg, when combined with its previously known X-ray luminosity, may provide useful constraints on the various models that have been proposed for this interesting object, once its orbital period is known.

Spectral observations of Be stars in the visible range. I - Phi Per, Psi Per, 11 Cam, and Phi And

NASA Astrophysics Data System (ADS)

Krugov, V. D.

1986-02-01

Phi Per was found to display considerable variations of emission in H-alpha and H-beta. The H-alpha and H-beta emission profiles of Psi Per appeared to vary with a period of several years. A complete disappearance of H-alpha emission was observed for 11 Cam. Finally, the H-alpha emission for Phi And did not display intensity variations during the entire period of observations in 1983.

Determining the Location of the Water Snowline in an Externally-Photoevaporated Solar Nebula

NASA Astrophysics Data System (ADS)

Kalyaan, Anusha; Desch, Steven

2016-06-01

Recent studies using the Atacama Large Millimeter Array (ALMA) have imaged the location of the CO snowline in protoplanetary disks [1][2]. Water snowlines are present closer to the star and thus harder to detect, though their location may be inferred [3][4]. In the light of future direct observations of water snowlines, it is important to consider how photoevaporation may affect the snowline's location, as half of all disks are likely to be externally photoevaporated by a nearby massive star [5]. In the solar nebula, the water snowline is argued to be present at 2.7 AU, corresponding to the water sublimation temperature (~170K). But snowlines should depend as much on radial transport of volatiles, such as the outward diffusion of water vapor and the inward drift of ices, which can both settle into a steady cyclical flow across the snowline in the first few Myr [6][7]. We argue that external processes (e.g. photoevaporation) can disturb this cycle, potentially shifting the snowline inward and dehydrating the disk.To test this hypothesis, we have first built a 1+1D disk evolution model, incorporating viscosity from the magnetorotational instability with a non-uniform α across disk radius, ionization equilibrium with dust, and external photoevaporation [8]. Our simulation results suggest that the structure of the photoevaporated disk is likely more complex than previously thought, with the following features: (i) very steep Σ profile (Σ(r)=Σ0 r-p, where slope p = 3 - 5, > pMMSN=1.5) due to the varying α profile, that is further steepened by the presence of dust and photoevaporation, and (ii) transition radius (where net disk mass flow changes from inward flow to outward) present very close to the star (~3AU). We now apply these new results and radial transport processes to study the distribution of water in the solar nebula. References: 1]Qi, C., et al. (2013), Science, 341, 360 [2] Mathews, G.S. et al. (2013), A&A, 557, A132 [3]Zhang, K., et al. (2015), ApJ, 806, L7[4] Meijerink, R., et al.(2009), ApJ, 704, 1471 [5]Lada, C.J. & Lada, E.A.(2003), ARA&A, 41, 57 [6]Cuzzi, J .N ., & Zahnle, K .J., (2004), ApJ, 614, 490 [7]Ciesla, F. J., & Cuzzi, J. N. (2006) Icarus,181,178 [8] Kalyaan, A. et al. (2015) ApJ, 815, 112

Spectroscopic study of the star Canum Venat (G0)

NASA Astrophysics Data System (ADS)

Mentese, H. H.

In this work the effective temperature and surface gravity of the star BetaCVn were determined by means of the theoretical profiles calculated by De Jager and Neven (1967-1968). The best agreement was obtained for T(eff) = 5940 K and log g = 4. The values of the excitation temperatures for Ti, Cr, Mn, and Fe were calculated and found to be very close to each other. The abundances of the elements were obtained by the growth curve method and found to be normal.

A Heuristic Model of Primordial Chemical Evolution in the Reionization Era

NASA Astrophysics Data System (ADS)

McArdle, Ryan T.; Stancil, Phillip C.

2017-06-01

We develop a model of the evolution of the chemical composition of the early Universe under the influence of Population III (Pop III) stars. Solving rate equations for primordial atomic and molecular species subject to the Cosmic Background Radiation (CBR), we predict the fractional abundances of these species as a function of redshift (z). The CBR, however, eventually becomes negligible after the first stars become active. To extend the recombination era model (Gay et al. 2011), we simulate the formation of many stars from a cloud of a given mass, constrained by the Initial Mass Function (IMF), and assign to each star a mass appropriate lifetime, effective temperature, and radius (Schaerer 2002). We randomly distribute the stars across a parcel of gas with the number being controlled by the star formation rate as a function of z (Hartwig et al. 2015). Runs of our chemistry code are then spawned for each star in parallel once a star turns on. We model the propagation of the radiation front as it expands and ionizes the surrounding region, until the star has lived its lifetime. Taking the average of the data sets produce by the collection of stars in the region, we are able to obtain a prediction of the evolution of the chemical composition of the entire modeled region from the Recombination era into the Reionization era.Gay, C., et al. 2011, ApJ, 735, 44Hartwig, T., et al. 2015, MNRAS, 447, 3892Schaerer, D. 2002, A&A, 382, 28The work of RTM was partially supported by a UGA Center for Undergraduate Research Opportunities Award.

VizieR Online Data Catalog: Rapidly pulsating sdB stars search with GALEX (Boudreaux+, 2017)

NASA Astrophysics Data System (ADS)

Boudreaux, T. M.; Barlow, B. N.; Fleming, S. W.; Soto, A. V.; Million, C.; Reichart, D. E.; Haislip, J. B.; Linder, T. R.; Moore, J. P.

2018-04-01

Here we present a search for short-period hot subdwarf B (sdB) pulsations in the archived GALEX data set using gPhoton (Million+ 2016ApJ...833..292M). An initial sample of 5613 hot subdwarfs (Geier+ 2017, J/A+A/600/A50), which represents a good approximation of all cataloged hot subdwarf stars, was down-selected based on magnitudes, coordinates, and total exposure time available in the gPhoton database, described fully in Section 2. These selection criteria yielded 1881 targets upon which we focused our investigation. Calibrated light curves with time bins of 30s were generated for each target using gPhoton. (4 data files).

Radio wavelength observations of magnetic fields on active dwarf M, RS CVn and magnetic stars

NASA Technical Reports Server (NTRS)

Lang, Kenneth R.

1986-01-01

The dwarf M stars, YZ Canis Minoris and AD Leonis, exhibit narrow-band, slowly varying (hours) microwave emission that cannot be explained by conventional thermal radiation mechanisms. The dwarf M stars, AD Leonis and Wolf 424, emit rapid spikes whose high brightness temperatures similarly require a nonthermal radiation process. They are attributed to coherent mechanisms such as an electron-cyclotron maser or coherent plasma radiation. If the electron-cyclotron maser emits at the second or third harmonic gyrofrequency, the coronal magnetic field strength equals 250 G or 167 G, and constraints on the plasma frequency imply an electron density of 6 x 10 to the 9th/cu cm. Radio spikes from AD Leonis and Wolf 424 have rise times less than or equal to 5 ms, indicating a linear size of less than or equal to 1.5 x 10 to the 8th cm, or less than 0.005 of the stellar radius. Although Ap magnetic stars have strong dipole magnetic fields, they exhibit no detectable gyroresonant radiation, suggesting that these stars do not have hot, dense coronae. The binary RS CVn star UX Arietis exhibits variable emission at 6 cm wavelength on time scales ranging from 30 s to more than one hour.

LAD Prize Talk: Lab Astro and the Origins of the Chemical Elements

NASA Astrophysics Data System (ADS)

Lawler, James E.

2017-06-01

Only a few of the lightest or primordial nuclei were made just after the Big Bang. Other light nuclei up to the Fe-group are made by fusion in stars. Heavier nuclei are made primarily via r(apid)-process and s(low)-process n(eutron)-capture events. Although the s-process n-capture is fairly well understood, the r-process n-capture events remain poorly understood. The relative role of Core Collapse SNe and n-star mergers will likely be understood in the next few decades. I will discuss recent studies of old Metal-Poor stars that are revealing some new details of nucleosynthesis. This progress is due to the availability of high resolution spectra from large ground based telescopes, access to the UV via HST, and better laboratory data. Our laboratory astrophysics program has focused primarily on the measurement of transition probabilities by combining radiative lifetimes with emission branching fractions. The use of Time Resolved Laser Induced Fluorescence (TRLIF) to measure radiative lifetimes in metallic atoms and ions provides an absolute scale for transition probabilities accurate to a few percent [e.g. 1]. The development and application of TRLIF to neutral and ionized atoms of nearly all elements is due to a simple, versatile, and reliable atom/ion beam source based on a hollow cathode discharge [2, 3]. Fourier transform spectrometers (FTSs) are essential in the measurement of emission branching fractions for atoms and ions with dense spectra such as the rare earths [e.g. 4, 5]. A 3 m focal length echelle spectrometer is important to the measurement of weak branches which might otherwise be obscured by multiplex noise in FTS data [6, 7]. References: [1] E. A. Den Hartog et al., ApJS 194: 35 (2011). [2] D. W. Duquette et al., Phys. Rev. A24, 2847 (1981). [3] S. Salih & J. E. Lawler, Phys. Rev. A29, 3753, (1983). [4] J. W. Brault, J. Opt. Soc. Am. 66, 1081 (1976). [5] J. E. Lawler et al., ApJS 182, 51 (2009). [6] M. P. Wood & J. E. Lawler, Appl. Opt. 51, 8407 (2012). [7] C. Sneden et al., ApJ 817:53 (2016).

The Beta Pictoris Phenomenon in Young Stars With Accreting Gas

NASA Technical Reports Server (NTRS)

Grady, Carol A.

1999-01-01

Program Hae2BPIC resulted in usable ISO spectra of three young, Herbig Ae stars: HR 5999 (A7e, t=0.6 Myr), SV Cep (al-2e, t=1-3 Myr), and MW Vul (Al-2e, t=1-3 Myr). While too small a sample to pursue our original goal of surveying the silicate emission in these young, protoplanetary disk systems, comparison of these data with ground-based IR spectra, and published ISO observations of other HAe stars (especially the posters at PPIV) reveals the following: The known binary stars in the sample show signatures of partially crystal line silicate features by t=0.6 Myr, at an epoch when ostensibly single Herbig Ae stars have substantially stronger silicate emission dominated by amorphous grains. The known binary stars also show deficits in the optically thick continuum flux relative to coeval single stars. Comparison of ISO spectra indicates that the flux deficit seen in WD 163296 over 10-100 microns relative to AB Aur reflects a real deficit of material interior to 300.

VizieR Online Data Catalog: Proper motions in M 11 (Su+ 1998)

NASA Astrophysics Data System (ADS)

Su, C.-G.; Zhao, J.-L.; Tian, K.-P.

1997-07-01

Relative proper motions of 872 stars in the open cluster M 11 region are reduced using 10 plate pairs taken over time baselines of 16~70 years with the double astrograph telescope of Shanghai Observatory. The scale is 30"/mm. The plates were measured with the PDS machines in the Purple Mountain Observatory in Nanjing and the Institute of Technology and Communication in Luoyang, China. The average proper motion accuracy is about 1.1mas/yr with 85% of the data better than 1mas/yr. Membership probabilities of 785 stars within 25' centred on M 11 are determined based on their proper motions. The method used is suggested by Su et al. (1995AcApS..15..217S) with some improvements of Zhao & He (1990A&A...237...54Z), in which the space distribution and magnitude dependencies for cluster stars are taken into account. The results are significantly good. The total integrated membership probabilities for all these stars is 547 and the number of stars with probabilities higher than 0.7 is 541. It can be found after the membership determination that there exists mass segregation in M 11. Some comparisons and discussion are also given. (1 data file).

VizieR Online Data Catalog: Photometric variability of BeSS-KELT stars (Labadie-Bartz+, 2017)

NASA Astrophysics Data System (ADS)

Labadie-Bartz, J.; Pepper, J.; McSwain, M. V.; Bjorkman, J. E.; Bjorkman, K. S.; Lund, M. B.; Rodriguez, J. E.; Stassun, K. G.; Stevens, D. J.; James, D. J.; Kuhn, R. B.; Siverd, R. J.; Beatty, T. G.

2018-04-01

Kilodegree Extremely Little Telescope (KELT) is a photometric survey using two small-aperture (42 mm) wide-field (26°x26°) telescopes, with a northern location at Winer Observatory in Arizona in the United States, and a southern location at the South African Astronomical Observatory near Sutherland, South Africa. The Be Star Spectra (BeSS) database is a continually updated catalog that attempts to include all known Be stars, as well as their stellar parameters. This catalog is based primarily on the catalog of classical Be stars published by Jaschek et al. (1982, Cat. III/67) but also includes more recently discovered Be stars from a variety of sources (e.g., Neiner et al. 2005ApJS..156..237N; Martayan et al. 2006A&A...445..931M). From the BeSS database, we compiled a list of all the classical Be stars with 7

Inhomogeneous galactic chemical evolution of r-process elements

NASA Astrophysics Data System (ADS)

Wehmeyer, Benjamin

2018-01-01

Stars provide a fundamental contribution to the cosmic life cycle. Gas clouds form and collapse to stars, experiencing different evolutionary stages according to their properties like mass and metal content. Small stars like our Sun end their life as planetary nebulae, while more massive stars end their evolution with violent explosions like supernovae or hypernovae, leaving behind either a neutron star or a black hole. These compact objects may also merge, leading to a new ejection of material. Today the origin of the heaviest elements is still matter of debate. The relative contributions of the proposed sources of r-process elements (e.g., Supernovae, Neutron Star Mergers) in the early galaxy as well as in the Sun is one of the main uncertainties. We use the inhomogeneous chemical evolution tool “ICE” [1, 2] to study the role of some of the main parameters of the cosmic life cycle. With ICE's high resolution (≥ 20parsec/cell) runs, we are able to get converged simulations of the inhomogeneities in the early Galactic evolution stages, and of the observed scatter of r-process elements in metal-poor stars [3].[1] B. Wehmeyer, M. Pignatari, F.-K. Thielemann, 2015 MNRAS 452, 1970–1981[2] B. Wehmeyer, M. Pignatari, F.-K. Thielemann, 2016 AIPC 1743, 040009[3] I. Roederer et al., 2010 ApJ 724:975–993

A CN Band Survey of Red Giants in the Globular Cluster M53

NASA Astrophysics Data System (ADS)

Martell, S. L.; Smith, G. H.

2004-12-01

We investigate the star-to-star variations in λ 3883 CN bandstrength among red giant stars in the low-metallicity globular cluster M53 ([Fe/H] = --2.0). Our data were taken with the Kast spectrograph on the 3-meter Shane telescope at Lick Observatory in April 2001. Star-to-star variations in CN bandstrength are common in intermediate- and high-metallicity globular clusters ([Fe/H] ≥ --1.6). Our data were obtained to test whether that variation will also be present in a low-metallicity globular cluster, or whether it will be suppressed by the overall lack of metals in the stars. Our preliminary result is that the λ 3883 CN band is weak in our program stars, which span the brightest magnitude of the red giant branch. On visual inspection, the M53 giants appear to be similar in their CN bandstrength to the four CN-weak giants in NGC 6752 whose average spectrum is plotted in Fig. 4 of Norris et al. (1981, ApJ, 244, 205). This work is planned to form part of a larger study of the metallicity dependence of CN bandstrength and carbon abundance behavior on the upper giant branch of globular clusters. This work is supported by NSF grant AST 00-98453 and by an award from the ARCS foundation, Northern California Chapter.

Formation of young massive clusters from turbulent molecular clouds

NASA Astrophysics Data System (ADS)

Fujii, Michiko; Portegies Zwart, Simon

2015-08-01

We simulate the formation and evolution of young star clusters using smoothed-particle hydrodynamics (SPH) and direct N-body methods. We start by performing SPH simulations of the giant molecular cloud with a turbulent velocity field, a mass of 10^4 to 10^6 M_sun, and a density between 17 and 1700 cm^-3. We continue the SPH simulations for a free-fall time scale, and analyze the resulting structure of the collapsed cloud. We subsequently replace a density-selected subset of SPH particles with stars. As a consequence, the local star formation efficiency exceeds 30 per cent, whereas globally only a few per cent of the gas is converted to stars. The stellar distribution is very clumpy with typically a dozen bound conglomerates that consist of 100 to 10000 stars. We continue to evolve the stars dynamically using the collisional N-body method, which accurately treats all pairwise interactions, stellar collisions and stellar evolution. We analyze the results of the N-body simulations at 2 Myr and 10 Myr. From dense massive molecular clouds, massive clusters grow via hierarchical merging of smaller clusters. The shape of the cluster mass function that originates from an individual molecular cloud is consistent with a Schechter function with a power-law slope of beta = -1.73 at 2 Myr and beta = -1.67 at 10 Myr, which fits to observed cluster mass function of the Carina region. The superposition of mass functions have a power-law slope of < -2, which fits the observed mass function of star clusters in the Milky Way, M31 and M83. We further find that the mass of the most massive cluster formed in a single molecular cloud with a mass of M_g scales with 6.1 M_g^0.51 which also agrees with recent observation in M51. The molecular clouds which can form massive clusters are much denser than those typical in the Milky Way. The velocity dispersion of such molecular clouds reaches 20 km/s and it is consistent with the relative velocity of the molecular clouds observed near NGC 3603 and Westerlund 2, for which a triggered star formation by cloud-cloud collisions is suggested.

SIMULATIONS OF BOOSTER INJECTION EFFICIENCY FOR THE APS-UPGRADE

DOE Office of Scientific and Technical Information (OSTI.GOV)

Calvey, J.; Borland, M.; Harkay, K.

2017-06-25

The APS-Upgrade will require the injector chain to provide high single bunch charge for swap-out injection. One possible limiting factor to achieving this is an observed reduction of injection efficiency into the booster synchrotron at high charge. We have simulated booster injection using the particle tracking code elegant, including a model for the booster impedance and beam loading in the RF cavities. The simulations point to two possible causes for reduced efficiency: energy oscillations leading to losses at high dispersion locations, and a vertical beam size blowup caused by ions in the Particle Accumulator Ring. We also show that themore » efficiency is much higher in an alternate booster lattice with smaller vertical beta function and zero dispersion in the straight sections.« less

Galactic evolution of oxygen. OH lines in 3D hydrodynamical model atmospheres

NASA Astrophysics Data System (ADS)

González Hernández, J. I.; Bonifacio, P.; Ludwig, H.-G.; Caffau, E.; Behara, N. T.; Freytag, B.

2010-09-01

Context. Oxygen is the third most common element in the Universe. The measurement of oxygen lines in metal-poor unevolved stars, in particular near-UV OH lines, can provide invaluable information about the properties of the Early Galaxy. Aims: Near-UV OH lines constitute an important tool to derive oxygen abundances in metal-poor dwarf stars. Therefore, it is important to correctly model the line formation of OH lines, especially in metal-poor stars, where 3D hydrodynamical models commonly predict cooler temperatures than plane-parallel hydrostatic models in the upper photosphere. Methods: We have made use of a grid of 52 3D hydrodynamical model atmospheres for dwarf stars computed with the code CO5BOLD, extracted from the more extended CIFIST grid. The 52 models cover the effective temperature range 5000-6500 K, the surface gravity range 3.5-4.5 and the metallicity range -3 < [Fe/H] < 0. Results: We determine 3D-LTE abundance corrections in all 52 3D models for several OH lines and ion{Fe}{i} lines of different excitation potentials. These 3D-LTE corrections are generally negative and reach values of roughly -1 dex (for the OH 3167 with excitation potential of approximately 1 eV) for the higher temperatures and surface gravities. Conclusions: We apply these 3D-LTE corrections to the individual O abundances derived from OH lines of a sample the metal-poor dwarf stars reported in Israelian et al. (1998, ApJ, 507, 805), Israelian et al. (2001, ApJ, 551, 833) and Boesgaard et al. (1999, AJ, 117, 492) by interpolating the stellar parameters of the dwarfs in the grid of 3D-LTE corrections. The new 3D-LTE [O/Fe] ratio still keeps a similar trend as the 1D-LTE, i.e., increasing towards lower [Fe/H] values. We applied 1D-NLTE corrections to 3D ion{Fe}{i} abundances and still see an increasing [O/Fe] ratio towards lower metallicites. However, the Galactic [O/Fe] ratio must be revisited once 3D-NLTE corrections become available for OH and Fe lines for a grid of 3D hydrodynamical model atmospheres.

Insights into molecular architecture of terpenes using small angle neutron scattering

NASA Astrophysics Data System (ADS)

Rai, Durgesh K.; Annamraju, Aparna; Pingali, Sai Venkatesh; O'Neill, Hugh M.; Mewalal, Ritesh; Gunter, Lee E.; Tuskan, Gerald A.

Understanding macromolecular architectures is vital to engineering prospective terpene candidates for advanced biofuels. Eucalyptus plants store terpenes in specialized cavity-like structures in the leaves called oil glands, which comprises of volatile (VTs) and non-volatile (NVTs) terpenes. Using small-angle neutron scattering, we have investigated the structure and phase behavior of the supramolecular assembly formed by Geranyl beta-D-glucoside (GDG), a NVT and compare the results with that of beta-octyl glucoside (BOG). The formation of micellar structures was observed in the concentration range of 0.5-5 v/v% in water using small angle neutron scattering (SANS) where Schultz sphere model was used in quantifying structural parameters of micelles. SANS studies determine that GDG and BOG behave like amphiphiles forming micellar structures in aqueous solution. The micelles swell upon addition of alpha-Pinene (AP) indicating partition to the core region of the micelles. The general behavior of the micellar growth after partitioning of AP to form thermodynamically stable sizes varies with the NVT concentration. Our studies reveal that the presence of steric hindrance in the GDG via the unsaturated bonds could help stabilize VTs inside the oil glands. LDRD project LOIS ID 7428, SNS, CSMB, HFIR, ORNL, DOE Office of Science User Facilities.

Very Low Mass Stars with Extremely Low Metallicity in the Milky Way's Halo

NASA Astrophysics Data System (ADS)

Aoki, Wako; Beers, Timothy C.; Takuma, Suda; Honda, Satoshi; Lee, Young Sun

2015-08-01

Large surveys and follow-up spectroscopic studies in the past few decades have been providing chemical abundance data for a growing number of very metal-poor ([Fe/H] <-2) stars. Most of them are red giants or main-sequence turn-off stars having masses near 0.8 solar masses. Lower mass stars with extremely low metallicity ([Fe/H] <-3) have yet to be well explored. Our high-resolution spectroscopic study for very metal-poor stars found with SDSS has identified four cool main-sequence stars with [Fe/H] <-2.5 among 137 objects (Aoki et al. 2013, AJ, 145, 13). The effective temperatures of these stars are 4500--5000 K, corresponding to a mass of around 0.5 solar masses. Our standard analysis of the high-resolution spectra based on 1D-LTE model atmospheres have obtained self-consistent chemical abundances for these objects, assuming small values of micro-turbulent velocities compared with giants and turn-off stars. The low temperature of the atmospheres of these objects enables us to measure their detailed chemical abundances. Interestingly, two of the four stars have extreme chemical abundance patterns: one has the largest excesses of heavy neutron-capture elements associated with the r-process abundance pattern known to date (Aoki et al. 2010, ApJL 723, L201), and the other exhibits low abundances of the alpha-elements and odd-Z elements, suggested to be the signatures of the yields of very massive stars ( >100 solar masses; Aoki et al. 2014, Science 345, 912). Although the sample size is still small, these results indicate the potential of very low-mass stars as probes to study the early stages of the Milky Way's halo formation.

Niobium in R And (S6, 6e) and HR 1105 (S5, 3). [S star abundance

NASA Technical Reports Server (NTRS)

Davis, D. N.

1985-01-01

Lines of the first multiplet of niobium are strong in R And and HR 1105. These lines are also present in other S stars: HR 8714, R Cam, V Cnc, R CMi, and T Sgr. They are also visible in the M stars, Beta-Peg and Mu-UMa. An approximation to the abundance ratio, Nb/Fe, has been deduced from pairs of lines having nearly equal intensity. In R And, the ratio is about 200 times the solar value. It is hoped that good plates will soon be obtained for the near infrared region, so that the significant Nb/Rb abundance ratio may be determined.

Dust discs around low-mass main-sequence stars

NASA Technical Reports Server (NTRS)

Wolstencroft, R. D.; Walker, Helen J.

1988-01-01

The current understanding of the formation of circumstellar disks as a natural accompaniment to the process of low-mass star formation is examined. Models of the thermal emission from the dust disks around the prototype stars Alpha Lyr, Alpha PsA, Beta Pic, and Epsilon Eri are discussed, which indicate that the central regions of three of these disks are almost devoid of dust within radii ranging between 17 and 26 AU, with the temperature of the hottest zone lying between about 115 and 210 K. One possible explanation of the dust-free zones is the presence of a planet at the inner boundary of each cloud which sweeps up grains crossing its orbit.

Hot Jupiters Aren't As Lonely As We Thought

NASA Astrophysics Data System (ADS)

Kohler, Susanna

2016-01-01

The Friends of Hot Jupiters (FOHJ) project is a systematic search for planetary- and stellar-mass companions in systems that have known hot Jupiters short-period, gas-giant planets. This survey has discovered that many more hot Jupiters may have companions than originally believed.Missing FriendsFOHJ was begun with the goal of better understanding the systems that host hot Jupiters, in order to settle several longstanding issues.The first problem was one of observational statistics. We know that roughly half of the Sun-like stars nearby are in binary systems, yet weve only discovered a handful of hot Jupiters around binaries. Are binary systems less likely to host hot Jupiters? Or have we just missed the binary companions in the hot-Jupiter-hosting systems weve seen so far?An additional issue relates to formation mechanisms. Hot Jupiters probably migrated inward from where they formed out beyond the ice lines in protoplanetary disks but how?This median-stacked image, obtained with adaptive optics, shows one of the newly-discovered stellar companions to a star hosting a hot Jupiter. The projected separation is ~180 AU. [Ngo et al. 2015]Observations reveal two populations of hot Jupiters: those with circular orbits aligned with their hosts spins, and those with eccentric, misaligned orbits. The former population support a migration model dominated by local planet-disk interactions, whereas the latter population suggest the hot Jupiters migrated through dynamical interactions with distant companions. A careful determination of the companion rate in hot-Jupiter-hosting systems could help establish the ability of these two models to explain the observed populations.Search for CompanionsThe FOHJ project began in 2012 and studied 51 systems hosting known, transiting hot Jupiters with roughly half on circular, aligned orbits and half on eccentric, misaligned orbits. The survey consisted of three different, complementary components:Study 1Lead author: Heather Knutson (Caltech)Technique: Long-term radial velocity monitoringSearching for: Planetary companions at 120 AU from the starStudy 2Lead author: Henry Ngo (Caltech)Technique: Adaptive-optics imagingSearching for: Stellar companions at 502000 AU from the starStudy 3Lead author: Danielle Piskorz (Caltech)Technique: SpectroscopySearching for: Any additional stellar companions at 125 AU from the starThe companion fraction found within Study 2, the adaptive-optics imagine search. The three curves show the total, the systems with hot Jupiters on aligned and circular orbits, and those with hot Jupiters on misaligned and eccentric orbits. [Ngo et al. 2015]Migration ImplicationsUsing these three different techniques, the team found a significant number of both planetary and stellar companions that had not been previously detected. After correcting their results for completeness, they found a multiple-star rate of ~50% for these systems, resolving the problem of the missing companions. So really, we just werent looking hard enough for the companions previously.Intriguingly, the binary companion rate found for these hot Jupiter systems is higher than the average rate for the field stars (which is below 25% for the semimajor-axis range the FOHJ studies are sensitive to). This suggests that companion stars may indeed play a role in hot Jupiter formation and migration.That said, none of the three studies found a significant difference in the binary fraction for aligned versus misaligned hot Jupiters which means that the answer is not as simple as thought, with companion stars causing the misaligned planets. Thus, while hot Jupiters friends may play a role in their formation and migration, we still have work to do in understanding what that role is.CitationDanielle Piskorz et al 2015 ApJ 814 148. doi:10.1088/0004-637X/814/2/148Henry Ngo et al 2015 ApJ 800 138. doi:10.1088/0004-637X/800/2/138Heather A. Knutson et al 2014 ApJ 785 126. doi:10.1088/0004-637X/785/2/126

The near-contact binary star RZ Dra revisited

NASA Astrophysics Data System (ADS)

Erdem, A.; Zola, S.; Winiarski, M.

2011-01-01

This paper presents the absolute parameters of RZ Dra. New CCD observations were made at the Mt. Suhora Observatory in 2007. Two photometric data sets (1990 BV and 2007 BVRI) were analysed using modern light-curve synthesis methods. Large asymmetries in the light curves may be explained in terms of a dark starspot on the primary component, an A6 type star. Due to this magnetic activity, the primary component would appear to belong to the class of Ap-stars and would show small amplitude with δ Scuti-type pulsations. With this in mind, a time-series analysis of the residual light curves was made. However, we found no evidence of pulsation behaviour in RZ Dra. Combining the solutions of our light curves and Rucinski et al. (2000)'s radial velocity curves, the following absolute parameters of the components were determined: M1 = 1.63 ± 0.03 M ⊙, M2 = 0.70 ± 0.02 M ⊙, R1 = 1.65 ± 0.02R ⊙, R2 = 1.15 ± 0.02 R ⊙, L1 = 9.72 ± 0.30 L ⊙ and L2 = 0.74 ± 0.10 L ⊙. The distance to RZ Dra was calculated as 400 ± 25 pc, taking into account interstellar extinction. The orbital period of the system was studied using updated O- C information. It was found that the orbital period varied in its long-period sinusoidal form, superimposed on a downward parabola. The parabolic term shows a secular period decrease at a slow rate of 0.06 ± 0.02 s per century and is explained by the mass loss via magnetized wind of the Ap-star primary. The tilted sinusoidal form of the period variation may be considered as an apparent change and may be interpreted in terms of the light-time effect due to the presence of a third body.

The recondite intricacies of Zeeman Doppler mapping

NASA Astrophysics Data System (ADS)

Stift, M. J.; Leone, F.; Cowley, C. R.

2012-02-01

We present a detailed analysis of the reliability of abundance and magnetic maps of Ap stars obtained by Zeeman Doppler mapping (ZDM). It is shown how they can be adversely affected by the assumption of a mean stellar atmosphere instead of appropriate 'local' atmospheres corresponding to the actual abundances in a given region. The essence of the difficulties was already shown by Chandrasekhar's picket-fence model. The results obtained with a suite of Stokes codes written in the ADA programming language and based on modern line-blanketed atmospheres are described in detail. We demonstrate that the high metallicity values claimed to have been found in chemically inhomogeneous (horizontally and vertically) Ap star atmospheres would lead to local temperature structures, continuum and line intensities, and line shapes that differ significantly from those predicted by a mean stellar atmosphere. Unfortunately, past applications of ZDM have consistently overlooked the intricate aspects of metallicity with their all-pervading effects. The erroneous assumption of a mean atmosphere for a spotted star can lead to phase-dependent errors of uncomfortably large proportions at varying wavelengths both in the Stokes I and V profiles, making precise mapping of abundances and magnetic field vectors largely impossible. The relation between core and wings of the Hβ line changes, too, with possible repercussions on the determination of gravity and effective temperature. Finally, a ZDM analysis of the synthetic Stokes spectra of a spotted star reveals the disturbing differences between the respective abundance maps based on a mean atmosphere on the one hand, and on appropriate 'local' atmospheres on the other. We then discuss what this all means for published ZDM results. Our discussion makes it clear that realistic local atmospheres must be used, especially if credible small-scale structures are to be obtained. Recondite: dealing with very profound, difficult or abstruse subject matter; requiring special knowledge to be understood ().

Evidence for the pulsational origin of the Long Secondary Periods: The red supergiant star V424 Lac (HD 216946)

NASA Astrophysics Data System (ADS)

Messina, Sergio

2007-10-01

The results of a long-term UBV photometric monitoring of the red supergiant (RSG) star V424 Lac are presented. V424 Lac shows multiperiodic brightness variations which can be attributed to pulsational oscillations. A much longer period ( P = 1601 d), that allows us to classify this star as a long secondary period variable star (LSPV) has been also detected. The B - V and U - B color variations related to the long secondary period (LSP) are similar to those related to the shorter periods, supporting the pulsational nature of LSP. The long period brightness variation of V424 Lac is accompanied by a near-UV (NUV) excess, which was spectroscopically detected in a previous study [Massey, P., Plez, B., Levesque, E.M., et al., 2005. ApJ 634, 1286] and which is now found to be variable from photometry. On the basis of the results found for V424 Lac, the NUV excess recently found in a number of RSGs may be due not solely to circumstellar dust but may also have a contribution from a still undetected LSP variability.

The ultraviolet flux distribution of Alpha-2 Canum Venaticorum

NASA Technical Reports Server (NTRS)

Leckrone, D. S.; Snijders, M. A. J.

1979-01-01

Intermediate- and narrow-band UV spectrophotometry from Copernicus, OAO 2, the S2-68 experiment on TD 1, and a sounding-rocket experiment are combined with ground-based observations to define the absolute flux distribution of the bright magnetic Ap star Alpha-2 CVn over the wavelength range from 1030 to 7580 A. Two flux distributions are presented which coincide more or less with the rare-earth maximum and minimum in the star's cycle. The results are compared with those for two normal stars, the UV variability of Alpha-2 CVn is characterized as a function of wavelength, and non-LTE effects on the UV continua of C I and Si I are analyzed. Some physical properties of Alpha-2 CVn are estimated, and the evolutionary age of the star is estimated to be between 220 million and 300 million years. It is concluded that Alpha-2 CVn is old enough to have been magnetically braked to its current rotational velocity by either the centrifugal-wind or the accretion mechanism and to have developed its chemical peculiarities by either mechanism.

Featured Image: Orbiting Stars Share an Envelope

NASA Astrophysics Data System (ADS)

Kohler, Susanna

2016-03-01

This beautiful series of snapshots from a simulation (click for a better look!) shows what happens when two stars in a binary system become enclosed in the same stellar envelope. In this binary system, one of the stars has exhausted its hydrogen fuel and become a red giant, complete with an expanding stellar envelope composed of hydrogen and helium. Eventually, the envelope expands so much that the companion star falls into it, where it releases gravitational potential energy into the common envelope. A team led by Sebastian Ohlmann (Heidelberg Institute for Theoretical Studies and University of Wrzburg) recently performed hydrodynamic simulations of this process. Ohlmann and collaborators discovered that the energy release eventually triggers large-scale flow instabilities, which leads to turbulence within the envelope. This process has important consequences for how these systems next evolve (for instance, determining whether or not a supernova occurs!). You can check out the authors video of their simulated stellar inspiral below, or see their paper for more images and results from their study.CitationSebastian T. Ohlmann et al 2016 ApJ 816 L9. doi:10.3847/2041-8205/816/1/L9

Magnetic Doppler imaging of α2 Canum Venaticorum in all four Stokes parameters. Unveiling the hidden complexity of stellar magnetic fields

NASA Astrophysics Data System (ADS)

Kochukhov, O.; Wade, G. A.

2010-04-01

Context. Strong organized magnetic fields have been studied in the upper main sequence chemically peculiar stars for more than half a century. However, only recently have observational methods and numerical techniques become sufficiently mature to allow us to record and interpret high-resolution four Stokes parameter spectra, leading to the first assumption-free magnetic field models of these stars. Aims: Here we present a detailed magnetic Doppler imaging analysis of the spectropolarimetric observations of the prototypical magnetic Ap star α2 CVn. This is the second star for which the magnetic field topology and horizontal chemical abundance inhomogeneities have been inferred directly from phase-resolved observations of line profiles in all four Stokes parameters, free from the traditional assumption of a low-order multipolar field geometry. Methods: We interpret the rotational modulation of the circular and linear polarization profiles of the strong Fe II and Cr II lines in the spectra of α2 CVn recorded with the MuSiCoS spectropolarimeter. The surface abundance distributions of the two chemical elements and a full vector map of the stellar magnetic field are reconstructed in a self-consistent inversion using our state-of-the-art magnetic Doppler imaging code Invers10. Results: We succeeded in reproducing most of the details of the available spectropolarimetric observations of α2 CVn with a magnetic map which combines a global dipolar-like field topology with localized spots of higher field intensity. We demonstrate that these small-scale magnetic structures are inevitably required to fit the linear polarization spectra; however, their presence cannot be inferred from the Stokes I and V observations alone. We also found high-contrast surface distributions of Fe and Cr, with both elements showing abundance minima in the region of weaker and topologically simpler magnetic field. Conclusions: Our magnetic Doppler imaging analysis of α2 CVn and previous results for 53 Cam support the view that the upper main sequence stars can harbour fairly complex surface magnetic fields which resemble oblique dipoles only at the largest spatial scales. Spectra in all four Stokes parameters are absolutely essential to unveil and meaningfully characterize this field complexity in Ap stars. We therefore suggest that understanding magnetism of stars in other parts of the H-R diagram is similarly incomplete without investigation of their linear polarization spectra. Based on data obtained using the Télescope Bernard Lyot at Observatoire du Pic du Midi.

Amyloid-beta peptide oligomers disrupt axonal transport through an NMDA receptor-dependent mechanism that is mediated by glycogen synthase kinase 3beta in primary cultured hippocampal neurons.

PubMed

Decker, Helena; Lo, Karen Y; Unger, Sandra M; Ferreira, Sergio T; Silverman, Michael A

2010-07-07

Disruption of axonal transport is a hallmark of several neurodegenerative diseases, including Alzheimer's disease (AD). Even though defective transport is considered an early pathologic event, the mechanisms by which neurodegenerative insults impact transport are poorly understood. We show that soluble oligomers of the amyloid-beta peptide (AbetaOs), increasingly recognized as the proximal neurotoxins in AD pathology, induce disruption of organelle transport in primary hippocampal neurons in culture. Live imaging of fluorescent protein-tagged organelles revealed a marked decrease in axonal trafficking of dense-core vesicles and mitochondria in the presence of 0.5 microm AbetaOs. NMDA receptor (NMDAR) antagonists, including d-AP5, MK-801, and memantine, prevented the disruption of trafficking, thereby identifying signals for AbetaO action at the cell membrane. Significantly, both pharmacological inhibition of glycogen synthase kinase-3beta (GSK-3beta) and transfection of neurons with a kinase-dead form of GSK-3beta prevented the transport defect. Finally, we demonstrate by biochemical and immunocytochemical means that AbetaOs do not affect microtubule stability, indicating that disruption of transport involves a more subtle mechanism than microtubule destabilization, likely the dysregulation of intracellular signaling cascades. Results demonstrate that AbetaOs negatively impact axonal transport by a mechanism that is initiated by NMDARs and mediated by GSK-3beta and establish a new connection between toxic Abeta oligomers and AD pathology.

A-type Stellar Abundances: A Corollary to Herschel Observations of Debris Disks

NASA Astrophysics Data System (ADS)

Draper, Zachary H.; Matthews, Brenda; Venn, Kim; Lambert, David; Kennedy, Grant; Sitnova, Tatyana

2018-04-01

In order to assess the relationship between metallicity and exoplanetary systems, we compare the abundances of AF-type main-sequence stars with debris disk properties assessed using Herschel observations of an unbiased survey of nearby stars. Hot stars are not as commonly observed, given their unique constraints in data reduction, lack of metal lines, and “astrophysical noise” from rotation speed. Here, we address that deficiency using new and archival spectra of 83 AF-type stars. We measure the abundances of a few species in addition to Fe in order to classify the stars with Ap/Am or Lambda Boo signatures. Lambda Boo stars have a chemical signature of solar-abundant volatile species and sub-solar refractory abundances that is hypothesized to be altered by the pollution of volatiles. Overall, we see no correlation between debris disks and metallicity, primarily because the sample size is cut significantly when using only reliable fits to the spectroscopic data. The abundance measured from the Mg II 4481 blend is a useful diagnostic because it can be reliably measured at large v·sin(i) and is found to be lower around stars with bright debris disks. We find that Lambda Boo stars have brighter debris disks compared to a bias-free sample of AF stars. The trend with disk brightness and Mg abundances suggests pollution effects can be significant and used as a marker for the stability of planetary systems. We explore trends with other species, such as with the C/O ratios, but are significantly limited by the low number of reliable detections.

Molecular mechanism to recruit galectin-3 into multivesicular bodies for polarized exosomal secretion.

PubMed

Bänfer, Sebastian; Schneider, Dominik; Dewes, Jenny; Strauss, Maximilian T; Freibert, Sven-A; Heimerl, Thomas; Maier, Uwe G; Elsässer, Hans-Peter; Jungmann, Ralf; Jacob, Ralf

2018-05-08

The beta-galactoside binding lectin galectin-3 (Gal3) is found intracellularly and in the extracellular space. Secretion of this lectin is mediated independently of the secretory pathway by a not yet defined nonclassical mechanism. Here, we found Gal3 in the lumen of exosomes. Superresolution and electron microscopy studies visualized Gal3 recruitment and sorting into intraluminal vesicles. Exosomal Gal3 release depends on the endosomal sorting complex required for transport I (ESCRT-I) component Tsg101 and functional Vps4a. Either Tsg101 knockdown or expression of dominant-negative Vps4a E228Q causes an intracellular Gal3 accumulation at multivesicular body formation sites. In addition, we identified a highly conserved tetrapeptide P(S/T)AP motif in the amino terminus of Gal3 that mediates a direct interaction with Tsg101. Mutation of the P(S/T)AP motif results in a loss of interaction and a dramatic decrease in exosomal Gal3 secretion. We conclude that Gal3 is a member of endogenous non-ESCRT proteins which are P(S/T)AP tagged for exosomal release.

VizieR Online Data Catalog: The Cannon: a new approach to determine masses (Ness+, 2016)

NASA Astrophysics Data System (ADS)

Ness, M.; Hogg, D. W.; Rix, H.-W.; Martig, M.; Pinsonneault, M. H.; Ho, A. Y. Q.

2016-08-01

We make use of The Cannon (Ness et al. 2015, J/ApJ/808/16), which is a data-driven method for determining stellar parameters and abundances (see section 2.1 for further explanations). APOGEE is a Sloan Digital Sky Survey (SDSS) (Eisenstein et al. 2011AJ....142...72E) infrared survey of the Milky Way disk, bulge, and halo and has provided H-band spectra (1500-1700nm) of about 150000 stars in the public data release DR12. The three labels of Teff, logg, and [Fe/H] delivered with The Cannon were demonstrated in Ness et al. (2015, J/ApJ/808/16). In this work we train on and then determine two additional labels: [α/Fe] and mass. (1 data file).

VizieR Online Data Catalog: Milky Way L/T/M-dwarfs identified in BoRG survey (Holwerda+, 2014)

NASA Astrophysics Data System (ADS)

Holwerda, B. W.; Trenti, M.; Clarkson, W.; Sahu, K.; Bradley, L.; Stiavelli, M.; Pirzkal, N.; de Marchi, G.; Andersen, M.; Bouwens, R.; Ryan, R.

2017-07-01

Our principal data set is the WFC3 data from the BoRG (HST GO/PAR-11700; Trenti et al. 2011ApJ...727L..39T; Bradley et al. 2012ApJ...760..108B) survey to identify Milky Way dwarf stars from their morphology and color. The BoRG observations are undithered HST/WFC3 conducted in pure-parallel with the telescope pointing to a primary spectroscopic target with the Cosmic Origin Spectrograph (COS; typically a high-z QSO at high Galactic latitude). The limitations for such observations are primarily that no dithering strategy can be used (final images are at WFC3 native pixel scale) and total exposure times are dictated by the primary program. (5 data files).

A Combined Very Large Telescope and Gemini Study of the Atmosphere of the Directly Imaged Planet, Beta Pictoris b

NASA Technical Reports Server (NTRS)

Currie, Thayne; Burrows, Adam; Madhusudhan, Nikku; Fukagawa, Misato; Girard, Julien H.; Dawson, Rebekah; Murray-Clay, Ruth; Kenyon, Scott; Kuchner, Marc J.; Matsumura, Soko;

Effects and underlying mechanisms of curcumin on the proliferation of vascular smooth muscle cells induced by Chol:M{beta}CD

DOE Office of Scientific and Technical Information (OSTI.GOV)

Qin Li; Division of Pharmacoproteomics, Institute of Pharmacy and Pharmacology, University of South China, Hengyang 421001; Yang Yunbo

Proliferation of vascular smooth muscle cells (VSMCs) contributes to the development of various cardiovascular diseases. Curcumin, extracted from Curcumae longae, has been shown a variety of beneficial effects on human health, including anti-atherosclerosis by mechanisms poorly understood. In the present study, we attempted to investigate whether curcumin has any effect on VSMCs proliferation and the potential mechanisms involved. Our data showed curcumin concentration-dependently abrogated the proliferation of primary rat VSMCs induced by Chol:M{beta}CD. To explore the underlying cellular and molecular mechanisms, we found that curcumin was capable of restoring caveolin-1 expression which was reduced by Chol:M{beta}CD treatment. Moreover, curcumin abrogatedmore » the increment of phospho-ERK1/2 and nuclear accumulation of ERK1/2 in primary rat VSMCs induced by Chol:M{beta}CD, which led to a suppression of AP-1 promoter activity stimulated by Chol:M{beta}CD. In addition, curcumin was able to reverse cell cycle progression induced by Chol:M{beta}CD, which was further supported by its down-regulation of cyclinD1 and E2F promoter activities in the presence of Chol:M{beta}CD. Taking together, our data suggest curcumin inhibits Chol:M{beta}CD-induced VSMCs proliferation via restoring caveolin-1 expression that leads to the suppression of over-activated ERK signaling and causes cell cycle arrest at G1/S phase. These novel findings support the beneficial potential of curcumin in cardiovascular disease.« less

Astrophysics in 2004

NASA Astrophysics Data System (ADS)

Trimble, Virginia; Aschwanden, Markus

2005-04-01

In this 14th edition of ApXX,1 we bring you the Sun (§ 2) and Stars (§ 4), the Moon and Planets (§ 3), a truly binary pulsar (§ 5), a kinematic apology (§ 6), the whole universe (§§ 7 and 8), reconsideration of old settled (§ 9) and unsettled (§ 10) issues, and some things that happen only on Earth, some indeed only in these reviews (§§ 10 and 11).

BVRI photometry of ASASSN-15qi using the Tautenburg Schmidt telescope

NASA Astrophysics Data System (ADS)

Stecklum, Bringfried; Eisloeffel, Jochen; Scholz, Alexander

2015-10-01

We report on photometric observations of the optical transient ASASSN-15qi performed at the Th & uuml;ringer Landessternwarte Tautenburg. The brightening of this source was discovered by the All-Sky Automated Survey for Supernovae (ASAS-SN, Shappee et al. 2014, ApJ, 788, 48). The object is located west of the HII region SH2-148 and a likely member of the star forming region.

Sourcing and Global Distribution of Medical Supplies

DTIC Science & Technology

2014-01-01

dots in this figure represent OCONUS MTFs and the yellow star icons indicate locations of the OCONUS theater lead agents for medical materiel (TLAMMs... Symbol Definition AFMOA Air Force Medical Operations Agency AMC Air Mobility Command APS Army prepositioned stock Cat A Category A CJCS chairman of...provide medical materiel to military units. DLA has enacted PV and other contracts to support all military units that make it possible for units around

A Survey of Stellar Families Multiplicity of Solar-Type Stars

DTIC Science & Technology

2010-09-01

Henry, S. M. 2000, AJ, 120, 1006 Gatewood, G., Han, I., & Black, D. C. 2001, ApJ, 548, L61 Ghez, A. M., McCarthy, D. W., Patience, J. L., & Beck , T...Gaume, R., & Wycoff, G. L. 2004a, BAAS , 36, 1418 Zacharias, N., Urban, S. E., Zacharias, M. I., Wycoff, G. L., Hall, D. M., Monet, D. G., & Rafferty, T. J. 2004b, AJ, 127, 3043

VizieR Online Data Catalog: Statistical test on binary stars non-coevality (Valle+, 2016)

NASA Astrophysics Data System (ADS)

Valle, G.; Dell'Omodarme, M.; Valle, G.; Prada Moroni, P. G.; Degl'Innocenti, S.

2016-01-01

The table contains the W0.95 critical values, for the 1087 binary systems considered in the paper. Tha table also lists the parameters of the beta distributions approximating the empirical W distributions. (1 data file).

VizieR Online Data Catalog: Extinction law in the Cep OB3b young cluster (Allen+, 2014)

NASA Astrophysics Data System (ADS)

Allen, T. S.; Prchlik, J. J.; Megeath, S. T.; Gutermuth, R. A.; Pipher, J. L.; Naylor, T.; Jeffries, R. D.

2017-06-01

We use Johnson V and Cousins Rc (hereafter called VR) band phot from the Isaac Newton Telescope (INT), compiled in the catalog of Littlefair et al. (2010, J/MNRAS/403/545). The R-band photometry was obtained using the Sloan r filter. It was calibrated against photometric standard stars measured in the Cousins Rc filter with an arbitrary zero point. Moderate resolution ((λ/Δλ)~1000-2000, FWHM resolution of about 6 Å) optical spectra (covering 4000-9000 Å) were obtained for ~1700 sources toward Cep OB3b using the multi-fiber spectrograph Hectospec on the MMT telescope. About 600 sources were selected for observation because they were determined to be possible cluster members (Allen et al. 2012, J/ApJ/750/125), based on indicators of youth, such as IR emission due to circumstellar dusty material and heightened X-ray activity. We use an extinction map from Allen et al. (2012, J/ApJ/750/125) to initially estimate the extinction toward each source. This map is derived using the 2MASS Point Source Catalog (Skrutskie et al. 2006AJ....131.1163S, Cat. VII/233) H and Ks band photometry of background stars. (1 data file).

Beta Pic observations requested for BRITE-Constellation

NASA Astrophysics Data System (ADS)

Waagen, Elizabeth O.

2017-01-01

The AAVSO is part of the BRITE-Constellation Ground Based Observations Team (GBOT), supporting cutting-edge science from the BRITE-Constellation satellites and coordinating with BRITE-Constellation scientist Dr. Konstanze Zwintz (Universitaet Innsbruck) and her team. The delta Scuti star beta Pic (NSV 16683) (3.80-3.86V) is one of the BRITE stars being focused on during this season. Bet Pic is particularly interesting now because a transit of the star's planet's Hill sphere (the region around a planet in which it dominates the attraction of satellites) is predicted to occur during 2017-2018. Ongoing observations beginning now are valuable to establish a baseline prior to the transit. The AAVSO's webpage on the BRITE target stars was updated in November with information on bet Pic from Dr. Zwintz. AAVSO observers with appropriate equipment and located at a southern enough latitude are encouraged to observe bet Pic. Its brightness makes bet Pic well suited to PEP and DSLR photometry; CCD photometry is also possible. However, great care must be taken by all observers, especially those using CCD, to avoid saturation. As the amplitude of this star is very small, visual observations are very difficult, but they are welcome. Multicolor (BVR) photometry better than 0.01 magnitude and time-series observations with a cadence of a few minutes (less than 10 minutes) are requested beginning now and continuing at least through 2017 and likely through 2018. The precision and cadence required are essential in order for the data to be most useful for studying the transit. Spectroscopists wishing to participate should submit their spectra directly to Dr. Konstanze Zwintz (konstanze.zwintz@uibk.ac.at). Finder charts with sequence may be created using the AAVSO Variable Star Plotter (https://www.aavso.org/vsp). Observations should be submitted to the AAVSO International Database. See full Alert Notice for more details.

Bone sialoprotein stimulates focal adhesion-related signaling pathways: role in migration and survival of breast and prostate cancer cells.

PubMed

Gordon, Jonathan A R; Sodek, Jaro; Hunter, Graeme K; Goldberg, Harvey A

2009-08-15

Bone sialoprotein (BSP) is a secreted glycoprotein found in mineralized tissues however, BSP is aberrantly expressed in a variety of osteotropic tumors. Elevated BSP expression in breast and prostate primary carcinomas is directly correlated with increased bone metastases and tumor progression. In this study, the intracellular signaling pathways responsible for BSP-induced migration and tumor survival were examined in breast and prostate cancer cells (MDA-MB-231, Hs578T and PC3). Additionally, the effects of exogenous TGF-beta1 and EGF, cytokines associated with tumor metastasis and present in high-levels in the bone microenvironment, were examined in BSP-expressing cancer cells. Expression of BSP but not an integrin-binding mutant (BSP-KAE) in tumor cell lines resulted in increased levels of alpha(v)-containing integrins and number of mature focal adhesions. Adhesion of cells to recombinant BSP or the expression of BSP stimulated focal adhesion kinase and ERK phosphorylation, as well as activated AP-1-family proteins. Activation of these pathways by BSP expression increased the expression of the matrix metalloproteinases MMP-2, MMP-9, and MMP-14. The BSP-mediated activation of the FAK-associated pathway resulted in increased cancer cell invasion in a Matrigel-coated Boyden-chamber assay and increased cell survival upon withdrawal of serum. Addition of EGF or TGF-beta1 to the BSP-expressing cell lines significantly increased ERK phosphorylation, AP-1 activation, MMP-2 expression, cell migration and survival compared to untreated cells expressing BSP. This study thus defines the cooperative mechanisms by which BSP can enhance specific factors associated with a metastatic phenotype in tumor cell lines, an effect that is increased by circulating TGF-beta1 and EGF. (c) 2009 Wiley-Liss, Inc.

Organization, regulatory sequences, and alternatively spliced transcripts of the mucosal addressin cell adhesion molecule-1 (MAdCAM-1) gene

DOE Office of Scientific and Technical Information (OSTI.GOV)

Sampaio, S.O.; Mei, C.; Butcher, E.C.

The mucosal addressin cell adhesion molecule-1 (MAdCAM-1) is expressed selectively at venular sites of lymphocyte extravasation into mucosal lymphoid tissues and lamina propria, where it directs local lymphocyte trafficking. MAdCAM-1 is a multifunctional type I transmembrane adhesion molecule comprising two distal Ig domains involved in {alpha}4{beta}7 integrin binding, a mucin-like region able to display L-selectin-binding carbohydrates, and a membrane-proximal Ig domain homologous to IgA. We show in this work that the MAdCAM-1 gene is located on chromosome 10 and contains five exons. The signal peptide and each one of the three Ig domains are encoded by a distinct exon, whereasmore » the transmembrane, cytoplasmic tail, and 3{prime}-untranslated region of MAdCAM-1 are combined on a single exon. The mucin-like region and the third Ig domain are encoded together on exon 4. An alternatively spliced MAdCAM-1 mRNA is identified that lacks the mucin/IgA-homologous exon 4-encoded sequences. This short variant of MAdCAM-1 may be specialized to support {alpha}4{beta}7-dependent adhesion strengthening, independent of carbohydrate-presenting function. Sequences 5{prime} of the transcription start site include tandem nuclear factor-KB sites; AP-1, AP-2, and signal peptide-1 binding sites; and an estrogen response element. Our findings reinforce the correspondence between the multidomain structure and versatile functions of this vascular addressin, and suggest an additional level of regulation of carbohydrate-presenting capability, and thus of its importance in lectin-mediated vs. {alpha}4{beta}7-dependent adhesive events in lymphocyte trafficking. 46 refs., 6 figs., 1 tab.« less

National Epidemiologic Surveys of Enterobacter aerogenes in Belgian Hospitals from 1996 to 1998

PubMed Central

De Gheldre, Y.; Struelens, M. J.; Glupczynski, Y.; De Mol, P.; Maes, N.; Nonhoff, C.; Chetoui, H.; Sion, C.; Ronveaux, O.; Vaneechoutte, M.

2001-01-01

Two national surveys were conducted to describe the incidence and prevalence of Enterobacter aerogenes in 21 Belgian hospitals in 1996 and 1997 and to characterize the genotypic diversity and the antimicrobial resistance profiles of clinical strains of E. aerogenes isolated from hospitalized patients in Belgium in 1997 and 1998. Twenty-nine hospitals collected 10 isolates of E. aerogenes, which were typed by arbitrarily primed PCR (AP-PCR) using two primers and pulsed-field gel electrophoresis. MICs of 10 antimicrobial agents were determined by the agar dilution method. Beta-lactamases were detected by the double-disk diffusion test and characterized by isoelectric point. The median incidence of E. aerogenes colonization or infection increased from 3.3 per 1,000 admissions in 1996 to 4.2 per 1000 admissions in the first half of 1997 (P < 0.01). E. aerogenes strains (n = 260) clustered in 25 AP-PCR types. Two major types, BE1 and BE2, included 36 and 38% of strains and were found in 21 and 25 hospitals, respectively. The BE1 type was indistinguishable from a previously described epidemic strain in France. Half of the strains produced an extended-spectrum beta-lactamase, either TEM-24 (in 86% of the strains) or TEM-3 (in 14% of the strains). Over 75% of the isolates were resistant to ceftazidime, piperacillin-tazobactam, and ciprofloxacin. Over 90% of the strains were susceptible to cefepime, carbapenems, and aminoglycosides. In conclusion, these data suggest a nationwide dissemination of two epidemic multiresistant E. aerogenes strains in Belgian hospitals. TEM-24 beta-lactamase was frequently harbored by one of these epidemic strains, which appeared to be genotypically related to a TEM-24-producing epidemic strain from France, suggesting international dissemination. PMID:11230400

Modeling Resonant Structure in the Kuiper Belt

NASA Astrophysics Data System (ADS)

Holmes, E. K.; Dermott, S. F.; Grogan, K.

1999-09-01

There is a possible connection between structure in circumstellar disks and the presence of planets, our own zodiacal cloud being the prime example. Asymmetries in such a disk could be diagnostic of planets which would be otherwise undetectable. At least three different types of asymmetries can serve to indicate bodies orbiting a star in a disk: (1) a warp in the plane of symmetry of the disk, (2) an offset in the center of symmetry of the disk with respect to the central star, and (3) density anomalies in the plane of the disk due to resonant trapping of dust particles. In the asteroid belt, collisions between asteroids supply dust particles to the zodiacal cloud. By comparison, it has been postulated that collisions between KBOs could initiate a collisional cascade which would produce a Kuiper dust disk. In fact, the Kuiper Belt is the region of our solar system that is most analogous to the planetary debris disks we see around other stars such as Vega, beta Pic, Fomalhaut, and epsilon Eridani (Backman and Paresce 1993). A Kuiper Disk would most likely have a resonant structure, with two concentrations in brightness along the ecliptic longitude. This large scale structure arises because many of the KBOs, the Plutinos, are in the 2:3 mean motion resonance with Neptune. By running numerical integrations of particles in Pluto-like orbits, the resonant structure of the Kuiper belt can be studied by determining the percentage of particles trapped in the resonance as a function of their initial velocity and beta, where beta = Frad/Fgrav. The dynamical evolution of the particles is followed from source to sink with Poynting Robertson light drag, solar wind drag, radiation pressure, and the effects of planetary gravitational perturbations included. This research was funded in part by a NASA GSRP grant.

Final report of supplementary comparison AFRIMETS.AUV.A-S1: primary pressure calibration of LS2aP microphones according to IEC 61094-2, over the frequency range 1 Hz to 31.5 kHz.

NASA Astrophysics Data System (ADS)

Nel, R.; Barrera-Figueroa, S.; Dobrowolska, D.; Defilippo Soares, Z. M.; Maina, A. K.; Hof, C.

2016-01-01

This is the final report of the AFRIMETS.AUV-S1 comparison of the pressure sensitivity, modulus and phase, of LS2aP microphones in the frequency range 1 Hz to 31.5 kHz in accordance with IEC 61094-2. Six national metrology institutes from three different regional metrology organisations participated in the comparison for which two LS2aP microphones were circulated simultaneously to all the participants in a hybrid-star configuration. The comparison reference values were calculated as the weighted mean for modulus and phase for each individual microphone. Main text To reach the main text of this paper, click on Final Report. Note that this text is that which appears in Appendix B of the BIPM key comparison database kcdb.bipm.org/. The final report has been peer-reviewed and approved for publication by the CCAUV, according to the provisions of the CIPM Mutual Recognition Arrangement (CIPM MRA).

THE BANANA PROJECT. IV. TWO ALIGNED STELLAR ROTATION AXES IN THE YOUNG ECCENTRIC BINARY SYSTEM EP CRUCIS: PRIMORDIAL ORIENTATION AND TIDAL ALIGNMENT

DOE Office of Scientific and Technical Information (OSTI.GOV)

Albrecht, Simon; Winn, Joshua N.; Setiawan, Johny

With observations of the EP Cru system, we continue our series of measurements of spin-orbit angles in eclipsing binary star systems, the BANANA project (Binaries Are Not Always Neatly Aligned). We find a close alignment between the sky projections of the rotational and orbital angular momentum vectors for both stars ({beta}{sub p} = -1. Degree-Sign 8 {+-} 1. Degree-Sign 6 and |{beta}{sub s}| < 17 Degree-Sign ). We also derive precise absolute dimensions and stellar ages for this system. The EP Cru and DI Her systems provide an interesting comparison: they have similar stellar types and orbital properties, but DImore » Her is younger and has major spin-orbit misalignments, raising the question of whether EP Cru also had a large misalignment at an earlier phase of evolution. We show that tidal dissipation is an unlikely explanation for the good alignment observed today, because realignment happens on the same timescale as spin-orbit synchronization, and the stars in EP Cru are far from synchronization (they are spinning nine times too quickly). Therefore it seems that some binaries form with aligned axes, while other superficially similar binaries are formed with misaligned axes.« less

VizieR Online Data Catalog: BI light curves of DDO210 pulsating variables (Ordonez+, 2016)

NASA Astrophysics Data System (ADS)

Ordonez, A. J.; Sarajedini, A.

2016-07-01

The data set used by Cole et al. (2014ApJ...794...64M) is very deep and covers a time baseline conducive to identifying short-period variable stars. These observations of DDO210 were originally intended for use in a detailed SFH analysis for this dwarf, and thus cover a significant portion of the galaxy while reaching photometric depths to the main-sequence turnoff. The observations consisting of 22920s in F475W and 33480s in F814W were taken with a cadence well suited for identifying short-period variable stars. We retrieved these images from the Mikulski Archive for Space Telescopes (MAST) for use in our study. (2 data files).

VizieR Online Data Catalog: APOKASC catalog of KIC dwarfs and subgiants (Serenelli+, 2017)

NASA Astrophysics Data System (ADS)

Serenelli, A.; Johnson, J.; Huber, D.; Pinsonneault, M.; Ball, W. H.; Tayar, J.; Aguirre, V. S.; Basu, S.; Troup, N.; Hekker, S.; Kallinger, T.; Stello, D.; Davies, G. R.; Lund, M. N.; Mathur, S.; Mosser, B.; Stassun, K. G.; Chaplin, W. J.; Elsworth, Y.; Garcia, R. A.; Handberg, R.; Holtzman, J.; Hearty, F.; Garcia-Hernandez, D. A.; Gaulme, P.; Zamora, O.

2018-02-01

The catalog consists of stars with detected solar-like oscillations in Kepler short-cadence data as reported in Chaplin+ (2011Sci...332..213C) and with spectroscopic observations from the APOGEE-1 survey (Majewski+ 2017AJ....154...94M). APOGEE spectra cover the H band, between 1.51 and 1.7um, at a resolution R=22500. This work extends the first APOKASC red giants catalog presented in Pinsonneault+ (2014, J/ApJS/215/19) to include 415 dwarf and subgiant stars. It is based on global seismic parameters Δν and νmax obtained from Kepler short-cadence asteroseismic data with length of light curves spanning from 30 up to 1055 days. (3 data files).

VizieR Online Data Catalog: PHAT X. UV-IR photometry of M31 stars (Williams+, 2014)

NASA Astrophysics Data System (ADS)

Williams, B. F.; Lang, D.; Dalcanton, J. J.; Dolphin, A. E.; Weisz, D. R.; Bell, E. F.; Bianchi, L.; Byler, N.; Gilbert, K. M.; Girardi, L.; Gordon, K.; Gregersen, D.; Johnson, L. C.; Kalirai, J.; Lauer, T. R.; Monachesi, A.; Rosenfield, P.; Seth, A.; Skillman, E.

2015-01-01

The data for the Panchromatic Hubble Andromeda Treasury (PHAT) survey were obtained from 2010 July 12 to 2013 October 12 using the Advanced Camera for Surveys (ACS) Wide Field Channel (WFC), the Wide Field Camera 3 (WFC3) IR (infrared) channel, and the WFC3 UVIS (ultraviolet-optical) channel. The observing strategy is described in detail in Dalcanton et al. (2012ApJS..200...18D). A list of the target names, observing dates, coordinates, orientations, instruments, exposure times, and filters is given in Table 1. Using the ACS and WFC3 cameras aboard HST, we have photometered 414 contiguous WFC3/IR footprints covering 0.5deg2 of the M31 star-forming disk. (4 data files).

Substantial reservoirs of molecular hydrogen in the debris disks around young stars.

PubMed

Thi, W F; Blake, G A; van Dishoeck, E F; van Zadelhoff, G J; Horn, J M; Becklin, E E; Mannings, V; Sargent, A I; van Den Ancker, M E; Natta, A

2001-01-04

Circumstellar accretion disks transfer matter from molecular clouds to young stars and to the sites of planet formation. The disks observed around pre-main-sequence stars have properties consistent with those expected for the pre-solar nebula from which our own Solar System formed 4.5 Gyr ago. But the 'debris' disks that encircle more than 15% of nearby main-sequence stars appear to have very small amounts of gas, based on observations of the tracer molecule carbon monoxide: these observations have yielded gas/dust ratios much less than 0.1, whereas the interstellar value is about 100 (ref. 9). Here we report observations of the lowest rotational transitions of molecular hydrogen (H2) that reveal large quantities of gas in the debris disks around the stars beta Pictoris, 49 Ceti and HD135344. The gas masses calculated from the data are several hundreds to a thousand times greater than those estimated from the CO observations, and yield gas/dust ratios of the same order as the interstellar value.

Evolution of close binary systems: Observational aspects

NASA Technical Reports Server (NTRS)

Plavec, M. J.

1981-01-01

Detached close binary systems define the main sequence band satisfactorily, but very little is known about the masses of giants and supergiants. High dispersion international ultraviolet explorer satellite observations promise an improvement, since blue companions are now frequently found to late type supergiants. Mu Sagittaril and in particular Xi Aurigae are discussed in more detail. The barium star abundance anomaly appears to be due to mass transfer in interacting systems. The symbiotic stars are another type of binary systems containing late type giants; several possible models for the hotter star and for the type of interaction are discussed. The W Serpentis stars appear to be Algols in the rapid phase of mass transfer, but a possible link relating them to the symbiotics is also indicated. Evidence of hot circumstellar plasmas has now been found in several ordinary Algols; there may exist a smooth transition between very quiescent Algols and the W Serpentis stars. Beta Lyrae is discussed in the light of new spectrophotometric results.

A photometric map of interstellar reddening within 100 PC

NASA Astrophysics Data System (ADS)

Perry, C. L.; Johnston, L.; Crawford, D. L.

1982-12-01

Color excesses and distances are calculated for 300 bright, northern, late F stars using uvby beta photometric indices. The data allow an extension of the earlier maps by Perry and Johnston of the spatial distribution of interstellar reddening into the local (r less than 100 pc) solar neighborhood. Some definite conclusions are made regarding the distribution of interstellar dust in the northern hemisphere and within 300 pc of the sun by merging these results and the polarimetric observations by Tinbergen (1982) for 180 stars within 35 pc of the sun.

Origin of superluminal radio jets in microquasars

NASA Astrophysics Data System (ADS)

Yadav, J. S.; Bhandare, R. S.

In Microquasars, superluminal radio jets are seen at large distances from few hundred AU to 5000 AU with very high radio luminosity. We suggest that these superluminal jets are due to internal shocks which form in the previously generated slowly moving wind (from the accretion disk or the companion star) with beta < 0.01 as the fast moving discrete jet with beta sim 1 catches up and interacts with it. The black hole X-ray binaries with transient radio emission (mostly LMXBs) produce superluminal jets with beta_app > 1 when the accretion rate is high and the bolometric luminosity, L_bol approaches the Eddington Luminosity, L_Edd. On the other hand, the black hole X-ray binaries with persistent radio emission (mostly HMXBs) produce superluminal jets with beta_app < 1 at relatively low accretion rate. Our work here brings Galactic microquasars closer to extragalactic AGNs and quasars as the environment plays an important role in the formation of superluminal jets.

Looking for rings and things

NASA Astrophysics Data System (ADS)

Kenworthy, Matthew

2017-04-01

It's not often that an astronomical object gets its own dedicated observatory, but as the planet Beta Pictoris b moves in front of its host star, its every move will be watched by bRing, eager to discover more about the planet's Hill sphere, explains Matthew Kenworthy.

Enzymatic carotenoid cleavage in star fruit (Averrhoa carambola).

PubMed

Fleischmann, Peter; Watanabe, Naoharu; Winterhalter, Peter

2003-05-01

This paper presents the first description of an enzyme fraction exhibiting carotenoid cleavage activity isolated from fruit skin of Averrhoa carambola. Partial purification of the enzyme could be achieved by acetone precipitation, ultrafiltration (300 kDa, 50 kDa), isoelectric focusing (pH 3-10) and sodium dodecyl sulfate polyacrylamide gel electrophoresis (7.5%). In this way, an enzymatically active protein fraction was obtained, consisting of four proteins in the molecular weight range of between 12 and 90 kDa. Using beta-carotene as substrate, the enzyme activity was detected spectrophotometrically at 505 nm. The main reaction product, detected by GC analysis, was beta-ionone. This proves that the isolated enzymes are closely related to aroma metabolism and release of star fruit. The time constant of the reaction was 16.6 min, the Michaelis Constant K(m)=3.6 micromol 1(-1) and the maximum velocity V(max)=10.5 x 10(-3) micromol l(-1) s(-1) mg((Protein))(-1). The optimum temperature was 45 degrees C.

SPECTROPOLARIMETRY OF THE CLASSICAL T TAURI STAR BP TAU

DOE Office of Scientific and Technical Information (OSTI.GOV)

Chen, Wei; Johns-Krull, Christopher M., E-mail: wc2@rice.edu, E-mail: cmj@rice.edu

We implement a least-squares deconvolution (LSD) code to study magnetic fields on cool stars. We first apply our code to high-resolution optical echelle spectra of 53 Cam (a magnetic Ap star) and three well-studied cool stars (Arcturus, 61 Cyg A, and ξ Boo A) as well as the Sun (by observing the asteroid Vesta) as tests of the code and the instrumentation. Our analysis is based on several hundred photospheric lines spanning the wavelength range 5000 Å to 9000 Å. We then apply our LSD code to six nights of data on the Classical T Tauri Star BP Tau. Amore » maximum longitudinal field of 370 ± 80 G is detected from the photospheric lines on BP Tau. A 1.8 kG dipole tilted at 129° with respect to the rotation axis and a 1.4 kG octupole tilted at 104° with respect to the rotation axis, both with a filling factor of 0.25, best fit our LSD Stokes V profiles. Measurements of several emission lines (He I 5876 Å, Ca II 8498 Å, and 8542 Å) show the presence of strong magnetic fields in the line formation regions of these lines, which are believed to be the base of the accretion footpoints. The field strength measured from these lines shows night-to-night variability consistent with rotation of the star.« less

The Water Content of Exo-earths in the Habitable Zone around Low-mass Stars

NASA Astrophysics Data System (ADS)

Mulders, Gijs Dirk; Ciesla, Fred; Pascucci, Ilaria; apai, Daniel

2015-08-01

Terrestrial planets in the habitable zones of low-mass M dwarf stars have become the focus of many astronomical studies: they are more easily accessible to detection and characterization than their counterparts around sunlike stars. The habitability of these planets, however, faces a number of challenges, including inefficient or negligible water delivery during accretion. To understand the water content of planets in and around the habitable zone, simulations of the final stages of planet formation are necessary.We present detailed accretion simulations of wet and dry planetary embryos around a range of stellar masses. We focus on different pathways of delivering water from beyond the snow line to terrestrial planets in the habitable zone. We explore the impact of using either asteroid-like or comet-like bodies, and the effects of a dispersion in snow line locations. We derive the probability distribution of water abundances for terrestrial sized planets in the habitable zone.While these models predict that the bulk of terrestrial planets in the habitable zones of M stars will be dry, a small fraction receives earth-like amounts of water. Given their larger numbers and higher planet occurrence rates, this population of water-enriched worlds in the habitable zone of M stars may equal that around sun-like stars in numbers.References:Ciesla, Mulders et al. 2015Mulders et al. ApJ subm.

Computing Models of M-type Host Stars and their Panchromatic Spectral Output

NASA Astrophysics Data System (ADS)

Linsky, Jeffrey; Tilipman, Dennis; France, Kevin

2018-06-01

We have begun a program of computing state-of-the-art model atmospheres from the photospheres to the coronae of M stars that are the host stars of known exoplanets. For each model we are computing the emergent radiation at all wavelengths that are critical for assessingphotochemistry and mass-loss from exoplanet atmospheres. In particular, we are computing the stellar extreme ultraviolet radiation that drives hydrodynamic mass loss from exoplanet atmospheres and is essential for determing whether an exoplanet is habitable. The model atmospheres are computed with the SSRPM radiative transfer/statistical equilibrium code developed by Dr. Juan Fontenla. The code solves for the non-LTE statistical equilibrium populations of 18,538 levels of 52 atomic and ion species and computes the radiation from all species (435,986 spectral lines) and about 20,000,000 spectral lines of 20 diatomic species.The first model computed in this program was for the modestly active M1.5 V star GJ 832 by Fontenla et al. (ApJ 830, 152 (2016)). We will report on a preliminary model for the more active M5 V star GJ 876 and compare this model and its emergent spectrum with GJ 832. In the future, we will compute and intercompare semi-empirical models and spectra for all of the stars observed with the HST MUSCLES Treasury Survey, the Mega-MUSCLES Treasury Survey, and additional stars including Proxima Cen and Trappist-1.This multiyear theory program is supported by a grant from the Space Telescope Science Institute.

A Herschel-Detected Correlation between Planets and Debris Disks

NASA Astrophysics Data System (ADS)

Bryden, Geoffrey; Krist, J. E.; Stapelfeldt, K. R.; Kennedy, G.; Wyatt, M.; Beichman, C. A.; Eiroa, C.; Marshall, J.; Maldonado, J.; Montesinos, B.; Moro-Martin, A.; Matthews, B. C.; Fischer, D.; Ardila, D. R.; Kospal, A.; Rieke, G.; Su, K. Y.

2013-01-01

The Fomalhaut, beta Pic, and HR 8799 systems each have directly imaged planets and prominent debris disks, suggesting a direct link between the two phenomena. Unbiased surveys with Spitzer, however, failed to find a statistically significant correlation. We present results from SKARPS (the Search for Kuiper belts Around Radial-velocity Planet Stars) a Herschel far-IR survey for debris disks around solar-type stars known to have orbiting planets. The identified disks are generally cold and distant 50 K/100 AU), i.e. well separated from the radial-velocity-discovered planets. Nevertheless, we find a strong correlation between the inner planets and outer disks, with disks around planet-bearing stars tending to be much brighter than those not known to have planets.

The Hyades main sequence

NASA Astrophysics Data System (ADS)

Eggen, O. J.

1982-11-01

Intermediate band, H-beta and RI observations of 72 Hyades cluster stars to V = 11 mag are reported and discussed. A modulus of 3.2 mag is derived on the basis of a comparison with field stars of large parallax. Also presented are observations of 98 main-sequence stars of the Hyades group that were previously found to be group members from kinematical considerations. Parallaxes of the group stars, computed on the assumption that they are members of an extended Hyades cluster, yield mean values of (U, V, W) = (+40.5, -18.4, -4.9) km/s, with dispersions of (2.3, 2.3, 6.0) km/s, compared with (+41.7, -18.4, -2.0) and (2.6, 1.3, 1.9) km/s for the brightest cluster members. It is noted that all the stars discussed can be considered as members of a supercluster in which only a slight relaxation control of the W velocities is present for stars far from the nucleus. Evidence is found, including that of the Praesepe cluster at Z = +80 pc, for some interchange between the U, V, and W velocities in stars farthest from the galactic plane, with the total cluster velocity being maintained.

KamLAND Sensitivity to Neutrinos from Pre-supernova Stars

NASA Astrophysics Data System (ADS)

Asakura, K.; Gando, A.; Gando, Y.; Hachiya, T.; Hayashida, S.; Ikeda, H.; Inoue, K.; Ishidoshiro, K.; Ishikawa, T.; Ishio, S.; Koga, M.; Matsuda, S.; Mitsui, T.; Motoki, D.; Nakamura, K.; Obara, S.; Oura, T.; Shimizu, I.; Shirahata, Y.; Shirai, J.; Suzuki, A.; Tachibana, H.; Tamae, K.; Ueshima, K.; Watanabe, H.; Xu, B. D.; Kozlov, A.; Takemoto, Y.; Yoshida, S.; Fushimi, K.; Piepke, A.; Banks, T. I.; Berger, B. E.; Fujikawa, B. K.; O'Donnell, T.; Learned, J. G.; Maricic, J.; Matsuno, S.; Sakai, M.; Winslow, L. A.; Efremenko, Y.; Karwowski, H. J.; Markoff, D. M.; Tornow, W.; Detwiler, J. A.; Enomoto, S.; Decowski, M. P.; KamLAND Collaboration

2016-02-01

In the late stages of nuclear burning for massive stars (M > 8 M⊙), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta decay on free hydrogen. This is the golden channel for liquid scintillator detectors because the coincidence signature allows for significant reductions in background signals. We find that the kiloton-scale liquid scintillator detector KamLAND can detect these pre-supernova neutrinos from a star with a mass of 25 M⊙ at a distance less than 690 pc with 3σ significance before the supernova. This limit is dependent on the neutrino mass ordering and background levels. KamLAND takes data continuously and can provide a supernova alert to the community.

Determining Mass-Loss Rates of Evolved Stars in the Galactic Bulge from Infrared Surveys

NASA Astrophysics Data System (ADS)

Riley, Allyssa; Sargent, Benjamin A.; Srinivasan, Sundar; Meixner, Margaret; Kastner, Joel H.

2018-06-01

To investigate the relationship between mass loss from evolved stars and host galaxy metallicity, we are computing the dust mass loss budget due to red supergiant (RSG) and asymptotic giant branch (AGB) stars in the Galactic Bulge and comparing this result to that previously obtained for the Magellanic Clouds. We construct spectral energy distributions (SEDs) for our candidate RSG and AGB stars using observations from various infrared surveys, including the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE). Because Robitaille et al (2008, AJ, 136, 2413) have already identified Intrinsically Red Objects from the GLIMPSE I and II surveys, we use their method as a starting point and expand the study by using the GLIMPSE 3D survey. Because AGB stars can be variable, we also match the GLIMPSE I, II, and 3D sources to other surveys, such as DEEP GLIMPSE, WISE, VVV, and DENIS, in order to characterize the variability across the spectral energy distribution (SED) of each source. This allows us to determine the source’s average SED over multiple epochs. We use extinction curves derived from Spitzer studies of extinction in the Galaxy to determine the extinction corrections for our sample. To establish mass-loss rates of evolved stars in the Bulge, we use the Grid of Red supergiant and Asymptotic giant branch ModelS (GRAMS) of dust-enshrouded evolved stars (2011, A&A, 532, A54; 2011, ApJ, 728, 93). This allows us to determine the total mass return to the Bulge from these stars. This work has been supported by NASA ADAP grant 80NSSC17K0057.

Spectro-astrometry Of H2O And OH In A Protoplanetary Disk

NASA Astrophysics Data System (ADS)

Brown, Logan R.; Gibb, E. L.; Troutman, M. R.

2012-05-01

To understand how life originated on Earth, we must investigate how the necessary water and other prebiotic molecules were distributed through the protoplanetary disk from which the solar system formed. To infer this, we study analogs to the early solar system, T Tauri stars, which are surrounded by circumstellar disks. These disks generally have masses on the order of tens of Jupiter masses and extend outward to about 100 AU. These disks have a flared geometry. Of particular interest here is the chemistry of these objects. Disks have three main chemical regions: the cold midplane, warm molecular layer, and hot ionized region (Walsh et. al. 2010). The cold midplane is a cold, dense region where molecules freeze onto dust grains. In the warm molecular layer above that, molecular synthesis is stimulated by increasing temperatures and the evaporation of molecules from dust grains. Above that, stellar and cosmic radiation dissociates and ionizes molecules into constituent radicals, atoms, and ions in the hot ionized disk atmosphere. Spitzer Space Telescope observations found a rich water emission spectrum toward T Tauri star AA Tau (Salyk et al. 2008). How this water is distributed through a protoplanetary disk is of particular interest. This can be determined using a technique called spectro-astrometry that measures the spatial dependence of a spectral feature. We present high-resolution, near-infrared spectroscopic data from the T Tauri star DR Tau, obtained on 16 -18 February 2011 using NIRSPEC at the Keck II telescope. We detected both water and OH in emission and report our spectro-astrometric signals and the derived spatial extent of the gas emission in the disk. Supported by NSF 0908230. Salyk, C. et al. 2008, ApJ, 676, 49 Walsh, C., Miller, T. J., & Nomura, H. 2010 ApJ, 722, 1607

Molecular analysis of a GM2-activator deficiency in two patients with GM2-gangliosidosis AB variant.

PubMed Central

Schepers, U.; Glombitza, G.; Lemm, T.; Hoffmann, A.; Chabas, A.; Ozand, P.; Sandhoff, K.

1996-01-01

Lysosomal degradation of ganglioside GM2 by beta-hexosaminidase A (hex A) requires the presence of the GM2 activator protein (GM2AP) as an essential cofactor. A deficiency of the GM2 activator causes the AB variant of GM2 gangliosidosis, a recessively inherited disorder characterized by excessive neuronal accumulation of GM2 and related glycolipids. Two novel mutations in the GM2 activator gene (GM2A) have been identified by the reverse-transcriptase-PCR method--a three-base deletion, AAG262-264, resulting in a deletion of Lys88, and a single-base deletion, A410, that causes a frameshift. The latter results in substitution of 33 amino acids and the loss of another 24 amino acid residues. Both patients are homoallelic for their respective mutations inherited from their parents, who are heteroallelic at the GM2A locus. Although the cultured fibroblasts of both patients produce normal levels of activator mRNA, they lack a lysosomal form of GM2AP. Pulse/chase labeling of cultured fibroblasts of the patients, in presence and absence of brefeldin A, indicates a premature degradation of both--mutant and truncated--GM2APs in the endoplasmic reticulum or Golgi. These results were supported by in vitro translation experiments and expression of the mutated proteins. When the mutated GM2APs were expressed in Escherichia coli, both mature GM2AP forms turned proved to exhibit only residual activities in an in vitro assay. Images Figure 2 Figure 3 Figure 4 Figure 5 Figure 6 Figure 7 PMID:8900233

Molecular analysis of a GM2-activator deficiency in two patients with GM2-gangliosidosis AB variant

DOE Office of Scientific and Technical Information (OSTI.GOV)

Schepers, U.; Glombitza, G.; Lemm, T.

1996-11-01

Lysosomal degradation of ganglioside GM2 by {beta}-hexosaminidase A (hex A) requires the presence of the GM2 activator protein (GM2AP) as an essential cofactor. A deficiency of the GM2 activator causes the AB variant of GM2 gangliosidosis, a recessively inherited disorder characterized by excessive neuronal accumulation of GM2 and related glycolipids. Two novel mutations in the GM2 activator gene (GM2A) have been identified by the reverse-transcriptase-PCR method - a three-base deletion, AAG{sup 262-264}, resulting in a deletion of Lys{sup 88}, and a single-base deletion, A{sup 410}, that causes a frameshift. The latter results in substitution of 33 amino acids and themore » loss of another 24 amino acid residues. Both patients are homoallelic for their respective mutations inherited from their parents, who are heteroallelic at the GM2A locus. Although the cultured fibroblasts of both patients produce normal levels of activator mRNA, they lack a lysosomal form of GM2AP. Pulse/chase labeling of cultured fibroblasts of the patients, in presence and absence of brefeldin A, indicates a premature degradation of both-mutant and truncated-GM2APs in the endoplasmic reticulum or Golgi. These results were supported by in vitro translation experiments and expression of the mutated proteins. When the mutated GM2APs were expressed in Escherichia coli, both mature GM2AP forms turned proved to exhibit only residual activities in an in vitro assay. 26 refs., 7 figs.« less

VizieR Online Data Catalog: APOGEE kinematics. I. Galactic bulge overview (Ness+, 2016)

NASA Astrophysics Data System (ADS)

Ness, M.; Zasowski, G.; Johnson, J. A.; Athanassoula, E.; Majewski, S. R.; Garcia Perez, A. E.; Bird, J.; Nidever, D.; Schneider, D. P.; Sobeck, J.; Frinchaboy, P.; Pan, K.; Bizyaev, D.; Oravetz, D.; Simmons, A.

2016-05-01

We use the APOGEE spectra (R=22500) from the SDSS-III Data Release 12 (DR12; Ahn et al. 2014ApJS..211...17A) for about 20000 stars toward the Galactic bulge and surrounding disk. The APOGEE survey, part of the SDSS-III project (Eisenstein et al. 2011AJ....142...72E), operates at the 2.5m telescope of the Apache Point Observatory. (1 data file).

Circular polarimetry of fifteen interesting objects.

NASA Technical Reports Server (NTRS)

Kemp, J. C.; Wolstencroft, R. D.; Swedlund, J. B.

1972-01-01

The results of a search are presented for circular polarization of visible light in 15 objects, including two eclipsing binaries, six magnetic Ap stars, three planetary nebulae, Hubble's Nebula, M87, Sirius, and the Orion A region. On the whole, the results were null, down to typical upper limits for q of 0.01 per cent. A complete description of the used photoelastic polarimeter is given, with special attention to the incidental linear-circular conversion.

Cardiac interbeat interval dynamics from childhood to senescence : comparison of conventional and new measures based on fractals and chaos theory

NASA Technical Reports Server (NTRS)

Pikkujamsa, S. M.; Makikallio, T. H.; Sourander, L. B.; Raiha, I. J.; Puukka, P.; Skytta, J.; Peng, C. K.; Goldberger, A. L.; Huikuri, H. V.

1999-01-01

BACKGROUND: New methods of R-R interval variability based on fractal scaling and nonlinear dynamics ("chaos theory") may give new insights into heart rate dynamics. The aims of this study were to (1) systematically characterize and quantify the effects of aging from early childhood to advanced age on 24-hour heart rate dynamics in healthy subjects; (2) compare age-related changes in conventional time- and frequency-domain measures with changes in newly derived measures based on fractal scaling and complexity (chaos) theory; and (3) further test the hypothesis that there is loss of complexity and altered fractal scaling of heart rate dynamics with advanced age. METHODS AND RESULTS: The relationship between age and cardiac interbeat (R-R) interval dynamics from childhood to senescence was studied in 114 healthy subjects (age range, 1 to 82 years) by measurement of the slope, beta, of the power-law regression line (log power-log frequency) of R-R interval variability (10(-4) to 10(-2) Hz), approximate entropy (ApEn), short-term (alpha(1)) and intermediate-term (alpha(2)) fractal scaling exponents obtained by detrended fluctuation analysis, and traditional time- and frequency-domain measures from 24-hour ECG recordings. Compared with young adults (<40 years old, n=29), children (<15 years old, n=27) showed similar complexity (ApEn) and fractal correlation properties (alpha(1), alpha(2), beta) of R-R interval dynamics despite lower spectral and time-domain measures. Progressive loss of complexity (decreased ApEn, r=-0.69, P<0.001) and alterations of long-term fractal-like heart rate behavior (increased alpha(2), r=0.63, decreased beta, r=-0.60, P<0.001 for both) were observed thereafter from middle age (40 to 60 years, n=29) to old age (>60 years, n=29). CONCLUSIONS: Cardiac interbeat interval dynamics change markedly from childhood to old age in healthy subjects. Children show complexity and fractal correlation properties of R-R interval time series comparable to those of young adults, despite lower overall heart rate variability. Healthy aging is associated with R-R interval dynamics showing higher regularity and altered fractal scaling consistent with a loss of complex variability.

Ageing introduces a complex pattern of changes in several rat brain transcription factors depending on gender and anatomical localization.

PubMed

Sanguino, Elena; Roglans, Núria; Rodríguez-Calvo, Ricardo; Alegret, Marta; Sánchez, Rosa M; Vázquez-Carrera, Manuel; Laguna, Juan C

2006-04-01

As ageing changes the activity of several transcription factors in the rat cortex, we were interested in determining whether similar changes also appear in the hippocampus of old rats. We determined by electrophoretic gel shift assays the binding activity of nuclear factor kappa B (NFkappaB), activator protein-1 (AP-1), peroxisome proliferator-activated receptor (PPAR), and liver X receptor (LXR) in cortex and hippocampus samples from young (3-month-old), and old (18-month-old) male and female Sprague-Dawley rats. NFkappaB activity increased in old male and female rats, though only in cortex samples, while AP-1 activity decreased only in the cortex and hippocampus of old female animals. LXR activity decreased in all conditions, except in old male cortexes; whereas PPAR activity only decreased in the hippocampus of old female rats. Decreases in AP-1 and PPAR activities restricted to old female rats did not result from an age-related decline in plasma 17beta-estradiol concentration, as their activities did not change in samples obtained from ovariectomized young female rats. Our results indicate that ageing induces a complex pattern of changes in the brain-binding activity of NFkappaB, AP-1, PPAR and LXR, depending on the anatomical origin of the samples (cortex or hippocampus), and the sex of the animals studied.

The Uppermost Surface of the Moon

NASA Technical Reports Server (NTRS)

Noble, Sarah K.

2009-01-01

The Ap16 Clam shell Sampling Devices (CSSDs) were designed to sample the uppermost surface of lunar soil. The two devices used beta cloth (69003) and velvet (69004) to collect soil from the top 100 and 500 micrometers of the soil, respectively. Due to the difficulty of the sampling method, little material was collected and as a result little research has been done on these samples. Initial studies attempted to look at the material which had fallen off of the fabrics and was subsequently collected from inside the sample containers. However, this material was highly fractionated and did not provide an adequate picture of the uppermost surface. Recently, samples were obtained directly from the beta cloth using carbon tape. While still fractionated, these samples provide a unique glimpse into the undisturbed soil exposed at the lunar surface.

Using reverse genetics to manipulate the NSs gene of the Rift Valley fever virus MP-12 strain to improve vaccine safety and efficacy.

PubMed

Kalveram, Birte; Lihoradova, Olga; Indran, Sabarish V; Ikegami, Tetsuro

2011-11-01

Rift Valley fever virus (RVFV), which causes hemorrhagic fever, neurological disorders or blindness in humans, and a high rate abortion and fetal malformation in ruminants, has been classified as a HHS/USDA overlap select agent and a risk group 3 pathogen. It belongs to the genus Phlebovirus in the family Bunyaviridae and is one of the most virulent members of this family. Several reverse genetics systems for the RVFV MP-12 vaccine strain as well as wild-type RVFV strains, including ZH548 and ZH501, have been developed since 2006. The MP-12 strain (which is a risk group 2 pathogen and a non-select agent) is highly attenuated by several mutations in its M- and L-segments, but still carries virulent S-segment RNA, which encodes a functional virulence factor, NSs. The rMP12-C13type (C13type) carrying 69% in-frame deletion of NSs ORF lacks all the known NSs functions, while it replicates as efficient as does MP-12 in VeroE6 cells lacking type-I IFN. NSs induces a shut-off of host transcription including interferon (IFN)-beta mRNA and promotes degradation of double-stranded RNA-dependent protein kinase (PKR) at the post-translational level. IFN-beta is transcriptionally upregulated by interferon regulatory factor 3 (IRF-3), NF-kB and activator protein-1 (AP-1), and the binding of IFN-beta to IFN-alpha/beta receptor (IFNAR) stimulates the transcription of IFN-alpha genes or other interferon stimulated genes (ISGs), which induces host antiviral activities, whereas host transcription suppression including IFN-beta gene by NSs prevents the gene upregulations of those ISGs in response to viral replication although IRF-3, NF-kB and activator protein-1 (AP-1) can be activated by RVFV7. Thus, NSs is an excellent target to further attenuate MP-12, and to enhance host innate immune responses by abolishing the IFN-beta suppression function. Here, we describe a protocol for generating a recombinant MP-12 encoding mutated NSs, and provide an example of a screening method to identify NSs mutants lacking the function to suppress IFN-beta mRNA synthesis. In addition to its essential role in innate immunity, type-I IFN is important for the maturation of dendritic cells and the induction of an adaptive immune response. Thus, NSs mutants inducing type-I IFN are further attenuated, but at the same time are more efficient at stimulating host immune responses than wild-type MP-12, which makes them ideal candidates for vaccination approaches.

VizieR Online Data Catalog: Far-UV spectral atlas of O-type stars (Smith, 2012)

NASA Astrophysics Data System (ADS)

Smith, M. A.

2012-10-01

In this paper, we present a spectral atlas covering the wavelength interval 930-1188Å for O2-O9.5 stars using Far-Ultraviolet Spectroscopic Explorer archival data. The stars selected for the atlas were drawn from three populations: Galactic main-sequence (classes III-V) stars, supergiants, and main-sequence stars in the Magellanic Clouds, which have low metallicities. For several of these stars, we have prepared FITS files comprised of pairs of merged spectra for user access via the Multimission Archive at Space Telescope (MAST). We chose spectra from the first population with spectral types O4, O5, O6, O7, O8, and O9.5 and used them to compile tables and figures with identifications of all possible atmospheric and interstellar medium lines in the region 949-1188Å. Our identified line totals for these six representative spectra are 821 (500), 992 (663), 1077 (749), 1178 (847), 1359 (1001), and 1798 (1392) lines, respectively, where the numbers in parentheses are the totals of lines formed in the atmospheres, according to spectral synthesis models. The total number of unique atmospheric identifications for the six main-sequence O-star template spectra is 1792, whereas the number of atmospheric lines in common to these spectra is 300. The number of identified lines decreases toward earlier types (increasing effective temperature), while the percentages of "missed" features (unknown lines not predicted from our spectral syntheses) drop from a high of 8% at type B0.2, from our recently published B-star far-UV atlas (Cat. J/ApJS/186/175), to 1%-3% for type O spectra. The percentages of overpredicted lines are similar, despite their being much higher for B-star spectra. (4 data files).

Yet Another Model for the Gamma-Ray Bursts

NASA Astrophysics Data System (ADS)

Leonard, P. J. T.

2000-05-01

We consider whether a gamma-ray burst can result from a merger between a neutron star and a massive main-sequence star in a binary system following a supernova explosion. The scenario for how this can happen is outlined in Leonard, Hills & Dewey 1994, ApJ, 423, L19-L22. The initially more massive star in a massive binary system evolves and undergoes core collapse to produce a neutron star and supernova. Since the outer layers of the originally more massive star have been transferred to the other star, then the supernova may be hydrogen deficient. The newly-formed neutron star receives a random kick during the explosion. In a small fraction of the cases, the kick has the appropriate direction and amplitude to remove most of the orbital angular momentum of the post-supernova binary system. The result is an orbit with a pericenter smaller than the radius of the non-exploding star. The neutron star rather quickly becomes embedded in the other star, and sinks to its center, giving the envelope of the merged object a lot of rotational angular momentum in the process. Leonard, Hills & Dewey estimate the rate of this process in the Galaxy to be 0.06 per square kpc per Myr for secondaries more massive than 15 solar masses. The fate of the merged object has been the source of much speculation, and we shall assume that a collapsar-like scenario results. That is, the neutron star experiences runaway accretion, collapses into a black hole, which continues to accrete, and produces a pair of jets that bore their way out of the merged object. Observers who lie in the direction of either jet will see a gamma-ray burst. Roughly 1% of supernovae in massive binary systems result in neutron stars quickly becoming embedded in the secondaries, and of those which produce black holes, only 1% would be observable as gamma-ray bursts, if the jets are beamed into 1% of the sky.

Featured Image: Mixing Chemicals in Stars

NASA Astrophysics Data System (ADS)

Kohler, Susanna

2017-10-01

How do stars mix chemicals in their interiors, leading to the abundances we measure at their surfaces? Two scientists from the Planetary Science Institute in Arizona, Tamara Rogers (Newcastle University, UK) and Jim McElwaine (Durham University, UK), have investigated the role that internal gravity waves have in chemical mixing in stellar interiors. Internal gravity waves not to be confused with the currently topical gravitational waves are waves that oscillate within a fluid that has a density gradient. Rogers and McElwaine used simulations to explore how these waves can cause particles in a stars interior to move around, gradually mixing the different chemical elements. Snapshots from four different times in their simulation can be seen below, with the white dots marking tracer particles and the colors indicating vorticity. You can see how the particles move in response to wave motion after the first panel. For more information, check out the paper below!CitationT. M. Rogers and J. N. McElwaine 2017 ApJL 848 L1. doi:10.3847/2041-8213/aa8d13

VizieR Online Data Catalog: Lithium abundances of a large sample of red giants (Liu+, 2014)

NASA Astrophysics Data System (ADS)

Liu, Y. J.; Tan, K. F.; Wang, L.; Zhao, G.; Sato, B.; Takeda, Y.; Li, H. N.

2017-06-01

The sample stars analyzed here are comprised of 321 giants from the Okayama Planet Search Program (Sato et al. 2003ApJ...597L.157S) and 57 giants from the Xinglong Planet Search Program (Liu et al. 2008ApJ...672..553L). Both programs aim to detect planets around intermediate mass G type (and early K type) giants. The spectra were taken with the High Dispersion Echelle Spectrograph at Okayama Astrophysical Observatory (OAO), which was equipped at the coude focus of the 1.88 m telescope during 2008-2010. Before 2008 October, one CCD system with wavelength coverage of 5000-6200 Å was used, and after that the new mosaic 3 CCD system with wavelength a coverage of 4000-7540 Å replaced it. (2 data files).

Interstellar Dust in the Heliosheath: Tentative Discovery of the Magnetic Wall of the Heliosphere

NASA Astrophysics Data System (ADS)

Frisch, P. C.

2005-12-01

The evident identification of interstellar dust grains entrained in the magnetic wall of the heliosphere is reported. It is shown that the distribution of dust grains causing the weak polarization of light from nearby stars is consistent with polarization by small charged interstellar dust grains captured in the heliosphere magnetic wall (Tinbergen 1982, Frisch 2005). There is an offset between the deflected small charged polarizing dust grains, radius less than 0.2 microns, and the undeflected large grain population, radius larger than 0.2 microns. The region of maximum polarization is towards ecliptic coordinates lambda,beta = 295,0 deg, which is offset along the ecliptic longitude by about 35 deg from the heliosphere nose and extends to low ecliptic latitudes where the heliosphere magnetic wall is expected. An offset is also found between the best aligned dust grains, near lambda=281 deg to 220 deg, and the upwind direction of the undeflected inflow of large grains seen by Ulysses and Galileo. In the aligned-grain region, the polarization strength anti-correlates with ecliptic latitude, indicating that the magnetic wall was predominantly at negative ecliptic latitudes when these data were acquired. These data are consistent with model predictions for an interstellar magnetic field which is tilted by 60 deg with respect to the ecliptic plane, and parallel to the galactic plane. References: Tinbergen, 1982: AA, v105, p53; Frisch, 2005: to appear in ApJL.

Inhibition of GSK3 differentially modulates NF-{kappa}B, CREB, AP-1 and {beta}-catenin signaling in hepatocytes, but fails to promote TNF-{alpha}-induced apoptosis

DOE Office of Scientific and Technical Information (OSTI.GOV)

Goetschel, Frank; Kern, Claudia; Lang, Simona

2008-04-01

Glycogen synthase kinase-3 (GSK-3) is known to modulate cell survival and apoptosis through multiple intracellular signaling pathways. However, its hepatoprotective function and its role in activation of NF-{kappa}B and anti-apoptotic factors are poorly understood and remain controversial. Here we investigated whether inhibition of GSK-3 could induce apoptosis in the presence of TNF-{alpha} in primary mouse hepatocytes. We show that pharmacological inhibition of GSK-3 in primary mouse hepatocytes does not lead to TNF-{alpha}-induced apoptosis despite reduced NF-{kappa}B activity. Enhanced stability of I{kappa}B-{alpha} appears to be responsible for lower levels of nuclear NF-{kappa}B and hence reduced transactivation. Additionally, inhibition of GSK-3 wasmore » accompanied by marked upregulation of {beta}-catenin, AP-1, and CREB transcription factors. Stimulation of canonical Wnt signaling and CREB activity led to elevated levels of anti-apoptotic factors. Hence, survival of primary mouse hepatocytes may be caused by the activation and/or upregulation of other key regulators of liver homeostasis and regeneration. These signaling molecules may compensate for the compromised anti-apoptotic function of NF-{kappa}B and allow survival of hepatocytes in the presence of TNF-{alpha} and GSK-3 inhibition.« less

Making sense of listening: the IMAP test battery.

PubMed

Barry, Johanna G; Ferguson, Melanie A; Moore, David R

2010-10-11

The ability to hear is only the first step towards making sense of the range of information contained in an auditory signal. Of equal importance are the abilities to extract and use the information encoded in the auditory signal. We refer to these as listening skills (or auditory processing AP). Deficits in these skills are associated with delayed language and literacy development, though the nature of the relevant deficits and their causal connection with these delays is hotly debated. When a child is referred to a health professional with normal hearing and unexplained difficulties in listening, or associated delays in language or literacy development, they should ideally be assessed with a combination of psychoacoustic (AP) tests, suitable for children and for use in a clinic, together with cognitive tests to measure attention, working memory, IQ, and language skills. Such a detailed examination needs to be relatively short and within the technical capability of any suitably qualified professional. Current tests for the presence of AP deficits tend to be poorly constructed and inadequately validated within the normal population. They have little or no reference to the presenting symptoms of the child, and typically include a linguistic component. Poor performance may thus reflect problems with language rather than with AP. To assist in the assessment of children with listening difficulties, pediatric audiologists need a single, standardized child-appropriate test battery based on the use of language-free stimuli. We present the IMAP test battery which was developed at the MRC Institute of Hearing Research to supplement tests currently used to investigate cases of suspected AP deficits. IMAP assesses a range of relevant auditory and cognitive skills and takes about one hour to complete. It has been standardized in 1500 normally-hearing children from across the UK, aged 6-11 years. Since its development, it has been successfully used in a number of large scale studies both in the UK and the USA. IMAP provides measures for separating out sensory from cognitive contributions to hearing. It further limits confounds due to procedural effects by presenting tests in a child-friendly game-format. Stimulus-generation, management of test protocols and control of test presentation is mediated by the IHR-STAR software platform. This provides a standardized methodology for a range of applications and ensures replicable procedures across testers. IHR-STAR provides a flexible, user-programmable environment that currently has additional applications for hearing screening, mapping cochlear implant electrodes, and academic research or teaching.

IGF-binding proteins mediate TGF-beta 1-induced apoptosis in bovine mammary epithelial BME-UV1 cells.

PubMed

Gajewska, Małgorzata; Motyl, Tomasz

2004-10-01

TGF-beta 1 is an antiproliferative and apoptogenic factor for mammary epithelial cells (MEC) acting in an auto/paracrine manner and thus considered an important local regulator of mammary tissue involution. However, the apoptogenic signaling pathway induced by this cytokine in bovine MEC remains obscure. The present study was focused on identification of molecules involved in apoptogenic signaling of transforming growth factor-beta 1 (TGF-beta 1) in the model of bovine mammary epithelial cell line (BME-UV1). Laser scanning cytometry (LSC), Western blot and electrophoretic mobility shift assay (EMSA) were used for analysis of expression and activity of TGF-beta 1-related signaling molecules. The earliest response occurring within 1-2 h after TGF-beta 1 administration was an induction and activation of R-Smads (Smad2 and Smad3) and Co-Smad (Smad4). An evident formation of Smad-DNA complexes began from 2nd hour after MEC exposure to TGF-beta 1. Similarly to Smads, proteins of AP1 complex: phosphorylated c-Jun and JunD appeared to be early reactive molecules; however, an increase in their expression was detected only in cytosolic fraction. In the next step, an increase of IGF binding protein-3 (IGFBP-3) and IGFBP-4 expression was observed from 6th hour followed by a decrease in the activity of protein kinase B (PKB/Akt), which occurred after 24 h of MEC exposure to TGF-beta 1. The decrease in PKB/Akt activity coincided in time with the decline of phosphorylated Bad expression (inactive form). Present study supported additional evidence that stimulation of insulin-like growth factor I (IGF-I) was associated with complete abrogation of TGF-beta 1-induced activation of Bad and Bax and in the consequence protection against apoptosis. In conclusion, apoptotic effect of TGF-beta 1 in bovine MEC is mediated by IGFBPs and occurs through IGF-I sequestration, resulting in inhibition of PKB/Akt-dependent survival pathway.

An expert computer program for classifying stars on the MK spectral classification system

DOE Office of Scientific and Technical Information (OSTI.GOV)

Gray, R. O.; Corbally, C. J.

2014-04-01

This paper describes an expert computer program (MKCLASS) designed to classify stellar spectra on the MK Spectral Classification system in a way similar to humans—by direct comparison with the MK classification standards. Like an expert human classifier, the program first comes up with a rough spectral type, and then refines that spectral type by direct comparison with MK standards drawn from a standards library. A number of spectral peculiarities, including barium stars, Ap and Am stars, λ Bootis stars, carbon-rich giants, etc., can be detected and classified by the program. The program also evaluates the quality of the delivered spectralmore » type. The program currently is capable of classifying spectra in the violet-green region in either the rectified or flux-calibrated format, although the accuracy of the flux calibration is not important. We report on tests of MKCLASS on spectra classified by human classifiers; those tests suggest that over the entire HR diagram, MKCLASS will classify in the temperature dimension with a precision of 0.6 spectral subclass, and in the luminosity dimension with a precision of about one half of a luminosity class. These results compare well with human classifiers.« less

Automatic phylogenetic classification of bacterial beta-lactamase sequences including structural and antibiotic substrate preference information.

PubMed

Ma, Jianmin; Eisenhaber, Frank; Maurer-Stroh, Sebastian

2013-12-01

Beta lactams comprise the largest and still most effective group of antibiotics, but bacteria can gain resistance through different beta lactamases that can degrade these antibiotics. We developed a user friendly tree building web server that allows users to assign beta lactamase sequences to their respective molecular classes and subclasses. Further clinically relevant information includes if the gene is typically chromosomal or transferable through plasmids as well as listing the antibiotics which the most closely related reference sequences are known to target and cause resistance against. This web server can automatically build three phylogenetic trees: the first tree with closely related sequences from a Tachyon search against the NCBI nr database, the second tree with curated reference beta lactamase sequences, and the third tree built specifically from substrate binding pocket residues of the curated reference beta lactamase sequences. We show that the latter is better suited to recover antibiotic substrate assignments through nearest neighbor annotation transfer. The users can also choose to build a structural model for the query sequence and view the binding pocket residues of their query relative to other beta lactamases in the sequence alignment as well as in the 3D structure relative to bound antibiotics. This web server is freely available at http://blac.bii.a-star.edu.sg/.

Abundances in metal-rich stars. Detailed abundance analysis of 47 G and K dwarf stars with [Me/H] > 0.10 dex

NASA Astrophysics Data System (ADS)

Feltzing, S.; Gustafsson, B.

1998-04-01

We have derived elemental abundances of O, Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Co, Ni as well as for a number of s-elements for 47 G and K dwarf, with [Me/H]>0.1 dex. The selection of stars was based on their kinematics as well as on their uvby-beta photometry. One sample of stars on rather eccentric orbits traces the chemical evolution interior to the solar orbit and another, on circular orbits, the evolution around the solar orbit. A few Extreme Population I stars were included in the latter sample. The stars have -0.1 dex < [Fe/H] < 0.42 dex. The spectroscopic [Fe/H] correlate well with the [Me/H] derived from uvby-beta photometry. We find that the elemental abundances of Mg, Al, Si, Ca, Ti, Cr and Ni all follow [Fe/H]. Our data put further constraints on models of galactic chemical evolution, in particular of Cr, Mn and Co which have not previously been studied for dwarf stars with [Me/H] >0.1 dex. The increase in [Na/Fe] and [Al/Fe] as a function of [Fe/H] found previously by \\cite[Edvardsson et al. (1993a)]{Edv93} has been confirmed for [Na/Fe]. This upturning relation, and the scatter around it, are shown not to be due to a mixture of populations with different mean distances to the galactic centre. We do not confirm the same trend for aluminium, which is somewhat surprising since both these elements are thought to be produced in the same environments in the pre-supernova stars. Nor have we been able to trace any tendency for relative abundances of O, Si, and Ti relative to Fe to vary with the stellar velocities, i.e. the stars present mean distance to the galactic centre. These results imply that there is no significant difference in the chemical evolution of the different stellar populations for stars with [Me/H]>0.1 dex. We find that [O/Fe] continue to decline with increasing [Fe/H] and that oxygen and europium correlate well. However [Si/Fe] and [Ca/Fe] seem to stay constant. A real (``cosmic'') scatter in [Ti/Fe] at given [Fe/H] is suggested as well as a decreasing abundance of the s-elements relative to iron for the most metal-rich dwarf stars. We discuss our results in the context of recent models of galactic chemical evolution. In our sample we have included a few very metal rich stars, sometimes called SMR (super metal rich) stars. We find these stars to be among the most iron-rich in our sample but far from as metal-rich as indicated by their photometric metallicities. SMR stars on highly eccentric orbits, alleged to trace the evolution of the chemical evolution in the galactic Bulge, have previously been found overabundant in O, Mg and Si. We have included three such stars from the study by \\cite[Barbuy & Grenon (1990)]{Bar90}. We find them to be less metal rich and the other elemental abundances remain puzzling. Detailed spectroscopic abundance analyses of K dwarf stars are rare. Our study includes 5 K dwarf stars and has revealed what appears to be a striking example of overionization. The overionization is especially prominent for Ca, Cr and Fe. The origin of this apparent overionization is not clear and we discuss different explanations in some detail. Based on observations at the McDonald Observatory.

alpha-DNA II. Synthesis of unnatural alpha-anomeric oligodeoxyribonucleotides containing the four usual bases and study of their substrate activities for nucleases.

PubMed Central

Morvan, F; Rayner, B; Imbach, J L; Thenet, S; Bertrand, J R; Paoletti, J; Malvy, C; Paoletti, C

1987-01-01

This paper describes for the first time the synthesis of alpha-oligonucleotides containing the four usual bases. Two unnatural hexadeoxyribonucleotides: alpha-[d(CpApTpGpCpG)] and alpha-[d(CpGpCpApTpG)], consisting only of alpha-anomeric nucleotide units, were obtained by an improved phosphotriester method, in solution. Starting material was the four base-protected alpha-deoxyribonucleosides 3a-d. Pyrimidine alpha-deoxynucleosides 3a and 3b were prepared by self-anomerization reactions followed by selective deprotection of sugar hydroxyles, while the two purine alpha-deoxynucleosides 3c and 3d were prepared by glycosylation reactions. In the case of guanine alpha-nucleoside derivative a supplementary base-protecting group: N,N-diphenylcarbamoyl was introduced on O6-position in order to avoid side-reactions during oligonucleotide assembling. The hexadeoxynucleotide alpha-[d(CpApTpGpCpG)] was tested as substrate of selected endo- and exonucleases. In conditions where the natural corresponding beta-hexamer was completely degradated by nuclease S1 and calf spleen phosphodiesterase, the alpha-oligonucleotide remained almost intact. PMID:3575096

Studies of extra-solar Oort clouds and the Kuiper disk

NASA Technical Reports Server (NTRS)

Stern, S. Alan

1996-01-01

We are conducting research designed to enhance our understanding of the evolution and detectability of comet clouds and disks. According to 'standard' theory, both the Kuiper Belt and the Oort Cloud are (at least in part) natural products of the planetary accumulation stage of solar system formation. One expects such assemblages to be a common attribute of other solar systems. Therefore, searches for comet disks and clouds orbiting other stars offer a new method for inferring the presence of planetary systems. This project consists of two efforts: (1) observational work to predict and search for the signatures of Oort Clouds and comet disks around other stars; and (2) modelling studies of the formation and evolution of the Kuiper Belt (KB) and similar assemblages that may reside around other stars, including beta Pic.

Search for Pulsating Stars in the Open Cluster NGC 1502

NASA Astrophysics Data System (ADS)

Stęślicki, M.

2006-04-01

We present results of a variability search in the field of the young open cluster NGC 1502. We confirm that a beta Cephei suspect WEBDA 26 is indeed pulsating with a period of 0.09612 d and semi-amplitude of about 3 mmag in V. A new VI light curve of the bright eclipsing binary and cluster member SZ Cam was obtained. In addition, we found two new variable stars. One is an interesting eclipsing binary showing total eclipses, which can be used to derive the distance to the cluster once radial velocities of the components will be obtained.

HIGH-ENERGY X-RAY PINHOLE CAMERA FOR HIGH-RESOLUTION ELECTRON BEAM SIZE MEASUREMENTS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Yang, B.; Morgan, J.; Lee, S.H.

The Advanced Photon Source (APS) is developing a multi-bend achromat (MBA) lattice based storage ring as the next major upgrade, featuring a 20-fold reduction in emittance. Combining the reduction of beta functions, the electron beam sizes at bend magnet sources may be reduced to reach 5 – 10 µm for 10% vertical coupling. The x-ray pinhole camera currently used for beam size monitoring will not be adequate for the new task. By increasing the operating photon energy to 120 – 200 keV, the pinhole camera’s resolution is expected to reach below 4 µm. The peak height of the pinhole imagemore » will be used to monitor relative changes of the beam sizes and enable the feedback control of the emittance. We present the simulation and the design of a beam size monitor for the APS storage ring.« less

Optical and X-ray studies of chromospherically active stars: FR Cancri, HD 95559 and LO Pegasi

NASA Technical Reports Server (NTRS)

Pandey, J. C.; Singh, K. P.; Drake, S. A.; Sagar, R.

2005-01-01

We present a multiwavelength study of three chromospherically active stars, namely FR Cnc (= BD +16 degrees 1753), HD 95559 and LO Peg (=BD +22 degrees 4409), including newly obtained optical photometry, (for FR Cnc) low-resolution optical spectroscopy, as well as archival IR and X-ray observations. The BVR photometry carried out during the years 2001 - 2004 has found significant photometric variability to be present in all three stars. For FR Cnc, a photometric period 0.826685 +/- 0.000034 d has been established. The strong variation in the phase and amplitude of the FR Cnc light curves when folded on this period implies the presence of evolving and migrating spots or spot groups on its surface. Two independent spots with migration periods of 0.97 and 0.93 years respectively are inferred. The photometry of HD 95559 suggests the formation of a spot (group) during the interval of our observations. We infer the existence of two independent spots or groups in the photosphere of LO Peg, one of which has a migration period of 1.12 years. The optical spectroscopy of FR Cnc carried out during 2002-2003, reveals the presence of strong and variable Ca I1 H and K, H(sub beta) and H(sub alpha) emission features indicative of high level of chromospheric activity. The value of 5.3 for the ratio of the excess emission in H(sub alpha) to H(sub beta), EH(sub alpha)/EH(sub beta), suggests that the chromospheric emission may arise from an extended off-limb region. We have searched for the presence of color excesses in the near-IR JHK bands of these stars using 2MASS data, but none of them appear to have any significant color excess. We have also analyzed archival X-ray observations of HD 95559 and LO Peg carried out by with the ROSAT observatory. The best fit models to their X-ray spectra imply the presence of two coronal plasma components of differing temperatures and with sub-solar metal abundances. The inferred emission measures and temperatures of these systems are similar to those found for other active dwarf stars. The kinematics of FR Cnc suggest that it is a very young (35 - 55 Myrs) main-sequence star and a possible member of the IC 2391 supercluster. LO Peg also has young disk-type kinematics and has been previously suggested to be a member of the 100 Mys old Local Association (Pleiades Moving Group). The kinematics of HD 95559 indicate it is a possible member of the 600 Myrs old Hyades supercluster.

Analysis of the IUE spectra of the strongly interacting binary beta Lyrae

NASA Technical Reports Server (NTRS)

Mccluskey, George E., Jr.

1993-01-01

The six-band ultraviolet light curves of beta Lyrae obtained with the Orbiting Astronomical Observatory A-2 in 1970 exhibited a very unusual behavior. The secondary minimum deepened at shorter wavelength, indicating that one was not observing light variations caused primarily by the eclipses of two stars having a roughly Planckian energy distribution. It was then suggested that the light variations were caused by a viewing angle effect of an optically-thick, ellipsoidal circumbinary gas cloud. Since 1978 beta Lyrae has been observed with the International Ultraviolet Explorer (IUE) satellite. We have constructed ultraviolet light curves from the IUE archival data for comparison with the OAO-A2 results. We find that they are in substantial agreement with each other. The Voyager ultraviolet spectrometer was also used to observe this binary during a period covered by IUE observations. The Voyager results agree with those of the two other satellite observatories at wavelengths longer than about 1350 A. However, in the wavelength region shorter than the Lyman-alpha line at 1216 A, the light curves at 1085 A and 965 A show virtually no light variation except an apparent flaring near phase 0.7, which is also in evidence at longer wavelengths. We suggest that the optically-thick circumbinary gas cloud, which envelops the two stars completely, assumes a roughly spherical shape when observed at these shorter wavelengths.

Ultraviolet light curves of beta Lyrae: Comparison of OAO A-2, IUE, and Voyager Observations

NASA Technical Reports Server (NTRS)

Kondo, Yoji; Mccluskey, George E.; Silvis, Jeffery M. S.; Polidan, Ronald S.; Mccluskey, Carolina P. S.; Eaton, Joel A.

1994-01-01

The six-band ultraviolet light curves of beta Lyrae obtained with the Orbiting Astronomical Observatory (OAO) A-2 in 1970 exhibited a very unusual behavior. The secondary minimum deepened at shorter wavelength, indicating that one was not observing light variations caused primarily by the eclipses of two stars having a roughly Planckian energy distribution. It was then suggested that the light variations were caused by a viewing angle effect of an optically thick, ellipsoidal circumbinary gas cloud. Since 1978 beta Lyrae has been observed with the International Ultraviolet Explorer (IUE) satellite. We have constructed ultraviolet light curves from the IUE archival data for comparison with the OAO A-2 results. We find that they are in substantial agreement with each other. The Voyager ultraviolet spectrometer was also used to observe this binary during a period covered by IUE observations. The Voyager results agree with those of the two other satellite observatories at wavelengths longer than about 1350 A. However, in the wavelength region shorter than the Lyman-alpha line at 1216 A, the light curves at 1085 and 965 A show virtually no light variation except an apparent flaring near phase 0.7, which is also in evidence at longer wavelengths. We suggest that the optically thick circumbinary gas cloud, which envelops the two stars completely, assumes a roughly spherical shape when observed at these shorter wavelengths.

VizieR Online Data Catalog: z<1 3CR radio galaxies and quasars star formation (Westhues+, 2016)

NASA Astrophysics Data System (ADS)

Westhues, C.; Haas, M.; Barthel, P.; Wilkes, B. J.; Willner, S. P.; Kuraszkiewicz, J.; Podigachoski, P.; Leipski, C.; Meisenheimer, K.; Siebenmorgen, R.; Chini, R.

2018-03-01

This work studies a sample of 87 sources from the 3CR catalog (Edge et al. 1959, Cat. VIII/1; Bennett 1962MNRAS.125...75B; Laing et al. 1983, J/MNRAS/204/151; Spinrad et al. 1985, J/PASP/97/932). With the Herschel Space Observatory (Pilbratt et al. 2010A&A...518L...1P) we measured the FIR/submm spectral energy distributions (SEDs) of the 3CR sources in two complementary proposals: one at redshift 1

VizieR Online Data Catalog: GLASS. VII. Hα maps (Vulcani+, 2016)

NASA Astrophysics Data System (ADS)

Vulcani, B.; Treu, T.; Schmidt, K. B.; Morishita, T.; Dressler, A.; Poggianti, B. M.; Abramson, L.; Bradac, M.; Brammer, G. B.; Hoag, A.; Malkan, M.; Pentericci, L.; Trenti, M.

2017-04-01

The Grism Lens-Amplified Survey from Space (GLASS) is a 140 orbit slitless spectroscopic survey conducted with HST in cycle 21. It has observed the cores of 10 massive galaxy clusters with the WFC3 NIR grisms G102 and G141 providing an uninterrupted wavelength coverage from 0.8um to 1.7um. The 10 clusters are listed in Table 1. Observations for GLASS were completed in 2015 January. Building on our pilot study presented in Vulcani+ (2015ApJ...814..161V), we have continued our exploration of the spatial distribution of star formation in galaxies at 0.3<=z<=0.7, as traced by the Hα emission in the field of view of the 10 GLASS clusters, detailing and strengthening our previous results. We have produced Hα maps, taking advantage of the HST/WFC3 G102 and WFC3-G141 data at two orthogonal position angles. In a companion paper (Paper VIII; Vulcani+ 2017ApJ...837..126V), we investigate trends with cluster properties, such as the hot gas density as traced by the X-ray emission, the total surface mass density as inferred from gravitational lens models, and the local number density, to inspect whether or not local cluster conditions have an impact on the extent and location of the star formation. (2 data files).

Putting atomic diffusion theory of magnetic ApBp stars to the test: evaluation of the predictions of time-dependent diffusion models

NASA Astrophysics Data System (ADS)

Kochukhov, O.; Ryabchikova, T. A.

2018-02-01

A series of recent theoretical atomic diffusion studies has address the challenging problem of predicting inhomogeneous vertical and horizontal chemical element distributions in the atmospheres of magnetic ApBp stars. Here we critically assess the most sophisticated of such diffusion models - based on a time-dependent treatment of the atomic diffusion in a magnetized stellar atmosphere - by direct comparison with observations as well by testing the widely used surface mapping tools with the spectral line profiles predicted by this theory. We show that the mean abundances of Fe and Cr are grossly underestimated by the time-dependent theoretical diffusion model, with discrepancies reaching a factor of 1000 for Cr. We also demonstrate that Doppler imaging inversion codes, based either on modelling of individual metal lines or line-averaged profiles simulated according to theoretical three-dimensional abundance distribution, are able to reconstruct correct horizontal chemical spot maps despite ignoring the vertical abundance variation. These numerical experiments justify a direct comparison of the empirical two-dimensional Doppler maps with theoretical diffusion calculations. This comparison is generally unfavourable for the current diffusion theory, as very few chemical elements are observed to form overabundance rings in the horizontal field regions as predicted by the theory and there are numerous examples of element accumulations in the vicinity of radial field zones, which cannot be explained by diffusion calculations.

FIRST ZEEMAN DOPPLER IMAGING OF A COOL STAR USING ALL FOUR STOKES PARAMETERS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Rosén, L.; Kochukhov, O.; Wade, G. A.

Magnetic fields are ubiquitous in active cool stars, but they are in general complex and weak. Current Zeeman Doppler imaging (ZDI) studies of cool star magnetic fields chiefly employ circular polarization observations because linear polarization is difficult to detect and requires a more sophisticated radiative transfer modeling to interpret. But it has been shown in previous theoretical studies, and in the observational analyses of magnetic Ap stars, that including linear polarization in the magnetic inversion process makes it possible to correctly recover many otherwise lost or misinterpreted magnetic features. We have obtained phase-resolved observations in all four Stokes parameters ofmore » the RS CVn star II Peg at two separate epochs. Here we present temperature and magnetic field maps reconstructed for this star using all four Stokes parameters. This is the very first such ZDI study of a cool active star. Our magnetic inversions reveal a highly structured magnetic field topology for both epochs. The strength of some surface features is doubled or even quadrupled when linear polarization is taken into account. The total magnetic energy of the reconstructed field map also becomes about 2.1–3.5 times higher. The overall complexity is also increased as the field energy is shifted toward higher harmonic modes when four Stokes parameters are used. As a consequence, the potential field extrapolation of the four Stokes parameter ZDI results indicates that magnetic field becomes weaker at a distance of several stellar radii due to a decrease of the large-scale field component.« less

The LBTI Hunt for Observable Signatures of Terrestrial Systems (HOSTS) Survey: a Key NASA Science Program on the Road to Exoplanet Imaging Missions (SPIE Proceedings 2)

NASA Technical Reports Server (NTRS)

Danchi, William C.; Bailey, V.; Defrere, D.; Haniff, C.; Hinz, P.; Kennedy, G.; Mennesson, B.; Millan-Gabet, R.; Rieke, G.; Roberge, Aki;

VizieR Online Data Catalog: Kepler follow-up observation program. I. Imaging (Furlan+, 2017)

NASA Astrophysics Data System (ADS)

Furlan, E.; Ciardi, D. R.; Everett, M. E.; Saylors, M.; Teske, J. K.; Horch, E. P.; Howell, S. B.; van Belle, G. T.; Hirsch, L. A.; Gautier, T. N.; Adams, E. R.; Barrado, D.; Cartier, K. M. S.; Dressing, C. D.; Dupree, A. K.; Gilliland, R. L.; Lillo-Box, J.; Lucas, P. W.; Wang, J.

2017-07-01

We present results from six years of follow-up imaging observations of KOI host stars, including work done by teams from the Kepler Community Follow-up Observation Program (CFOP; https://exofop.ipac.caltech.edu/cfop.php) and by other groups. Several observing facilities were used to obtain high-resolution images of KOI host stars. Table1 lists the various telescopes, instruments used, filter bandpasses, typical Point Spread Function (PSF) widths, number of targets observed, and main references for the published results. The four main observing techniques employed are adaptive optics (Keck, Palomar, Lick, MMT), speckle interferometry (Gemini North, WIYN, DCT), lucky imaging (Calar Alto), and imaging from space with HST. A total of 3557 KOI host stars were observed at 11 facilities with 9 different instruments, using filters from the optical to the near-infrared. In addition, 10 of these stars were also observed at the 8m Gemini North telescope by Ziegler et al. 2016 (AJ accepted, arXiv:1605.03584) using laser guide star adaptive optics. The largest number of KOI host stars (3320) were observed using Robo-AO at the Palomar 1.5m telescope (Baranec et al. 2014ApJ...790L...8B; Baranec et al. 2016, Cat. J/AJ/152/18; Law et al. 2014, Cat. J/ApJ/791/35; Ziegler et al. 2016, AJ accepted, arXiv:1605.03584). A total of 8332 observations were carried out from 2009 September to 2015 October covering 3557 stars. We carried out observations at the Keck, Palomar, and Lick Observatory using the facility adaptive optics systems and near-infrared cameras from 2009 to 2015. At Keck, we observed with the 10m Keck II telescope and Near-Infrared Camera, second generation (NIRC2). The pixel scale of NIRC2 was 0.01''/pixel, resulting in a field of view of about 10''*10''. We observed our targets in a narrow K-band filter, Brγ, which has a central wavelength of 2.1686μm. In most cases, when a companion was detected, we also observed the target in a narrow-band J filter, Jcont, which is centered at 1.2132μm. At Palomar, we used the 5m Hale telescope with the Palomar High Angular Resolution Observer (PHARO). We used the 0.025''/pixel scale, which yielded a field of view of about 25''*25''. As at Keck, we typically used a narrow-band filter in the K-band, Brγ centered at 2.18μm, to observe our targets. When a companion was detected, we usually also observed our targets in the J filter (centered at 1.246μm). At Lick, we used the 3m Shane telescope and the IR Camera for Adaptive Optics at Lick (IRCAL). With its 0.075''/pixel scale, it offered a field of view of about 19''*19''. We observed our targets with the J filter (centered at 1.238μm) or the H filter (centered at 1.656μm). Our team also carried out speckle imaging using the Differential Speckle Survey Instrument (DSSI) at Gemini North, the Wisconsin-Indiana-Yale-NOAO (WIYN) telescope, and at the Discovery Channel Telescope (DCT) from 2010 to 2015. Table5 lists the various observing dates at the three telescopes. At the 8m Gemini North telescope, 158 unique KOI host stars were observed, while at the 3.5m WIYN telescope, 681 stars were targeted. The more recent observing runs at the 4m DCT telescope covered 75 stars. Overall, at all three telescopes, the observations were directed at 828 unique KOI host stars. Targets were observed simultaneously in two bands, centered at 562nm and 692nm (both with a bandwidth of 40nm), or at 692nm and 880nm (the latter with a bandwidth of 50nm). Some targets have data in all three bands. The field of view of the speckle images is smaller than that of the AO images, about 3'' on each side, but the PSF widths are narrower (0.02''-0.05''), resulting in better spatial resolution. Some of the results on DSSI observations of KOIs can be found in Howell et al. 2011 (Cat. J/AJ/142/19), Horch et al. ( 2012AJ....144..165H, 2014ApJ...795...60H), Everett et al. (2015AJ....149...55E), and Teske et al. (2015AJ....150..144T). Wang et al. (2015ApJ...806..248W, 2015ApJ...813..130W) used the adaptive optics systems at Keck and Palomar with NIRC2 and PHARO, respectively, and typically observed each target with the J-, H-, and K-band filters. Adams et al. 2012 (Cat. J/AJ/144/42), Adams et al. (2013AJ....146....9A) and Dressing et al. (2014AJ....148...78D) mainly used the Ks filter in their AO observations at the MMT; in addition, they often used the J-band filter when a companion was detected in the Ks image. The field of view of the ARIES instrument on the MMT was 20''*20'', somewhat smaller than that of PHARO at Palomar, and the FWHM of the stellar images varied between about 0.1'' and 0.6''. Kraus et al. 2016 (Cat. J/AJ/152/8) employed adaptive optics imaging and also non-redundant aperture-mask interferometry at Keck with the NIRC2 instrument; the latter technique is limited only by the diffraction limit of the 10m Keck telescope. They used the K' filter for their observations. Baranec et al. 2016 (Cat. J/AJ/152/18) and Ziegler et al. 2016 (AJ accepted, arXiv:1605.03584) observed a sample of KOI host stars at Keck using mostly the K' filter on NIRC2. With the Robo-AO imaging at the Palomar 1.5m telescope, Law et al. 2014 (Cat. J/ApJ/791/35), Baranec et al. 2016 (Cat. J/AJ/152/18), and Ziegler et al. 2016 (AJ accepted, arXiv:1605.03584) covered a total of 3320 KOI host stars. For most observations, they used a long-pass filter whose window starts at 600nm (LP600), which is similar to the Kepler bandpass; they also took data for some stars in the Sloan i-band filter and, more rarely, Sloan r and z filters. The typical FWHM of the observed stellar PSF amounted to 0.12''-0.15''; the images covered a field of view of 44''*44''. Lillo-Box et al. (2012, Cat. J/A+A/546/A10; 2014, Cat. J/A+A/566/A103) used the 2.2m Calar Alto telescope with the AstraLux instrument to obtain diffraction-limited imaging with the lucky imaging technique, typically observing in the i- and z-band filters. This technique involves taking a very large number of short exposures and then combining only those images with the best quality (i.e., with the highest Strehl ratios). The FWHM of the stellar PSF in their 24''*24'' images was typically 0.21'', which is somewhat larger than the value from AO images (~0.15''). HST imaging using WFC3 was carried out in the F555W and F775W bands (Cartier et al. 2015ApJ...804...97C; Gilliland et al. 2015AJ....149...24G). The images spanned a relatively large field of view of 40''*40'', and the typical FWHM of the stellar PSF was 0.08''. One additional facility, the 8m Large Binocular Telescope, was used with LMIRCam to observe 24 KOI host stars in the Ks band, but results have not yet been published and are not available on CFOP. Except for 1 of these 24 stars (which has only one false positive transit signal), all have been observed with one or more other facilities too. The Kepler field was observed at the United Kingdom Infrared Telescope (UKIRT) in 2010 using the UKIRT Wide Field Camera (WFCAM). The images were taken in the J band and have a typical spatial resolution of 0.8''-0.9''. Everett et al. (2012PASP..124..316E) carried out a survey of the Kepler field in 2011 using the NOAO Mosaic-1.1 Wide Field Imager on the WIYN 0.9m telescope. They observed the field in UBV filters; the FWHM of the stellar PSF due to seeing ranged from 1.2'' to 2.5'' in the V-band (with somewhat larger values in the U and B band). The source catalog and the images are available on CFOP. (6 data files).

VizieR Online Data Catalog: Spectral Classes in the Galaxy Anticenter (Chargeishsvili, 1988)

NASA Astrophysics Data System (ADS)

Chargeishvili, K.

2014-11-01

The catalogue is compiled on the basis of the spectral data obtained with the 70-cm meniscus telescope of Abastumani Astrophysical Observatory using the 8° objective prism (dispersion 166Å/mm near Hγ; in the short-wave region, the spectrum extends up to 3500Å).The field of the meniscus telescope is 4.5x4.5°.The area of 140 square degrees, under study, was overlapped by nine centers. Kodak IIa-O, Kodak IIIa-J and Kodak IIIa-F plates were used. A limiting apparent magnitude in V for the stars is between 12.5 photographic mag. and 15.0 photographic mag. for M stars. The errors of our determinations are: ±0.6 for spectral subtype and ±0.5 for luminosity class. The catalogue contains 558 objects with peculiarities in the spectrum Ap, Am, BaII and composite spectrum stars, 86 emission stars O, B, M and objects with Hα-emission as well as 453 M and 36 C-stars.Among 558 peculiar stars an overwhelming majority, namely 549, are first found. The stars in the Catalogue are arranged in the order of increasing right ascension. The stars are numbered according to zones of 1° in declination. The printed catalogue is provided with suitable stellar charts reproduced from the Lick Catalogue. The reference system on the charts refers to 1950 epoch and it is plotted according to the Smithsonian Astrophysical Observatory (SAO) catalogue. Clusters NGC 2168, NGC 1969 and OLC 0436 Whose sites in the charts are denoted with the circles, are supplies with the charts reproduced from relatively large-scale plates taken on the meniscus telescope. (1 data file).

Searching for New Variable Stars: an Educational Project to Mine Archival Data

NASA Astrophysics Data System (ADS)

Walls, B. D.; Redmond, C. E.; Murdick, L. J.; Caton, D. B.

1998-12-01

As a Senior Seminar project,. three students were each assigned a night of images of a field containing a variable star observed under our eclipsing binary photometry program. Each field was eight arc-minutes square, with the images coming from the DFM 32-inch telescope at our Dark Sky Observatory. The exposures used a Photometrics CH250 camera with a Tektronix 1024(2) CCD and V-filter. Darks were obtained throughout the night, as well as sky flats at dusk or dawn. The fields were around the systems V442 Cas, WW Cyg, and V345 Lac. The students used Axiom Research's MIRA AP software for doing the aperture photometry, using one initial coordinates file for all of the reasonably bright stars in the field. This number varied from about 60 to almost 200 stars. The MIRA software is easy to use, with auto-centroiding and calibration built in, so it was just a matter of loading images and applying the calibration. One of the student/authors (BDW) wrote an application in Microsoft Visual BASIC to scan the output data files and produce new files, per star. These data sets were examined using PSI-Plot, to look for variability. Errors due to occasional drift led to centroiding problems, a lesson in itself! There were still some residual variations in a few stars that may be real. Follow-up observations will be made to verify these suspicions.

Observational studies of the clearing phase in proto-planetary disk systems

NASA Technical Reports Server (NTRS)

Grady, Carol A.

1994-01-01

A summary of the work completed during the first year of a 5 year program to observationally study the clearing phase of proto-planetary disks is presented. Analysis of archival and current IUE data, together with supporting optical observations has resulted in the identification of 6 new proto-planetary disk systems associated with Herbig Ae/Be stars, the evolutionary precursors of the beta Pictoris system. These systems exhibit large amplitude light and optical color variations which enable us to identify additional systems which are viewed through their circumstellar disks including a number of classical T Tauri stars. On-going IUE observations of Herbig Ae/Be and T Tauri stars with this orientation have enabled us to detect bipolar emission plausibly associated with disk winds. Preliminary circumstellar extinction studies were completed for one star, UX Ori. Intercomparison of the available sample of edge-on systems, with stars ranging from 1-6 solar masses, suggests that the signatures of accreting gas, disk winds, and bipolar flows and the prominence of a dust-scattered light contribution to the integrated light of the system decreases with decreasing IR excess.

Lepton effects on the protoneutron stars with the hadron-quark mixed phase in the Nambu-Jona-Lasinio model

DOE Office of Scientific and Technical Information (OSTI.GOV)

Yasutake, Nobutoshi; Kashiwa, Kouji

2009-02-15

We study the structures of hybrid stars with leptons at finite temperature under beta equilibrium. For the quark phase, we use the three flavor Nambu-Jona-Lasinio (NJL) model. For the hadron phase, we adopt the nuclear equation of state (EOS) by Shen et al.. This EOS is in the framework of the relativistic mean field theory including the tree body effects. For the hadron-quark phase transition, we impose the bulk Gibbs construction or the Maxwell construction to take into account uncertainties by finite-size effects. We find that the pure quark phase does not appear in stable star cores in all cases.more » With the phase transition, the maximum masses increase {approx}10% for high lepton fraction. On the contrary, without the transition, they decrease {approx}10%. We also find that, in the NJL model, the lepton fraction is more important for structures of unstable stars than the temperature. This result is important for many astrophysical phenomena such as the core collapse of massive stars.« less

Function of multiple Lis-Homology domain/WD-40 repeat-containing proteins in feed-forward transcriptional repression by silencing mediator for retinoic and thyroid receptor/nuclear receptor corepressor complexes.

PubMed

Choi, Hyo-Kyoung; Choi, Kyung-Chul; Kang, Hee-Bum; Kim, Han-Cheon; Lee, Yoo-Hyun; Haam, Seungjoo; Park, Hyoung-Gi; Yoon, Ho-Geun

2008-05-01

Lis-homology (LisH) motifs are involved in protein dimerization, and the discovery of the conserved N-terminal LisH domain in transducin beta-like protein 1 and its receptor (TBL1 and TBLR1) led us to examine the role of this domain in transcriptional repression. Here we show that multiple beta-transducin (WD-40) repeat-containing proteins interact to form oligomers in solution and that oligomerization depends on the presence of the LisH domain in each protein. Repression of transcription, as assayed using Gal4 fusion proteins, also depended on the presence of the LisH domain, suggesting that oligomerization is a prerequisite for efficient transcriptional repression. Furthermore, we show that the LisH domain is responsible for the binding to the hypoacetylated histone H4 tail and for stable chromatin targeting by the nuclear receptor corepressor complex. Mutations in conserved residues in the LisH motif of TBL1 and TBLR1 block histone binding, oligomerization, and transcriptional repression, supporting the functional importance of the LisH motif in transcriptional repression. Our results indicate that another WD-40 protein, TBL3, also preferentially binds to the N-terminal domain of TBL1 and TBLR1, and forms oligomers with other WD-40 proteins. Finally, we observed that the WD-40 proteins RbAp46 and RbAp48 of the sin3A corepressor complex failed to dimerize. We also found the specific interaction UbcH/E2 with TBL1, but not RbAp46/48. Altogether, our results thus indicate that the presence of multiple LisH/WD-40 repeat containing proteins is exclusive to nuclear receptor corepressor/ silencing mediator for retinoic and thyroid receptor complexes compared with other class 1 histone deacetylase-containing corepessor complexes.

Rapid Assessment of the Role of Microstructural Variability in the Fatigue Behavior of Structural Alloys using Ultrasonic Fatigue

DTIC Science & Technology

2007-06-23

6 %AI-2%Sn- 4 %Zr- 6 %Mo in the very high cycle regime. The microstructure is a two-phase structure with primary a grains (ap grains) in a transformed [3...aluminum [2], magnesium [3], nickel-based [ 4 ], and titanium [5,6] alloy systems. Fatigue crack initiation is known to consume the majority of fatigue...microstructural neighborhood affects this process. In fatigue studies of alpha + beta titanium alloys, [ 6 -9] cyclic deformation localization is first observed in

Falling Evaporating Bodies around Beta Pictoris

NASA Astrophysics Data System (ADS)

Beust, H.

2014-09-01

The edge-on orientation of the beta Pictoris disk as viewed from the Earth enabled the detection of its gaseous counterpart by absorption spectroscopy. This was done as early as 1985 (Vidal-Madjar et al.). Surprisingly, the detected circumstellar absorptions in Ca II, Mg II, etc... lines appeared to often present, next to a central stable component, highly time- variable additional features, Doppler shifted by a few tens, sometimes up to a few hundreds km/s. A huge sample of such features, sometimes presenting very different shapes, has been recorded since that time, especially in the last 10 years thanks to the survey by the HARPS spectrograph. Modeling work in the late 1980's led to propose that these transient spectral events could be due to star-grazing, evaporating planetesimals arising from the disk, that cross the line of sight close to periastron. The absorption components would be due to the gaseous coma around the object, and the Doppler shift to the projection of its velocity onto the line of sight. This model has been thus termed the ÓFalling Evaporating BodiesÓ (FEB) model. Detailed modeling and simulations (Beust et al. 1990, 1996; Karmann et al. 2001, 2003; Fernandez et al. 2006) helped to constrain the physics of the phenomenon and to specify the characteristics of the suspected FEBs, which number may be as large as several hundreds per year. The large number of available data enabled a statistical approach of these events and of their characteristics. It rapidly turned out that the infall of FEBs towards beta Pictoris from the disk was not isotropic. This raised the issue of the dynamical origin of this phenomenon. In the late 1990's, Beust & Morbidelli (1996, 2000) proposed that FEBs could originate from 4:1 and 3:1 mean-motion resonances with a hypothetical giant planet, and fall towards the star thanks to a drastic increase of their eccentricities thanks to the resonances. Exhaustive dynamical simulations led to propose that the suspected planet could orbit the star at ~10 AU one a moderately eccentric orbit (e~0.05-0.1). Further investigations (Beust & Valiron 2007) also depicted the possible role of FEBs in the generation of detected gas at high latitude above the disk mid-plane (Brandeker et al. 2004). The imaged planet beta Pictoris b shares many common characteristics with the FEB generating planet suspected 15 years ago. It is then tempting to merge them. A considerable effort has been done in recent years to refine the orbital determination of beta Pictoris b (Chauvin et al. 2012), and to improve the statistical analysis of the available FEB data. It has been recently shown (Kiefer et al. 2014) that two separate families of FEBs are probably present, perhaps originating from distinct resonances with the planet. A few other stars have been shown to present FEB-like spectral events that have been claimed to originate from the same phenomenon. Although none is as convincing as Beta Pictoris itself, some of them are possible analogs. The dynamical phenomenon triggering the FEB phenomenon as rather generic. A similar phenomenon is suspected to have occurred in the early ages of the Solar System, giving birth to the so-called Kirkwood gaps. But the detectability of the phenemenon from the Earth is a subtle combination of suitable stellar type, viewing geometry and age range.

The galactic reddening law - The evidence from uvby-beta photometry of B stars

NASA Astrophysics Data System (ADS)

Tobin, W.

1985-01-01

Values of interstellar reddening derived from uvby photometry of intermediate and high latitude B stars are used to test between the conflicting ideas of total galactic reddening expounded by Burstein and Heiles (1982) and de Vaucouleurs and Buta (1983). B stars are useful tracers of the galactic reddening because of their empirically and theoretically well-defined colours, and their large distances, but peculiar colours can result in an overestimate of the interstellar reddening, and Nicolet's (1982) B-star estimates of the polar reddening are too high because of this. Selection criteria are developed to exclude B stars with peculiar colours, and 72 selected B stars more than 250 pc from the galactic plane support the Burstein and Heiles zero-point of galactic reddening. The evidence of a few stars supports Burstein and Heiles' use of deep galaxy counts to provide a first-order correction for variations in the dust-to-gas ratio, but for corrections E (b - y) > 0.03 the accuracy may be less than their claimed 10%. However, the comparison of photometrically-derived values of interstellar reddening with values predicted by some model is inevitably partly subjective unless an extensive study is made of every individual star because otherwise any insufficiently red star can always plausibly be discounted as not outside all of the galactic dust, and any star that is too red can always plausibly be discounted as e.g. an undetected binary or emission-line star. The Burstein and Heiles maps are used to determine the intrinsic colours of some slightly-reddened B stars. B stars with projected rotational velocities of 250-300 km s-1 do not appear to be significantly redder than the Crawford (1978) standard relation.

Observing videos of a baby crying or smiling induces similar, but not identical, electroencephalographic responses in biological and adoptive mothers.

PubMed

Hernández-González, M; Hidalgo-Aguirre, R M; Guevara, M A; Pérez-Hernández, M; Amezcua-Gutiérrez, C

2016-02-01

It is well-known that adoptive mothers respond to cues from their babies in similar ways to biological mothers, and that cortical processing is critical for adequate motive-emotional maternal responses. This study used electroencephalographic activity (EEG) to characterize prefrontal, parietal and temporal functioning in biological mothers (BM), adoptive mothers (AM), and non-mothers (NM), while viewing videos of a baby smiling or crying. The BM presented higher absolute power (AP) in the delta and theta bands (associated with pleasant, positive emotional experiences) in the frontal and parietal areas under all conditions. In response to the smiling video, both types of mothers presented a lower AP in alpha1 in the three cortices (indicative of increased attention) and, mainly in temporal areas, a higher AP in the fast frequencies (beta and gamma, reflecting increased alertness to sensory stimuli and cognitive processing). This EEG pattern in the BM and AM could reflect the greater attention and, probably, the positive mood caused by the smiling video, showing that both are sensitive to these pleasant stimuli. When viewing the video of a baby crying, the AM had higher AP in the fast frequencies (temporal and parietal areas), indicating that they were more reactive to this unpleasant video, while the NM presented only a lower AP in alpha1 in all cortices, a finding that could be associated with the general activation induced by these unpleasant stimuli as a consequence of their lack of maternal experience. These findings should help improve our understanding of the neural mechanisms involved in the processing of sensorial stimuli that establish affective-emotional links during motherhood. Copyright © 2015 Elsevier Inc. All rights reserved.

Atmospheric Modeling And Sensor Simulation (AMASS) study

NASA Technical Reports Server (NTRS)

Parker, K. G.

1984-01-01

The capabilities of the atmospheric modeling and sensor simulation (AMASS) system were studied in order to enhance them. This system is used in processing atmospheric measurements which are utilized in the evaluation of sensor performance, conducting design-concept simulation studies, and also in the modeling of the physical and dynamical nature of atmospheric processes. The study tasks proposed in order to both enhance the AMASS system utilization and to integrate the AMASS system with other existing equipment to facilitate the analysis of data for modeling and image processing are enumerated. The following array processors were evaluated for anticipated effectiveness and/or improvements in throughput by attachment of the device to the P-e: (1) Floating Point Systems AP-120B; (2) Floating Point Systems 5000; (3) CSP, Inc. MAP-400; (4) Analogic AP500; (5) Numerix MARS-432; and (6) Star Technologies, Inc. ST-100.

UVBY beta photometry of the young southern cluster NGC3293 and comparison with other young clusters

NASA Astrophysics Data System (ADS)

Shobbrook, R. R.

1980-09-01

Stromgren uvby photometry has been obtained for 42 members and beta photometry for 37 members of the young southern galactic cluster NGC 3293. The distance modulus obtained from using Crawford's beta/M(V) calibration is 12.75 mag, corresponding to a distance of 3.55 kpc. Comparison of the colour/colour and the HR diagrams of NGC 3293 with those of the five other young northern and southern clusters reveals large differences between the clusters which may possibly be due to metal abundance variations across the Galaxy. Apparently correlated with this effect is a variation of the luminosities of the lower main sequences over about 1 mag. The fainter stars in the southern clusters appear to be an average of 0.7 mag brighter than those in the northern clusters, but it is not certain at present how much of this difference is due to possible systematic errors in the beta index zero point between the northern and southern hemispheres.

Disruption of circumstellar discs by large-scale stellar magnetic fields

NASA Astrophysics Data System (ADS)

ud-Doula, Asif; Owocki, Stanley P.; Kee, Nathaniel Dylan

2018-05-01

Spectropolarimetric surveys reveal that 8-10% of OBA stars harbor large-scale magnetic fields, but thus far no such fields have been detected in any classical Be stars. Motivated by this, we present here MHD simulations for how a pre-existing Keplerian disc - like that inferred to form from decretion of material from rapidly rotating Be stars - can be disrupted by a rotation-aligned stellar dipole field. For characteristic stellar and disc parameters of a near-critically rotating B2e star, we find that a polar surface field strength of just 10 G can significantly disrupt the disc, while a field of 100 G, near the observational upper limit inferred for most Be stars, completely destroys the disc over just a few days. Our parameter study shows that the efficacy of this magnetic disruption of a disc scales with the characteristic plasma beta (defined as the ratio between thermal and magnetic pressure) in the disc, but is surprisingly insensitive to other variations, e.g. in stellar rotation speed, or the mass loss rate of the star's radiatively driven wind. The disc disruption seen here for even a modest field strength suggests that the presumed formation of such Be discs by decretion of material from the star would likely be strongly inhibited by such fields; this provides an attractive explanation for why no large-scale fields are detected from such Be stars.