Line analysis of EUV Spectra from Molybdenum and Tungsten Injected with Impurity Pellets in LHD

NASA Astrophysics Data System (ADS)

Chowdhuri, Malay Bikas; Morita, Shigeru; Goto, Motoshi; Nishimura, Hiroaki; Nagai, Keiji; Fujioka, Shinsuke

Spectroscopic data on high-Z materials for impurity diagnostics are important due to its possible use as a plasma facing component in the next generation fusion device. For this purpose molybdenum and tungsten are injected by an impurity pellet injector into the large helical device (LHD) plasmas. Emissions from such highly ionized elements mostly fall in extreme ultraviolet (EUV) and soft X-ray ranges. The EUV spectra in a range of 20-500 Å are recorded using a flat-field EUV spectrometer. The observed emissions are identified with the help of its temporal evolution and detailed analysis is done with electron temperature profiles. At high central electron temperature (˜2.2 keV) molybdenum appears as an Al-, Mg- and Na-like ionization stages. Typical examples of identified transitions are Mo XXXI 190.46 Å (3 s2 1S-3s3p 3P) and Mo XXXII 176.63 Å (3s 2S-3p 2P). For tungsten, on the other hand, three well-separated bands appear in wavelength range of 24-80 Å. The transitions around 33 Å have been tentatively identified with the help of calculated values. Most of the isolated lines on the top of pseudo-continuum bands around 50 and 60 Å are identified, and the wavelengths are compared with previous experimental studies and also with calculated values.

[Peredo's Inferno: a Mexican physician-translator in the XIX century].

PubMed

Delgado García, Guillermo; Estañol Vidal, Bruno

2013-01-01

Manuel Peredo (1830-1890) participated fully in Mexico's national literary circles during the second half of the 19th century. Besides being recognized for his translation of Basch's Memories of Mexico, Peredo also translated the first tercets of Inferno's Canto XXXIII. Although forgotten today, his contribution is significant since it is the second Mexican translation of Dante, and particularly, the first Mexican translation of Canto XXXIII.

78 FR 59854 - Defense Federal Acquisition Regulation Supplement: Acquisitions in Support of Operations in...

Federal Register 2010, 2011, 2012, 2013, 2014

2013-09-30

...)(xxvi); 0 b. Removing paragraph (f)(xxvii) and redesignating paragraphs (f)(xxviii) through (xxxii) as.... Adding a new paragraph (f)(xxxii); and 0 e. Revising paragraphs (f)(xxxiv) and (xxxv). The revisions and... National Defense Authorization Act for Fiscal Year 2008 (Pub. L. 110-181). * * * * * (xxxii) Use the clause...

76 FR 53631 - BioPreferred Program

Federal Register 2010, 2011, 2012, 2013, 2014

2011-08-29

... title 7 of the Code of Federal Regulations (CFR) to chapter XXXII of title 7 of the CFR. DATES: This..., even though chapter XXXII of the CFR is assigned to OPPM. This direct final rule will relocate all elements of the BioPreferred Program from chapter XXIX of the CFR to chapter XXXII, as OPPM has sole...

Comparison of growth-related traits and gene expression profiles between the offspring of neomale (XX) and normal male (XY) rainbow trout.

PubMed

Kocmarek, Andrea L; Ferguson, Moira M; Danzmann, Roy G

2015-04-01

All-female lines of fish are created by crossing sex reversed (XX genotype) males with normal females. All-female lines avoid the deleterious phenotypic effects that are typical of precocious maturation in males. To determine whether all-female and mixed sex populations of rainbow trout (Oncorhynchus mykiss) differ in performance, we compared the growth and gene expression profiles in progeny groups produced by crossing a XX male and a XY male to the same five females. Body weight and length were measured in the resulting all-female (XX) and mixed sex (XX/XY) offspring groups. Microarray experiments with liver and white muscle were used to determine if the gene expression profiles of large and small XX offspring differ from those in large and small XX/XY offspring. We detected no significant differences in body length and weight between offspring groups but XX offspring were significantly less variable in the value of these traits. A large number of upregulated genes were shared between the large XX and large XX/XY offspring; the small XX and small XX/XY offspring also shared similar expression profiles. No GO category differences were seen in the liver or between the large XX and large XX/XY offspring in the muscle. The greatest differences between the small XX and small XX/XY offspring were in the genes assigned to the "small molecule metabolic process" and "cellular metabolic process" GO level 3 categories. Similarly, genes within these categories as well as the category "macromolecule metabolic process" were more highly expressed in small compared to large XX fish.

Microbiological Burden on the Surfaces of Explorer XXXIII Spacecraft1

PubMed Central

Powers, Edmund M.

1967-01-01

The Explorer XXXIII Spacecraft (Anchored Interplanetary Monitoring Platform, or AIMP) was decontaminated to prevent gross contamination of the moon with terrestrial microorganisms. Assay of the total spacecraft surface before and after decontamination showed that the decontamination procedure reduced the viable microbiological burden from 1.40 × 106 to 3.60 × 104. However, assembly of parts which were not decontaminated for engineering reasons or were not assembled under cleanroom conditions increased the viable microbial burden at the time of launch to 2.62 × 105. Images Fig. 2 PMID:6053173

A challenge for probing the statistics of interstellar magnetic fields: beyond the Planck resolution with Herschel

NASA Astrophysics Data System (ADS)

Bracco, Andrea; André, Philippe; Boulanger, Francois

2015-08-01

The recent Planck results in polarization at sub-mm wavelengths allow us to gain insight into the Galactic magnetic field topology, revealing its statistical correlation with matter, from the diffuse interstellar medium (ISM), to molecular clouds (MCs) (Planck intermediate results. XXXII, XXXIII, XXXV). This correlation has a lot to tell us about the dynamics of the turbulent ISM, stressing the importance of considering magnetic fields in the formation of structures, some of which eventually undergo gravitational collapse producing new star-forming cores.Investigating the early phases of star formation has been a fundamental scope of the Herschel Gould Belt survey collaboration (http://gouldbelt-herschel.cea.fr), which, in the last years, has thoroughly characterized, at a resolution of few tens of arcseconds, the statistics of MCs, such as their filamentary structure, kinematics and column density.Although at lower angular resolution, the Planck maps of dust emission at 353GHz, in intensity and polarization, show that all MCs are complex environments, where we observe a non-trivial correlation between the magnetic field and their density structure. This result opens new perspectives on their formation and evolution, which we have started to explore.In this talk, I will present first results of a comparative analysis of the Herschel-Planck data, where we combine the high resolution Herschel maps of some MCs of the Gould Belt with the Planck polarization data, which sample the structure of the field weighted by the density.In particular, I will discuss the large-scale envelopes of the selected MCs, and, given the correlation between magnetic field and matter, I will show how to make use of the high resolution information of the density structure provided by Herschel to investigate the statistics of interstellar magnetic fields in the Planck data.

Statistical Inference for Cultural Consensus Theory

DTIC Science & Technology

2014-02-24

Social Network Conference XXXII , Redondo Beach, California, March 2012. Agrawal, K. (Presenter), and Batchelder, W. H. Cultural Consensus Theory...Aggregating Complete Signed Graphs Under a Balance Constraint -- Part 2. International Sunbelt Social Network Conference XXXII , Redondo Beach

Natural Occurrence of Fe2SiO4 - in Shocked Umbarger l6 Chondrite

NASA Astrophysics Data System (ADS)

Xie, Z.; Sharp, T. G.

2001-12-01

Fe2SiO4 with the spinel structure was synthesized by Ringwood [1] and inferred to be important in Earth's upper mantle [1,2], but it has not previously been found in nature. Umbarger is an L6 chondrite, which contains a series of high-pressure phases: ring-woodite, akimotoite, augite and hollandite-structured plagioclase [3-6]. Transmission electron microscopy also revealed a Fe2SiO4-spinel and stishovite assem-blage in a Fe-rich zone of a melt pocket. Phyllosili-cates and glass are also associated with the Fe2SiO4-spinel, indicating post-shock aqueous glass alteration. The Fe2SiO4-spinel grains are equant to irregular, with sizes from 100 to 400 nm. Diffraction patterns can only be indexed as a spinel structure, but the unit cell is a little large (a= 8.46 Å) relative to synthetic Fe2SiO4-spinel (a=8.234 Å [1]). EDS analyses show that the spinel has a fayalite compositon with Fe/(Fe+Mg) ratio ranging from 62% to 97%. Stishovite occurs as elongated prismatic crystals up to 1 mm long and up to 100 mm wide. The alteration products in Umbarger are phyllosilicates rich in Fe and Si, with a basal layer spacing of about 9.7 Å. Crystallization of melt veins began with akimotoite and ringwoodite at pressures up to 25 GPa and ended with augite at pressure less than 18 GPa [3, 4]. Mg2SiO4-spinel and stishovite are stable in the pres-sure range from 15 GPa to 25 GPa in the enstatite-forsterite system [7], while Fe2SiO4-spinel and stishovite is stable at lower pressure. Fe2SiO4-spinel and stishovite assemblage, like that of Akimotoite plus ringwoodite, is a sub-solidus assemblage, indicating crystallization of a supercooled liquid during rapid cooling and decompression associated with shock pres-sure release. Reference: [1] Ringwood A.E. (1958) GCA,15, 18-29. [2] Irifune T. (1993) The Island Arc, 2, 55-71. [3] Xie Z. and Sharp T. G. (2000a) LPS XXXI, 2065.pdf. [4] Xie Z. and Sharp T. G. (2000b) MAPS, 35 A172. [5] Xie Z. et al.(2001) LPS XXXII, 1805.pdf. [6] Sharp T.G. (2001) LPS XXXII, 2159.pdf. [7] Gasparik T. (1992) JGR, 97, 15181-15188.

Brazil for Sale? Does Sino-Brazilian Trade or Investment Significantly Influence Brazil’s United Nations General Assembly (UNGA) Voting Pattern?

DTIC Science & Technology

2011-12-01

for Trade in Brazil? An Application of the Gravity Model. Anais do XXXI Encontro Nacional de Economia [Proceedings of the 31th Brazilian Economics...FDI Matter for Trade in Brazil? An Application of the Gravity Model. Anais do XXXI Encontro Nacional de Economia [Proceedings of the 31th

Special Issue: Annotated Bibliography for Volumes XIX-XXXII.

ERIC Educational Resources Information Center

Pullin, Richard A.

1998-01-01

This annotated bibliography lists 310 articles from the "Journal of Cooperative Education" from Volumes XIX-XXXII, 1983-1997. Annotations are presented in the order they appear in the journal; author and subject indexes are provided. (JOW)

75 FR 5071 - Mississippi L&D 21, LLC, Mississippi River No. 21 Hydropower Company Lock + TM

Federal Register 2010, 2011, 2012, 2013, 2014

2010-02-01

... Lock + \\TM\\ Hydro Friends Fund XXXII, LLC; Notice of Preliminary Permit Applications Accepted for..., Lock + TM Hydro Friends Fund XXXII, LLC (Lock + Hydro) filed an application for a preliminary permit...

77 FR 54636 - Self-Regulatory Organizations; Financial Industry Regulatory Authority, Inc.; Notice of Filing of...

Federal Register 2010, 2011, 2012, 2013, 2014

2012-09-05

...)(A)(xxxii) to mean a ``long'' and ``short'' position in different call option series, different put...)(xxxii) (renumbered as 4210(f)(2)(A)(xxvii)) that defines an OTC option as an over-the-counter option...

77 FR 33527 - Self-Regulatory Organizations; Financial Industry Regulatory Authority, Inc.; Notice of Filing of...

Federal Register 2010, 2011, 2012, 2013, 2014

2012-06-06

... definition of a spread in FINRA Rule 4210(f)(2)(A)(xxxii) to mean a ``long'' and ``short'' position in...)(2)(A)(xxxii) (renumbered as 4210(f)(2)(A)(xxvii)) that defines an OTC option as an over-the-counter...

Terrestrial microbes in martian and chondritic meteorites

NASA Astrophysics Data System (ADS)

Airieau, S.; Piceno, Y.; Andersen, G.

2007-08-01

Good extraterrestrial analogs for microbiology are SNC meteorites as Mars analogs, and chondrites as early planet analogs. Chondrites and SNCs are used to trace processes in the early solar system and on Mars. Yet, questions about terrestrial contamination and its effects on the isotopic, chemical and mineral characteristics often arise. A wide biodiversity was found in 21 chondrites of groups CR, CV, CK, CO from ANSMET, CI and CM Falls, and 8 SNCs. Studies documented the alteration of meteorites by weathering and biology [1]-[6], and during aqueous extraction for oxygen isotopic analysis [7], visible biofilms grew in the meteorite solutions in days. To assess biological isotopic and chemical impacts, cultures were incubated 11 months and analyzed by PCR. The sequences for 2 isolates from EET 87770 and Leoville were of a good quality with long sequence reads. In EET 87770, the closest matches were in the genus Microbacterium. Soil and plant isolates were close relatives by sequence comparison. Bacillus, a common soil bacterial genus, grew in a Leoville culture. All SNCs exhibited biological activity measured independently by LAL but only 1 colony was successfully cultured from grains of the SNC Los Angeles. Isotopic analyses of samples with various amounts of microbial contamination could help quantified isotopic impact of microbes on protoplanetary chemistry in these rocks. References: [1] Gounelle, M.& Zolensky M. (2001) LPS XXXII, Abstract #999. [2] Fries, M. et al. (2005) Meteoritical Society Meeting 68, Abstract # 5201. [3] Burckle, L. H. & Delaney, J. S (1999) Meteoritics & Planet. Sci., 32, 475. [4] Whitby, C. et al. (2000) LPS XXXI, Abstract #1732. [5] Tyra M. et al., (2007) Geochim. Cosmochim. Acta, 71, 782 [6] Toporski, J. & Steele A., (2007) Astrobiology, 7, 389 [7]Airieau, S. et al (2005) Geochim. Cosmochim. Acta, 69, 4166.

Energy levels and life times calculations of Mo XXXI

NASA Astrophysics Data System (ADS)

Wajid, Abdul; Jabeen, S.; Husain, Abid

2018-05-01

Fine-structure energy levels belonging to 2p63s2, 2p63s3p, 2p63p2 and 2p63p3d for Mo XXXI have been calculated using the multi-configuration Dirac-Fock method including Quantum electrodynamics (QED) corrections. Most of our calculations of energy levels show good agreement with experimental data available on NIST. Lifetimes for excited levels have also been calculated.

XX/XY Sex Chromosomes in the South American Dwarf Gecko (Gonatodes humeralis).

PubMed

Gamble, Tony; McKenna, Erin; Meyer, Wyatt; Nielsen, Stuart V; Pinto, Brendan J; Scantlebury, Daniel P; Higham, Timothy E

2018-05-11

Sex-specific genetic markers identified using restriction site-associated DNA sequencing, or RADseq, permits the recognition of a species' sex chromosome system in cases where standard cytogenetic methods fail. Thus, species with male-specific RAD markers have an XX/XY sex chromosome system (male heterogamety) while species with female-specific RAD markers have a ZZ/ZW sex chromosome (female heterogamety). Here, we use RADseq data from 5 male and 5 female South American dwarf geckos (Gonatodes humeralis) to identify an XX/XY sex chromosome system. This is the first confidently known sex chromosome system in a Gonatodes species. We used a low-coverage de novo G. humeralis genome assembly to design PCR primers to validate the male-specificity of a subset of the sex-specific RADseq markers and describe how even modest genome assemblies can facilitate the design of sex-specific PCR primers in species with diverse sex chromosome systems.

48,XXYY, 48,XXXY and 49,XXXXY syndromes: not just variants of Klinefelter syndrome

PubMed Central

Tartaglia, Nicole; Ayari, Natalie; Howell, Susan; D’Epagnier, Cheryl; Zeitler, Philip

2012-01-01

Sex chromosome tetrasomy and pentasomy conditions occur in 1:18 000–1:100 000 male births. While often compared with 47,XXY/Klinefelter syndrome because of shared features including tall stature and hypergonadotropic hypogonadism, 48,XXYY, 48,XXXY and 49,XXXXY syndromes are associated with additional physical findings, congenital malformations, medical problems and psychological features. While the spectrum of cognitive abilities extends much higher than originally described, developmental delays, cognitive impairments and behavioural disorders are common and require strong treatment plans. Future research should focus on genotype–phenotype relationships and the development of evidence-based treatments. Conclusion The more complex physical, medical and psychological phenotypes of 48,XXYY, 48,XXXY and 49,XXXXY syndromes make distinction from 47,XXY important; however, all of these conditions share features of hypergonadotropic hypogonadism and the need for increased awareness, biomedical research and the development of evidence-based treatments. PMID:21342258

Recidivous offence in sadistic homosexual pedophile with karyotype 48, XXXY after testicular pulpectomy. A case report.

PubMed

Lachman, M; Brzek, A; Mellan, J; Hampl, R; Starka, L; Motlik, K

1991-01-01

The case of recidivous sexual offender with genetically caused mental retardation and primary hypogonadism (Klinefelter's syndrome with karyotype 48, XXXY) is described. He was examined after sadistic abuse of a boy aged 13 that he had committed 19 years after performed testicular pulpectomy. Plasmatic level of testosterone was found 4x higher than mean level in men after orchidectomy. Histological examination of residual scrotal tissues proved that the source of androgens were hyperplastic nodules of extratesticular Leydig cells.

Tabulation of comet observations.

NASA Astrophysics Data System (ADS)

1993-01-01

Concerning comets: 1973 XII Kohoutek, 1975 IX Kobayashi-Berger-Milon, 1976 VI West, 1976 XI P/d'Arrest, 1977 XIV Kohler, 1979 X Bradfield, 1980 X P/Stephan-Oterma, 1980 XV Bradfield, 1981 II Panther, 1982 VI Austin, 1983 V Sugano-Saigusa-Fujikawa, 1983 VII IRAS-Araki-Alcock, 1983 XIII P/Kopff, 1984 XIII Austin, 1984 XXIII Levy-Rudenko, 1985 XIII P/Giacobini-Zinner, 1985 XVII Hartley-Good, 1985 XIX Thiele, 1986 I P/Boethin, 1986 III P/Halley, 1986 XVIII Terasako, 1987 II Sorrells, 1987 III Nishikawa-Takamizawa-Tago, 1987 X P/Grigg-Skjellerup, 1987 XXIII Rudenko, 1987 XXIX Bradfield, 1987 XXXII McNaught, 1987 XXXIII P/Borrelly, 1988 IV Furuyama, 1988 V Liller, 1988 XIV P/Tempel 2, 1988 XV Machholz, 1988 XX Yanaka, 1988 XXIV Yanaka, 1989 X P/Brorsen-Metcalf, 1989 XV P/Schwassmann-Wachmann 1, 1989 XIX Okazaki-Levy-Rudenko, 1989 XXI Helin-Roman-Alu, 1989 XXII Aarseth-Brewington, 1990 III Černis-Kiuchi-Nakamura, 1990 VI Skorichenko-George, 1990 VIII P/Schwassmann-Wachmann 3, 1990 IX P/Peters-Hartley, 1990 X P/Wild 4, 1990 XIV P/Honda Mrkos-Pajdušáková, 1990 XVII Tsuchiya-Kiuchi, 1990 XXI P/Encke, 1990 XXVI Arai, 1991 XI P/Levy, 1991 XV P/Hartley 2, 1991 XVI P/Wirtanen, 1991 XVII P/Arend-Rigaux, 1991 XXI P/Faye, 1991 XXIII P/Shoemaker 1, 1991 XXIV Shoemaker-Levy, 1991l Helin-Lawrence, 1991ο P/Chernykh, 1991r Helin-Alu, 1991a1 Shoemaker-Levy, 1991g1 Zanotta-Brewington, 1991h1 Mueller, 1912d Tanaka-Machholz, 1992f P/Shoemaker-Levy 8, 1992k Machholz, 1992l P/Giclas, 1992p P/Brewington, 1992q Helin-Lawrence, 1992s P/Ciffréo, 1992t P/Swift-Tuttle, 1992u P/Väisälä, 1992x P/Schaumasse, 1992y Shoemaker, 1992a1 Ohshita, 1993a Mueller, P/Smirnova-Chernykh.

Slope Gullies on Devon Island, Canadian Arctic: Possible Analogs for Gullies on Mars and Evidence for Recent Transient Environmental Change on Mars.

NASA Astrophysics Data System (ADS)

Lee, P.

2002-12-01

The origin and evolution of the relatively youthful slope gully features on Mars first reported by Malin and Edgett (2000) remain enigmatic. Two prevailing hypotheses concerning their formation involve the discharge of subsurface H2O at the gully sites: groundwater seepage (1) and/or the melting of ground-ice (2, 3). In the course of geologic field investigations on Devon Island, Canadian Arctic, we have identified morphologic and contextual analogs for the martian gullies that result from a radically different mechanism of formation (4). The gullies on Devon result mainly from the episodic melting of transient surface snow and ice deposits, with little contribution from subsurface H2O reservoirs. Timescales for gully formation on Devon Island are ­š104 years (5). The gullies on Devon suggest that the formation of gully features on Mars might not necessarily have involved discharges of subsurface H2O at the gully sites. Instead, gullies on Mars might be the result of transient surface snow and ice melting, which in turn might be the result of short-term changes in regional surface environmental conditions (on time-scales of ­š105-108 years?) possibly in association with high obliquity-induced climate change (6, 7) and/or volcanic activity. Acknowledgements: This research was conducted under the auspices of the NASA Haughton-Mars Project (HMP) with support from NASA and the National Geographic Society. References: (1) Malin, M. C. and K. S. Edgett 2000. Science 288, 2330-2335. (2) Mellon, M. T. and R. J. Phillips 2001. J. Geophys. Res. 106, 23165-23179. (3) Costard, F. et al. 2002. Science 295, 110-112. (4) Lee, P. et al. 2001. LPSC. XXXII, Houston, TX, Mar 12-16, 2001. (5) Lee, P, et al. 2002. LPSC XXXIII, Houston, TX, Mar 11-15, 2002. (6) Ward, W. R. (1973) Science 181, 260-262. (7) Touma, J. and J. Wisdom (1993) Science 259, 1294-1296.

33 CFR 67.50-25 - Eighth Coast Guard District.

Code of Federal Regulations, 2010 CFR

2010-07-01

... 27°00′ N., longitude 97°17′.5 W., thence to; (xxxii) A point at latitude 26°04′.1 N., longitude 97°08... Lat. 29°45′.6 N., Long. 93°13′.7 W., thence to; (xxxii) A point at Lat. 29°45′.6 N., Long. 93°17′.3 W...

Excitation rates for transitions in Kr XXXII

NASA Astrophysics Data System (ADS)

Aggarwal, K. M.; Keenan, F. P.; Lawson, K. D.

2009-04-01

In this paper we report our results for collision strengths and effective collision strengths for transitions among the lowest 125 levels of the 2s22p, 2s2p2, 2p3, 2s23ell, 2s2p3ell, and 2p23ell configurations of Kr XXXII. For our calculations both the FAC and DARC codes have been employed.

Channel-specific dielectronic recombination of Ge(XXXII), Se(XXXIV), and Kr(XXXVI)

NASA Astrophysics Data System (ADS)

El Machtoub, G.

2004-04-01

We present explicit calculations of channel-specific dielectronic recombination cross sections for hydrogen-like germanium, Ge(XXXII); selenium, Se(XXXIV); and krypton, Kr(XXXVI). The convoluted cross sections characterize K-shell emission spectra over a wide energy range where contributions from high-n (n = 2-10), satellite lines are included. The high-n contributions presented are important for better diagnostics in the domain of high-temperature plasmas.

21 CFR 177.1350 - Ethylene-vinyl acetate copolymers.

Code of Federal Regulations, 2013 CFR

2013-04-01

...), (xxvii), (xxx), and (xxxiii) of this chapter, and colorants used in accordance with § 178.3297 of this... (xxx) of this chapter and colorants for polymers used in accordance with the provisions of § 178.3297...

21 CFR 177.1350 - Ethylene-vinyl acetate copolymers.

Code of Federal Regulations, 2011 CFR

2011-04-01

...), (xxvii), (xxx), and (xxxiii) of this chapter, and colorants used in accordance with § 178.3297 of this... (xxx) of this chapter and colorants for polymers used in accordance with the provisions of § 178.3297...

21 CFR 177.1350 - Ethylene-vinyl acetate copolymers.

Code of Federal Regulations, 2012 CFR

2012-04-01

...), (xxvii), (xxx), and (xxxiii) of this chapter, and colorants used in accordance with § 178.3297 of this... (xxx) of this chapter and colorants for polymers used in accordance with the provisions of § 178.3297...

Homeland Security is Hometown Security: Comparison and Case Studies of Vertically Synchronized Catastrophe Response Plans

DTIC Science & Technology

2015-09-01

with her, in person, but I know I have in spirit. ii THIS PAGE INTENTIONALLY LEFT BLANK 1 I. INTRODUCTION A. BACKGROUND Catastrophe...Roosevelt, XXXII President of the United States: 1933–1945. 52—Executive Order 8757 Establishing the Office of Civilian Defense. May 20, 1941,” American...www.dhs.gov/xlibrary/assets/presidential-policy- directive-8-national-preparedness.pdf. Woolley, John, and Gerhard Peters. “Franklin D. Roosevelt, XXXII

42 CFR 88.1 - Definitions.

Code of Federal Regulations, 2011 CFR

2011-10-01

... RELATED ACTIVITIES WORLD TRADE CENTER HEALTH PROGRAM § 88.1 Definitions. Act means the Title XXXIII of the..., or a WTC-related health condition or a health condition medically associated with a WTC-related... medicine, environmental medicine, trauma-related psychiatry and psychology, and social services counseling...

42 CFR 88.1 - Definitions.

Code of Federal Regulations, 2012 CFR

2012-10-01

... RELATED ACTIVITIES WORLD TRADE CENTER HEALTH PROGRAM § 88.1 Definitions. Act means the Title XXXIII of the..., or a WTC-related health condition or a health condition medically associated with a WTC-related... medicine, environmental medicine, trauma-related psychiatry and psychology, and social services counseling...

Tabulation of comet observations.

NASA Astrophysics Data System (ADS)

1991-07-01

Concerning comets: 1957 III Arend-Roland, 1957 V Mrkos, 1958 III Burnham, 1959 III Bester-Hoffmeister, 1959 VI Alcock, 1959 VIII P/Giacobini-Zinner, 1960 I P/Wild 1, 1960 II Burnham, 1960 III P/Schaumasse, 1960 VIII P/Finlay, 1961 V Wilson-Hubbard, 1961 VIII Seki, 1962 III Seki-Lines, 1962 VIII Humason, 1963 I Ikeya, 1963 III Alcock, 1963 V Pereyra, 1964 VI Tomita-Gerber-Honda, 1964 VIII Ikeya, 1964 IX Everhart, 1979 X Bradfield, 1980 X P/Stephan-Oterma, 1980 XII Meier, 1980 XIII P/Tuttle, 1981 II Panther, 1982 I Bowell, 1982 IV P/Grigg-Skjellerup, 1982 VII P/d'Arrest, 1986 III P/Halley, 1987 IV Shoemaker, 1987 XII P/Hartley 3, 1987 XIX P/Schwassmann-Wachmann 2, 1987 XXIX Bradfield, 1987 XXX Levy, 1987 XXXII McNaught, 1987 XXXIII P/Borrelly, 1987 XXXVI P/Parker-Hartley, 1987 XXXVII P/Helin- Roman-Alu 1, 1988 III Shoemaker-Holt, 1988 V Liller, 1988 VIII P/Ge-Wang, 1988 XI P/Shoemaker-Holt 2, 1988 XIV P/Tempel 2, 1988 XV Machholz, 1988 XX Yanaka, 1988 XXI Shoemaker, 1988 XXIV Yanaka, 1989 III Shoemaker, 1989 V Shoemaker-Holt-Rodriquez, 1989 VIII P/Pons-Winnecke, 1989 X P/Brorsen-Metcalf, 1989 XI P/Gunn, 1989 XIII P/Lovas 1, 1989 XVIII McKenzie-Russell, 1989 XIX Okazaki-Levy-Rudenko, 1989 XX P/Clark, 1989 XXI Helin-Ronan-Alu, 1989 XXII Aarseth-Brewington, 1989h P/Van Biesbroeck, 1989t P/Wild 2, 1989u P/Kearns-Kwee, 1989c1 Austin, 1989e1 Skorichenko-George, 1990a P/Wild 4, 1990b Černis-Kiuchi-Nakamura, 1990c Levy, 1990e P/Wolf-Harrington, 1990f P/Honda-Mrkos-Pajdušáková, 1990g McNaught-Hughes, 1990i Tsuchiya-Kiuchi, 1990n P/Taylor, 1990ο P/Shoemaker-Levy 1, 1991a P/Metcalf-Brewington, 1991b Arai, 1991c P/Swift-Gehrels, 1991d Shoemaker-Levy, 1991e P/Shoemaker-Levy 3, 1991h P/Takamizawa, 1991j P/Hartley 1, 1991k P/Mrkos, 1991l Helin-Lawrence, 1991n P/Faye, 1991q P/Levy, 1991t P/Hartley 2, P/Encke, P/Schwassmann-Wachmann 1.

The WIYN Open Cluster Study: A 15-Year Report

NASA Astrophysics Data System (ADS)

Mathieu, Robert D.; WOCS Collaboration

2013-06-01

The WIYN 3.5m telescope combines large aperture, wide field of view and superb image quality. The WIYN consortium includes investigators in numerous areas of open cluster research. The combination spawned the WIYN Open Cluster Study (WOCS) over a decade ago, with the goals of producing 1) comprehensive photometric, astrometric and spectroscopic data for new fundamental open clusters and 2) addressing key astrophysical problems with these data. The set of core WOCS open clusters spans age and metallicity. Low reddening, solar proximity and richness were also desirable features in selecting core open clusters. More than 50 WIYN Open Cluster Study papers have been published in refereed journals. Highlights include: deep and wide-field photometry of NGC 188, NGC 2168 (M35), and NGC 6819 (WOCS I, II, XI and LII); deep and wide-field proper-motion studies of the old open clusters NGC 188, NGC 2682 (M67) and NGC 6791 (WOCS XVII, XXXIII and XLVI); comprehensive radial-velocity surveys of NGC 188, NGC 2168 and NGC 6819 (WOCS XXXII, XXIV, and XXXVIII); metallicity and lithium abundances in NGC 2168 (WOCS V); comprehensive definition of the hard-binary populations of NGC 188 and NGC 2168 (WOCS XXII and XLVIII); rotation period distributions in NGC 1039 (M34) and NGC 2168 (WOCS XXXV, XLIII, and XLV); study of chromospheric activity in NGC 2682 (WOCS XVIII); photometric variability surveys in NGC 188 and NGC 2682 (IX and XV); new Bayesian techniques for determination of cluster parameters (WOCS XXIII); a new infrared age-diagnostic for open clusters (WOCS XL); theoretical studies of stellar rotation (WOCS XIII and XIV); sophisticated N-body simulations of NGC 188 (WOCS LI); and the discovery of a high binary frequency and white dwarf companions among NGC 188 blue stragglers. While the WIYN 3.5m telescope remains at its heart, today the WIYN Open Cluster Study collaboration extends beyond both the WIYN observatory and consortium, and continues as a vital and productive exploration into these fundamental stellar systems. Publication list can be found at http://www.astro.ufl.edu ata/wocs/pubs.html. The WIYN Open Cluster Study has been continuously supported by grants from the National Science Foundation.

Change of the heterogametic sex from male to female in the frog.

PubMed Central

Ogata, M; Ohtani, H; Igarashi, T; Hasegawa, Y; Ichikawa, Y; Miura, I

2003-01-01

Two different types of sex chromosomes, XX/XY and ZZ/ZW, exist in the Japanese frog Rana rugosa. They are separated in two local forms that share a common origin in hybridization between the other two forms (West Japan and Kanto) with male heterogametic sex determination and homomorphic sex chromosomes. In this study, to find out how the different types of sex chromosomes differentiated, particularly the evolutionary reason for the heterogametic sex change from male to female, we performed artificial crossings between the West Japan and Kanto forms and mitochondrial 12S rRNA gene sequence analysis. The crossing results showed male bias using mother frogs with West Japan cytoplasm and female bias using those with Kanto cytoplasm. The mitochondrial genes of ZZ/ZW and XX/XY forms, respectively, were similar in sequence to those of the West Japan and Kanto forms. These results suggest that in the primary ZZ/ZW form, the West Japan strain was maternal and thus male bias was caused by the introgression of the Kanto strain while in the primary XX/XY form and vice versa. We therefore hypothesize that sex ratio bias according to the maternal origin of the hybrid population was a trigger for the sex chromosome differentiation and the change of heterogametic sex. PMID:12807781

Lunar and Planetary Science XXXIII

NASA Technical Reports Server (NTRS)

2002-01-01

This CD-ROM publication contains the extended abstracts that were accepted for presentation at the 33rd Lunar and Planetary Science Conference held in Houston, TX, March 11-15, 2002. The papers are presented in PDF format and are indexed by author, keyword, meteorite, program and samples for quick reference.

Thiokol 260-SL Nozzle Development Program

DTIC Science & Technology

1967-01-01

Pigure 1 Candidate Throat Inserts ............................ 7 2 Laminate Temperature versus Coating Thickness for Selectron 5003 Specimens...32 Photo Cross Adhesive Pattern ....................... 111 33 Photo Parallel Adhesive Pattern ..................... 112 34 Adhesive Applicator Teeth ...Ablative Material .... 88 XXXIII Task 9: Corlar Coating of Graphite Materials Throat, IS 11004-01-02, 156-ZC-1 ............ ....... 90 XXXIV Adapter

[Contribution to the study of Microphallidae Travassos 1920 (trematoda). XXXII. Microphallus breviatus n. sp., a species with an abbreviated evolutive cycle from a Mediterranean pond in the Languedoc].

PubMed

Deblock, S; Maillard, C

1975-01-01

Contribution to the study of Microphallidae Travassos, 1920 (Trematoda). XXXII. - Microphallus breviatus n. sp., a short life-cycle species of a mediterranean pond of Languedoc. The whole larval life-cycle of M. breviatus takes place in one host, Hydrobia ventrosa (Montagu), Mollusc Hydrobiidae. Hepato-pancreatic sporocysts produce morphologically altered xiphidio-cercariae which become encysted metacercariae in the sporocyts themselves. This species is defined in the genus by the anatomic characteristics of its cercariae and metacercariae, allied with its uncommon biology including two hosts only.

Cytogenetics of the Brazilian whiptail lizard Cnemidophorus littoralis (Teiidae) from a restinga area (Barra de Maricá) in Southeastern Brazil.

PubMed

Peccinini-Seale, D; Rocha, C F D; Almeida, T M B; Araújo, A F B; De Sena, M A

2004-08-01

Chromosomes of Cnemidophorus littoralis, a new species of teiid lizard recently described, were studied. The animals are from a restinga area in Barra de Maricá, RJ. The karyotype presents a diploid number of 2n = 46 chromosomes and a chromosomal sex determination mechanism of the type XX:XY. Nucleolar organizer regions, Ag-NORs, are at the sixth pair of chromosomes; there is variability of size and number of the Ag-stained nucleoli on the 50 interphase nuclei for each specimen analyzed. These nucleoli are related to NOR patterns that also demonstrated variability in size and number. This paper presents the first description of the karyotype of Cnemidophorus littoralis and of a chromosomal sex determination mechanism of the XX:XY type in the genus Cnemidophorus from Southeastern Brazil.

Processing of A New Digital Orthoimage Map of The Martian Western Hemisphere Using Data Obtained From The Mars Orbiter Camera At A Resolution of 256 Pixel/deg

NASA Astrophysics Data System (ADS)

Wählisch, M.; Niedermaier, G.; van Gasselt, S.; Scholten, F.; Wewel, F.; Roatsch, T.; Matz, K.-D.; Jaumann, R.

We present a new digital orthoimage map of Mars using data obtained from the CCD line scanner Mars Orbiter Camera (MOC) of the Mars Global Surveyor Mis- sion (MGS) [1,2]. The map covers the Mars surface from 0 to 180 West and from 60 South to 60 North with the MDIM2 resolution of 256 pixel/degree and size. Image data processing has been performed using multiple programs, developed by DLR, Technical University of Berlin [3], JPL, and the USGS. 4,339 Context and 183 Geodesy images [2] were included. After radiometric corrections, the images were Mars referenced [4], geometrically corrected [5] and orthoprojected using a global Martian Digital Terrain Model (DTM) with a resolution of 64 pixel/degree, developed at DLR and based on MGS Mars Orbiter Laser Altimeter (MOLA) data [6]. To elim- inate major differences in brightness between the individual images of the mosaics, high- and low-pass filter processing techniques were applied for each image. After filtering, the images were mosaicked without registering or using block adjustment techniques in order to improve the geometric quality. It turns out that the accuracy of the navigation data has such a good quality that the orthoimages fit very well to each other. When merging the MOC mosaic with the MOLA data using IHS- trans- formation, we recognized very good correspondence between these two datasets. We create a topographic image map of the Coprates region (MC­18) adding contour lines derived from the global DTM to the mosaic. These maps are used for geological and morphological interpretations in order to review and improve our current Viking-based knowledge about the Martian surface. References: [1] www.mssss.com, [2] Caplinger, M. and M. Malin, "The Mars Or- biter Camera Geodesy Campaign, JGR, in press, [3] Scholten, F., Vol XXXI, Part B2, Wien 1996, p.351-356, [4] naïf.jpl.nasa.gov, [5] R.L.Kirk. et al. (2001), "Geometric Calibration of the Mars Orbiter Cameras and Coalignment with Mars Orbiter Laser Altimeter", LPSC XXXII, [6] wufs.wustl.edu

Comparative anatomy of the female genitalia of generic-level taxa in tribe Aedini (Diptera: Culicidae). Part XXXIII. Genus Lewnielsenius Reinert, Harbach and Kitching

USDA-ARS?s Scientific Manuscript database

A morphological analysis of the female genitalia of the species included in genus Lewnielsenius Reinert, Harbach and Kitching was conducted. The genitalia of the type species of the genus, Ln. muelleri (Dyar), are illustrated. Treatment of the genital morphology of the genus includes a detailed de...

The autopsy was conducted "Under most inauspicious circumstances:" John Turner, Harvey Cushing's case XXXII, and his unwitting contributions to the early understanding of acromegaly.

PubMed

Pendleton, Courtney; Wand, Gary; Quinones-Hinojosa, Alfredo

2010-12-01

Harvey Cushing's monograph The Pituitary Body and Its Disorders describes Case XXXII, a 36-year-old man who presented with gigantism in 1910. The detailed post-mortem exam findings are prefaced with a cryptic statement, describing "inauspicious circumstances" surrounding the autopsy. Although contemporary biographies of Cushing have offered insight into these circumstances, the original surgical file for Case XXXII has not been previously reviewed. The original Johns Hopkins Hospital surgical records were reviewed, and the case of John Turner, who Cushing identified by name in his monograph The Pituitary Body and Its Disorders, was selected for further review. A review of the original surgical file revealed a typewritten note by Dr. Crowe, one of the surgeons who performed the post-mortem exam, with a handwritten addendum by Dr. Cushing. This document provides detail regarding the "inauspicious circumstances" surrounding the autopsy. Namely, the autopsy was conducted without permission of the family, during the funeral service, following a payment to the undertaker. The new information regarding the autopsy of John Turner offers insight into the previously incompletely described circumstances surrounding the autopsy. Additionally, the case illuminates the obligations and ethical quandaries that physician-scientists face.

Social Function in Multiple X and Y Chromosome Disorders: XXY, XYY, XXYY, XXXY

PubMed Central

Visootsak, Jeannie; Graham, John M.

2014-01-01

Klinefelter syndrome (47,XXY) was initially described in the context of its endocrinologic and physical features; however, subsequent studies have revealed specific impairments in verbal skills and social functioning. Males with sex chromosomal aneuploidies are known to have variability in their developmental profile with the majority presenting with expressive language deficits. As a consequence of language delays, they have an increased likelihood of language-based learning disabilities and social-emotional problems that may persist through adulthood. Studies on males with 47,XXY have revealed unique behavioral and social profiles with possible vulnerability to autistic traits. The prevalence of males with more than one extra sex chromosome (e.g., 48,XXYY and 48,XXXY) and an additional Y (e.g., 47,XYY) is less common, but it is important to understand their social functioning as it provides insight into treatment implications. PMID:20014367

Federal Funds for Research and Development: Fiscal Years 1983, 1984, and 1985. Volume XXXIII. Detailed Statistical Tables. Surveys of Science Resources Series.

ERIC Educational Resources Information Center

National Science Foundation, Washington, DC. Div. of Science Resources Studies.

Detailed statistical tables showing the funding levels of 92 federal agencies for research and development (R&D) are provided in this document. These tables are organized into the following sections: research, development, and R&D plant; R&D agency, character of work, and performer; total basic and applied applied research--agency,…

The eXtroardinarY Babies Study: Natural History of Health and Neurodevelopment in Infants and Young Children With Sex Chromosome Trisomy

ClinicalTrials.gov

2018-01-10

Klinefelter Syndrome; Trisomy X; XYY Syndrome; XXXY and XXXXY Syndrome; Xxyy Syndrome; Xyyy Syndrome; Xxxx Syndrome; Xxxxx Syndrome; Xxxyy Syndrome; Xxyyy Syndrome; Xyyyy Syndrome; Male With Sex Chromosome Mosaicism

Naval Research Reviews. Volume XXXIII. Number 2,

DTIC Science & Technology

1981-01-01

and filler metal addition. ratio weld is a characteristic of a keyhole -produced The most distinctive feature of LB welding , weld . T /h III laser Ii...evolved from these radiation for precision operation, such as hole-drill- efforts include a 3kW CO. laser /workstation system ing, trimming, and welding ...asso- Laser Surface Modifications ciated with thick-section welding of naval structure and surface modification for improved corrosion and The high

XX/XY System of Sex Determination in the Geophilomorph Centipede Strigamia maritima

PubMed Central

Green, Jack E.; Dalíková, Martina; Sahara, Ken; Marec, František; Akam, Michael

2016-01-01

We show that the geophilomorph centipede Strigamia maritima possesses an XX/XY system of sex chromosomes, with males being the heterogametic sex. This is, to our knowledge, the first report of sex chromosomes in any geophilomorph centipede. Using the recently assembled Strigamia genome sequence, we identified a set of scaffolds differentially represented in male and female DNA sequence. Using quantitative real-time PCR, we confirmed that three candidate X chromosome-derived scaffolds are present at approximately twice the copy number in females as in males. Furthermore, we confirmed that six candidate Y chromosome-derived scaffolds contain male-specific sequences. Finally, using this molecular information, we designed an X chromosome-specific DNA probe and performed fluorescent in situ hybridization against mitotic and meiotic chromosome spreads to identify the Strigamia XY sex-chromosome pair cytologically. We found that the X and Y chromosomes are recognizably different in size during the early pachytene stage of meiosis, and exhibit incomplete and delayed pairing. PMID:26919730

A Rare Case of Klinefelter Syndrome Patient with Quintuple Mosaic Karyotype, Diagnosed by GTG-Banding and FISH

PubMed Central

Karimi, Hamideh; Sabbaghian, Marjan; Haratian, Kaveh; Vaziri Nasab, Hamed; Farrahi, Faramarz; Moradi, Shabnam Zari; Tavakolzadeh, Tayebeh; Beheshti, Zahra; Gourabi, Hamid; Meybodi, Anahita Mohseni

2014-01-01

Klinefelter syndrome (KS) is the most common sex chromosomal disorder in men. Most of these patients show the 47,XXY karyotype, whereas approximately 15% of them are mosaics with variable phenotype. A 39-year-old male investigated for primary infertility, was clinically normal with small firm testes and elevated levels of FSH, LH and low level of testosterone. Total azoospermia was confirmed on semen analysis. Testicular histopathology revealed no spermatogenesis and absence of germ cells. Karyotype from whole blood culture showed cells with 47,XXY/46,XX/ 45,X/48,XXXY/ 46,XY mosaicism. The predominant cell line was 47,XXY (83.67%). This was confirmed by fluorescence in situ hybridization (FISH). Also the presence of a small population of cells with the 48,XXXY and 45,X karyotypes was detected by FISH. This case illustrates the utility of FISH as an adjunct to conventional cytogenetics in assess the chromosome copy number in each cell line of a mosaic. PMID:25083188

A Rare Case of Klinefelter Syndrome Patient with Quintuple Mosaic Karyotype, Diagnosed by GTG-Banding and FISH.

PubMed

Karimi, Hamideh; Sabbaghian, Marjan; Haratian, Kaveh; Vaziri Nasab, Hamed; Farrahi, Faramarz; Moradi, Shabnam Zari; Tavakolzadeh, Tayebeh; Beheshti, Zahra; Gourabi, Hamid; Meybodi, Anahita Mohseni

2014-07-01

Klinefelter syndrome (KS) is the most common sex chromosomal disorder in men. Most of these patients show the 47,XXY karyotype, whereas approximately 15% of them are mosaics with variable phenotype. A 39-year-old male investigated for primary infertility, was clinically normal with small firm testes and elevated levels of FSH, LH and low level of testosterone. Total azoospermia was confirmed on semen analysis. Testicular histopathology revealed no spermatogenesis and absence of germ cells. Karyotype from whole blood culture showed cells with 47,XXY/46,XX/ 45,X/48,XXXY/ 46,XY mosaicism. The predominant cell line was 47,XXY (83.67%). This was confirmed by fluorescence in situ hybridization (FISH). Also the presence of a small population of cells with the 48,XXXY and 45,X karyotypes was detected by FISH. This case illustrates the utility of FISH as an adjunct to conventional cytogenetics in assess the chromosome copy number in each cell line of a mosaic.

Semiconductor Electrodes. XXXIII. Photoelectrochemistry of n-Type WSe2 in Acetonitrile.

DTIC Science & Technology

1981-01-06

with an E. G. & G. (Salem, Mass.) Model 550 radio - imeter/photometer and a Scientech 361 power meter. RESULTS Capacitance measurements and cyclic...H. Gerischer, C. Clemen , and E. Bucher, Ber. Bunsenges. Phys. Chem., 83, 655 (1979); (g) J. Gobrecht, H. Gerischer, and H. Tributsch, J. Electrochem...Charleston Road Cleveland, Ohio 41135 1 Mountain View, California 94040 H Dr. B. Brummer Dr. P. P. Schmidt EIC Incorporated Department of Cheristry 55 Chapel

Preface

NASA Astrophysics Data System (ADS)

Barnes, Austin J.; Schmitt, Michael

2015-06-01

EUCMOS XXXII, the 32nd European Congress on Molecular Spectroscopy, was held during August 24-29, 2014, at the Heinrich-Heine University, Düsseldorf, Germany. The meeting was organised by the Institute of Physical Chemistry of the Heinrich-Heine University.

A Topographic Image Map of The Mc-18 Quadrangle "coprates" At 1: 2,000,000 Using Data Obtained From The Mars Orbiter Camera and The Mars Orbiter Laser Altimeter of Mars Global Surveyor

NASA Astrophysics Data System (ADS)

Niedermaier, G.; Wählisch, M.; van Gasselt, S.; Scholten, F.; Wewel, F.; Roatsch, T.; Matz, K.-D.; Jaumann, R.

We present a new topographic image map of Mars using 8 bit data obtained from the Mars Orbiter Camera (MOC) of the Mars Global Surveyor (MGS) [1]. The new map covers the Mars surface from 270 E (90 W) to 315 E (45 W) and from 0 North to 30 South with a resolution of 231.529 m/pixel (256 pixel/degree). For map creation, digital image processing methods have been applied. Furthermore, we managed to de- velop a general processing method for creating image mosaics based on MOC data. From a total amount of 66,081 images, 4,835 images (4,339 Context and 496 Geodesy images [3]) were finally used for the creation of the mosaic. After radiometric and brightness corrections, the images were Mars referenced [5], geometrically [6] cor- rected and sinusoidal map projected [4] using a global Martian Digital Terrain Model (DTM), developed by the DLR and based on MGS Mars Orbiter Laser Altimeter (MOLA) topographic datasets [2]. Three layers of MOC mosaics were created, which were stacked afterwards. The upper layer contains the context images with a resolution < 250 m/pixel. The middle layer contains the images of the Geodesy Campaign with a resolution < 250 m/pixel. The bottom layer consists of the Geodesy Campaign im- ages with a resolution > 250 m/pixel and < 435 m/pixel. The contour lines have been extracted from the global Martian DTM, developed at DLR. The contour data were imported as vector data into Macromedia Freehand as separate layer and corrected interactively. The map format of 1,15 m × 1,39 m represents the western part of the MDIM2 j quadrangle. The map is used for geological and morphological interpreta- tions in order to review and improve our current Viking-based knowledge about the Martian surface. References: [1] www.msss.com [2] wufs.wustl.edu [3] Caplinger, M. and M. Malin, The Mars Orbiter Camera Geodesy Campaign, JGR, in press. [4] Scholten, F., Vol XXXI, Part B2, Wien, 1996, p.351-356 [5] naif.jpl.nasa.gov [6] Kirk, R.L. et al., Geometric Calibration of the Mars Orbiter Cameras and Coalignment with Mars Orbiter Laser Altimeter, (abstract #1863), LPSC XXXII, 2001

76 FR 38913 - World Trade Center Health Program Requirements for Enrollment, Appeals, Certification of Health...

Federal Register 2010, 2011, 2012, 2013, 2014

2011-07-01

...Title I of the James Zadroga Health and Compensation Act of 2010 amended the Public Health Service Act (PHS Act) by adding Title XXXIII, which establishes the World Trade Center (WTC) Health Program. Sections 3311, 3312, and 3321 of Title XXXIII of the PHS Act require that the WTC Program Administrator develop regulations to implement portions of the WTC Health Program established within the Department of Health and Human Services (HHS). The WTC Health Program, which will be administered in part by the Director of the National Institute for Occupational Safety and Health (NIOSH), within the Centers for Disease Control and Prevention (CDC), will provide medical monitoring and treatment to eligible firefighters and related personnel, law enforcement officers, and rescue, recovery and cleanup workers who responded to the September 11, 2001, terrorist attacks in New York City, Shanksville, PA, and at the Pentagon, and to eligible survivors of the New York City attacks. This interim final rule establishes the processes by which eligible responders and survivors may apply for enrollment in the WTC Health Program, obtain health monitoring and treatment for WTC-related health conditions, and appeal enrollment and treatment decisions. This interim final rule also establishes a process for the certification of health conditions, and reimbursement rates for providers who provide initial health evaluations, treatment, and health monitoring.

33 CFR 67.50-25 - Eighth Coast Guard District.

Code of Federal Regulations, 2012 CFR

2012-07-01

... point at latitude 27°49′.5 N., longitude 97°01′.2 W., thence to; (xxx) A point on the 10 fathom curve at... W., thence to; (xxx) A point at Lat. 29°44′.6 N., Long. 93°07′.9 W., thence to; (xxxi) A point at...

33 CFR 67.50-25 - Eighth Coast Guard District.

Code of Federal Regulations, 2011 CFR

2011-07-01

... point at latitude 27°49′.5 N., longitude 97°01′.2 W., thence to; (xxx) A point on the 10 fathom curve at... W., thence to; (xxx) A point at Lat. 29°44′.6 N., Long. 93°07′.9 W., thence to; (xxxi) A point at...

33 CFR 67.50-25 - Eighth Coast Guard District.

Code of Federal Regulations, 2013 CFR

2013-07-01

... point at latitude 27°49′.5 N., longitude 97°01′.2 W., thence to; (xxx) A point on the 10 fathom curve at... W., thence to; (xxx) A point at Lat. 29°44′.6 N., Long. 93°07′.9 W., thence to; (xxxi) A point at...

33 CFR 67.50-25 - Eighth Coast Guard District.

Code of Federal Regulations, 2014 CFR

2014-07-01

... point at latitude 27°49′.5 N., longitude 97°01′.2 W., thence to; (xxx) A point on the 10 fathom curve at... W., thence to; (xxx) A point at Lat. 29°44′.6 N., Long. 93°07′.9 W., thence to; (xxxi) A point at...

Social Function in Multiple X and Y Chromosome Disorders: XXY, XYY, XXYY, XXXY

ERIC Educational Resources Information Center

Visootsak, Jeannie; Graham, John M., Jr.

2009-01-01

Klinefelter syndrome (47,XXY) was initially described in the context of its endocrinologic and physical features; however, subsequent studies have revealed specific impairments in verbal skills and social functioning. Males with sex chromosomal aneuploidies are known to have variability in their developmental profile with the majority presenting…

Developmental Arrest at the Logographic Stage: Impaired Literacy Functions in Klinefelter's XXXY Syndrome.

ERIC Educational Resources Information Center

Seymour, Philip H. K.; Evans, Henryka M.

1988-01-01

Reports a case study of the reading and spelling processes of a developmentally disabled child indicating that there was almost a complete lack of alphabetic functions, that reading appeared to be based on a "logographic lexicon," and that spelling was based on a letter sequence generator. (RS)

Lunar and Planetary Science XXXI

NASA Technical Reports Server (NTRS)

2000-01-01

This CD-ROM presents papers presented to the Thirty-first Lunar and Planetary Science Conference, March 13-17, 2000, Houston, Texas. Eighty-one conference sessions, and over one thousand extended abstracts are included. Abstracts cover topics such as Martian surface properties and geology, meteoritic composition, Martian landing sites and roving vehicles, planned Mars Sample Return Missions, and general astrobiology.

Comparative anatomy of the female genitalia of generic-level taxa in tribe Aedini (Diptera: Culicidae). Part XXXI. Genus Sallumia Reinert, Harbach and Kitching

USDA-ARS?s Scientific Manuscript database

A morphological analysis of the female genitalia of species included in genus Sallumia Reinert, Harbach and Kitching was conducted. The genitalia of the type species of the genus, Sl. hortator (Dyar and Knab), are illustrated. Treatment of the genital morphology of the genus includes a description...

Mars Exploration Rover Landing Site Hectometer Slopes

NASA Astrophysics Data System (ADS)

Haldemann, A. F.; Anderson, F. S.

2002-12-01

The Mars Exploration Rover (MER) airbag landing system imposes a maximum slope of 5 degrees over 100 m length-scales. This limit avoids dangerous changes in elevation over the horizontal travel distance of the lander on its parachute between the time of the last radar altimeter detection of the surface and the time the retro-rockets fire and the bridle to the airbags is cut. Stereo imagery from the MGS MOC can provide information at this length scale, but MOC stereo coverage is sparse, even when targeted to MER landing sites. Additionally, MGS spacecraft stability issues affect the DEMs at precisely the hectometric length-scale1. The MOLA instrument provides global coverage pulse-width measurements2 over a single MOLA-pulse footprint, which is about 100 m in diameter. However, the pulse spread only provides an upper bound on the 100 m slope. We chose another approach. We sample the inter-pulse root-mean-square (RMS) height deviations for MOLA track segments restricted to pixels of 0.1 deg latitude by 0.1 deg longitude. Then, under the assumption of self-affine topography, we determine the scale-dependence of the RMS deviations and extrapolate that behavior over the range of 300 m to 1.2 km downward to the 100 m scale. Shepard et al.3 clearly summarize the statistical properties of the RMS deviation (noting that it also goes by the name structure function, variogram or Allan deviation), and we follow their nomenclature. The RMS deviation is a useful measure in that it can be directly converted to RMS-slope for a given length-scale. We map the results of this self-affine extrapolation method for each of the proposed MER landing sites as well as Viking Lander 1 (VL1) and Pathfiner (MPF). In order of decreasing average hectometer RMS-slopes, Melas (about 4.5 degrees) > Elysium EP80 > Gusev > MPF > Elysium EP78 > VL1 > Athabasca > Isidis > Hematite (about 1 degree). We also map the scaling parameter (Hurst exponent); its behavior in the MER landing site regions is interesting in how it ties together the regional behavior of kilometer slopes (directly measured with MOLA) with the decameter and meter slopes (locally derived from stereo image analysis or radar scattering). 1Kirk, R. L., E. Howington-Kraus, and B. A. Archinal, Int. Arch. Photogramm. Remote Sens., XXVIII(B4), 476 (CD-ROM), 2001; Kirk, R. L., E. Howington-Kraus, and B. A. Archinal, Lunar Planet Sci., XXXIII, abs 1988, 2002. 2Garvin, J. B., and J. J. Frawley, Lunar Planet. Sci., XXXI, abs 1884, 2000. 3Shepard, M. K., R. A. Brackett, and R. E. Arvidson, J. Geophys. Res., 100, 11709-11718, 1995.; Shepard, M. K., et al., J. Geophys. Res., 106, 32777-32796, 2001.

Lunar and Planetary Science XXXII

NASA Technical Reports Server (NTRS)

2001-01-01

This CD-ROM publication contains the extended abstracts that were accepted for presentation at the 32nd Lunar and Planetary Science Conference held at Houston, TX, March 12-16, 2001. The papers are presented in PDF format and are indexed by author, keyword, meteorite, program and samples for quick reference.

Book review: Research techniques in animal ecology: Controversies and consequences, by Luigi Boitani and Todd K. Fuller

USGS Publications Warehouse

Johnson, D.H.

2001-01-01

Review of: Research Techniques in Animal Ecology: Controversies and Consequences. Edited by Luigi Boitani and Todd K. Fuller. Columbia University Press, New York, USA. 2000. xxxii + 442 pp., index. $75.00, ISBN 0231113404 (cloth); $32.00, ISBN 0231113412 (paper).

Catharanthus alkaloids XXXII: isolation of alkaloids from Catharanthus trichophyllus roots and structure elucidation of cathaphylline.

PubMed

Cordell, G A; Farnsworth, N R

1976-03-01

Further examination of the cytotoxic alkaloid fractions of Catharanthus trichophyllus roots afforded nine alkaloids. Two of these alkaloids, lochnericine and horhammericine, are responsible for part of the cytotoxic activity. The structure elucidation of cathaphylline, a new beta-anilino acrylate derivative, is described.

Ferrous Ion Sites in Angrite Pyroxenes: A Mössbauer Spectroscopy Study

NASA Astrophysics Data System (ADS)

Hoffman, E. J.

2002-03-01

Mössbauer spectra of angrites D'Orbigny and Sahara 99555 show that pyroxene ferrous ion is preominantly in the M1 site, not the M2 as for Angora dos Reis. These results are consistent with IR spectral data (Burbine et al., 2001, LPS XXXII,1857).

Federal Funds for Research and Development: Fiscal Years 1981, 1982, and 1983. Volume XXXI. Detailed Statistical Tables. Surveys of Science Resources Series.

ERIC Educational Resources Information Center

National Science Foundation, Washington, DC. Div. of Science Resources Studies.

Detailed statistical tables on federal funds for research and development (R&D) activities are provided in this document. Tables are organized into the following sections: research, development, and R&D plant; R&D- agency, character of work, and performer; total research- agency, performer, and field of science; basic research- agency,…

B and Mg isotopic variations in Leoville mrs-06 type B1 cai:origin of 10Be and 26Al

NASA Astrophysics Data System (ADS)

Chaussidon, M.; Robert, F.; Russel, S. S.; Gounelle, M.; Ash, R. D.

2003-04-01

The finding [1-3] in Ca-Al-rich refractory inclusions (CAI) of primitive chondrites of traces of the in situ decay of radioactive 10Be (half-life 1.5Myr) indicates that irradiation of the protosolar nebula by the young Sun in its T-Tauri phase has produced significant amounts of the Li-Be-B elements. This irradiation may have produced also some or all of the short-lived 26Al (half-life 0.7Myr) and 41Ca (half-life 0.1Myr) previously detected in CAIs. To constrain the origin of 10Be and 10Al it is important to look for coupled variations in the 10Be/9Be and 26Al/27Al ratios in CAIs and to understand the processes responsible for these variations (e.g. variations in the fluences of irradiation, secondary perturbations of the CAIs, ...) We have thus studied the Li and B isotopic compositions and the Be/Li and Be/B concentration ratios in one CAI (MRS-06) from the Leoville CV3 chondrite in which large variations of the Mg isotopic compositions showing both the in situ decay of 26Al and the secondary redistribution of Mg isotopes have been observed [4]. The results show large variations for the Li and B isotopic compositions (^7Li/^6Li ranging from 11.02±0.21 to 11.82±0.07, and 10B/11B ratios ranging from 0.2457±0.0053 to 0.2980±0.0085). The ^7Li/^6Li ratio tend to decrease towards the rim of the inclusion. The 10B/11B ratios are positively correlated with the ^9Be/11B ratios indicating the in situ decay of 10Be. However perturbations of the 10Be/B system are observed. They would correspond to an event which occurred approximately 2Myr after the formation of the CAI and the irradiation of the CAI precursors which is responsible for the 10Be observed in the core of the CAI. These perturbations seem compatible with those observed for the 26Al/Mg system but they might be due to an irradiation of the already-formed, isolated CAI which would have resulted in increased 10Be/^9Be ratios and low ^7Li/^6Li ratios in the margin of the CAI. [1] McKeegan K. D. et al. (2000) Science, 90, 1334-1337. [2] Sugiura N. et al. et al. (2001) Meteoritics &Planet. Sci., 36, 1397-1408. [3] McPherson G. J. and Huss G. R. (2001) LPS XXXII, Abstract #1882. [4] Ash R. D. et al. (2002) LPS XXXIII, Abstract #2063.

Studies in the History of Astronomy. Issue 32 %t Istoriko-Astronomicheskie Issledovaniya. Vypusk XXXII

NASA Astrophysics Data System (ADS)

Idlis, G. M.

This collection contains papers covering a wide scope of problems in the history of astronomy. Its basic headlines are: Cosmology and cosmogony of the 20th century; History of observations and astronomical organizations; Scientists and their works; Astronomy and society; Publications and memoirs; Astronomy and astrology; Memory of scientists

Widening Cultural Horizons: Recommended Approaches to Intercultural Education. Curriculum Bulletin No. 339. Vol. XXXII.

ERIC Educational Resources Information Center

Dixon, R. Joseph; Van Til, William

American schools need to encourage better human relations among Americans of varied racial, religious, ethnic, and socioeconomic backgrounds, according to the authors. They list useful strategies to encourage true integration, a list that they compiled from a review of integration approaches used historically. They surveyed the literature on…

Electron impact excitation of Kr XXXII

NASA Astrophysics Data System (ADS)

Aggarwal, K. M.; Keenan, F. P.; Lawson, K. D.

2009-09-01

Collision strengths (Ω) have been calculated for all 7750 transitions among the lowest 125 levels belonging to the 2s2p,2s2p,2p,2s3ℓ,2s2p3ℓ, and 2p3ℓ configurations of boron-like krypton, Kr XXXII, for which the Dirac Atomic R-matrix Code has been adopted. All partial waves with angular momentum J⩽40 have been included, sufficient for the convergence of Ω for forbidden transitions. For allowed transitions, a top-up has been included in order to obtain converged values of Ω up to an energy of 500 Ryd. Resonances in the thresholds region have been resolved in a narrow energy mesh, and results for effective collision strengths (ϒ) have been obtained after averaging the values of Ω over a Maxwellian distribution of electron velocities. Values of ϒ are reported over a wide temperature range below 107.3K, and the accuracy of the results is assessed. Values of ϒ are also listed in the temperature range 7.3⩽logTe(K)⩽9.0, obtained from the nonresonant collision strengths from the Flexible Atomic Code.

Wood Anatomy of the Neotropical Sapotaceae. XXXI. Pouteria.

DTIC Science & Technology

1982-10-01

Pouteria that have been excluded for various reasons (see Notes for details). General: Sapwood light brown to brown; heartwood apparently late in formation...and, when present, is usually dark brown or reddish brown and sharply demar- cated from the lighter colored sapwood . Wood hard and heavy, with a...specific gravity range of 0.60 (branchwood) to 1.30 (heartwood); the overall average for all specimens was 0.91 and the majority of these were sapwood or in

An Unusual Accumulation of Ribosomal Multigene Families and Microsatellite DNAs in the XX/XY Sex Chromosome System in the Trans-Andean Catfish Pimelodella cf. chagresi (Siluriformes:Heptapteridae).

PubMed

Conde-Saldaña, Cristhian Camilo; Barreto, Cynthia Aparecida Valiati; Villa-Navarro, Francisco Antonio; Dergam, Jorge Abdala

2018-02-01

This work constitutes the first cytogenetic characterization of a trans-Andean species of Heptapteridae. The catfish Pimelodella cf. chagresi from the Upper Rio Magdalena was studied, applying standard cytogenetic techniques (Giemsa, C-banding, and argyrophilic nucleolar organizer region [Ag-NOR]) and fluorescence in situ hybridization techniques using repetitive DNA probes: microsatellites (CA 15 and GA 15 ) and ribosomal RNA (rRNA) multigene families (18S and 5S recombinant DNA [rDNA] probes). The species showed a unique diploid chromosome number 2n = 50 (32m [metacentrics] +14sm [submetacentrics] +4st [subtelocentrics]) and a XX/XY sex chromosomal system, where the heteromorphic Y-chromosome revealed a conspicuous accumulation of all the assayed domains of repetitive DNA. P. cf. chagresi karyotype shares common features with other Heptapteridae, such as the predominance of metacentric and submetacentric chromosomes, and one pair of subtelomeric nucleolar organizer regions (NORs). These results reflect an independent karyological identity of a trans-Andean species and the relevance of repetitive DNA sequences in the process of sex chromosome differentiation in fish; it is the first case of syntenic accumulation of rRNA multigene families (18S and 5S rDNA) and microsatellite sequences (CA 15 and GA 15 ) in a differentiated sex chromosome in Neotropical fish.

Comparative anatomy of the female genitalia of generic-level taxa in tribe Aedini (Diptera: Culicidae). Part XXXII. Genus Jarnellius Reinert, Harbach and Kitching

USDA-ARS?s Scientific Manuscript database

A comparative, morphological analysis of the female genitalia of species included in genus Jarnellius Reinert, Harbach and Kitching was conducted. The female genitalia of the genus are characterized and a comparison with other taxa is provided. The type species of the genus, Ja. varipalpus (Coquil...

Federal Funds for Research and Development. Fiscal Years 1982, 1983, and 1984. Volume XXXII. Final Report. Surveys of Science Resources Series.

ERIC Educational Resources Information Center

National Science Foundation, Washington, DC. Div. of Science Resources Studies.

This report discusses the support of research and development (R&D) by the federal government through appropriate agencies; it uses data from an annual survey of federal agencies following the preparation of their budgets for 1984. Therefore, this information reflects the continuation of Reagan administration policies to strengthen the United…

Starting Where the People Are: The African Medical and Research Foundation (AMREF). Carnegie Quarterly, Volume XXXII, Number 2.

ERIC Educational Resources Information Center

Carnegie Quarterly, 1987

1987-01-01

This issue of the "Carnegie Quarterly" describes three projects that are being conducted by the African Medical and Research Foundation (AMREF). The projects are the following: (1) building community participation in health care at Lake Kenyatta; (2) the role of community education in disease control among the Turkana people at…

40 CFR 86.1 - Reference materials.

Code of Federal Regulations, 2010 CFR

2010-07-01

....007-17, 86.1806-01, 86.1806-04, 86.1806-05. (xxxii) SAE J1979, Revised May 2007, (R) E/E Diagnostic... J2012, Revised April 2002, (R) Diagnostic Trouble Code Definitions Equivalent to ISO/DIS 15031-6: April... Vehicle Programming, IBR approved for §§ 86.096-38, 86.004-38, 86.007-38, 86.010-38, 86.1808-01, 86.1808...

Federal Funds for Research and Development. Fiscal Years 1982, 1983, and 1984. Volume XXXII. Detailed Statistical Tables. Surveys of Science Resources Series.

ERIC Educational Resources Information Center

National Science Foundation, Washington, DC. Div. of Science Resources Studies.

Detailed statistical tables on federal funds for research and development (R&D) are provided in this document. Tables are organized into the following sections: research, development, and R&D plant; R&D--agency, character of work, and performer; total research--agency, performer, and field of science; basic research--agency, performer,…

Climate for Learning: A Symposium. Creating a Climate for Learning, and the Humanizing Process. The Principal and School Discipline. Curriculum Bulletin Vol. XXXII, No. 341.

ERIC Educational Resources Information Center

Johnson, Simon O.; Chaky, June

This publication contains two articles focusing on creating a climate for learning. In "Creating a Climate for Learning, and the Humanizing Process," Simon O. Johnson offers practical suggestions for creating a humanistic learning environment. The author begins by defining the basic concepts--humanism, affective education, affective situation,…

[Is radiotherapy of the lymph node stages useful after the conservative treatment of the initial stage of breast carcinoma?].

PubMed

Gava, A; Coghetto, F

1989-05-01

Twenty-four lectures were reviewed of the XXXIII SIRMN National Congress (Rome, October 1988) on the conservative radiosurgical treatment of breast cancer. A whole of 3462 cases were divided into 2 groups: group A--2824 patients who underwent targeted radiotherapy after conservative surgery (mostly quadrantectomy)--and group B--638 patients where, in case of N+ and internal quadrant tumors, irradiation was extended to lymph nodes. No significant differences were demonstrated between group A and group B as far as loco-regional relapses were concerned. Thus, no significant advantage seems to be yielded by lymph node irradiation in the early treatment of breast cancer.

Origin of sex chromosomes in six groups of Rana rugosa frogs inferred from a sex-linked DNA marker.

PubMed

Oike, Akira; Watanabe, Koichiro; Min, Mi-Sook; Tojo, Koji; Kumagai, Masahide; Kimoto, Yuya; Yamashiro, Tadashi; Matsuo, Takanori; Kodama, Maho; Nakamura, Yoriko; Notsu, Masaru; Tochimoto, Takeyoshi; Fujita, Hiroyuki; Ota, Maki; Ito, Etsuro; Yasumasu, Shigeki; Nakamura, Masahisa

2017-08-01

Each vertebrate species, as a general rule, has either the XX/XY or ZZ/ZW chromosomes by which sex is determined. However, the Japanese Rana (R.) rugosa frog is an exception, possessing both sex-determining combinations within one species, varying with region of origin. We collected R. rugosa frogs from 104 sites around Japan and South Korea and determined the nucleotide sequences of the mitochondrial 12S ribosomal RNA gene. Based on the sequences, R. rugosa frogs were divided into four groups from Japan and one from South Korea. The ZZ/ZW type is reportedly derived from the XX/XY type, although recently a new ZZ/ZW type of R. rugosa was reported. However, it still remains unclear from where the sex chromosomes in the five groups of this species were derived. In this study, we successfully isolated a sex-linked DNA maker and used it to classify R. rugosa frogs into several groupings. From the DNA marker as well as from nucleotide analysis of the promoter region of the androgen receptor (AR) gene, we identified another female heterogametic group, designated, West-Central. The sex chromosomes in the West-Central originated from the West and Central groups. The results indicate that a sex-linked DNA marker is a verifiable tool to determine the origin of the sex chromosomes in R. rugosa frogs in which the sex-determining system has changed, during two independent events, from the male to female heterogamety. © 2017 Wiley Periodicals, Inc.

Sex-specific markers developed by next-generation sequencing confirmed an XX/XY sex determination system in bighead carp (Hypophthalmichehys nobilis) and silver carp (Hypophthalmichthys molitrix).

PubMed

Liu, Haiyang; Pang, Meixia; Yu, Xiaomu; Zhou, Ying; Tong, Jingou; Fu, Beide

2018-01-05

Sex-specific markers are powerful tools for identifying sex-determination system in various animals. Bighead carp (Hypophthalmichehys nobilis) and silver carp (Hypophthalmichthys molitrix) are two of the most important edible fish in Asia, which have a long juvenility period that can lasts for 4-5 years. In this study, we found one sex-specific marker by next-generation sequencing together with bioinformatics analysis in bighead carp. The male-specific markers were used to perform molecular sexing in the progenies of artificial gynogenetic diploids and found all progenies (n = 160) were females. Meanwhile, around 1 : 1 sex ratio was observed in a total of 579 juvenile offspring from three other families. To further extend the male-specific region, we performed genome walking and got a male-specific sequence of 8,661 bp. Five pairs of primers were designed and could be used to efficiently distinguish males from females in bighead carp and silver carp. The development of these male-specific markers and results of their molecular sexing in different populations provide strong evidence for a sex determination system of female homogametry or male heterogametry (XX/XY) in bighead carp and silver carp. To the best of our knowledge, this is the first report of effective sex-specific markers in these two large carp species. © The Author(s) 2018. Published by Oxford University Press on behalf of Kazusa DNA Research Institute.

Climate-driven shifts in adult sex ratios via sex reversals: the type of sex determination matters.

PubMed

Bókony, Veronika; Kövér, Szilvia; Nemesházi, Edina; Liker, András; Székely, Tamás

2017-09-19

Sex reversals whereby individuals of one genetic sex develop the phenotype of the opposite sex occur in ectothermic vertebrates with genetic sex-determination systems that are sensitive to extreme temperatures during sexual differentiation. Recent rises in global temperatures have led researchers to predict that sex reversals will become more common, resulting in the distortion of many populations' sex ratios. However, it is unclear whether susceptibility to climate-driven sex-ratio shifts depends on the type of sex determination that varies across species. First, we show here using individual-based theoretical models that XX/XY (male-heterogametic) and ZZ/ZW (female-heterogametic) sex-determination systems can respond differentially to temperature-induced sex reversals. Interestingly, the impacts of climate warming on adult sex ratio (ASR) depend on the effects of both genotypic and phenotypic sex on survival and reproduction. Second, we analyse the temporal changes of ASR in natural amphibian populations using data from the literature, and find that ASR shifted towards males in ZZ/ZW species over the past 60 years, but did not change significantly in XX/XY species. Our results highlight the fact that we need a better understanding of the interactions between genetic and environmental sex-determining mechanisms to predict the responses of ectotherms to climate change and the associated extinction risks.This article is part of the themed issue 'Adult sex ratios and reproductive decisions: a critical re-examination of sex differences in human and animal societies'. © 2017 The Author(s).

Genetics of dioecy and causal sex chromosomes in plants.

PubMed

Kumar, Sushil; Kumari, Renu; Sharma, Vishakha

2014-04-01

Dioecy (separate male and female individuals) ensures outcrossing and is more prevalent in animals than in plants. Although it is common in bryophytes and gymnosperms, only 5% of angiosperms are dioecious. In dioecious higher plants, flowers borne on male and female individuals are, respectively deficient in functional gynoecium and androecium. Dioecy is inherited via three sex chromosome systems: XX/XY, XX/X0 and WZ/ZZ, such that XX or WZ is female and XY, X0 or ZZ are males. The XX/XY system generates the rarer XX/X0 and WZ/ZZ systems. An autosome pair begets XY chromosomes. A recessive loss-of-androecium mutation (ana) creates X chromosome and a dominant gynoecium-suppressing (GYS) mutation creates Y chromosome. The ana/ANA and gys/GYS loci are in the sex-determining region (SDR) of the XY pair. Accumulation of inversions, deleterious mutations and repeat elements, especially transposons, in the SDR of Y suppresses recombination between X and Y in SDR, making Y labile and increasingly degenerate and heteromorphic from X. Continued recombination between X and Y in their pseudoautosomal region located at the ends of chromosomal arms allows survival of the degenerated Y and of the species. Dioecy is presumably a component of the evolutionary cycle for the origin of new species. Inbred hermaphrodite species assume dioecy. Later they suffer degenerate-Y-led population regression. Cross-hybridization between such extinguishing species and heterologous species, followed by genome duplication of segregants from hybrids, give rise to new species.

The Karyotype of Microsternarchus aff. bilineatus: A First Case of Y Chromosome Degeneration in Gymnotiformes.

PubMed

Batista, Jéssica Almeida; Cardoso, Adauto Lima; Milhomem-Paixão, Susana Suely Rodrigues; Ready, Jonathan Stuart; Pieczarka, Julio Cesar; Nagamachi, Cleusa Yoshiko

2017-06-01

Various species and lineages that until recently were identified as Microsternarchus bilineatus (Hypopomidae, Gymnotiformes) have a widespread distribution in the Amazon and Orinoco River basins and across the Guiana shield. Recent molecular studies show five distinct lineages for Microsternarchus from different localities. These results suggest that this previously monotypic genus actually consists of more than one species. Here, we describe the karyotype of M. aff. bilineatus from the Cururutuia River (Bragança, Pará, Brazil). The diploid number of 48 chromosomes (14 meta-submetacentric/34 subtelo-acrocentric) is found for males and females, with an XX/XY sex chromosome system. The nucleolar organizer region is found in the short arm of pair 9. Constitutive heterochromatin occurs in the pericentromeric region of all chromosomes, in the distal region of 3p, 5p, 7p, 8q, 9q, 16q, and Xq, in the interstitial region in 2p, 10q, 11q, and 12q and all along 4p, and in a large block of the Y chromosome. These results indicate extensive karyotype divergence between this population and samples from Igarapé Tarumã Grande (Negro River, Amazonas, Brazil) studied by other researchers. Moreover, despite the diversity of sex chromosome systems found in Gymnotiformes, the XX/XY sex chromosome system of M. aff. bilineatus is the first case of Y chromosome degeneration in this order. The present data are valuable to help understand karyotype evolution in Hypopomidae.

Reform in Secondary Education: The Continuing Efforts to Reform Secondary Education, and a Modest Proposal. Curriculum Bulletin Vol. XXXII, No. 340.

ERIC Educational Resources Information Center

Saylor, Galen

The author begins by examining the functions of the school and the basic principles governing the provision of education in the American democracy as a way of providing a framework for analyzing proposals for the reform of secondary education. He then examines proposals for reform. His major focus is on ten proposals made by agencies,…

Getting to Know the Neighbors: Deep Imaging of the Andromeda Satellite Dwarf Galaxy Cassiopeia III with WIYN pODI

NASA Astrophysics Data System (ADS)

Smith, Madison; Rhode, Katherine L.; Janowiecki, Steven

2016-01-01

We present results from WIYN pODI imaging of Cassiopeia III/Andromeda XXXII (Cas III/And XXXII), an Andromeda satellite dwarf galaxy recently discovered by Martin et al. (2013) in Pan-STARRS1 survey data. Detailed studies of satellite dwarf galaxies in the Local Group and its environs provide important insight into how low-mass galaxies form and evolve as well as how more massive galaxies are assembled in a hierarchical universe. The goal of this project is to obtain deep, wide-field photometry of Cas III in order to study its stellar population in more detail. The images used for this analysis were taken in October 2013 with the 24' x 24' pODI camera on the WIYN 3.5-m telescope in the SDSS g and i filters. Calibrated photometry was performed on all point sources in the g and i images and then used to quantify the radial distribution of stars in Cas III and to construct a color-magnitude diagram (CMD). We present this CMD along with a map of the resolved stellar population and measurements of the galaxy magnitude and structural properties. This research was supported by the NSF Research Experiences for Undergraduates program (grant number AST-1358980).

[Intersexuality in domestic mammals].

PubMed

Cribiu, E P; Chaffaux, S

1990-01-01

With the exception of bovine freemartinism, intersexuality is rarely reported in domestic animals. The few cases of intersexuality reported here in dogs, cattle, goats, sheep and horses were classified according to the karyotype. The XX intersexes described here included goats which were either polled male pseudohermaphrodites or true hermaphrodites and dogs which were female pseudohermaphrodites. Among the XY intersexes studied, one dog was a true hermaphrodite, whereas the others were male pseudohermaphrodites, all mares showed gonadal dysgenesis and one cow was a female pseudohermaphrodite. XX/XY intersexes were detected in ovine cases of freemartinism.

Ultraviolet photometry from the Orbiting Astronomical Observatory. XXXIII - The symbiotic star AG Pegasi

NASA Technical Reports Server (NTRS)

Gallagher, J. S.; Webbink, R. F.; Holm, A. V.; Anderson, C. M.

1979-01-01

Ultraviolet broadband photometry obtained with the Wisconsin Experiment Package on OAO 2 is presented for the symbiotic binary star AG Peg. The hot component of the binary is found to be a luminous ultraviolet source, with an energy distribution consistent with its WN6 optical spectral type. Total luminosities of 1000 and 17,000 suns are found for the hot star by assuming, respectively, that the giant primary of AG Peg is a normal M3 III star and that it fills its Roche lobe. The eruptive behavior of AG Peg is shown to require the higher luminosity, and the activity in AG Peg is discussed in terms of a very slow novalike nuclear-powered event.

Modeling of Small Martian Volcanoes: A Changing View of Volcanic Shield and Cone Fields

NASA Astrophysics Data System (ADS)

Sakimoto, S. E.; Bradley, B. A.; Garvin, J. B.

2001-05-01

The small volcanic features on Mars (channels, flows, shields, and cratered cones) are key to understanding eruption styles, rates, and volumes because they are ubiquitous and simple enough to attempt modeling. Several of these small features have been suggested to be geologically recent [1,2,3]. This study measures and models small (3-50 km) volcanic edifices. Recent Mars Global Surveyor data reveal that these small features are more common that we had previously thought from the lower resolution Viking mission data (e.g., [3,4]). Furthermore, there are clear geometric differences in the Mars Orbiter Laser Altimeter (MOLA) data between regions suggesting local and regional eruption styles may vary with latitude. While a few of the pre-MGS construction models predict the martian mid-latitude volcanic shield shapes fairly well, the small explosive volcanic edifice shapes were not well predicted by existing models (see[5]), and there are a host of types-mostly polar-that are not well described by prior modeling. We compare small edifice construction model results for a percolation style model of effusive and mixed effusive and explosive edifices to prior model results for several martian volcanic regions. While mid-latitude edifices match well to predicted cross-section shapes, steeper flank slopes (See [6]; Glaze and Sakimoto, this volume) for the polar edifices suggest that the magma supply rate or the edifice permeability may be higher in the polar regions for some edifices types. However, polar edifice flank slopes do not commonly reach the greater than 10 degree flanks expected from prior explosive edifice models. Additionally, we do not observe shallow flank slope shields in the polar regions. This suggests that simple shield building may be significantly influenced or modified by volatile involvement near the martian poles, while a range of poorly understood explosive activity may be active in both regions. [1] Keszthelyi et al. JGR 105, 15027-15049, 2000. [2] Hartmann and Berman, JGR, 105, 15011-15025, 2000. [3] Garvin, et al., Icarus, 145, 648-652, 2000. [4] Sakimoto, et al., LPSC XXXII, CDROM, abstract #1808, 2001. [5] Glaze and Baloga LPSC XXXII, CDROM, abstract #1209, 2001. [6] Wong, et al., LPSC XXXII, CDROM, abstract #1563, 2001.

Effects of 17α-Methyltestosterone and Aromatase Inhibitor Letrozole on Sex Reversal, Gonadal Structure, and Growth in Yellow Catfish Pelteobagrus fulvidraco.

PubMed

Shen, Zhi-Gang; Fan, Qi-Xue; Yang, Wei; Zhang, Yun-Long; Wang, Han-Ping

2015-04-01

Monosex populations are in demand in many fish species with sexual dimorphism, e.g., better growth performance, higher gonad value, superior ornamental value. From the point of view of research, a monosex population is one of the best materials for investigating sex-determining mechanisms, sex differentiation, and sex-linked markers. Sex reversal of females (phenotypic reversal from XX female to XX male) is the first step in all-female production in species with an XX/XY system for sex determination. In the present study, masculinization of yellow catfish, a species with XX/XY sex determination, was investigated by oral administration of various doses of 17α-methyltestosterone (MT) or an aromatase inhibitor (AI) letrozole (LZ); effects on survival, growth performance, sex ratio, and changes in gonadal structure were evaluated. Three doses (20, 50, and 100 mg kg(-1) diet) of oral MT or LZ were administered to fry from 10 days post-hatching (DPH) to 59 DPH. Oral administration of MT at all doses did not significantly change the ratio of males (45.8%, 33.3%, and 50.0% respectively) compared to the control group (37.5%), while yielding intersex fish at all doses (4.2% to 8.3%). Oral administration of LZ produced a significantly higher proportion of males in all doses (75.5%, 83.3%, and 75.0%, respectively). Additionally, the lowest dose of LZ improved the growth of treated fish compared to the control, and all doses of LZ enhanced spermatogenesis in treated males. © 2015 Marine Biological Laboratory.

Psychology of computer use: XXXII. Computer screen-savers as distractors.

PubMed

Volk, F A; Halcomb, C G

1994-12-01

The differences in performance of 16 male and 16 female undergraduates on three cognitive tasks were investigated in the presence of visual distractors (computer-generated dynamic graphic images). These tasks included skilled and unskilled proofreading and listening comprehension. The visually demanding task of proofreading (skilled and unskilled) showed no significant decreases in performance in the distractor conditions. Results showed significant decrements, however, in performance on listening comprehension in at least one of the distractor conditions.

A New Type of Toxin A-Negative, Toxin B-Positive Clostridium difficile Strain Lacking a Complete tcdA Gene

PubMed Central

Marín, Mercedes; Martín, Adoración; Rupnik, Maja

2014-01-01

Toxins A and B are the main virulence factors of Clostridium difficile and are the targets for molecular diagnostic tests. Here, we describe a new toxin A-negative, toxin B-positive, binary toxin CDT (Clostridium difficile transferase)-negative (A− B+ CDT−) toxinotype (XXXII) characterized by a variant type of pathogenicity locus (PaLoc) without tcdA and with atypical organization of the PaLoc integration site. PMID:25428159

Physical studies of asteroids. XXXII. Rotation periods and UBVRI-colours for selected asteroids

NASA Astrophysics Data System (ADS)

Piironen, J.; Lagerkvist, C.-I.; Erikson, A.; Oja, T.; Magnusson, P.; Festin, L.; Nathues, A.; Gaul, M.; Velichko, F.

1998-03-01

We present lightcurves of selected asteroids. Most of the asteroids were included to obtain refined spin periods. Enhanced periods were determined for 11 Parthenope, 306 Unitas and 372 Palma. We confirmed the spin periods of 8 Flora, 13 Egeria, 71 Niobe, 233 Asterope, 291 Alice, 409 Aspasia, 435 Ella and 512 Taurinensis. We determined also BV-colours for most of the included asteroids and UBVRI-colours for a total of 22 asteroids.

Stereoselective reactions. XXXII. Enantioselective deprotonation of 4-tert-butylcyclohexanone by fluorine-containing chiral lithium amides derived from 1-phenylethylamine and 1-(1-naphthyl)ethylamine.

PubMed

Aoki, K; Koga, K

2000-04-01

Enantioselective deprotonation of 4-tert-butylcyclohexanone was examined using 1-phenylethylamine- and 1-(1-naphthyl)ethylamine-derived chiral lithium amides having an alkyl or a fluoroalkyl substituent at the amide nitrogen. The lithium amides having a 2,2,2-trifluoroethyl group on the amide nitrogen are easily accessible in both enantiomeric forms, and were found to induce good enantioselectivity in the present reaction.

Carotenoids in Fish. XXXII. Content of carotenoids in eggs utilized in the form of caviar.

PubMed

Czeczuga, B

1982-01-01

The author has investigated the carotenoids in the eggs utilized in form of caviar of 4 species of fishes. By means of columnar and thin-layer chromatography, the following carotenoids were found to be present: beta-carotene, beta-cryptoxanthin, echinenone, canthaxanthin, lutein, tunaxanthin, isozeaxanthin, zeaxanthin, salmoxanthin, adobixanthin, adonixanthin ester, astaxanthin and astaxanthin ester. The total carotenoid varied from 0.229 (Th. chlacogramma) to 1.669 microgram/g fresh weight (O. nerka).

Five new triterpene saponins, polygalasaponins XXVIII-XXXII from the root of Polygala japonica Houtt.

PubMed

Zhang, D; Miyase, T; Kuroyanagi, M; Umehara, K; Ueno, A

1996-04-01

Five new oleanane-type saponins, polygalasaponins XXVIII-XXXII, along with one known saponin, polygalasaponin XXIV, and one known acylated sucrose, tenuifoliside C, were isolated from the root of Polygala japonica. The structures of these new compounds were elucidated as 3-O-beta-D-glucopyranosyl pesenegenin 28-O-beta-D-xylopyranosyl (1-->4)-alpha-L-rhamnopyranosyl (1-->2)-beta-D-fucopyranosyl ester, 3-O-beta-D-glucopyranosyl presenegenin 28-O-beta-D-galactopyranosyl (1-->5)-beta-D-apiofuranosyl (1-->4)-beta-D-xylopyranosyl (1-->4)-alpha-L-rhamno-pyranosyl (1-->2)-beta-D-fucopyranosyl ester, 3-O-beta-D-glucopyranosyl presenegenin 28-O-beta-D-galactopyranosyl (1-->4)-beta-D-xylopyranosyl (1-->4)-alpha-L-rhamnopyranosyl (1-->2)-[4-O-p-methoxycinnamoyl]-[beta-D-glucopyranosyl (1-->3)]-beta-D-fucopyranosyl ester, 3-O-beta-D-glucopyranosyl presenegenin 28-O-alpha-L-arabinopyranosyl (1-->3)-beta-D-xylopyranosyl (1-->4)-[beta-D-apiofuranosyl (1-->3)]-alpha-L-rhamnopyranosyl (1-->2)-[4-O-3,4,5-trimethoxycinnamoyl]-beta-D-fucopyranosyl ester, 3-O-beta-D-glucopyranosyl persenegenin 28-O-alpha-L-arabinopyranosyl (1-->3)-beta-D-xylopyranosyl (1-->4)-[beta-D-apiofuranosyl (1-->3)-alpha-L-rhamnopyranosyl (1-->2)-[4-O-p-methoxycinnamoyl]-[alpha-L-rhamnopyranosyl (1-->3)-beta-D-fucopyranosyl ester, respectively, on the basis of spectroscopic and chemical evidence.

Effects of sex chromosome dosage on corpus callosum morphology in supernumerary sex chromosome aneuploidies.

PubMed

Wade, Benjamin S C; Joshi, Shantanu H; Reuter, Martin; Blumenthal, Jonathan D; Toga, Arthur W; Thompson, Paul M; Giedd, Jay N

2014-01-01

Supernumerary sex chromosome aneuploidies (sSCA) are characterized by the presence of one or more additional sex chromosomes in an individual's karyotype; they affect around 1 in 400 individuals. Although there is high variability, each sSCA subtype has a characteristic set of cognitive and physical phenotypes. Here, we investigated the differences in the morphometry of the human corpus callosum (CC) between sex-matched controls 46,XY (N =99), 46,XX (N =93), and six unique sSCA karyotypes: 47,XYY (N =29), 47,XXY (N =58), 48,XXYY (N =20), 47,XXX (N =30), 48,XXXY (N =5), and 49,XXXXY (N =6). We investigated CC morphometry using local and global area, local curvature of the CC boundary, and between-landmark distance analysis (BLDA). We hypothesized that CC morphometry would vary differentially along a proposed spectrum of Y:X chromosome ratio with supernumerary Y karyotypes having the largest CC areas and supernumerary X karyotypes having significantly smaller CC areas. To investigate this, we defined an sSCA spectrum based on a descending Y:X karyotype ratio: 47,XYY, 46,XY, 48,XXYY, 47,XXY, 48,XXXY, 49,XXXXY, 46,XX, 47,XXX. We similarly explored the effects of both X and Y chromosome numbers within sex. Results of shape-based metrics were analyzed using permutation tests consisting of 5,000 iterations. Several subregional areas, local curvature, and BLDs differed between groups. Moderate associations were found between area and curvature in relation to the spectrum and X and Y chromosome counts. BLD was strongly associated with X chromosome count in both male and female groups. Our results suggest that X- and Y-linked genes have differential effects on CC morphometry. To our knowledge, this is the first study to compare CC morphometry across these extremely rare groups.

Characterization of Tetraploid Somatic Cell Nuclear Transfer-Derived Human Embryonic Stem Cells.

PubMed

Shin, Dong-Hyuk; Lee, Jeoung-Eun; Eum, Jin Hee; Chung, Young Gie; Lee, Hoon Taek; Lee, Dong Ryul

2017-12-01

Polyploidy is occurred by the process of endomitosis or cell fusion and usually represent terminally differentiated stage. Their effects on the developmental process were mainly investigated in the amphibian and fishes, and only observed in some rodents as mammalian model. Recently, we have established tetraploidy somatic cell nuclear transfer-derived human embryonic stem cells (SCNT-hESCs) and examined whether it could be available as a research model for the polyploidy cells existed in the human tissues. Two tetraploid hESC lines were artificially acquired by reintroduction of remained 1st polar body during the establishment of SCNT-hESC using MII oocytes obtained from female donors and dermal fibroblasts (DFB) from a 35-year-old adult male. These tetraploid SCNT-hESC lines (CHA-NT1 and CHA-NT3) were identified by the cytogenetic genotyping (91, XXXY,-6, t[2:6] / 92,XXXY,-12,+20) and have shown of indefinite proliferation, but slow speed when compared to euploid SCNT-hESCs. Using the eight Short Tendem Repeat (STR) markers, it was confirmed that both CHA-NT1 and CHA-NT3 lines contain both nuclear and oocyte donor genotypes. These hESCs expressed pluripotency markers and their embryoid bodies (EB) also expressed markers of the three embryonic germ layers and formed teratoma after transplantation into immune deficient mice. This study showed that tetraploidy does not affect the activities of proliferation and differentiation in SCNT-hESC. Therefore, tetraploid hESC lines established after SCNT procedure could be differentiated into various types of cells and could be an useful model for the study of the polyploidy cells in the tissues.

Characterization of Tetraploid Somatic Cell Nuclear Transfer-Derived Human Embryonic Stem Cells

PubMed Central

Shin, Dong-Hyuk; Lee, Jeoung-Eun; Eum, Jin Hee; Chung, Young Gie; Lee, Hoon Taek; Lee, Dong Ryul

2017-01-01

ABSTRACT Polyploidy is occurred by the process of endomitosis or cell fusion and usually represent terminally differentiated stage. Their effects on the developmental process were mainly investigated in the amphibian and fishes, and only observed in some rodents as mammalian model. Recently, we have established tetraploidy somatic cell nuclear transfer-derived human embryonic stem cells (SCNT-hESCs) and examined whether it could be available as a research model for the polyploidy cells existed in the human tissues. Two tetraploid hESC lines were artificially acquired by reintroduction of remained 1st polar body during the establishment of SCNT-hESC using MII oocytes obtained from female donors and dermal fibroblasts (DFB) from a 35-year-old adult male. These tetraploid SCNT-hESC lines (CHA-NT1 and CHA-NT3) were identified by the cytogenetic genotyping (91, XXXY,-6, t[2:6] / 92,XXXY,-12,+20) and have shown of indefinite proliferation, but slow speed when compared to euploid SCNT-hESCs. Using the eight Short Tendem Repeat (STR) markers, it was confirmed that both CHA-NT1 and CHA-NT3 lines contain both nuclear and oocyte donor genotypes. These hESCs expressed pluripotency markers and their embryoid bodies (EB) also expressed markers of the three embryonic germ layers and formed teratoma after transplantation into immune deficient mice. This study showed that tetraploidy does not affect the activities of proliferation and differentiation in SCNT-hESC. Therefore, tetraploid hESC lines established after SCNT procedure could be differentiated into various types of cells and could be an useful model for the study of the polyploidy cells in the tissues. PMID:29359202

Polygalasaponin XXXII from Polygala tenuifolia root improves hippocampal-dependent learning and memory.

PubMed

Xue, Wei; Hu, Jin-feng; Yuan, Yu-he; Sun, Jian-dong; Li, Bo-yu; Zhang, Dong-ming; Li, Chuang-jun; Chen, Nai-hong

2009-09-01

The aim of this study was to investigate the cognition-enhancing activity and underlying mechanisms of a triterpenoid saponin (polygalasaponin XXXII, PGS32) isolated from the roots of Polygala tenuifolia Willd. The Morris water maze was used to evaluate the spatial learning and memory of mice. To detect the basic properties of synaptic transmission and long-term potentiation (LTP) in the dentate gyrus of rats, electrophysiological recordings were made of evoked potentials. Western blotting analysis and immunofluorescence assays were used to determine the phosphorylation of extracellular signal-regulated kinase (ERK), cAMP response element-binding protein (CREB), synapsin I and the expression of brain derived neurotrophic factor (BDNF). When administered at 0.125, 0.5, or 2 mg/kg, PGS32 could significantly prevent scopolamine-induced cognitive impairments in mice. Intracerebroventricular (icv) administration of PGS32 greatly enhanced basic synaptic transmission in the dentate gyrus of rats and induced LTP. In primary hippocampal neurons, as well as in the hippocampus of maze-trained mice, PGS32 activated the mitogen-activated protein (MAP) kinase cascade by promoting phosphorylation of ERK, CREB and synapsin I. The expression of BDNF was also greatly enhanced in the hippocampus. Our findings suggest that PGS32 can improve hippocampus-dependent learning and memory, possibly through improvement of synaptic transmission, activation of the MAP kinase cascade and enhancement of the level of BDNF. Therefore, PGS32 shows promise as a potential cognition-enhancing therapeutic drug.

Polygalasaponin XXXII from Polygala tenuifolia root improves hippocampal-dependent learning and memory

PubMed Central

Xue, Wei; Hu, Jin-feng; Yuan, Yu-he; Sun, Jian-dong; Li, Bo-yu; Zhang, Dong-ming; Li, Chuang-jun; Chen, Nai-hong

2009-01-01

Aim: The aim of this study was to investigate the cognition-enhancing activity and underlying mechanisms of a triterpenoid saponin (polygalasaponin XXXII, PGS32) isolated from the roots of Polygala tenuifolia Willd. Methods: The Morris water maze was used to evaluate the spatial learning and memory of mice. To detect the basic properties of synaptic transmission and long-term potentiation (LTP) in the dentate gyrus of rats, electrophysiological recordings were made of evoked potentials. Western blotting analysis and immunofluorescence assays were used to determine the phosphorylation of extracellular signal-regulated kinase (ERK), cAMP response element-binding protein (CREB), synapsin I and the expression of brain derived neurotrophic factor (BDNF). Results: When administered at 0.125, 0.5, or 2 mg/kg, PGS32 could significantly prevent scopolamine-induced cognitive impairments in mice. Intracerebroventricular (icv) administration of PGS32 greatly enhanced basic synaptic transmission in the dentate gyrus of rats and induced LTP. In primary hippocampal neurons, as well as in the hippocampus of maze-trained mice, PGS32 activated the mitogen-activated protein (MAP) kinase cascade by promoting phosphorylation of ERK, CREB and synapsin I. The expression of BDNF was also greatly enhanced in the hippocampus. Conclusion: Our findings suggest that PGS32 can improve hippocampus-dependent learning and memory, possibly through improvement of synaptic transmission, activation of the MAP kinase cascade and enhancement of the level of BDNF. Therefore, PGS32 shows promise as a potential cognition-enhancing therapeutic drug. PMID:19684611

Direct observation of a Γ -X energy spectrum transition in narrow AlAs quantum wells

NASA Astrophysics Data System (ADS)

Khisameeva, A. R.; Shchepetilnikov, A. V.; Muravev, V. M.; Gubarev, S. I.; Frolov, D. D.; Nefyodov, Yu. A.; Kukushkin, I. V.; Reichl, C.; Tiemann, L.; Dietsche, W.; Wegscheider, W.

2018-03-01

Spectra of magnetoplasma excitations have been investigated in two-dimensional electron systems in AlAs quantum wells (QWs) of different widths. The magnetoplasma spectrum has been found to change profoundly when the quantum well width becomes thinner than 5.5 nm, indicating a drastic change in the conduction electron energy spectrum. The transformation can be interpreted in terms of transition from the in-plane strongly anisotropic Xx-Xy valley occupation to the out-of-plane isotropic Xz valley in the QW plane. Strong enhancement of the cyclotron effective mass over the band value in narrow AlAs QWs is reported.

Rhodomollanol A, a Highly Oxygenated Diterpenoid with a 5/7/5/5 Tetracyclic Carbon Skeleton from the Leaves of Rhododendron molle.

PubMed

Zhou, Junfei; Zhan, Guanqun; Zhang, Hanqi; Zhang, Qihua; Li, Ying; Xue, Yongbo; Yao, Guangmin

2017-07-21

A novel diterpenoid with an unprecedented carbon skeleton, rhodomollanol A (1), and a new grayanane diterpenoid, rhodomollein XXXI (2), were isolated from the leaves of Rhododendron molle. Their structures were elucidated using comprehensive spectroscopic methods and single-crystal X-ray diffraction. Compound 1 possesses a unique cis/trans/trans/cis/cis-fused 3/5/7/5/5/5 hexacyclic ring system featuring a rare 7-oxabicyclo[4.2.1]nonane core decorated with three cyclopentane units. The plausible biosynthetic pathway for 1 was proposed. Compound 1 exhibited moderate PTP1B inhibitory activity.

NASA/DoD Aerospace Knowledge Diffusion Research Project. XXXIII - Technical communications practices and the use of information technologies as reported by Dutch and U.S. aerospace engineers

NASA Technical Reports Server (NTRS)

Barclay, Rebecca O.; Pinelli, Thomas E.; Tan, Axel S. T.; Kennedy, John M.

1993-01-01

As part of Phase 4 of the NASA/DOD Aerospace Knowledge Diffusion Research Project, two studies were conducted that investigated the technical communications practices of Dutch and U.S. aerospace engineers and scientists. A self-administered questionnaire was distributed to aerospace engineers and scientists at the National Aerospace Laboratory (The Netherlands), and NASA Ames Research Center (U.S.), and the NASA Langley Research Center (U.S.). This paper presents responses of the Dutch and U.S. participants to selected questions about four of the seven project objectives: determining the importance of technical communications to aerospace engineering professionals, investigating the production of technical communications, examining the use and importance of computer and information technology, and exploring the use of electronic networks.

Electron impact excitation of highly charged sodium-like ions

NASA Technical Reports Server (NTRS)

Blaha, M.; Davis, J.

1978-01-01

Optical transition probabilities and electron collision strengths for Ca X, Fe XVI, Zn XX, Kr XXVI and Mo XXXII are calculated for transitions between n equal to 3 and n equal to 4 levels. The calculations neglect relativistic effects on the radial functions. A semi-empirical approach provides wave functions of the excited states; a distorted wave function without exchange is employed to obtain the excitation cross sections. The density dependence of the relative intensities of certain emission lines in the sodium isoelectronic sequence is also discussed.

Ultraviolet photometry from the Orbiting Astronomical Observatory. XXXII - An atlas of ultraviolet stellar spectra

NASA Technical Reports Server (NTRS)

Code, A. D.; Meade, M. R.

1979-01-01

Ultraviolet stellar fluxes are presented in graphs and tables for 164 bright stars in the spectral region from 1200 to 3600 A. The spectra represent a subset of OAO 2 spectrometer data on file at the National Space Science Data Center. The monochromatic flux is given in units of erg per (sq cm-s-A) with a spectral resolution of about 22 A in the region from 3600 to 1850 A and of approximately 12 A in the region from 1850 to 1160 A.

VizieR Online Data Catalog: WIYN open cluster study. LIX. RVs of NGC 6791 (Tofflemire+, 2014)

NASA Astrophysics Data System (ADS)

Tofflemire, B. M.; Gosnell, N. M.; Mathieu, R. D.; Platais, I.

2014-11-01

Our observations utilize the Hydra Multi-Object Spectrograph (MOS) on the WIYN 3.5m telescope. We use 3.1'' diameter fibers along with the bench spectrograph echelle grating, resulting in a spectral resolution of ~20000 (15km/s). See Geller et al. 2008 (cat. J/AJ/135/2264; Paper XXXII) for full details about our observing and data reduction procedures. Variations in our methods from previous WIYN Open Cluster Study (WOCS) radial velocity papers are given in Section 3. (3 data files).

Bioactive constituents from Chinese natural medicines. XXXII. aminopeptidase N and aldose reductase inhibitors from Sinocrassula indica: structures of sinocrassosides B(4), B(5), C(1), and D(1)-D(3).

PubMed

Morikawa, Toshio; Xie, Haihui; Wang, Tao; Matsuda, Hisashi; Yoshikawa, Masayuki

2008-10-01

From the methanolic extract of the whole plant of Sinocrassula indica (Crassulaceae), six new flavonol glycosides, sinocrassosides B(4) (1), B(5) (2), C(1) (3), D(1) (4), D(2) (5), and D(3) (6), were isolated together with 30 compounds. The structures of 1-6 were elucidated on the basis of chemical and physicochemical evidence. In addition, several constituents were found to show inhibitory effects on aminopeptidase N and aldose reductase.

Pathology of orbital bones. The XXXII Edward Jackson Memorial Lecture.

PubMed

Blodi, F C

1976-01-01

The orbital bones may show nearly all the pathologic changes observed in the skull and in the face. The congenital anomalies in this area are numerous and involve various forms of craniostenoses. Among the benign osseous tumors the osteoma is most frequently encountered in the orbit. Fibrous dysplasia is a tumefaction of indeterminate behavior that often involves the orbit. Osteosarcoma or other malignant neoplasms are rarely seen in this area. Eosinophilic granuloma and Hand-Schüller-Christian disease are tumor-like lesions that may involve the orbit.

[Andrological characteristics in males with X-chromosomal pathology].

PubMed

Iunda, I F; Dyshlovoĭ, V D; Imshinetskaia, L P; Koblianskaia, G N; Ryzhkova, L N

1979-01-01

The authors examined 32 patients with Klinefelter's syndrome: 21 with chromatine-positive (the 1st group), 11 with chromatine-negative (the 2nd group). In contrast to the patients of the 2nd group an altered karyotype was revealed in patients of the 1st group (47/XXY, 46XY/47XXY, 48XXXY/49XXXXY). Hormonal examination revelaed hypoandrogenia with a relative hyperestrogenuria in the majority of the patients of the 1st and 2nd groups. However, patients of the 2nd group displayed a greater preservation of the reserve testicular function. Further clinical, endocrinological and cytogenetic studies of the Klinefelter's syndrome is necessary for its differential diagnosis and correction.

Medicinal Flowers. XXXII. Structures of oleanane-type triterpene saponins, perennisosides VIII, IX, X, XI, and XII, from the flowers of Bellis perennis.

PubMed

Morikawa, Toshio; Li, Xuezheng; Nishida, Eriko; Nakamura, Seikou; Ninomiya, Kiyofumi; Matsuda, Hisashi; Hamao, Makoto; Muraoka, Osamu; Hayakawa, Takao; Yoshikawa, Masayuki

2011-01-01

Five new triterpene saponins perennisosides VIII (1), IX (2), X (3), XI (4), and XII (5) were isolated from the MeOH-eluated fraction of the methanolic extract from the flowers of Bellis perennis. The MeOH-eluted fraction of the methanolic extract from the flowers of B. perennis was found to inhibit gastric emptying in olive oil-loaded mice at a dose of 200 mg/kg, per os (p.o.). The stereostructures of 1-5 were elucidated on the basis of chemical and spectroscopic evidence.

Polynucleotides. XXXII. Further studies on the synthesis of oligonucleotides containing 8,2'-S-cycloadenosine.

PubMed Central

Ikehara, M; Tezuka, T

1975-01-01

A dinucleoside monophosphate, 8,2'-anhydro-8-mercapto-9-beta-D-arabinofuranosyladenine phosphoryl-(3'-5')-inosine (AspI) was synthesized by the condensation of protected 8-mercapto-adenosine 2',3'-cyclic phosphate and 2',3'-isopropylideneinosine with diphenylphosphorochloridate. 8-Mercaptoadenosine 2',3'-cyclic phosphate was polymerized by using tetraphenyl pyrophosphate as the condensing reagent. As oligonucleotides, thus obtained, contained some uncyclized 8-mercaptoadenosine residues and were cleaved at these sites with 0.3N KOH. As 5'-phosphate was synthesized and polymerized with DCC to give oligonucleotides with chain lengths 2 to 9. PMID:170595

Dust Devil Track Occurrence in Argyre Planitia.

NASA Astrophysics Data System (ADS)

Whelley, P. L.; Balme, M. R.; Greeley, R.

2002-12-01

Martian dust devil tracks were first observed in Viking Orbiter images [Thomas et al., 1985]. While the interpretation of these features was at first controversial, it is now widely accepted that the tracks are formed by the passage of small convective vortices (dust devils). As the dust devils travel across the surface the atmosphere is loaded with fine particles creating a visible trail inferred to be removal or deposition of material [Greeley et al., 2001]. Mars Global Surveyor (MGS) Mars Orbital Camera (MOC) images of dust devil tracks in Argyre Planitia were used to asses dust devil track abundance as a function of Martian season as well as elevation using Mars Orbiter Laser Altimeter (MOLA) data. Argyre Planitia is a large impact basin in the southern hemisphere (55° to 33°W and 35° to 58°S), with topographic relief of 7 km with the median at -1km. We have studied the 564 Narrow Angle MOC images (taken as of summer 2002) covering the area. The images were divided into two categories: those with devil tracks and those without. The Ls (solar longitude degrees as a fraction of orbit) and elevation of all of the images with and without devil tracks were noted. The elevation was recorded at the center point of each MOC image using MOLA data. A polar plot of all of the images shows a statistically random distribution throughout the Martian year. A context map of the images shows a representative distribution over the area of the crater itself. A polar plot of dust devil track occurrence within the area observed shows a major concentration of tracks between Ls 200° and 360° (southern spring to late summer). A seasonal breakdown of devil track occurrence as a percentage of total area observed yields: fall 11.25%, winter 2.24%, spring 27.21%, and summer 46.49%. We therefore conclude that dust devils tracks are formed preferentially in summer and are destroyed, fade or are covered, over a period of a few months. The elevation of all 564 images was measured and 1km bins were used to calculate the percent of occurrence. We discovered that, at 3km 0% of the observed area contain dust devil tracks, 2km 7.69%, 1km 12.90%, at Datum 15.95%, -1km 8.97%, -2km 28.92%, -3km% 50.00%, -4km 50.00%. Independent of the season a majority of the devil tracks were observed below -3km. Therefore elevation is a key factor governing the formation of dust devils or their ability to produce tracks. Our interpretation of these results is that dust devils are much more likely to form during the summer and, as suggested by recent experiments [Balme et al., 2002], that they are more efficient at moving materials on the surface in areas where the atmospheric pressure is greatest (in the lowest elevations). The short timescale for disappearance of tracks suggests that the distinct albedo variations of the tracks result from only the removal or deposition of a very thin layer of material. Thomas. P. et al., 1985, Science v. 230 Greeley. R. et al., 2001, LPSC XXXII Balme. M. et al., 2002, LPSC XXXIII

Effects of sex chromosome dosage on corpus callosum morphology in supernumerary sex chromosome aneuploidies

PubMed Central

2014-01-01

Background Supernumerary sex chromosome aneuploidies (sSCA) are characterized by the presence of one or more additional sex chromosomes in an individual’s karyotype; they affect around 1 in 400 individuals. Although there is high variability, each sSCA subtype has a characteristic set of cognitive and physical phenotypes. Here, we investigated the differences in the morphometry of the human corpus callosum (CC) between sex-matched controls 46,XY (N =99), 46,XX (N =93), and six unique sSCA karyotypes: 47,XYY (N =29), 47,XXY (N =58), 48,XXYY (N =20), 47,XXX (N =30), 48,XXXY (N =5), and 49,XXXXY (N =6). Methods We investigated CC morphometry using local and global area, local curvature of the CC boundary, and between-landmark distance analysis (BLDA). We hypothesized that CC morphometry would vary differentially along a proposed spectrum of Y:X chromosome ratio with supernumerary Y karyotypes having the largest CC areas and supernumerary X karyotypes having significantly smaller CC areas. To investigate this, we defined an sSCA spectrum based on a descending Y:X karyotype ratio: 47,XYY, 46,XY, 48,XXYY, 47,XXY, 48,XXXY, 49,XXXXY, 46,XX, 47,XXX. We similarly explored the effects of both X and Y chromosome numbers within sex. Results of shape-based metrics were analyzed using permutation tests consisting of 5,000 iterations. Results Several subregional areas, local curvature, and BLDs differed between groups. Moderate associations were found between area and curvature in relation to the spectrum and X and Y chromosome counts. BLD was strongly associated with X chromosome count in both male and female groups. Conclusions Our results suggest that X- and Y-linked genes have differential effects on CC morphometry. To our knowledge, this is the first study to compare CC morphometry across these extremely rare groups. PMID:25780557

Subtractive and differential hybridization molecular analyses of Ceratitis capitata XX/XY versus XX embryos to search for male-specific early transcribed genes.

PubMed

Salvemini, Marco; D'Amato, Rocco; Petrella, Valeria; Ippolito, Domenica; Ventre, Giuseppe; Zhang, Ying; Saccone, Giuseppe

2014-01-01

The agricultural pest Ceratitis capitata, also known as the Mediterranean fruit fly or Medfly, is a fruit crop pest of very high economic relevance in different continents. The strategy to separate Ceratitis males from females (sexing) in mass rearing facilities is a useful step before the sterilization and release of male-only flies in Sterile Insect Technique control programs (SIT). The identification of genes having early embryonic male-specific expression, including Y-linked genes, such as the Maleness factor, could help to design novel and improved methods of sexing in combination with transgenesis, aiming to confer conditional female-specific lethality or female-to-male sexual reversal. We used a combination of Suppression Subtractive Hybrydization (SSH), Mirror Orientation Selection (MOS) anddifferential screening hybridization (DSH) techniques to approach the problem of isolating corresponding mRNAs expressed in XX/XY embryos versus XX-only embryos during a narrow developmental window (8-10 hours after egg laying, AEL ). Here we describe a novel strategy we have conceived to obtain relatively large amounts of XX-only embryos staged at 8-10 h AEL and so to extract few micrograms of polyA+ required to apply the complex technical procedure. The combination of these 3 techniques led to the identification of a Y-linked putative gene, CcGm2, sharing high sequence identity to a paralogous gene, CcGm1, localized either on an autosome or on the X chromosome. We propose that CcGm2 is a first interesting putative Y-linked gene which could play a role in sex determination. The function exterted by this gene should be investigated by novel genetic tools, such as CRISPR-CAS9, which will permit to target only the Y-linked paralogue, avoiding to interfere with the autosomal or X-linked paralogue function.

Subtractive and differential hybridization molecular analyses of Ceratitis capitata XX/XY versus XX embryos to search for male-specific early transcribed genes

PubMed Central

2014-01-01

The agricultural pest Ceratitis capitata, also known as the Mediterranean fruit fly or Medfly, is a fruit crop pest of very high economic relevance in different continents. The strategy to separate Ceratitis males from females (sexing) in mass rearing facilities is a useful step before the sterilization and release of male-only flies in Sterile Insect Technique control programs (SIT). The identification of genes having early embryonic male-specific expression, including Y-linked genes, such as the Maleness factor, could help to design novel and improved methods of sexing in combination with transgenesis, aiming to confer conditional female-specific lethality or female-to-male sexual reversal. We used a combination of Suppression Subtractive Hybrydization (SSH), Mirror Orientation Selection (MOS) and differential screening hybridization (DSH) techniques to approach the problem of isolating corresponding mRNAs expressed in XX/XY embryos versus XX-only embryos during a narrow developmental window (8-10 hours after egg laying, AEL ). Here we describe a novel strategy we have conceived to obtain relatively large amounts of XX-only embryos staged at 8-10 h AEL and so to extract few micrograms of polyA+ required to apply the complex technical procedure. The combination of these 3 techniques led to the identification of a Y-linked putative gene, CcGm2, sharing high sequence identity to a paralogous gene, CcGm1, localized either on an autosome or on the X chromosome. We propose that CcGm2 is a first interesting putative Y-linked gene which could play a role in sex determination. The function exterted by this gene should be investigated by novel genetic tools, such as CRISPR-CAS9, which will permit to target only the Y-linked paralogue, avoiding to interfere with the autosomal or X-linked paralogue function. PMID:25472628

Polygalasaponin XXXII, a triterpenoid saponin from Polygalae Radix, attenuates scopolamine-induced cognitive impairments in mice.

PubMed

Zhou, Heng; Xue, Wei; Chu, Shi-Feng; Wang, Zhen-Zhen; Li, Chuang-Jun; Jiang, Yi-Na; Luo, Lin-Ming; Luo, Piao; Li, Gang; Zhang, Dong-Ming; Chen, Nai-Hong

2016-08-01

Recent studies show that the extract of a Chinese herb Polygalae Radix exerts cognition-enhancing actions in rats and humans. The aim of this study was to characterize the pharmacological profiles of active compounds extracted from Polygalae Radix. Two fractions P3 and P6 and two compounds PTM-15 and polygalasaponin XXXII (PGS32) were prepared. Neuroprotective effects were evaluated in primary cortical neurons exposed to high concentration glutamate, serum deficiency or H2O2. Anti-dementia actions were assessed in scopolamine-induced amnesia in mice using step-through avoidance tests and channel water maze tests. After conducting the channel water maze tests, TrkB phosphorylation in mouse hippocampus was detected using Western blotting. Long-term potentiation (LTP) was induced in the dentate gyrus in adult rats; PGS32 (5 μL 400 μmol/L) was injected into the lateral cerebral ventricle 20 min after high frequency stimulation (HFS). Compared to the fraction P6, the fraction P3 showed more prominent neuroprotective effects in vitro and cognition-enhancing effects in scopolamine-induced amnesia in mice. One active compound PGS32 in the fraction P3 exerted potent cognition-enhancing action: oral administration of PGS32 (0.125 mg·kg(-1)·d(-1)) for 19 days abolished scopolamine-induced memory impairment in mice. Furthermore, PGS32 (0.5 and 2 mg·kg(-1)·d(-1)) significantly stimulated the phosphorylation of TrkB in the hippocampus. Intracerebroventricular injection of PGS32 significantly enhanced HFS-induced LTP in the dentate gyrus of rats. PGS32 attenuates scopolamine-induced cognitive impairments in mice, suggesting that it has a potential for the treatment of cognitive dysfunction and dementia.

Polygalasaponin XXXII, a triterpenoid saponin from Polygalae Radix, attenuates scopolamine-induced cognitive impairments in mice

PubMed Central

Zhou, Heng; Xue, Wei; Chu, Shi-feng; Wang, Zhen-zhen; Li, Chuang-jun; Jiang, Yi-na; Luo, Lin-ming; Luo, Piao; Li, Gang; Zhang, Dong-ming; Chen, Nai-hong

2016-01-01

Aim: Recent studies show that the extract of a Chinese herb Polygalae Radix exerts cognition-enhancing actions in rats and humans. The aim of this study was to characterize the pharmacological profiles of active compounds extracted from Polygalae Radix. Methods: Two fractions P3 and P6 and two compounds PTM-15 and polygalasaponin XXXII (PGS32) were prepared. Neuroprotective effects were evaluated in primary cortical neurons exposed to high concentration glutamate, serum deficiency or H2O2. Anti-dementia actions were assessed in scopolamine-induced amnesia in mice using step-through avoidance tests and channel water maze tests. After conducting the channel water maze tests, TrkB phosphorylation in mouse hippocampus was detected using Western blotting. Long-term potentiation (LTP) was induced in the dentate gyrus in adult rats; PGS32 (5 μL 400 μmol/L) was injected into the lateral cerebral ventricle 20 min after high frequency stimulation (HFS). Results: Compared to the fraction P6, the fraction P3 showed more prominent neuroprotective effects in vitro and cognition-enhancing effects in scopolamine-induced amnesia in mice. One active compound PGS32 in the fraction P3 exerted potent cognition-enhancing action: oral administration of PGS32 (0.125 mg·kg−1·d−1) for 19 days abolished scopolamine-induced memory impairment in mice. Furthermore, PGS32 (0.5 and 2 mg·kg−1·d−1) significantly stimulated the phosphorylation of TrkB in the hippocampus. Intracerebroventricular injection of PGS32 significantly enhanced HFS-induced LTP in the dentate gyrus of rats. Conclusion: PGS32 attenuates scopolamine-induced cognitive impairments in mice, suggesting that it has a potential for the treatment of cognitive dysfunction and dementia. PMID:27180981

Istoriko-Astronomicheskie Issledovaniya. Vypusk XXXI %t Studies in the History of Astronomy. Issue 31

NASA Astrophysics Data System (ADS)

Idlis, G. M.

This collection contains papers covering a wide scope of problems in the history of astronomy, both domestic and international astronomy. Its basic headlines are: astronomy and cosmology of the 20th century; researches and findings; history of observatories and astronomical organisations; amateur astronomy in Russia. Among the most interesting problems investigated in this issue: the history of the observed structure and stability of planetary rings explanation, the history of prediction of giant vortexes in galaxies; the newest history of planetary cartography; the Old Russian calendars; the Russian observations of the 1874 Venus transit; the history of the Pulkovo Observatory for the last 50 years; the autobiography of the distinguished Russian astronomer academician V. G. Fesenkov; Byelorussian folk astronomy; and many others.

Quality and Safety in Health Care, Part XXXII: Additional Outcome Predictors for Transcatheter Aortic Valve Replacement.

PubMed

Harolds, Jay A

2018-02-01

Mortality 12 months after a transcatheter aortic valve replacement (TAVR) is partly due to a number of reasons in addition to the usual preprocedural medical patient risk factors. In patients who need a permanent pacemaker placed after the procedure, the mortality risk goes up. The death rate following a TAVR varies considerably at different institutions, and the past death rate of TAVR patients at an institution is predictive of the mortality rate of new patients having this procedure. In addition, the quality of life of the individual before the procedure is predictive of the 12-month mortality outcome after the TAVR is done.

Marine natural products. XXXII. Absolute configurations of C-4 of the manoalide family, biologically active sesterterpenes from the marine sponge Hyrtios erecta.

PubMed

Kobayashi, M; Okamoto, T; Hayashi, K; Yokoyama, N; Sasaki, T; Kitagawa, I

1994-02-01

Cytotoxic sesterterpenes, manoalide 25-acetals (1a, 1b), seco-manoalide (2), (E)-neomanoalide (3), (Z)-neomanoalide (4), and heteronemin (6), were isolated from the marine sponge Hyrtios erecta (collected at Amami Island, Kagoshima Prefecture, Japan) by bioassay-guided separation and the absolute configurations of these manoalide family members have been determined. Manoalide 25-acetals (1a, 1b) were shown to exhibit in vivo antitumor activity and to inhibit the DNA-relaxing activity of mouse DNA topoisomerase I and the DNA-unknotting activity of calf thymus DNA topoisomerase II.

78 FR 18855 - World Trade Center Health Program Eligibility Requirements for Shanksville, Pennsylvania and...

Federal Register 2010, 2011, 2012, 2013, 2014

2013-03-28

...Title I of the James Zadroga 9/11 Health and Compensation Act of 2010 amended the Public Health Service Act (PHS Act) by adding Title XXXIII, which establishes the World Trade Center (WTC) Health Program. The WTC Health Program is administered by the Director of the National Institute for Occupational Safety and Health (NIOSH), within the Centers for Disease Control and Prevention (CDC), in the Department of Health and Human Services (HHS), and provides medical monitoring and treatment to eligible firefighters and related personnel, law enforcement officers, and rescue, recovery, and cleanup workers who responded to the September 11, 2001, terrorist attacks in New York City, Shanksville, Pennsylvania, and at the Pentagon, and to eligible survivors of the New York City attacks. Section 3311(a)(2)(C) of the PHS Act requires the WTC Program Administrator (Administrator) to develop eligibility criteria for enrollment of Shanksville, Pennsylvania and Pentagon responders. This interim final rule establishes those eligibility criteria.

Studies on transfer ribonucleic acids and related compounds. XXXII. Synthesis of ribonucleotides corresponding to residues 1-5 and 6-10 of tRNAfMet from E. coli and their base conversion analogs.

PubMed Central

Ohtsuka, E; Tanaka, T; Ikehara, M

1979-01-01

E. Coli tRNAfMet fragments, C-G-C-G-Gp (bases 1-5), U-G-C-G-Gp (base 1 transition, analog) pG-G-C-G-Gp (base 1 transversion analog) and pG-G-s4U-G-Gp (bases 6-10) were synthesized by triester methods using 2'-O-(o-nitrobenzyl) nucleotides including a 3',5'-bisphosphorylated guanosine derivative. The s4U containing pentanucleotide was derived from the pG-G-C-G-Gp by treatment with liquid hydrogen sulfide. Images PMID:390499

Integrated gene mapping and synteny studies give insights into the evolution of a sex proto-chromosome in Solea senegalensis.

PubMed

Portela-Bens, Silvia; Merlo, Manuel Alejandro; Rodríguez, María Esther; Cross, Ismael; Manchado, Manuel; Kosyakova, Nadezda; Liehr, Thomas; Rebordinos, Laureana

2017-03-01

The evolution of genes related to sex and reproduction in fish shows high plasticity and, to date, the sex determination system has only been identified in a few species. Solea senegalensis has 42 chromosomes and an XX/XY chromosome system for sex determination, while related species show the ZZ/ZW system. Next-generation sequencing (NGS), multi-color fluorescence in situ hybridization (mFISH) techniques, and bioinformatics analysis have been carried out, with the objective of revealing new information about sex determination and reproduction in S. senegalensis. To that end, several bacterial artificial chromosome (BAC) clones that contain candidate genes involved in such processes (dmrt1, dmrt2, dmrt3, dmrt4, sox3, sox6, sox8, sox9, lh, cyp19a1a, amh, vasa, aqp3, and nanos3) were analyzed and compared with the same region in other related species. Synteny studies showed that the co-localization of dmrt1-dmrt2-drmt3 in the largest metacentric chromosome of S. senegalensis is coincident with that found in the Z chromosome of Cynoglossus semilaevis, which would potentially make this a sex proto-chromosome. Phylogenetic studies show the close proximity of S. senegalensis to Oryzias latipes, a species with an XX/XY system and a sex master gene. Comparative mapping provides evidence of the preferential association of these candidate genes in particular chromosome pairs. By using the NGS and mFISH techniques, it has been possible to obtain an integrated genetic map, which shows that 15 out of 21 chromosome pairs of S. senegalensis have at least one BAC clone. This result is important for distinguishing those chromosome pairs of S. senegalensis that are similar in shape and size. The mFISH analysis shows the following co-localizations in the same chromosomes: dmrt1-dmrt2-dmrt3, dmrt4-sox9-thrb, aqp3-sox8, cyp19a1a-fshb, igsf9b-sox3, and lysg-sox6.

Cross sections and rate coefficients for excitation of Δn = 1 transitions in Li-like ions with 6 < Z < 42.

NASA Astrophysics Data System (ADS)

Safronova, U. I.; Safronova, M. S.; Kato, T.

Excitation cross sections and rate coefficients by electron impact were calculated for the 1s22s - 1s2s2p, 1s22s - 1s2s2 and 1s22s - 1s2p2 transitions of the Li-like ions (C IV, N V, O VI, Ne VIII, Mg X, Al XI, Si XII, S XIV, Ar XVI, Ca XVIII, Ti XX, Fe XXIV, Ni XXVI, Zn XXVIII, Ge XXX, Se XXXII, Kr XXXIIV and Mo XXXX) by a Coulomb-Born approximation with exchange and including relativistic effects and configuration interactions. Level energies, mixing coefficients and transition wavelengths and probabilities were also computed.

[Hemoglobins, XXXII. Analysis of the primary structure of the monomeric hemoglobin CTT VIIA (erythrocruorin) or Chironomus thummi thummi, Diptera (author's transl)].

PubMed

Kleinschmidt, T; Braunitzer, G

1980-01-01

The dimeric hemoglobin CTT VIIA (erythrocruorin) was isolated from the hemolymph of the larva from Chironomus thummi thummi and purified by preparative polyacrylamide gel electrophoresis. Peptides obtained by limited tryptical digestion were sequenced by automatic Edman degradation. For the elucidation of the sequence in the C-terminal region of the chain, additional cleavages with proteinase of Staphylococcus aureus and chymotrypsin were necessary. CTT VIIA is compared with human beta-chains and other hemoglobins of Chironomus. The amino acid residues in the pocket are especially discussed. Most of them are invariant in all Chironomus hemoglobins, independent of the size of the heme pocket, which is normal in some components and enlarged in others.

Proceedings of conference XXXII; workshop on Future directions in evaluating earthquake hazards of Southern California

USGS Publications Warehouse

Brown, William M.; Kockelman, William J.; Ziony, Joseph I.

1986-01-01

Hydrologic data were collected at White Sands Missile Range, NM, in 1985. The total groundwater withdrawal in 1985 was 676,433 ,800 gallons. The 11 supply wells in the Post Headquarters well field produced 642,056,000 gallons, or about 95 percent of the total. The six Range area supply wells produced 34,377,800 gallons. The total groundwater withdrawal was 8,841,200 gallons less in 1985 than 1984. Water samples from six Post Headquarters supply wells were collected for major chemical analysis. Water samples from 19 other wells were collected for pH and specific-conductance analysis. Depth-to-water measurements in the Post Headquarters supply wells showed seasonal fluctuations as well as continued long-term declines. (USGS)

Intersexuality associated with XX/XY mosaicism in a horned goat.

PubMed

Bongso, T A; Thavalingam, M; Mukherjee, T K

1982-01-01

Anatomical, histological, and cytogenetic studies were undertaken on a horned intersex goat kid and three of its normal litter mates. The intersex had male type horns, male beard, vestigial mammary glands, female external genitalia, and an enlarged peniform clitoris, exuded a pungent male odor, had a male bleat, and came into estrus every 20 days. At laparotomy and subsequent slaughter, an ovotestes was observed on the right side and a testis and epididymal remnants on the left side. Uterine horn segments, cervix, vagina, and enlarged clitoris (2 cm) were also present. Histologically, spermatogenesis was not observed in either testis, but active Leydig cells were present. The ovary contained mature follicles. Chromosome analysis revealed 60XX/60XY cell populations in blood, bone marrow, and skin. Lymphocytic metaphases from the male and female cosibs showed single populations of 60XY and 60XX, respectively. Mosaicism associated with the horned condition in the intersex goat was established.

[The Hippocratic Oath: how many covenants, how many oaths?].

PubMed

Schubert, Charlotte; Scholl, Reinhold

2005-01-01

This study focuses on the ancient text of the Hippocratic Oath. Ancient authors refer to various oaths in the context of medical practice, but none of these closely resemble the Hippocratic Oath. The text of the Hippocratic Oath contains several contractual clauses, which clearly reflect a strictly structured community within an institutionalized professional framework. Comparison with the epigraphic and papyrological tradition suggests placing the text in the Hellenistic-Roman period. In particular, investigation of the oldest remaining ancient textual witness, the POxy XXXI 2547 of the third century A.D., reveals Christian influences in the use of language. This indicates a stage of development of the Hippocratic Oath in which the latter existed within a Christian context. The article concludes that, as early as the third century A.D., Christian influences played an equally significant role in the transmission of the Oath as pagan influences.

Dosage Compensation of the Sex Chromosomes

PubMed Central

Disteche, Christine M.

2013-01-01

Differentiated sex chromosomes evolved because of suppressed recombination once sex became genetically controlled. In XX/XY and ZZ/ZW systems, the heterogametic sex became partially aneuploid after degeneration of the Y or W. Often, aneuploidy causes abnormal levels of gene expression throughout the entire genome. Dosage compensation mechanisms evolved to restore balanced expression of the genome. These mechanisms include upregulation of the heterogametic chromosome as well as repression in the homogametic sex. Remarkably, strategies for dosage compensation differ between species. In organisms where more is known about molecular mechanisms of dosage compensation, specific protein complexes containing noncoding RNAs are targeted to the X chromosome. In addition, the dosage-regulated chromosome often occupies a specific nuclear compartment. Some genes escape dosage compensation, potentially resulting in sex-specific differences in gene expression. This review focuses on dosage compensation in mammals, with comparisons to fruit flies, nematodes, and birds. PMID:22974302

Computer simulation studies of anisotropic systems. XXXII. Field-induction of a smectic A phase in a Gay-Berne mesogen

NASA Astrophysics Data System (ADS)

Luckhurst, G. R.; Saielli, G.

2000-03-01

Molecular field theory predicts the induction of a smectic A phase by the application of a field, either magnetic or electric, to a nematic phase. This intriguing behavior results from an enhancement of the orientational order which is coupled to the translational order and so shifts the smectic A-nematic transition. To test this prediction we have investigated a system of Gay-Berne mesogenic molecules subject to an applied field of second rank using isothermal-isobaric Monte Carlo simulations. The results of our calculations are compared with the Kventsel-Luckhurst-Zewdie molecular field theory of smectogens, modified to include the effect of an external field. We have also used the simulations to explore the possibility of inducing more ordered smectic phases with stronger fields.

Studies on lectins. XXXII. Application of affinity electrophoresis to the study of the interaction of lectins and their derivatives with sugars.

PubMed

Horejsí, V; Tichá, M; Kocourek, J

1977-09-29

Affinity electrophoresis was used to study the sugar binding heterogeneity of lectins or their derivatives. Commercial and demetallized preparations of concanavalin A could be resolved by affinity electrophoresis into three components with different affinity to immobilized sugar. Similarly the Vicia cracca lectin obtained by affinity chromatography behaved on affinity gels as a mixture of active and inactive molecular species. Affinity electrophoresis has shown that the nonhemagglutinating acetylated lentil lectin and photo-oxidized or sulfenylated pea lectin retain their sugar binding properties; dissociation constants of saccharide complexes of these derivatives are similar to those of native lectins. The presence of specific immobilized sugar in the affinity gel improved the resolution of isolectins from Dolichos biflorus and Ricinus communis seeds.

Highlights of the XXI annual meeting of the Brazilian Society of Protozoology, the XXXII annual meeting on Basic Research in Chagas' disease & an international symposium on vesicle trafficking in parasitic Protozoa – 7 to 9 November 2005, Caxambu, Minas Gerais, Brazil

PubMed Central

Shaw, Jeffrey; Schenkman, Sergio; Rodrigues, Mauricio Martins

2006-01-01

This report focuses on the 2005 Annual meeting held in Caxambu, Minas Gerais, Brazil that was convened and organized by the Brazilian Society of Protozoology . This is an annual event and details of these meetings can be found on the Society's website. Within the space available it has been impossible to cover all the important and fascinating contributions and what is presented are our personal views of the meetings scientific highlights and new developments. The contents undoubtedly reflect each author's scientific interests and expertise. Fuller details of the round tables, seminars and posters can be consulted on line at . PMID:16916462

[Immunology in the medical practice.XXXII. Transplantation of autologous hematopoietic stem cells for treatment of refractory auto-immune diseases; preliminary favorable results with 35 patients].

PubMed

Vlieger, A M; van den Hoogen, F H; Brinkman, D M; van Laar, J M; Schipperus, M; Kruize, A A; Wulffraat, N M

2000-08-12

The objective of this study was to document the experiences in the first Dutch pilot studies of the effect of transplantation of autologous haematopoietic stem cells in patients with therapy-resistant autoimmune disease. The first results in 21 adults and 14 children are promising: remission of the disease was achieved in 13 patients, while in the others a significant reduction of disease activity was seen with a corresponding improvement of the quality of life. Infectious complications were frequently observed. Two children with systemic juvenile idiopathic arthritis developed a fatal infection-associated macrophage activation syndrome. Multicentre randomised studies are necessary to study the effects of autologous stem cell transplantation and modifications such as T-cell depletion.

Amino acids and peptides. XXXII: A bifunctional poly(ethylene glycol) hybrid of fibronectin-related peptides.

PubMed

Maeda, M; Izuno, Y; Kawasaki, K; Kaneda, Y; Mu, Y; Tsutsumi, Y; Lem, K W; Mayumi, T

1997-12-18

An amino acid type poly(ethylene glycol) (aaPPEG) was prepared and its application to a drug carrier was examined. The peptides, Arg-Gly-Asp (RGD) and Glu-Ile-Leu-Asp-Val (EILDV) which were reported as active fragments of Fibronectin (a cell adhesion protein), were conjugated with aaPEG (molecular weight, 10,000). The hybrid, RGD-aaPEG-EILDV, was prepared by a combination of the solid-phase method and the solution method. Antiadhesive activity of the peptides was not lost by its hybrid formation with the large aaPEG molecule. A mixture of RGD (0.43 mmol) and EILDV (0.43 mmol) did not demonstrate an antiadhesive effect, but the hybrid containing 0.43 mmol of each peptide did exhibit this effect.

Some Properties of Glass and Carbonate in the D'Orbigny Angrite

NASA Astrophysics Data System (ADS)

Kubny, A.; Banerjee, A.; Jagoutz, E.; Varela, M. E.; Brandstätter, F.; Kurat, G.

2003-04-01

Introduction: The angrite D'Orbigny is unusually rich in glass as compared to other members of the angrite group [1, 2]. The most common glass fills open spaces in druses and hollow shells. Carbonate fills in part the abundant open spaces. Inside hollow shells, in the center of the rocks, it forms crystal bushels and is white. In contrast, near the surface of the meteorite, it forms crusts and has an ochre color. Analytical Methods and Results: Glass in some of the abundant open spaces in D'Orbigny, druses and hollow shells, is black (brown in thin section) [1, 2]. Its chemical composition is similar to that of the bulk rock for major, minor and trace elements [1-3]. The glass easily dissolves in part in aqua regia producing a clear yellow solution and a white, porous residue. The white and porous leach residue preserved the shape of the original glass sample and consists mainly of SiO_2 (93 wt%) with low contents of TiO_2 (˜1 wt%), Al_2O_3 (3-4 wt%) and FeO (0.5-1.5 wt%), as determined by electron microprobe analysis. The determination of the ion concentrations of the solution also shows that all major elements, except Si and Ti were dissolved. In contrast to the reaction of D'Orbigny glass with aqua regia giving a residue, treating with 25% aqueous HCl produces a yellow solution which forms a yellow gel within some days. The Raman spectrum of the D'Orbigny glass shows the typical spectral features of an aluminosilicate glass, whereas that of its white leach residue shows bands which can be attributed to amorphous silica structured of four-membered siloxane rings of SiO_4 tetrahedra. The structure of the carbonate could be determined by Raman spectroscopy. The white bushels show the spectral features of pure calcite whereas the ochre crust exhibits Raman bands of disturbed calcite which are almost completely hidden by the highly fluorescent background. References: [1] Kurat G. et al. (2001) LPS XXXII, 1737.pdf; [2] Varela M. E. et al. (2001) LPS XXXII, 1803.pdf; [3] Varela M. E. et al. (2001) MAPS 36, A201.

World Trade Center Health Program requirements for the addition of new WTC-related health conditions. Final rule.

PubMed

2012-04-25

Title I of the James Zadroga 9/11 Health and Compensation Act of 2010 amended the Public Health Service Act (PHS Act) to establish the World Trade Center (WTC) Health Program. Sections 3311, 3312, and 3321 of Title XXXIII of the PHS Act require that the WTC Program Administrator develop regulations to implement portions of the WTC Health Program established within the Department of Health and Human Services (HHS). The WTC Health Program, which is administered by the Director of the National Institute for Occupational Safety and Health (NIOSH), within the Centers for Disease Control and Prevention (CDC), provides medical monitoring and treatment to eligible firefighters and related personnel, law enforcement officers, and rescue, recovery and cleanup workers who responded to the September 11, 2001, terrorist attacks in New York City, Shanksville, PA, and at the Pentagon, and to eligible survivors of the New York City attacks. This final rule establishes the processes by which the WTC Program Administrator may add a new condition to the list of WTC-related health conditions through rulemaking, including a process for considering petitions by interested parties to add a new condition.

Inherited XX sex reversal originating from wild medaka populations.

PubMed

Shinomiya, A; Otake, H; Hamaguchi, S; Sakaizumi, M

2010-11-01

The teleost fish, medaka (Oryzias latipes), has an XX/XY sex-determining mechanism. A Y-linked DM domain gene, DMY, has been isolated by positional cloning as the sex-determining gene in this species. Previously, we conducted a field survey of genotypic sex and found that approximately 1% of wild medaka are sex-reversed (XX males and XY females). Here, we performed genetic analyses of nine spontaneous XX sex-reversed males to elucidate its genetic basis. In all cases, the F(1) progeny were all females, whereas XX males reappeared in the backcross (BC) progeny, suggesting that XX sex reversal is a recessive trait. Although the incidences of sex reversal in the BC progeny were mostly low, 40% were males derived from one XX male. We performed linkage analysis using 55 BC males and located a single major factor, sda-1 (sex-determining autosomal factor-1), controlling sex reversal in an autosomal linkage group. Thus, genes involved in the sex-determining pathway can be isolated from spontaneous mutants in wild populations.

Genetic biases for showy males: Are some genetic systems especially conducive to sexual selection?

PubMed Central

Reeve, Hudson Kern; Pfennig, David W.

2003-01-01

Male secondary sexual characters (conspicuous ornaments, signals, colors) are among nature's most striking features. Yet, it is unclear why certain groups of organisms are more likely than others to evolve these traits. One explanation for such taxonomic biases is that some genetic systems may be especially conducive to sexual selection. Here, we present theory and simulation results demonstrating that rare alleles encoding either male ornaments or female preferences for those ornaments are better protected against random loss in species with ZZ/ZW or ZZ/ZO sex chromosome systems (male homogamety) than in species with XX/XY or XX/XO systems (male heterogamety). Moreover, this protection is much stronger in diploid than haplodiploid species. We also present empirical data showing that male secondary sexual characters are better developed in diploid than haplodiploid species and in diploid species with male homogamety than in those with male heterogamety. Thus, taxonomic biases for showy males may stem from differences in sex chromosome systems. PMID:12540829

Happiness and Defense Styles in Psychiatrists.

PubMed

Machado, Leonardo; Tavares, Hermano; Petribú, Kátia; Pinto, Tiago; Cantilino, Amaury

2016-03-01

The aim of this study was to measure happiness in a sample of Brazilian psychiatrists and correlate it with the defense styles used by them and sociodemographic data. This study was observational, cross-sectional, and analytical. Data were collected through self-administered questionnaires by Brazilian psychiatrists who participated in the XXXII Brazilian Congress of Psychiatry, 2014. In this sample of psychiatrists, happiness levels were high (scoring 5.69 of a total of 7), and mature defense styles prevailed, especially humor and anticipation. In a multivariate analysis, having children, good sleep quality, increased sexual interest, and use of defense styles such as humor, anticipation, and idealization all showed a positive relationship with happiness; on the other hand, using defense style such as acting out or annulment demonstrated a negative relationship with happiness. Despite the well-known professional burden that they bear, Brazilian psychiatrists surveyed presented, in general, high levels of subjective well-being and happiness.

NASA/DoD Aerospace Knowledge Diffusion Research Project. XXXII - A new era in international technical communication: American-Russian collaboration

NASA Technical Reports Server (NTRS)

Flammia, Madelyn; Barclay, Rebecca O.; Pinelli, Thomas E.; Keene, Michael L.; Burger, Robert H.; Kennedy, John M.

1993-01-01

Until the recent dissolution of the Soviet Union, the Communist Party exerted a strict control of access to and dissemination of scientific and technical information. This article presents models of the Soviet-style information society and the Western-style information society and discusses the effects of centralized governmental control of information on Russian technical communication practices. The effects of political control on technical communication are then used to interpret the results of a survey of Russian and U.S. aerospace engineers and scientists concerning the time devoted to technical communication, their collaborative writing practices and their attitudes toward collaboration, the kinds of technical documents they produce and use, their views regarding the appropriate content for an undergraduate technical communication course, and their use of computer technology. Finally, the implications of these findings for future collaboration between Russian and U.S. engineers and scientists are examined.

Polysaccharides in fungi. XXXII. Hypoglycemic activity and chemical properties of a polysaccharide from the cultural mycelium of Cordyceps sinensis.

PubMed

Kiho, T; Hui, J; Yamane, A; Ukai, S

1993-12-01

Crude polysaccharides were obtained from a hot-water extract and alkaline extracts of the cultural mycelium of Cordyceps sinensis. They showed significant activity in normal mice and streptozotocin-induced diabetic mice as a result of intraperitoneal (i.p.) injection. A crude polysaccharide (CS-OHEP) obtained from 5% sodium hydroxide extract slightly lowered the plasma glucose level in normal mice by oral (p.o.) administration. A neutral polysaccharide (CS-F30) exhibited higher hypoglycemic activity than its crude polysaccharide (CS-OHEP), exhibited by i.p. injection, and it significantly lowered the glucose level by p.o. administration (50 mg/kg). However, it hardly affected the plasma insulin level in normal mice. CS-F30 ([alpha]D + 21 degrees in water) is composed of galactose, glucose and mannose (molar percent, 62:28:10), and its molecular weight is about 45000.

Genetic analysis of tumorigenesis: XXXII. Localization of constitutionally amplified KRAS sequences to Chinese hamster chromosomes X and Y by in situ hybridization.

PubMed

Stenman, G; Anisowicz, A; Sager, R

1988-11-01

The KRAS gene is constitutionally amplified in the Chinese hamster. We have mapped the amplified sequences by in situ hybridization to two major sites on the X and Y chromosomes, Xq4 and Yp2. No autosomal site was detected despite a search under relaxed hybridization conditions. KRAS DNA is amplified about 50-fold compared to a human cell line known to have a diploid number of KRAS sequences, whereas mRNA expression is 5- to 10-fold lower than in normal human cells. While mRNA expression levels do not necessarily parallel gene copy number, the low expression level strongly suggests that the amplified sequences are transcriptionally silent. It is suggested that the amplified sequences arose from the original KRAS gene on chromosome 8 and that the KRAS sequences on the Y chromosome arose by X-Y recombination.

[Roaming through methodology. XXXII. False test results].

PubMed

van der Weijden, T; van den Akker, M

2001-05-12

The number of requests for diagnostic tests is rising. This leads to a higher chance of false test results. The false-negative proportion of a test is the proportion of negative test results among the diseased subjects. The false-positive proportion is the proportion of positive test results among the healthy subjects. The calculation of the false-positive proportion is often incorrect. For example, instead of 1 minus the specificity it is calculated as 1 minus the positive predictive value. This can lead to incorrect decision-making with respect to the application of the test. Physicians must apply diagnostic tests in such a way that the risk of false test results is minimal. The patient should be aware that a perfectly conclusive diagnostic test is rare in medical practice, and should more often be informed of the implications of false-positive and false-negative test results.

Highlights of the XXI annual meeting of the Brazilian Society of Protozoology, the XXXII annual meeting on Basic Research in Chagas' disease & an international symposium on vesicle trafficking in parasitic Protozoa--7 to 9 November 2005, Caxambu, Minas Gerais, Brazil.

PubMed

Shaw, Jeffrey; Schenkman, Sergio; Rodrigues, Mauricio Martins

2006-08-17

This report focuses on the 2005 Annual meeting held in Caxambu, Minas Gerais, Brazil that was convened and organized by the Brazilian Society of Protozoology http://www.sbpz.org.br/. This is an annual event and details of these meetings can be found on the Society's website. Within the space available it has been impossible to cover all the important and fascinating contributions and what is presented are our personal views of the meetings scientific highlights and new developments. The contents undoubtedly reflect each author's scientific interests and expertise. Fuller details of the round tables, seminars and posters can be consulted on line at http://www.sbpz.org.br/livroderesumos2005.php.

Parasites of domestic and wild animals in South Africa. XXXII. Ixodid ticks on scrub hares in the Transvaal.

PubMed

Horak, I G; Spickett, A M; Braack, L E; Penzhorn, B L

1993-09-01

A total of 264 scrub hares (Lepus saxatilis) were examined for ixodid ticks at various localities in the Kruger National Park, eastern Transvaal Lowveld. Thirteen tick species were recovered from these hares. The seasonal abundances of the immature stages of Amblyomma hebraeum, Amblyomma marmoreum, Hyalomma truncatum, Rhipicephalus appendiculatus, Rhipicephalus evertsi evertsi, Rhipicephalus simus and Rhipicephalus zambeziensis and all stages of a Rhipicephalus sp. (near R. pravus) were determined. Three scrub hares, examined in the north-western Transvaal Bushveld, were infested with five ixodid tick species. Ten hares examined in the eastern Transvaal Highveld harboured three species. A total of 15 ixodid tick species were recovered from the scrub hares examined in the three regions of the Transvaal. No haematozoa were found in blood smears made from the hares examined in the southern region of the Kruger National Park.

Planck intermediate results: XXXI. Microwave survey of Galactic supernova remnants

DOE PAGES

Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; ...

2016-02-09

The all-sky Planck survey in 9 frequency bands was used in this paper to search for emission from all 274 known Galactic supernova remnants. Of these, 16 were detected in at least two Planck frequencies. The radio-through-microwave spectral energy distributions were compiled to determine the mechanism for microwave emission. In only one case, IC 443, is there high-frequency emission clearly from dust associated with the supernova remnant. In all cases, the low-frequency emission is from synchrotron radiation. As predicted for a population of relativistic particles with energy distribution that extends continuously to high energies, a single power law is evidentmore » for many sources, including the Crab and PKS 1209-51/52. A decrease in flux density relative to the extrapolation of radio emission is evident in several sources. Their spectral energy distributions can be approximated as broken power laws, S ν ∝ ν -α, with the spectral index, α, increasing by 0.5–1 above a break frequency in the range 10–60 GHz. Finally, the break could be due to synchrotron losses.« less

Cross sections and rate coefficients for inner-shell excitation of Li-like ions with 6 < Z < 42

NASA Astrophysics Data System (ADS)

Safronova, U. I.; Safronova, M. S.; Kato, T.

1996-07-01

Excitation cross sections and rate coefficients by electron impact were calculated for the 1s22s-1s2s2p, 1s22s-1s2s2 and 1s22s-1s2p2 transitions of the Li-like ions (C IV, N V, O VI, Ne VIII, Mg X, Al XI, Si XII, S XIV, Ar XVI, Ca XVIII, Ti XX, Fe XXIV, Ni XXVI, Zn XXVIII, Ge XXX, Se XXXII, Kr XXXIV and Mo XXXX) in the Coulomb-Born approximation with exchange including relativistic effects and configuration interaction. Level energies, mixing coefficients and transition wavelengths and probabilities were also computed. Calculations performed by the 1/Z perturbation theory and Coulomb-Born approximation are compared with the R-matrix method and the distorted-wave approximation were Z is the nuclear charge. Formulae obtained for the angular factors of n-electron atomic system allow one to generalize this method to an arbitrary system of highly charged ions.

[Studies on chemical protectors against radiation. XXXII. Protective effects of methanol extracts of various Taiwan crude drugs on radiation injuries].

PubMed

Wang, C M; Ohta, S; Shinoda, M

1990-11-01

This study is to investigate radioprotective effects of 23 Taiwan crude drugs on X-ray induced bone marrow death and skin injury in mice. Each methanol extract of these Taiwan crude drugs was injected intraperitoneally into ICR male mice at 6 weeks of age before irradiation. Mice were whole-body irradiated with a soft X-ray generator. Radiation factors of the two screening tests used were as follows: 70 kVp, 10 mA, 10 mm acrylate filter, 70R/min, 2100R for survival test, and 30 kVp, 10 mA, 190R/min, 1100R for protective test on skin injury. As a result of these studies, the survival effect was recognized in Solani Incani Herba and Orthosiphi Aristati Herba. On the other hand, Mimosae Herba, Canarii Radix, Bombacis Radix, Arecae Fructus, Hedyotidis Diffusae Herba and Cynomorii Caulis were shown to have significant protective potency on skin injury.

Pharmacological properties of traditional medicine (XXXII): protective effects of hangeshashinto and the combinations of its major constituents on gastric lesions in rats.

PubMed

Kawashima, Keiko; Fujimura, Yu; Makino, Toshiaki; Kano, Yoshihiro

2006-09-01

The protective effect of Hangeshashinto (HST) and its major constituents, baicalin (BA), berberine (BE), saponin fraction of ginseng (GS) and glycyrrhizin (GL) on rat gastric lesion induced by ethanol was examined to clarify its active ingredients and action mechanism. Oral treatment with HST at the doses of 125 and 250 mg/kg suppressed ethanol-induced gastric lesions. The mixture of BA, BE, GL and GS (4M), each of BE, GL and GS at the dosage corresponded to HST (125 mg/kg) also suppressed the ethanol-induced gastric lesion in rats, but BA did not. Treatment of ethanol augmented the activity of myeloperoxidase (MPO) in the stomach, which was significantly suppressed by the administration of HST, BE, GL and GS. These results suggest that the protective effect of HST on ethanol-induced gastric lesion was depended on BE, GL and GS, by, in part, the reduction of MPO activity in stomach.

PERSEUS I: A DISTANT SATELLITE DWARF GALAXY OF ANDROMEDA

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

Martin, Nicolas F.; Laevens, Benjamin P. M.; Schlafly, Edward F.

We present the discovery of a new dwarf galaxy, Perseus I/Andromeda XXXIII, found in the vicinity of Andromeda (M31) in stacked imaging data from the Pan-STARRS1 3π survey. Located 27.°9 away from M31, Perseus I has a heliocentric distance of 785 ± 65 kpc, compatible with it being a satellite of M31 at 374{sub −10}{sup +14} kpc from its host. The properties of Perseus I are typical for a reasonably bright dwarf galaxy (M{sub V} = –10.3 ± 0.7), with an exponential half-light radius of r{sub h} = 1.7 ± 0.4 arcmin or r{sub h}=400{sub −85}{sup +105} pc at thismore » distance, and a moderate ellipticity (ϵ=0.43{sub −0.17}{sup +0.15}). The late discovery of Perseus I is due to its fairly low surface brightness (μ{sub 0}=25.7{sub −0.9}{sup +1.0} mag arcsec{sup –2}), and to the previous lack of deep, high quality photometric data in this region. If confirmed to be a companion of M31, the location of Perseus I, far east from its host, could place interesting constraints on the bulk motion of the satellite system of M31.« less

The Leukocyte Culture Method in the Diagnosis of Free-martinism

PubMed Central

Kanagawa, H.; Basrur, Parvathi K.

1968-01-01

The clinical application and reliability of the leukocyte culture method for the diagnosis of freemartinism were examined and the length of time that blood samples could be held at room temperature and in the refrigerator prior to culturing, was investigated. The chromosome findings by the leukocyte culture method in 14 freemartins and 9 non-freemartin females belonging to heterosexual twins or triplets revealed that XX-XY cell chimerism exists only in the former, whereas the latter were exclusively of normal female complement. The mitotic index in bovine blood after preservation for varying periods was studied on samples from two animals. Blood samples from these two animals stored at 5°C for 6 hours in a refrigerator showed the mitotic index to be 3.8 and 5.3 per cent which gradually decreased in samples stored for longer than 12 hours. After 72 hours, a very rapid decrease in mitotic index occurred in both cases, reaching zero in samples stored for 96 and 108 hours. Samples kept at room temperature followed a similar pattern as under refrigeration but with slightly lower values throughout. ImagesFig. 1.Fig. 2. PMID:4234791

Molecular Epidemiology of Malaria in Cameroon and Côte d'Ivoire. XXXI. Kelch 13 Propeller Sequences in Plasmodium falciparum Isolates before and after Implementation of Artemisinin-Based Combination Therapy.

PubMed

Djaman, Joseph Allico; Olefongo, Dagnogo; Ako, Aristide Berenger; Roman, Jocelyne; Ngane, Vincent Foumane; Basco, Leonardo K; Tahar, Rachida

2017-07-01

Artemisinin-resistant malaria has not been reported from Africa, but resistance can possibly spread from Asia or arise independently in Africa. The emergence of artemisinin resistance in Africa can be monitored by molecular assay of Kelch 13 (K13) propeller sequences. A total of 251 archived DNA samples of Plasmodium falciparum isolates collected in 2002, 2003, and 2006 in Yaounde, Cameroon, and 47 samples collected in 2006 and 2013 in Abidjan, Côte d'Ivoire, were analyzed for K13-propeller sequence polymorphism. Only one isolate carried a mutant K13-propeller allele (E602D). None of the isolates carried the key mutant alleles (Y493H, R539T, I543T, and C580Y) associated with artemisinin resistance in Cambodia. The presence of the mutant allele was not correlated with in vitro response to dihydroartemisinin determined by the classical hypoxanthine incorporation assay. There was no evidence of K13 mutations associated with artemisinin resistance before and soon after the introduction of artemisinin-based combination therapies in Cameroon and Côte d'Ivoire.

Evolution of sex determination systems with heterogametic males and females in silene.

PubMed

Slancarova, Veronika; Zdanska, Jana; Janousek, Bohuslav; Talianova, Martina; Zschach, Christian; Zluvova, Jitka; Siroky, Jiri; Kovacova, Viera; Blavet, Hana; Danihelka, Jiri; Oxelman, Bengt; Widmer, Alex; Vyskot, Boris

2013-12-01

The plant genus Silene has become a model for evolutionary studies of sex chromosomes and sex-determining mechanisms. A recent study performed in Silene colpophylla showed that dioecy and the sex chromosomes in this species evolved independently from those in Silene latifolia, the most widely studied dioecious Silene species. The results of this study show that the sex-determining system in Silene otites, a species related to S. colpophylla, is based on female heterogamety, a sex determination system that is unique among the Silene species studied to date. Our phylogenetic data support the placing of S. otites and S. colpophylla in the subsection Otites and the analysis of ancestral states suggests that the most recent common ancestor of S. otites and S. colpophylla was most probably dioecious. These observations imply that a switch from XX/XY sex determination to a ZZ/ZW system (or vice versa) occurred in the subsection Otites. This is the first report of two different types of heterogamety within one plant genus of this mostly nondioecious plant family. © 2013 The Author(s). Evolution © 2013 The Society for the Study of Evolution.

Different autosomes evolved into sex chromosomes in the sister genera of Salix and Populus

PubMed Central

Hou, Jing; Ye, Ning; Zhang, Defang; Chen, Yingnan; Fang, Lecheng; Dai, Xiaogang; Yin, Tongming

2015-01-01

Willows (Salix) and poplars (Populus) are dioecious plants in Salicaceae family. Sex chromosome in poplar genome was consistently reported to be associated with chromosome XIX. In contrast to poplar, this study revealed that chromosome XV was sex chromosome in willow. Previous studies revealed that both ZZ/ZW and XX/XY sex-determining systems could be present in some species of Populus. In this study, sex of S. suchowensis was found to be determined by the ZW system in which the female was the heterogametic gender. Gene syntenic and collinear comparisons revealed macrosynteny between sex chromosomes and the corresponding autosomes between these two lineages. By contrast, no syntenic segments were found to be shared between poplar's and willow's sex chromosomes. Syntenic analysis also revealed substantial chromosome rearrangements between willow's alternate sex chromatids. Since willow and poplar originate from a common ancestor, we proposed that evolution of autosomes into sex chromosomes in these two lineages occurred after their divergence. Results of this study indicate that sex chromosomes in Salicaceae are still at the early stage of evolutionary divergence. Additionally, this study provided valuable information for better understanding the genetics and evolution of sex chromosome in dioecious plants. PMID:25766834

Mechanisms of chromosomal evolution and its possible relation to natural history characteristics in Ancistrus catfishes (Siluriformes: Loricariidae).

PubMed

de Oliveira, R R; Feldberg, E; Dos Anjos, M B; Zuanon, J

2009-12-01

Ancistrus is the most speciose genus of the tribe Ancistrini, with 58 valid species and many yet to be described. Cytogenetic studies were conducted on five apparently undescribed species from the Amazon basin, which showed different diploid numbers: Ancistrus sp. Purus (2n = 34); Ancistrus sp. Macoari (2n = 46); Ancistrus sp. Dimona (2n = 52); Ancistrus sp. Vermelho (2n = 42) and Ancistrus sp. Trombetas (2n = 38). All species possessed only one pair of NOR-carrying chromosomes, but with extensive variation in both the location on the chromosome as well as in the position of the ribosomal sites on the karyotype. The karyotypic evolution of Ancistrus species seems to be based on chromosomal rearrangements, with a tendency to a reduction of the diploid number. Two new instances of XX/XY sex chromosomes for Ancistrus species, based on the heteromorphism in the male karyotype, were also recorded. The large karyotypic diversity among Ancistrus species may be related to biological and behavioural characteristics of these fish that include microhabitat preferences, territoriality and specialized reproductive tactics. These characteristics may lead to a fast rate of fixation of chromosomal mutations and eventually speciation across the basin.

X inactivation in a mammal species with three sex chromosomes.

PubMed

Veyrunes, Frédéric; Perez, Julie

2018-06-01

X inactivation is a fundamental mechanism in eutherian mammals to restore a balance of X-linked gene products between XY males and XX females. However, it has never been extensively studied in a eutherian species with a sex determination system that deviates from the ubiquitous XX/XY. In this study, we explore the X inactivation process in the African pygmy mouse Mus minutoides, that harbours a polygenic sex determination with three sex chromosomes: Y, X, and a feminizing mutant X, named X*; females can thus be XX, XX*, or X*Y, and all males are XY. Using immunofluorescence, we investigated histone modification patterns between the two X chromosome types. We found that the X and X* chromosomes are randomly inactivated in XX* females, while no histone modifications were detected in X*Y females. Furthermore, in M. minutoides, X and X* chromosomes are fused to different autosomes, and we were able to show that the X inactivation never spreads into the autosomal segments. Evaluation of X inactivation by immunofluorescence is an excellent quantitative procedure, but it is only applicable when there is a structural difference between the two chromosomes that allows them to be distinguished.

The Small Viral Membrane-Associated Protein P32 Is Involved in Bacteriophage PRD1 DNA Entry

PubMed Central

Grahn, A. Marika; Daugelavičius, Rimantas; Bamford, Dennis H.

2002-01-01

The lipid-containing bacteriophage PRD1 infects a variety of gram-negative cells by injecting its linear double-stranded DNA genome into the host cell cytoplasm, while the protein capsid is left outside. The virus membrane and several structural proteins are involved in phage DNA entry. In this work we identified a new infectivity protein of PRD1. Disruption of gene XXXII resulted in a mutant phenotype defective in phage reproduction. The absence of the protein P32 did not compromise the particle assembly but led to a defect in phage DNA injection. In P32-deficient particles the phage membrane is unable to undergo a structural transformation from a spherical to a tubular form. Since P32− particles are able to increase the permeability of the host cell envelope to a degree comparable to that found with wild-type particles, we suggest that the tail-tube formation is needed to eject the DNA from the phage particle rather than to reach the host cell interior. PMID:11967303

VizieR Online Data Catalog: WIYN open cluster study. LX. RV survey of NGC 6819 (Milliman+, 2014)

NASA Astrophysics Data System (ADS)

Milliman, K. E.; Mathieu, R. D.; Geller, A. M.; Gosnell, N. M.; Meibom, S.; Platais, I.

2014-10-01

The WOCS radial velocity target sample for NGC 6819 has 3895 stars that span 1° on the sky centered at RA=19h41m17.5s, DE=+40°11'47'' (J2000). The details of our radial velocity survey of NGC 6819 including the observing procedure, data reduction, and membership classification are discussed in depth in Hole et al. 2009 (cat. J/AJ/138/159; Paper XXIV) and Geller et al. 2008 (cat. J/AJ/135/2264; Paper XXXII). Observations of NGC 6819 with the Hydra Multi-Object Spectrograph (MOS) on the WIYN 3.5m telescope began in 1998 June and are still ongoing. We have almost 14000 spectra for over 2600 stars. These observations are augmented with 733 radial velocity measurements for 170 stars taken at the Harvard-Smithsonian Center for Astrophysics (CfA) facilities between 1988 May and 1995 by R. D. Mathieu and D. W Latham (Hole et al. 2009, cat. J/AJ/138/159; Paper XXIV). (4 data files).

Selim v Lele and the civil (industrial) conscription prohibition: constitutional protection against federal legislation controlling or privatising Australian public hospitals.

PubMed

Faunce, Thomas

2008-08-01

Selim v Lele (2008) 167 FCR 61; [2008] FCAFC 13 was a decision of the Federal Court which interpreted s 51(xxiiiA) of the Australian Constitution. This section accords the federal government, among other things, power to make laws with respect to the provision of "medical and dental services (but not so as to authorise any form of civil conscription)". The Federal Court decided that the phrase "civil conscription" was analogous to "industrial conscription". In that sense the Federal Court held that the prohibition was designed to preserve the employment autonomy of Australian medical practitioners or dentists, preventing federal laws that required them, either expressly or by practical compulsion, to work for the federal government or any industrial employer nominated or permitted by the federal government. The specific question in Selim v Lele was whether the imposition of standards and prohibition of "inappropriate practice" under the Health Insurance Act 1973 (Cth), ss 10, 20, 20A and Pt VAA, amounted to civil conscription. The court held they did not. The Federal Court also discussed in that context the sufficiency of "practical compulsion" in relation to the s 51(xxxiiiA) prohibition, The constitutional prohibition on "any form" of civil conscription provides one of the few rights protections in the Australian Constitution and may have an important role to play in shaping the limits of health care system privatisation in Australia.

Analysis of laser produced plasmas of gold in the 1-7 nm region

NASA Astrophysics Data System (ADS)

Li, Bowen; Higashiguchi, Takeshi; Otsuka, Takamitsu; Yugami, Noboru; Dunne, Padraig; Kilbane, Deirdre; Sokell, Emma; O'Sullivan, Gerry

2014-04-01

Extreme ultraviolet (EUV) spectra from gold laser produced plasmas were recorded in the 1-7 nm region using two Nd:YAG lasers with pulse lengths of 150 ps and 10 ns, respectively, operating at a range of power densities. The maximum focused peak power density was 9.5 × 1013 W cm-2 for the former and 5.3 × 1012 W cm-2 for the latter. Two intense quasicontinuous intensity bands resulting from n = 4-n = 4 and n = 4-n = 5 unresolved transition arrays dominate the 4-5.5 and 1.5-3.6 nm regions of both spectra. Comparison with atomic structure calculations performed with the Cowan suite of atomic structure codes as well as consideration of previous experimental and theoretical results aided identification of the most prominent features in the spectra. For the ns spectrum, the highest ion stage that could be identified from the n = 4-n = 5 arrays was Au28+ while for the ps plasma the presence of significantly higher stages was deduced and lines due to 4d104f-4d94f2 transitions in Ag-like Au32+ give rise to the strongest observed features within the n = 4-n = 4 array while in the n = 4-n = 5 array it was possible to identify a number of previously unidentified spectral features as resulting from 4f-5g transitions in the spectra of Au XX to Au XXXIII.

Use of Slopes of Small Martian Edifices to Discriminate Between Formation Mechanisms

NASA Astrophysics Data System (ADS)

Glaze, L. S.; Sakimoto, S. E.

2001-05-01

We have looked at Mars Orbiter Laser Altimeter (MOLA) topographic profiles of several small Martian edifices (3 - 50 km in size) in a variety of volcanic regions from the mid-latitudes to the poles. Viking and Mars Observer Camera (MOC) images and recent MOLA gridded topography data reveal a wide range of small edifice geometries (e.g., Garvin et al., 2000; Won et al., 2001), and a larger number of edifices than previously detected (e.g., Sakimoto, et al., 2001). We have attempted to characterize the average slopes of these edifices using a variety of statistics. Because of the curvature of many of the slopes, simple unweighted and weighted averages are not adequate for characterization. However, most of the flanks can be well described by a parabolic regression (R squared values greater than 90%). As a starting point, we have used the 'slope' term from the parabolic regression for comparison between the various features. The parabolic regression has the form: elevation = a - b sqrt(distance), where the constant 'a' is a vertical offset and 'b' is analogous to the slope. The true instantaneous slope at any point on the flank is found by taking the derivative of the expression above and is necessarily a function of location on the flank. The following table contains values of 'b' for the South and North facing flanks of several volcanic features found in different geologic settings: Feature: (South) (North)\\Polar moderate cratered cone (large crater) B1: (8.588) (7.46)\\Polar steep cratered cone (small crater) B5: (9.90) (10.613)\\Mid-latitude Tempe Terra shield TS1: (2.158) (1.964)\\Mid-latitude Tempe Terra cone TC1: (4.934) (4.591) As can be seen from the table, the individual features are very consistent between their South and North facing flanks. There is also a clear distinction between B5, TS1 and TC1. The uncertainty (standard error) in the 'b' values given above is typically less than 1, suggesting the possibility of at least three separate feature types represented above. In addition to this simple comparison between parabolic slopes, we can also compare the actual shapes of the features. For example, the TS1 shield-type feature has less curvature than the others and may be better characterized by a linear fit. This also distinguishes it from the other features purely by the shape of its flanks. These comparisons allow us to quantitatively document the differences between the small Martian shield volcanoes as a feature class from their more explosive counterparts. Garvin, J.B., et al., Icarus, 145, 648-652, 2000. Wong, M.P., et al., LPSC XXXII, CDROM, abstract #1563, 2001. Sakimoto, S.E.H., et al., LPSC XXXII, CDROM, abstract #1808, 2001.

Finding the factors of reduced genetic diversity on X chromosomes of Macaca fascicularis: male-driven evolution, demography, and natural selection.

PubMed

Osada, Naoki; Nakagome, Shigeki; Mano, Shuhei; Kameoka, Yosuke; Takahashi, Ichiro; Terao, Keiji

2013-11-01

The ratio of genetic diversity on X chromosomes relative to autosomes in organisms with XX/XY sex chromosomes could provide fundamental insight into the process of genome evolution. Here we report this ratio for 24 cynomolgus monkeys (Macaca fascicularis) originating in Indonesia, Malaysia, and the Philippines. The average X/A diversity ratios in these samples was 0.34 and 0.20 in the Indonesian-Malaysian and Philippine populations, respectively, considerably lower than the null expectation of 0.75. A Philippine population supposed to derive from an ancestral population by founding events showed a significantly lower ratio than the parental population, suggesting a demographic effect for the reduction. Taking sex-specific mutation rate bias and demographic effect into account, expected X/A diversity ratios generated by computer simulations roughly agreed with the observed data in the intergenic regions. In contrast, silent sites in genic regions on X chromosomes showed strong reduction in genetic diversity and the observed X/A diversity ratio in the genic regions cannot be explained by mutation rate bias and demography, indicating that natural selection also reduces the level of polymorphism near genes. Whole-genome analysis of a female cynomolgus monkey also supported the notion of stronger reduction of genetic diversity near genes on the X chromosome.

Estrogen rescues masculinization of genetically female medaka by exposure to cortisol or high temperature.

PubMed

Kitano, Takeshi; Hayashi, Yuki; Shiraishi, Eri; Kamei, Yasuhiro

2012-10-01

Medaka (Oryzias latipes) is a teleost fish with an XX/XY sex determination system. Recently, it was reported that XX medaka can be sex-reversed into phenotypic males by exposure to high water temperature (HT) during gonadal sex differentiation, possibly by elevation of cortisol, the major glucocorticoid produced by the interrenal cells in teleosts. Yet, it remains unclear how the elevation of cortisol levels by HT causes female-to-male sex reversal. This paper reports that exposure to cortisol or HT after hatching inhibited both the proliferation of female-type germ cells and the expression of ovarian-type aromatase (cyp19a1), which encodes a steroidogenic enzyme responsible for the conversion of androgens to estrogens, and induced the expression of gonadal soma-derived growth factor (gsdf) in XX gonads during gonadal sex differentiation. In contrast, exposure to either cortisol or HT in combination with 17β-estradiol (E2) did not produce these effects. Moreover, E2 completely rescued cortisol- and HT-induced masculinization of XX medaka. These results strongly suggest that cortisol and HT cause female-to-male sex reversal in medaka by suppression of cyp19a1 expression, with a resultant inhibition of estrogen biosynthesis. This mechanism may be common among animals with temperature-dependent sex determination. Copyright © 2012 Wiley Periodicals, Inc.

Karyotype Diversity and Evolutionary Trends in Armored Catfish Species of the Genus Harttia (Siluriformes: Loricariidae).

PubMed

Blanco, Daniel Rodrigues; Vicari, Marcelo Ricardo; Lui, Roberto Laridondo; Traldi, Josiane Baccarin; Bueno, Vanessa; Martinez, Juliana de Fátima; Brandão, Heleno; Oyakawa, Osvaldo Takeshi; Moreira Filho, Orlando

2017-04-01

Most species of the genus Harttia inhabits the headwaters of small tributaries, but some species are restricted to the main channel of some rivers. This feature, combined with limited dispersal ability, leads to the formation of small isolated populations with reduced gene flow. Currently, there are 23 taxonomically defined and recognized species, and 17 of these are found in Brazil, distributed in several hydrographic basins. Despite this diversity, few chromosomal data for the species belonging to this genus are found in the literature. Thus, this study analyzed, by classical and molecular cytogenetics methodologies, the chromosomal diversity of this genus, to discuss the processes that are involved in the evolution and karyotype differentiation of the species of the group. Seven species of Harttia were analyzed: H. kronei, H. longipinna, H. gracilis, H. punctata, H. loricariformis, H. torrenticola, and H. carvalhoi. The chromosomal diversity found in these species includes different diploid and fundamental numbers, distinct distribution of several repetitive sequences, the presence of supernumerary chromosomes in H. longipinna and multiple sex chromosome systems of the type XX/XY 1 Y 2 in H. carvalhoi and X 1 X 1 X 2 X 2 /X 1 X 2 Y in H. punctata. Lastly, our data highlight the genus Harttia as an excellent model for evolutionary studies.

MEXnICA, Mexican group in the MPD-NICA experiment at JINR

NASA Astrophysics Data System (ADS)

Rodríguez Cahuantzi, M.; MEXnICA Group

2017-10-01

The Nuclotron Ion Collider fAcility (NICA) accelerator complex is currently under construction at the Joint Institute for Nuclear Research (JINR) laboratory located in the city of Dubna in the Russian Federation. The main goal of NICA is to collide heavy ion nuclei to study the properties of the phase diagram of strongly interacting matter at high baryon density. In this accelerator complex, two big particle detectors are planned to be installed: Spin Physics Detector (SPD) and Multi-Purpose Detector (MPD). At the design luminosity, the event rate in the MPD interaction region is about 6 kHz; the total charged particle multiplicity would exceeds 1000 in the most central Au+Au collisions at \\sqrt{{sNN}} = 11 {{GeV}}. Since the middle of 2016 a group of researchers and students from Mexican institutions was formed (MEXnICA). The main goal of the MEXnICA group is to collaborate in the experimental efforts of MPD-NICA proposing a BEam-BEam counter detector which we called BEBE. In this written general aspects of MPD-NICA detector and BEBE are discussed. This material was shown in a contributed talk given at the XXXI Annual Meeting of the Mexican Division of Particles and Fields held in the Physics Department of CINVESTAV located in Mexico City during the last week of May 2017.

Finding the Factors of Reduced Genetic Diversity on X Chromosomes of Macaca fascicularis: Male-Driven Evolution, Demography, and Natural Selection

PubMed Central

Osada, Naoki; Nakagome, Shigeki; Mano, Shuhei; Kameoka, Yosuke; Takahashi, Ichiro; Terao, Keiji

2013-01-01

The ratio of genetic diversity on X chromosomes relative to autosomes in organisms with XX/XY sex chromosomes could provide fundamental insight into the process of genome evolution. Here we report this ratio for 24 cynomolgus monkeys (Macaca fascicularis) originating in Indonesia, Malaysia, and the Philippines. The average X/A diversity ratios in these samples was 0.34 and 0.20 in the Indonesian–Malaysian and Philippine populations, respectively, considerably lower than the null expectation of 0.75. A Philippine population supposed to derive from an ancestral population by founding events showed a significantly lower ratio than the parental population, suggesting a demographic effect for the reduction. Taking sex-specific mutation rate bias and demographic effect into account, expected X/A diversity ratios generated by computer simulations roughly agreed with the observed data in the intergenic regions. In contrast, silent sites in genic regions on X chromosomes showed strong reduction in genetic diversity and the observed X/A diversity ratio in the genic regions cannot be explained by mutation rate bias and demography, indicating that natural selection also reduces the level of polymorphism near genes. Whole-genome analysis of a female cynomolgus monkey also supported the notion of stronger reduction of genetic diversity near genes on the X chromosome. PMID:24026095

The management of pneumonia in internal medicine.

PubMed

Bouza, E; Giannella, M; Pinilla, B; Pujol, R; Capdevila, J A; Muñoz, P

2013-01-01

Pneumonia generates a high workload for internal medicine departments. Management of this disease is challenging, because patients are usually elderly and have multiple comorbid conditions. Furthermore, the interpretation and adherence to guidelines are far from clear in this setting. We report the opinion of 43 internists especially interested in infectious diseases that were questioned at the 2011 XXXII National Conference of Spanish Society of Internal Medicine about the main issues involved in the management of pneumonia in the internal medicine departments, namely, classification, admission criteria, microbiological workup, therapeutic management, discharge policy, and prevention of future episodes. Participants were asked to choose between 2 options for each statement by 4 investigators. Consensus could not be reached in many cases. The most controversial issues concerned recognition and management of healthcare-associated pneumonia (HCAP). Most participants were aware of the differences in terms of underlying diseases, etiological distribution, and outcome of HCAP compared with community-acquired pneumonia, but only a minority agreed to manage HCAP as hospital-acquired pneumonia, as suggested by some guidelines. A clinical patient-to-patient approach proved to be the option preferred by internists in the management of HCAP. Copyright © 2012 Elsevier España, S.L. All rights reserved.

Aggregation Properties and Liquid Crystal Phase of a Dye Based on Naphthalenetetracarboxylic Acid

NASA Astrophysics Data System (ADS)

Tomasik, Michelle; Collings, Peter

2007-03-01

R003 is a dye produced for thin film optical components by Optiva, Inc.^1 made from the sulfonation of the dibenzimidazole derivative of naphthalenetetracarboxylic acid. Its molecular structure is very different from the aggregating food dye previously investigated in our laboratory^2 and R003 forms a liquid crystal phase at significantly lower concentrations. We have performed polarizing microscopy, absorption spectroscopy, and x-ray diffraction experiments in order to determine the phase diagram and aggregate structure. In addition, we have included both translational and orientational entropy in the theoretical analysis of the aggregation process, and have used a more realistic lineshape in analyzing the absorption data. Our results indicate that the ``bond energy'' for molecules in an aggregate is even larger than for the previously studied dye and that the aggregate structure has a cross-sectional area equal to two or three molecular areas rather than one.^1Lazarev, P., N. Ovchinnikova, M. Paukshto, SID Int. Symp. Digest of Tech. Papers, San Jose, California, June XXXII, 571 (2001).^2V. R. Horowitz, L. A. Janowitz, A. L. Modic, P. A. Heiney, and P. J. Collings, Phys. Rev. E 72, 041710 (2005).

Venusian arachnoids revisited

NASA Astrophysics Data System (ADS)

Kostama, V.-P.; Tormanen, T.

The Venusian volcano-tectonic structures have been subject to many classification and characterisation schemes. Several structure-types have been identified (e.g. coronae, novae, arachnoids, calderas, and corona-novae). Of these groups, the relationship of arachnoids and coronae has been complicated, and is a subject to much debate. Some previous works and studies have fused these two categories together, and even promoted the view of non-existence of arachnoids at times. However, based on the recognisable differences in morphology and other characteristics (e.g. size, topography, volcanism), they should be treated as a separate class of structures. In our first global study of the volcano-tectonic features, we found 96 arachnoids [1, 2]. During the reanalysis of the features as a by-product of another study, the arachnoid population was re-evalueted, and more importantly, the identification criteria was rechecked. The revised population increases the arachnoid number to 130 features. The work also produced many examples of features that can be considered as transitional forms between different morphological groups. [1] Kostama, V.-P., M. Aittola, LPSC XXXII, Abstract#1185, 2001a. [2] Kostama, V.-P., M. Aittola, The Catalogue of Venusian Arachnoids, Coronae and Novae, http://cc.oulu.fi/tati/JR/Venus/volcanotectonics/catalogue.html, 2001b.

International Union of Pharmacology. XXXII. The mammalian calcitonin gene-related peptides, adrenomedullin, amylin, and calcitonin receptors.

PubMed

Poyner, David R; Sexton, Patrick M; Marshall, Ian; Smith, David M; Quirion, Remi; Born, Walter; Muff, Roman; Fischer, Jan A; Foord, Steven M

2002-06-01

The calcitonin family of peptides comprises calcitonin, amylin, two calcitonin gene-related peptides (CGRPs), and adrenomedullin. The first calcitonin receptor was cloned in 1991. Its pharmacology is complicated by the existence of several splice variants. The receptors for the other members the family are made up of subunits. The calcitonin-like receptor (CL receptor) requires a single transmembrane domain protein, termed receptor activity modifying protein, RAMP1, to function as a CGRP receptor. RAMP2 and -3 enable the same CL receptor to behave as an adrenomedullin receptor. Although the calcitonin receptor does not require RAMP to bind and respond to calcitonin, it can associate with the RAMPs, resulting in a series of receptors that typically have high affinity for amylin and varied affinity for CGRP. This review aims to reconcile what is observed when the receptors are reconstituted in vitro with the properties they show in native cells and tissues. Experimental conditions must be rigorously controlled because different degrees of protein expression may markedly modify pharmacology in such a complex situation. Recommendations, which follow International Union of Pharmacology guidelines, are made for the nomenclature of these multimeric receptors.

VizieR Online Data Catalog: Solar neighborhood. XXXII. L and M dwarfs (Dieterich+, 2014)

NASA Astrophysics Data System (ADS)

Dieterich, S. B.; Henry, T. J.; Jao, W.-C.; Winters, J. G.; Hosey, A. D.; Riedel, A. R.; Subasavage, J. P.

2015-01-01

We obtained VRI photometry for all targets in our sample using the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope for the brighter targets and the SOuthern Astrophysical Research (SOAR) Optical Imager camera on the SOAR 4.1m telescope for fainter targets. SOAR observations were conducted between 2009 September and 2010 December during six observing runs comprising NOAO programs 2009B-0425, 2010A-0185, and 2010B-0176. A total of 17 nights on SOAR were used for optical photometry. Table 1 shows the photometry in the photometric system used by the telescope with which the measurements were taken (Johnson-Kron-Cousins for the CTIO 0.9m telescope and Bessell for SOAR). Astrometric observations are based in part on observations obtained via the Cerro Tololo Inter-American Observatory Parallax Investigation (CTIOPI), at the Cerro Tololo 0.9m telescope. CTIOPI is a large and versatile astrometric monitoring program targeting diverse types of stellar and substellar objects in the solar neighborhood. Observations are taken using the CTIO 0.9m telescope and its sole instrument, a 2048*2048 Tektronix imaging CCD detector with a plate scale of 0.401''/pixel. (4 data files).

Doping control analysis at the Rio 2016 Olympic and Paralympic Games.

PubMed

Pereira, Henrique Marcelo Gualberto; Sardela, Vinicius Figueiredo; Padilha, Monica Costa; Mirotti, Luciana; Casilli, Alessandro; de Oliveira, Fabio Azamor; de Albuquerque Cavalcanti, Gustavo; Rodrigues, Lucas Martins Lisandro; de Araujo, Amanda Lessa Dutra; Levy, Rachel Santos; Teixeira, Pedro Antonio Castelo; de Oliveira, Felipe Alves Gomes; Duarte, Ana Carolina Giordani; Carneiro, Ana Carolina Dudenhoeffer; Evaristo, Joseph Albert Medeiros; Dos Santos, Gustavo Ramalho Cardoso; da Costa, Giovanni Carlo Verissimo; de Lima Castro, Fernando; Nogueira, Fabio Cesar Sousa; Scalco, Fernanda Bertão; Pizzatti, Luciana; de Aquino Neto, Francisco Radler

2017-11-01

This paper summarises the results obtained from the doping control analyses performed during the Summer XXXI Olympic Games (August 3-21, 2016) and the XV Paralympic Games (September 7-18, 2016). The analyses of all doping control samples were performed at the Brazilian Doping Control Laboratory (LBCD), a World Anti-Doping Agency (WADA)-accredited laboratory located in Rio de Janeiro, Brazil. A new facility at Rio de Janeiro Federal University (UFRJ) was built and fully operated by over 700 professionals, including Brazilian and international scientists, administrative staff, and volunteers. For the Olympic Games, 4913 samples were analysed. In 29 specimens, the presence of a prohibited substance was confirmed, resulting in adverse analytical findings (AAFs). For the Paralympic Games, 1687 samples were analysed, 12 of which were reported as AAFs. For both events, 82.8% of the samples were urine, and 17.2% were blood samples. In total, more than 31 000 analytical procedures were conducted. New WADA technical documents were fully implemented; consequently, state-of-the-art analytical toxicology instrumentation and strategies were applied during the Games, including different types of mass spectrometry (MS) analysers, peptide, and protein detection strategies, endogenous steroid profile measurements, and blood analysis. This enormous investment yielded one of the largest Olympic legacies in Brazil and South America. Copyright © 2017 John Wiley & Sons, Ltd. Copyright © 2017 John Wiley & Sons, Ltd.

Evolution of DMY, a newly emergent male sex-determination gene of medaka fish.

PubMed

Zhang, Jianzhi

2004-04-01

The Japanese medaka fish Oryzias latipes has an XX/XY sex-determination system. The Y-linked sex-determination gene DMY is a duplicate of the autosomal gene DMRT1, which encodes a DM-domain-containing transcriptional factor. DMY appears to have originated recently within Oryzias, allowing a detailed evolutionary study of the initial steps that led to the new gene and new sex-determination system. Here I analyze the publicly available DMRT1 and DMY gene sequences of Oryzias species and report the following findings. First, the synonymous substitution rate in DMY is 1.73 times that in DMRT1, consistent with the male-driven evolution hypothesis. Second, the ratio of the rate of nonsynonymous nucleotide substitution (d(N)) to that of synonymous substitution (d(S)) is significantly higher in DMY than in DMRT1. Third, in DMRT1, the d(N)/d(S) ratio for the DM domain is lower than that for non-DM regions, as expected from the functional importance of the DM domain. But in DMY, the opposite is observed and the DM domain is likely under positive Darwinian selection. Fourth, only one characteristic amino acid distinguishes all DMY sequences from all DMRT1 sequences, suggesting that a single amino acid change may be largely responsible for the establishment of DMY as the male sex-determination gene in medaka fish.

Genetic Diversity on the Sex Chromosomes

PubMed Central

Wilson Sayres, Melissa A

2018-01-01

Abstract Levels and patterns of genetic diversity can provide insights into a population’s history. In species with sex chromosomes, differences between genomic regions with unique inheritance patterns can be used to distinguish between different sets of possible demographic and selective events. This review introduces the differences in population history for sex chromosomes and autosomes, provides the expectations for genetic diversity across the genome under different evolutionary scenarios, and gives an introductory description for how deviations in these expectations are calculated and can be interpreted. Predominantly, diversity on the sex chromosomes has been used to explore and address three research areas: 1) Mating patterns and sex-biased variance in reproductive success, 2) signatures of selection, and 3) evidence for modes of speciation and introgression. After introducing the theory, this review catalogs recent studies of genetic diversity on the sex chromosomes across species within the major research areas that sex chromosomes are typically applied to, arguing that there are broad similarities not only between male-heterogametic (XX/XY) and female-heterogametic (ZZ/ZW) sex determination systems but also any mating system with reduced recombination in a sex-determining region. Further, general patterns of reduced diversity in nonrecombining regions are shared across plants and animals. There are unique patterns across populations with vastly different patterns of mating and speciation, but these do not tend to cluster by taxa or sex determination system. PMID:29635328

Sex-specific differences in the synaptonemal complex in the genus Oreochromis (Cichlidae).

PubMed

Campos-Ramos, Rafael; Harvey, Simon C; Penman, David J

2009-04-01

Total synaptonemal complex (SC) lengths were estimated from Oreochromis aureus Steindachner (which has a WZ/ZZ sex determination system), O. mossambicus Peters and O. niloticus L. (both of which have XX/XY sex determination systems). The total SC length in oocytes was greater than that in spermatocytes in all three species (194 +/- 30 microm and 134 +/- 13 microm, 187 +/- 22 microm and 127 +/- 17 microm, 193 +/- 37 microm and 144 +/- 19 microm, respectively). These sex-specific differences did not appear to be influenced by the type of sex determination system (the female/male total SC length ratio was 1.45 in O. aureus, 1.47 in O. mossambicus and 1.34 in O. niloticus) and do not correlate with the lack of any overall sex-specific length differences in the current Oreochromis linkage map. Although based on data from relatively few species, there appears to be no consistent relationship between sex-specific SC lengths and linkage map lengths in fish. Neomale (hormonally masculinized genetic female) O. aureus and O. mossambicus had total SC lengths of 138 +/- 13 microm and 146 +/- 13 microm respectively, more similar to normal males than to normal females. These findings agree with data from other vertebrate species that suggest that phenotypic sex, rather than genotype, determines traits such as total SC length, chiasmata position and recombination pattern, at least for the autosomes.

New insights into sex chromosome evolution in anole lizards (Reptilia, Dactyloidae).

PubMed

Giovannotti, M; Trifonov, V A; Paoletti, A; Kichigin, I G; O'Brien, P C M; Kasai, F; Giovagnoli, G; Ng, B L; Ruggeri, P; Cerioni, P Nisi; Splendiani, A; Pereira, J C; Olmo, E; Rens, W; Caputo Barucchi, V; Ferguson-Smith, M A

2017-03-01

Anoles are a clade of iguanian lizards that underwent an extensive radiation between 125 and 65 million years ago. Their karyotypes show wide variation in diploid number spanning from 26 (Anolis evermanni) to 44 (A. insolitus). This chromosomal variation involves their sex chromosomes, ranging from simple systems (XX/XY), with heterochromosomes represented by either micro- or macrochromosomes, to multiple systems (X 1 X 1 X 2 X 2 /X 1 X 2 Y). Here, for the first time, the homology relationships of sex chromosomes have been investigated in nine anole lizards at the whole chromosome level. Cross-species chromosome painting using sex chromosome paints from A. carolinensis, Ctenonotus pogus and Norops sagrei and gene mapping of X-linked genes demonstrated that the anole ancestral sex chromosome system constituted by microchromosomes is retained in all the species with the ancestral karyotype (2n = 36, 12 macro- and 24 microchromosomes). On the contrary, species with a derived karyotype, namely those belonging to genera Ctenonotus and Norops, show a series of rearrangements (fusions/fissions) involving autosomes/microchromosomes that led to the formation of their current sex chromosome systems. These results demonstrate that different autosomes were involved in translocations with sex chromosomes in closely related lineages of anole lizards and that several sequential microautosome/sex chromosome fusions lead to a remarkable increase in size of Norops sagrei sex chromosomes.

Monograph of Coccinia (Cucurbitaceae).

PubMed

Holstein, Norbert

2015-01-01

This monograph deals with all 95 names described in the Cucurbitaceae genus Coccinia and recognizes 25 species. Taxonomic novelties are Cocciniaadoensisvar.aurantiaca (C.Jeffrey) Holstein, stat. nov., Cocciniasessilifoliavar.variifolia (A.Meeuse) Holstein, stat. nov., and Cocciniaadoensisvar.jeffreyana Holstein, var. nov. For the 25 species 3157 collections were examined, of which 2024 were georeferenced to produce distribution maps. All species are distributed in sub-Saharan Africa with one species, Cocciniagrandis, extending from Senegal in West Africa east to Indonesia and being naturalized on Pacific Islands, in Australia, the Caribbean, and South America. Coccinia species are dioecious creepers or climbers with simple or bifid tendrils that occupy a range of habitats from arid scrubland, woodlands to lowland rainforest and mist forest. The corolla of Coccinia species is sympetalous, usually pale yellow to orange, and 1 to 4.5 cm long. Pollination is by bees foraging for pollen or nectar. After pollination, the developing ovary often exhibits longitudinal mottling, which usually disappears during maturation. All species produce berries with a pericarp in reddish colors (orange-red through to scarlet red), hence the generic name. The globose to cylindrical fruits contain numerous grayish-beige flat to lenticular seeds. Chromosome numbers are 2n = 20, 24, and 22 + XX/XY. Many Coccinia species are used for food, either as roasted tubers, greens as spinach, or the fruits as vegetables. Medicinal value is established in Cocciniagrandis, of which leaves and sap are used against diabetes.

Hydrological evolution of Atlantis basin, Sirenum Terrae, Mars. Preliminar analysis of MOC and THEMIS images.

NASA Astrophysics Data System (ADS)

de Pablo, M. A.; Márquez, A.; Centeno, J. D.

The Atlantis basin is one of the martian highlands areas where there was proposed the existence of an ancient lake during the early geological history of Mars [1] [2] [3] [4]. The existence of some morphological features inside the basin and in the surrounding area, allow to check the existence of liquid water in the past of the planet. On the other hand, other morphological features indicate the existence of snow and liquid groundwater in recent times. The detailed study of the geomorphologic features allows to make an approach to the hydrological evolution of the Atlantis basin. The study of the geomorphology of this region has been carried out by means of the analysis of MOC high resolution images obtained by the Mars Global Surveyor mission and the THEMIS images, in the visible spectrum, sent by Mars Odyssey spacecrafts. The most clearly morphological feature indicative of the existence of water in the surface of Mars in the past are the numerous channels that end into Atlantis basin from the highest terrains. In addiction to these fluvial channels, the existence of mass flow deposits is also indicative of the existence of water in the area. Some of these slumps are in the internal slopes of impact craters, but others cover huge extensions around the chaotic terrains of the studied area. The lobated ejecta deposits observed in the Atlantis basin region are indicative of the existence of groundwater (solid or liquid) [5]. Serrated reliefs and tables in the borders of the basins are indicative of the existence of a water sheet. Beneath this water sheet some deposits was formed which was eroded, due to the gradual desiccation of the basin, forming the tables and serrated reliefs. The existence of different chaotic terrains in the area implies the existence of huge amounts of water under the surface according to the different models of chaotic terrain formation [6] [7]. The existence of groundwater could be decided by the existence of collapses in the near to the chaotic terrain that it occupies the Atlantis basin centre [4]. Finally, the two features that indicate the existence of water in the most recent past of the basin are the gullies and icy dust surfaces. Gullies appears in the internal slopes of some impact craters located at the South of the Atlantis basin. Although different origins are discussed for the water that eroded these gullies [8] [9] [10] their formation implies the flow of water in surface during a relatively short time period. The mantels of icy dust have been described in several places of Mars and they imply the existence of frozen water in the most superficial layer [11] [12]. The low craterization of the deposits of the gullies and the icy dust surfaces indicates the extreme youth of these features. All these geomorphologic features show the existence of water in the surface or in subsurface of Mars in the region of the basin Atlantis in different moments of its geologic history. The previos studies of the MOLA topographic data (Mars Global Surveyor) [3] [13] indicate that this basin is part of the great Eridania Lake [3] whose gradual drying originated the formation of small lakes, one of them, the Atlantis lake [4], was located inside the studied basin. The fluvial channels observed in the edges of the basin should contribute with some water to this lake. The hypothesis of existence of a lake is supported by the existence of tables and serrated reliefs formed during the descent of the water sheet. The formation of the chaotic terrain, collapse areas, lobated ejecta of some impact craters and the mass flow deposits, all indicate the existence of water in the subsurface after the disappearance of the Atlantis Lake. Finally, the gullies and the icy dust surfaces indicate that water still exists at different depths in the ground. [1] Parker, T.J., Currey, D.R. 2001. Geomorphology, 37. 303-328. [2] de Pablo, M.A., Druet, M. 2002. XXXIII LPSC, Abstract #1032. [3] Irwin, R.P., et al. 2002. Science, 297, 2209-2212. [4] de Pablo, M.A., et al. 2004. XXXV LPSC, Abstracts. #1223. [5] Carr, 1996. Oxford University Press, New York. 229 p. [6] Komatsu, G. et al. 2000. XXXI LPSC, abstract # 1434. [7] Oyawa, Y., et al 2003. VI Int. Mars Conf., Abstract #3095. [8] Malin, M.C., Edgett, K.S. 2000. Science, 288. 2330-2335. [9] Costard, F., et al. 2002. Science, 295. 110-113. [10] Gilmore, M.S., Phillips, E.L. 2002. J. Gepphys. Res., 30. 1107-1110. [11] Mustard, J.F., et al. 2001. Nature, 412. 411-414. [12] Milliken, R.E., et al. 2003. J. Geophys. Res., 108 (E6). 5057. doi:10.1029/2002JE002005. [13] de Pablo, M.A. 2003. VI Internacional Conference on Mars, Abstract #3037.

Planck 2013 results. XXXII. The updated Planck catalogue of Sunyaev-Zeldovich sources

NASA Astrophysics Data System (ADS)

Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Aussel, H.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Barrena, R.; Bartelmann, M.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bikmaev, I.; Bobin, J.; Bock, J. J.; Böhringer, H.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burenin, R.; Burigana, C.; Butler, R. C.; Cardoso, J.-F.; Carvalho, P.; Catalano, A.; Challinor, A.; Chamballu, A.; Chary, R.-R.; Chen, X.; Chiang, H. C.; Chiang, L.-Y.; Chon, G.; Christensen, P. R.; Churazov, E.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Comis, B.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Da Silva, A.; Dahle, H.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J.-M.; Démoclès, J.; Désert, F.-X.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Feroz, F.; Ferragamo, A.; Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi, E.; Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.; Giardino, G.; Gilfanov, M.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Grainge, K. J. B.; Gratton, S.; Gregorio, A.; Groeneboom, N., E.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison, D.; Hempel, A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.; Hurley-Walker, N.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J.-M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leahy, J. P.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.; Li, C.; Liddle, A.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Mei, S.; Meinhold, P. R.; Melchiorri, A.; Melin, J.-B.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mikkelsen, K.; Mitra, S.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nastasi, A.; Nati, F.; Natoli, P.; Nesvadba, N. P. H.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Olamaie, M.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrott, Y. C.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J.-L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rumsey, C.; Rusholme, B.; Sandri, M.; Santos, D.; Saunders, R. D. E.; Savini, G.; Schammel, M. P.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Shimwell, T. W.; Spencer, L. D.; Starck, J.-L.; Stolyarov, V.; Stompor, R.; Streblyanska, A.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tramonte, D.; Tristram, M.; Tucci, M.; Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vibert, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; White, M.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.

2015-09-01

We update the all-sky Planck catalogue of 1227 clusters and cluster candidates (PSZ1) published in March 2013, derived from detections of the Sunyaev-Zeldovich (SZ) effect using the first 15.5 months of Planck satellite observations. As an addendum, we deliver an updated version of the PSZ1 catalogue, reporting the further confirmation of 86 Planck-discovered clusters. In total, the PSZ1 now contains 947 confirmed clusters, of which 214 were confirmed as newly discovered clusters through follow-up observations undertaken by the Planck Collaboration. The updated PSZ1 contains redshifts for 913 systems, of which 736 (~ 80.6%) are spectroscopic, and associated mass estimates derived from the Yz mass proxy. We also provide a new SZ quality flag for the remaining 280 candidates. This flag was derived from a novel artificial neural-network classification of the SZ signal. Based on this assessment, the purity of the updated PSZ1 catalogue is estimated to be 94%. In this release, we provide the full updated catalogue and an additional readme file with further information on the Planck SZ detections. The catalogue is 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/581/A14

A Self-consistent Thermal Emission Model for Io

NASA Astrophysics Data System (ADS)

Veeder, G. J.; Matson, D. L.; Johnson, T. V.; Davies, A. G.; Blaney, D. L.

2002-05-01

Io's unusual infrared properties first became evident in the 1960's when eclipse measurements and infrared radiometry yielded results that could not be easily explained by lunar-like models. When Voyager observations in 1979 discovered active volcanism and a geologically youthful surface some of the reasons for this bizarre behavior became evident. The first determination of Io's heat flow resulted from examining the signature of volcanic heat in telescopic observations (Matson et al., JGR, 86, 1664, 1981). Since then, numerous telescopic observations and Galileo observations have greatly expanded our understanding of Io's volcanism. However, significant problems remain. Any successful model must reconcile the various observations and constraints on Io's thermal output: 1. small volcanic hot spots; 2. multi-wavelength radiometry at all longitude; 3. multi-wavelength eclipse observations; and 4. temperature distributions observed by NIMS and PPR on Galileo. Two particularly difficult observational constraints have proved to be the daytime long-wavelength flux (20 microns) from Io, which is actually lower than expected for most passive models despite the obvious presence of volcanic contributions (Veeder et al., JGR, 99, 17095, 1994), and the surprising observation of ubiquitous warm regions at high latitudes in both the day and night (Spencer et al., Sci., 288, 1198, 2000; Rathbun et al., LPSC XXXIII, abs 1371, 2002). This paper presents preliminary results of a self-consistent thermal model that involves small volcanic hot spots, both high and low thermal inertia components on Io's surface, and significant thermal output from cooling lava flows preferentially at high latitudes. The resulting heat flow is ~ 3 W/m2, somewhat higher than previous estimates and well below the upper limit of 13.5 W/m2 derived earlier (Matson et al., JGR, 106, 33021, 2001).

High throughput transcriptome analysis of coffee reveals prehaustorial resistance in response to Hemileia vastatrix infection.

PubMed

Florez, Juan Carlos; Mofatto, Luciana Souto; do Livramento Freitas-Lopes, Rejane; Ferreira, Sávio Siqueira; Zambolim, Eunize Maciel; Carazzolle, Marcelo Falsarella; Zambolim, Laércio; Caixeta, Eveline Teixeira

2017-12-01

We provide a transcriptional profile of coffee rust interaction and identified putative up regulated resistant genes Coffee rust disease, caused by the fungus Hemileia vastatrix, is one of the major diseases in coffee throughout the world. The use of resistant cultivars is considered to be the most effective control strategy for this disease. To identify candidate genes related to different mechanism defense in coffee, we present a time-course comparative gene expression profile of Caturra (susceptible) and Híbrido de Timor (HdT, resistant) in response to H. vastatrix race XXXIII infection. The main objectives were to obtain a global overview of transcriptome in both interaction, compatible and incompatible, and, specially, analyze up-regulated HdT specific genes with inducible resistant and defense signaling pathways. Using both Coffea canephora as a reference genome and de novo assembly, we obtained 43,159 transcripts. At early infection events (12 and 24 h after infection), HdT responded to the attack of H. vastatrix with a larger number of up-regulated genes than Caturra, which was related to prehaustorial resistance. The genes found in HdT at early hours were involved in receptor-like kinases, response ion fluxes, production of reactive oxygen species, protein phosphorylation, ethylene biosynthesis and callose deposition. We selected 13 up-regulated HdT-exclusive genes to validate by real-time qPCR, which most of them confirmed their higher expression in HdT than in Caturra at early stage of infection. These genes have the potential to assist the development of new coffee rust control strategies. Collectively, our results provide understanding of expression profiles in coffee-H. vastatrix interaction over a time course in susceptible and resistant coffee plants.

Meiotic recombination counteracts male-biased mutation (male-driven evolution).

PubMed

Mawaribuchi, Shuuji; Ito, Michihiko; Ogata, Mitsuaki; Oota, Hiroki; Katsumura, Takafumi; Takamatsu, Nobuhiko; Miura, Ikuo

2016-01-27

Meiotic recombination is believed to produce greater genetic variation despite the fact that deoxyribonucleic acid (DNA)-replication errors are a major source of mutations. In some vertebrates, mutation rates are higher in males than in females, which developed the theory of male-driven evolution (male-biased mutation). However, there is little molecular evidence regarding the relationships between meiotic recombination and male-biased mutation. Here we tested the theory using the frog Rana rugosa, which has both XX/XY- and ZZ/ZW-type sex-determining systems within the species. The male-to-female mutation-rate ratio (α) was calculated from homologous sequences on the X/Y or Z/W sex chromosomes, which supported male-driven evolution. Surprisingly, each α value was notably higher in the XX/XY-type group than in the ZZ/ZW-type group, although α should have similar values within a species. Interestingly, meiotic recombination between homologous chromosomes did not occur except at terminal regions in males of this species. Then, by subdividing α into two new factors, a replication-based male-to-female mutation-rate ratio (β) and a meiotic recombination-based XX-to-XY/ZZ-to-ZW mutation-rate ratio (γ), we constructed a formula describing the relationship among a nucleotide-substitution rate and the two factors, β and γ. Intriguingly, the β- and γ-values were larger and smaller than 1, respectively, indicating that meiotic recombination might reduce male-biased mutations. © 2016 The Author(s).

The first case of 38,XX (SRY-positive) disorder of sex development in a cat.

PubMed

Szczerbal, Izabela; Stachowiak, Monika; Dzimira, Stanislaw; Sliwa, Krystyna; Switonski, Marek

2015-01-01

SRY-positive XX testicular disorder of sex development (DSD) caused by X;Y translocations was not yet reported in domestic animals. In humans it is rarely diagnosed and a majority of clinical features resemble those which are typical for Klinefelter syndrome (KS). Here we describe the first case of SRY-positive XX DSD in a tortoiseshell cat with a rudimentary penis and a lack of scrotum. Molecular analysis showed the presence of two Y-linked genes (SRY and ZFY) and a normal sequence of the SRY gene. Application of classical cytogenetic techniques revealed two X chromosomes (38,XX), but further FISH studies with the use of the whole X chromosome painting probe and BAC probes specific to the Yp chromosome facilitated identification of Xp;Yp translocation. The SRY gene was localised at a distal position of Xp. The karyotype of the studied case was described as: 38,XX.ish der(X)t(X;Y)(p22;p12)(SRY+). Moreover, the X inactivation status assessed by a sequential R-banding and FISH with the SRY-specific probe showed a random inactivation of the derivative X(SRY) chromosome. Our study showed that among DSD tortoiseshell cats, apart from XXY trisomy and XX/XY chimerism, also SRY-positive XX cases may occur. It is hypothesized that the extremely rare occurrence of this abnormality in domestic animals, when compared with humans, may be associated with a different organisation of the Yp arm in these species.

Molecular technique reveals high variability of 18S rDNA distribution in harvestmen (Opiliones, Phalangiidae) from South Africa

PubMed Central

Šťáhlavský, František; Opatova, Vera; Just, Pavel; Lotz, Leon N.; Haddad, Charles R.

2018-01-01

Abstract The knowledge of cytogenetics in the harvestmen family Phalangiidae has been based on taxa from the Northern Hemisphere. We performed cytogenetic analysis on Guruia africana (Karsch, 1878) (2n=24) and four species of the genus Rhampsinitus Simon, 1879 (2n=24, 26, 34) from South Africa. Fluorescence in situ hybridization with an 18S rDNA probe was used to analyze the number and the distribution of this cluster in the family Phalangiidae for the first time. The results support the cytogenetic characteristics typical for the majority of harvestmen taxa, i.e. the predominance of small biarmed chromosomes and the absence of morphologically well-differentiated sex chromosomes as an ancestral state. We identified the number of 18S rDNA sites ranging from two in R. qachasneki Kauri, 1962 to seven in one population of R. leighi Pocock, 1903. Moreover, we found differences in the number and localization of 18S rDNA sites in R. leighi between populations from two localities and between sexes of R. capensis (Loman, 1898). The heterozygous states of the 18S rDNA sites in these species may indicate the presence of XX/XY and ZZ/ZW sex chromosomes, and the possible existence of these systems in harvestmen is discussed. The variability of the 18S rDNA sites indicates intensive chromosomal changes during the differentiation of the karyotypes, which is in contrast to the usual uniformity in chromosomal morphology known from harvestmen so far. PMID:29675136

Molecular technique reveals high variability of 18S rDNA distribution in harvestmen (Opiliones, Phalangiidae) from South Africa.

PubMed

Šťáhlavský, František; Opatova, Vera; Just, Pavel; Lotz, Leon N; Haddad, Charles R

2018-01-01

The knowledge of cytogenetics in the harvestmen family Phalangiidae has been based on taxa from the Northern Hemisphere. We performed cytogenetic analysis on Guruia africana (Karsch, 1878) (2n=24) and four species of the genus Rhampsinitus Simon, 1879 (2n=24, 26, 34) from South Africa. Fluorescence in situ hybridization with an 18S rDNA probe was used to analyze the number and the distribution of this cluster in the family Phalangiidae for the first time. The results support the cytogenetic characteristics typical for the majority of harvestmen taxa, i.e. the predominance of small biarmed chromosomes and the absence of morphologically well-differentiated sex chromosomes as an ancestral state. We identified the number of 18S rDNA sites ranging from two in R. qachasneki Kauri, 1962 to seven in one population of R. leighi Pocock, 1903. Moreover, we found differences in the number and localization of 18S rDNA sites in R. leighi between populations from two localities and between sexes of R. capensis (Loman, 1898). The heterozygous states of the 18S rDNA sites in these species may indicate the presence of XX/XY and ZZ/ZW sex chromosomes, and the possible existence of these systems in harvestmen is discussed. The variability of the 18S rDNA sites indicates intensive chromosomal changes during the differentiation of the karyotypes, which is in contrast to the usual uniformity in chromosomal morphology known from harvestmen so far.

Discovery of the youngest sex chromosomes reveals first case of convergent co-option of ancestral autosomes in turtles.

PubMed

Montiel, E E; Badenhorst, D; Tamplin, J; Burke, R L; Valenzuela, N

2017-02-01

Most turtle species possess temperature-dependent sex determination (TSD), but genotypic sex determination (GSD) has evolved multiple times independently from the TSD ancestral condition. GSD in animals typically involves sex chromosomes, yet the sex chromosome system of only 9 out of 18 known GSD turtles has been characterized. Here, we combine comparative genome hybridization (CGH) and BAC clone fluorescent in situ hybridization (BAC FISH) to identify a macro-chromosome XX/XY system in the GSD wood turtle Glyptemys insculpta (GIN), the youngest known sex chromosomes in chelonians (8-20 My old). Comparative analyses show that GIN-X/Y is homologous to chromosome 4 of Chrysemys picta (CPI) painted turtles, chromosome 5 of Gallus gallus chicken, and thus to the X/Y sex chromosomes of Siebenrockiella crassicollis black marsh turtles. We tentatively assign the gene content of the mapped BACs from CPI chromosome 4 (CPI-4) to GIN-X/Y. Chromosomal rearrangements were detected in G. insculpta sex chromosome pair that co-localize with the male-specific region of GIN-Y and encompass a gene involved in sexual development (Wt1-a putative master gene in TSD turtles). Such inversions may have mediated the divergence of G. insculpta sex chromosome pair and facilitated GSD evolution in this turtle. Our results illuminate the structure, origin, and evolution of sex chromosomes in G. insculpta and reveal the first case of convergent co-option of an autosomal pair as sex chromosomes within chelonians.

Monograph of Coccinia (Cucurbitaceae)

PubMed Central

Holstein, Norbert

2015-01-01

Abstract This monograph deals with all 95 names described in the Cucurbitaceae genus Coccinia and recognizes 25 species. Taxonomic novelties are Coccinia adoensis var. aurantiaca (C.Jeffrey) Holstein, stat. nov., Coccinia sessilifolia var. variifolia (A.Meeuse) Holstein, stat. nov., and Coccinia adoensis var. jeffreyana Holstein, var. nov. For the 25 species 3157 collections were examined, of which 2024 were georeferenced to produce distribution maps. All species are distributed in sub-Saharan Africa with one species, Coccinia grandis, extending from Senegal in West Africa east to Indonesia and being naturalized on Pacific Islands, in Australia, the Caribbean, and South America. Coccinia species are dioecious creepers or climbers with simple or bifid tendrils that occupy a range of habitats from arid scrubland, woodlands to lowland rainforest and mist forest. The corolla of Coccinia species is sympetalous, usually pale yellow to orange, and 1 to 4.5 cm long. Pollination is by bees foraging for pollen or nectar. After pollination, the developing ovary often exhibits longitudinal mottling, which usually disappears during maturation. All species produce berries with a pericarp in reddish colors (orange-red through to scarlet red), hence the generic name. The globose to cylindrical fruits contain numerous grayish-beige flat to lenticular seeds. Chromosome numbers are 2n = 20, 24, and 22 + XX/XY. Many Coccinia species are used for food, either as roasted tubers, greens as spinach, or the fruits as vegetables. Medicinal value is established in Coccinia grandis, of which leaves and sap are used against diabetes. PMID:26312043

X-ray studies on crystalline complexes involving amino acids and peptides. XXXII. Effect of chirality on ionisation state, stoichiometry and aggregation in the complexes of oxalic acid with DL- and L-lysine.

PubMed

Venkatraman, J; Prabu, M M; Vijayan, M

1997-08-01

Crystals of the oxalic acid complex of DL-lysine (triclinic P1; a = 5.540(1), b = 10.764(2), c = 12.056(2) A, alpha = 77.8(1), beta = 80.6(1), gamma = 75.6(1).; R = 4.7% for 2023 observed reflections) contain lysine and semioxalate ions in the 1:1 ratio, whereas the ratio of lysine and semioxalate/oxalate ions is 2:3 in the crystals of the L-lysine complex (monoclinic P2(1); alpha = 4.906(1), b = 20.145(4), c = 12.455(1) A, beta = 92.5(1).; R = 4.4% for 1494 observed reflections). The amino acid molecule in the L-lysine complex has an unusual ionisation state with positively charged alpha- and side-chain amino groups and a neutral carboxyl group. The unlike molecules aggregate into separate alternating layers in the DL-lysine complex in a manner similar to that observed in several of the amino acid complexes. The L-lysine complex exhibits a new aggregation pattern which cannot be easily explained in terms of planar features, thus emphasizing the fundamental dependence of aggregation on molecular characteristics. Despite the differences in stoichiometry, ionisation state and long-range aggregation patterns, the basic element of aggregation in the two complexes exhibits considerable similarity.

On the Spectral Variance of MGS TES Spectra in the 300-500 cm-1 Range

NASA Astrophysics Data System (ADS)

Altieri, F.; Bellucci, G.

2001-11-01

The Thermal Emission Spectrometer (TES) aboard NASA mission Mars Global Surveyor (MGS) is collecting 200 - 1600 cm-1 thermal emission spectra since September 1997. The principal purpose of TES is to determine and map the Mars surface composition. Spectral features directly ascribable to surface minerals have been identified in the 300 - 500 cm-1 spectral range. Outcrops of hematite have been localized in Sinus Meridiani, Aram Chaos and Valles Marineris [1, 2] and areas with olivine have been individuated in Nili Fossae and in other limited regions [3]. On the other hand, TES spectra show, in general, significant variance between 300 and 500 cm-1; this variance is not directly attributable to surface mineralogical components. In this study we report some examples of spectra with typical hematite and olivine bands and spectra with a different spectral contrast. The spectral masking effect of a dust layer is suggested to explain this behaviour. Spectra characterized by hematite features have been localized also inside a crater near Baldet Crater. The MOC narrow-angle image M02-0039 acquired on the same area shows dark layers at the crater bottom. References: [1] Christensen P. R., et al., JGR, 105, 9623-9642, 2000. [2] Christensen P. R., et al., JGR, in press., 2001. [3] Hoefen T. M. and Clark R. N., LPS XXXII, 2049, 2001.

Increased high-density lipoprotein cholesterol levels in mice with XX versus XY sex chromosomes.

PubMed

Link, Jenny C; Chen, Xuqi; Prien, Christopher; Borja, Mark S; Hammerson, Bradley; Oda, Michael N; Arnold, Arthur P; Reue, Karen

2015-08-01

The molecular mechanisms underlying sex differences in dyslipidemia are poorly understood. We aimed to distinguish genetic and hormonal regulators of sex differences in plasma lipid levels. We assessed the role of gonadal hormones and sex chromosome complement on lipid levels using the four core genotypes mouse model (XX females, XX males, XY females, and XY males). In gonadally intact mice fed a chow diet, lipid levels were influenced by both male-female gonadal sex and XX-XY chromosome complement. Gonadectomy of adult mice revealed that the male-female differences are dependent on acute effects of gonadal hormones. In both intact and gonadectomized animals, XX mice had higher HDL cholesterol (HDL-C) levels than XY mice, regardless of male-female sex. Feeding a cholesterol-enriched diet produced distinct patterns of sex differences in lipid levels compared with a chow diet, revealing the interaction of gonadal and chromosomal sex with diet. Notably, under all dietary and gonadal conditions, HDL-C levels were higher in mice with 2 X chromosomes compared with mice with an X and Y chromosome. By generating mice with XX, XY, and XXY chromosome complements, we determined that the presence of 2 X chromosomes, and not the absence of the Y chromosome, influences HDL-C concentration. We demonstrate that having 2 X chromosomes versus an X and Y chromosome complement drives sex differences in HDL-C. It is conceivable that increased expression of genes escaping X-inactivation in XX mice regulates downstream processes to establish sexual dimorphism in plasma lipid levels. © 2015 American Heart Association, Inc.

Unique XCI evolution in Tokudaia: initial XCI of the neo-X chromosome in Tokudaia muenninki and function loss of XIST in Tokudaia osimensis.

PubMed

Zushi, Hideki; Murata, Chie; Mizushima, Shusei; Nishida, Chizuko; Kuroiwa, Asato

2017-12-01

X chromosome inactivation (XCI) is an essential mechanism to compensate gene dosage in mammals. Here, we show that XCI has evolved differently in two species of the genus Tokudaia. The Amami spiny rat, Tokudaia osimensis, has a single X chromosome in males and females (XO/XO). By contrast, the Okinawa spiny rat, Tokudaia muenninki, has XX/XY sex chromosomes like most mammals, although the X chromosome has acquired a neo-X region by fusion with an autosome. BAC clones containing the XIST gene, which produces the long non-coding RNA XIST required for XCI, were obtained by screening of T. osimensis and T. muenninki BAC libraries. Each clone was mapped to the homologous region of the X inactivation center in the X chromosome of the two species by BAC-FISH. XIST RNAs were expressed in T. muenninki females, whereas no expression was observed in T. osimensis. The sequence of the XIST RNA was compared with that of mouse, showing that the XIST gene is highly conserved in T. muenninki. XIST RNAs were localized to the ancestral X region (Xq), to the heterochromatic region (pericentromeric region), and partially to the neo-X region (Xp). The hybridization pattern correlated with LINE-1 accumulation in Xq but not in Xp. Dosage of genes located on the neo-X chromosome was not compensated, suggesting that the neo-X region is in an early state of XCI. By contrast, many mutations were observed in the XIST gene of T. osimensis, indicating its loss of function in the XO/XO species.

The chronostratigraphy of the Haua Fteah cave (Cyrenaica, northeast Libya).

PubMed

Douka, Katerina; Jacobs, Zenobia; Lane, Christine; Grün, Rainer; Farr, Lucy; Hunt, Chris; Inglis, Robyn H; Reynolds, Tim; Albert, Paul; Aubert, Maxime; Cullen, Victoria; Hill, Evan; Kinsley, Leslie; Roberts, Richard G; Tomlinson, Emma L; Wulf, Sabine; Barker, Graeme

2014-01-01

The 1950s excavations by Charles McBurney in the Haua Fteah, a large karstic cave on the coast of northeast Libya, revealed a deep sequence of human occupation. Most subsequent research on North African prehistory refers to his discoveries and interpretations, but the chronology of its archaeological and geological sequences has been based on very early age determinations. This paper reports on the initial results of a comprehensive multi-method dating program undertaken as part of new work at the site, involving radiocarbon dating of charcoal, land snails and marine shell, cryptotephra investigations, optically stimulated luminescence (OSL) dating of sediments, and electron spin resonance (ESR) dating of tooth enamel. The dating samples were collected from the newly exposed and cleaned faces of the upper 7.5 m of the ∼14.0 m-deep McBurney trench, which contain six of the seven major cultural phases that he identified. Despite problems of sediment transport and reworking, using a Bayesian statistical model the new dating program establishes a robust framework for the five major lithostratigraphic units identified in the stratigraphic succession, and for the major cultural units. The age of two anatomically modern human mandibles found by McBurney in Layer XXXIII near the base of his Levalloiso-Mousterian phase can now be estimated to between 73 and 65 ka (thousands of years ago) at the 95.4% confidence level, within Marine Isotope Stage (MIS) 4. McBurney's Layer XXV, associated with Upper Palaeolithic Dabban blade industries, has a clear stratigraphic relationship with Campanian Ignimbrite tephra. Microlithic Oranian technologies developed following the climax of the Last Glacial Maximum and the more microlithic Capsian in the Younger Dryas. Neolithic pottery and perhaps domestic livestock were used in the cave from the mid Holocene but there is no certain evidence for plant cultivation until the Graeco-Roman period. Copyright © 2013 Elsevier Ltd. All rights reserved.

Possible Phosphate Redistribution on the Martian Surface: Implication From Simulation Experiments

NASA Astrophysics Data System (ADS)

Dreibus, G.; Haubold, R.; Jagoutz, E.

2001-12-01

The chemical composition of Martian rocks and soils as measured with the APXS (Alpha Proton X-ray Spectrometer) of the Mars Pathfinder Mission are very different [1]. Surprisingly, only small differences of the phosphorous concentrations between soils and rocks were found. The P concentration of about 4000 ppm is similar to that measured in basaltic shergottites. Phosphates are the host mineral for the REE, Th and U. Leach experiments with slightly acidified brines on basaltic shergottites easily dissolved more than a half of the REEs and U whereas K remained insoluble. Therefore, we suggested the possibility of alteration and mobilization of phosphates in the Martian environment with the result of an enrichment of U, Th, and consequently P on the surface. However, the APXS measured no P enrichment in rocks and soil of the Martian crust, whereas a high Th concentration on the surface was measured with the gamma-spectroscopy from orbit by Mars-5 and Phobos-2 [2]. With leach experiments on terrestrial samples we studied the solubility of U and Th as in the case of shergottites, but also that of phosphorous. Furthermore, simulation experiments of reactions between slightly acidified calcium-phosphate solution and different terrestrial rock types were performed to clarify the redistribution of P at the Martian surface with its complex weathering history. Ref.: [1] Brueckner J. et al. (2001) Lunar Planet. Science. XXXII, 1293; [2] Surkov Yu. A. et al. (1989) Nature 341, 595.

Elemental abundance analyses with DAO spectrograms: XXXII. HR 6455 (A3 III), δ Aqr (A3 V), η Lep (F2 V), and 1 Boo (A1 V)

NASA Astrophysics Data System (ADS)

Yüce, K.; Adelman, S. J.; Gulliver, A. F.; Hill, G.

2011-08-01

We examine the sharp-lined stars HR 6455 (A3 III, v sin i = 8.7 km s-1) and η Lep (F2 V, v sin i = 13.5 km s-1) as well as δ Aqr (A3 V, v sin i = 81 km s-1) and 1 Boo (A1 V, v sin i = 59 km s-1) to increase the number consistently analyzed A and F stars using high dispersion and high S/N (≥200) spectrograms obtained with CCD detectors at the long Coudé camera of the 1.22-m telescope of the Dominion Astrophysical Observatory. Such studies contribute to understanding systematic abundance differences between normal and non-magnetic main-sequence band chemically peculiar A and early F stars. LTE fine analyses of HR 6455, δ Aqr, and 1 Boo using Kurucz's ATLAS suite programs show the same general elemental abundance trends with differences in the metal richness. Light and iron-peak element abundances are generally solar or overabundant while heavy element and rare earth element abundances are overabundant. HR 6455 is an evolved Am star while δ Aqr and 1 Boo show the phenomenon to different extents. Most derived abundances of η Lep are solar. Table 3 is available at the CDS via http://cdsarc.u-strasbg.fr/cgi-bin/qcat?J/AN/332/681

A Brief Review of the Lithology and Petrology of the Tagish Lake Meteorite Type Specimen

NASA Astrophysics Data System (ADS)

Herd, R. K.

2009-05-01

The mineralogical and textural characteristics of the type specimen of the Tagish Lake meteorite were described previously [1,2]. These initial descriptions recognized two lithologies, one relatively carbonate-poor, and the other relatively carbonate-rich. In addition numerous lithic fragments within the main lithologies were noted, essentially brecciated fragments within brecciated fragments [2,3]. Most research on the meteorite has generally assumed that only two lithologies were present. Many preliminary mineral and organic analyses done on pristine and non-pristine samples cannot be related to a particular matrix -- neither to the two supposed to be present, nor to any others. Distinction has sometimes been made between chondrule-bearing lithologies or fragments, and non-chondrule-bearing, or so-called dark dusty, lithologies preserved in the pristine specimen suite. To aid in a systematic approach to understanding this unique meteorite, the main petrographic features of the type specimen polished section are reviewed, based on back-scattered electron (BSE) images and electron- microprobe (EM) analyses. What is still needed is a consortium study of the pristine and non-pristine samples, that would define all the lithologies present and their inter-relationships, within the complete specimen suite, as the context and framework for ongoing research. [1] Brown, P.G. et al. (2000) Science, 290, 320-325. [2] Herd, R.K. et al. (2001) LPS XXXII, Abstract 1928. [3] Herd, R.K. and Herd, C.D.K. (2007) LPS XXXVIII, Abstract 2347.

ddRADseq reveals determinants for temperature-dependent sex reversal in Nile tilapia on LG23.

PubMed

Wessels, Stephan; Krause, Ina; Floren, Claudia; Schütz, Ekkehard; Beck, Jule; Knorr, Christoph

2017-07-14

In Nile tilapia sex determination is governed by a male heterogametic system XX/XY either on LG1 or LG23. The latter carries a Y-specific duplicate of the amh gene, which is a testis-determining factor. Allelic variants in the amh gene demonstrated to be major triggers for autosomal and temperature-dependent sex reversal. Further, QTL on LG23 and LG20 show a temperature-responsiveness with influence on the phenotypic sex relative to the sex chromosomes. Here we present a ddRADseq based approach to identify genomic regions that show unusual large differentiation in terms of fixation index (F ST ) between temperature-treated pseudomales and non-masculinized females using a comparative genome-scan. Genome-wide associations were identified for the temperature-dependent sex using a genetically all-female population devoid of amh-ΔY. Twenty-two thousand three hundred ninety-two SNPs were interrogated for the comparison of temperature-treated pseudomales and females, which revealed the largest differentiation on LG23. Outlier F ST -values (0.35-0.44) were determined for six SNPs in the genomic interval (9,190,077-11,065,693) harbouring the amh gene (9,602,693-9,605,808), exceeding the genome-wide low F ST of 0.013. Association analysis with a set of 9104 selected SNPs confirmed that the same genomic region on LG23 exerts a significant effect on the temperature-dependent sex. This study highlights the role of LG23 in sex determination, harbouring major determinants for temperature-dependent sex reversal in Nile tilapia. Furthermore F ST outlier detection proves a powerful tool for detection of sex-determining regions in fish genomes.

High temperature increases the masculinization rate of the all-female (XX) rainbow trout "Mal" population.

PubMed

Valdivia, Karina; Jouanno, Elodie; Volff, Jean-Nicolas; Galiana-Arnoux, Delphine; Guyomard, René; Helary, Louise; Mourot, Brigitte; Fostier, Alexis; Quillet, Edwige; Guiguen, Yann

2014-01-01

Salmonids are generally considered to have a robust genetic sex determination system with a simple male heterogamety (XX/XY). However, spontaneous masculinization of XX females has been found in a rainbow trout population of gynogenetic doubled haploid individuals. The analysis of this masculinization phenotype transmission supported the hypothesis of the involvement of a recessive mutation (termed mal). As temperature effect on sex differentiation has been reported in some salmonid species, in this study we investigated in detail the potential implication of temperature on masculinization in this XX mal-carrying population. Seven families issued from XX mal-carrying parents were exposed from the time of hatching to different rearing water temperatures ((8, 12 and 18°C), and the resulting sex-ratios were confirmed by histological analysis of both gonads. Our results demonstrate that masculinization rates are strongly increased (up to nearly two fold) at the highest temperature treatment (18°C). Interestingly, we also found clear differences between temperatures on the masculinization of the left versus the right gonads with the right gonad consistently more often masculinized than the left one at lower temperatures (8 and 12°C). However, the masculinization rate is also strongly dependent on the genetic background of the XX mal-carrying families. Thus, masculinization in XX mal-carrying rainbow trout is potentially triggered by an interaction between the temperature treatment and a complex genetic background potentially involving some part of the genetic sex differentiation regulatory cascade along with some minor sex-influencing loci. These results indicate that despite its rather strict genetic sex determinism system, rainbow trout sex differentiation can be modulated by temperature, as described in many other fish species.

The new Andean Regional Office of Astronomy for Development (ROAD)

NASA Astrophysics Data System (ADS)

Char, Farid; Forero-Romero, Jaime

2015-08-01

The Andean Regional Office of Astronomy for Development (ROAD) is a new effort in South America to serve several goals in astronomical development. Six countries (Bolivia, Colombia, Chile, Ecuador, Perú and Venezuela) will work together, representing a common language block in the Andean region and focusing on develop strategies to strengthen the professional research, education and popularization of astronomy. Our current Working Structure comprises a ROAD Coordinator and Coordinators per Task Force, as well as Organizing Committees, Collaborators and Volunteers.The participating institutions of this new ROAD have been involved in many projects involving each of the current OAD’s Task Forces: research, schools and children and public, exploring educational activities/material to be shared among the Andean countries, standardizing the knowledge and creating inspirational experiences. We expect to generate many efforts in order to bring a more homogeneous activity in each Andean country, taking into account the special role of Chile in global astronomy, due to its great conditions for astronomy and the involvement of many professional observatories, universities and astronomy institutions.Our current (and upcoming) most relevant activities includes: Andean Schools on Astronomy, Andean Graduate Program and Massive Open Online Courses (TF1); Virtual Training Sessions and Teaching material for the visually impaired students; Annual TF2 meeting to gather all the collaborators (TF2); Development for planetariums and Communicating Astronomy with the Public (TF3). The Andean region, in the other hand, will also be involved in at least two important events: the CAP Meeting in May 2016 and the XV LARIM in October 2016 (both in Colombia); and Chile will bid to host the XXXI IAU GA in 2021, with the aim of show the great advances in astronomical development from the Andean region and South America.

High Temperature Increases the Masculinization Rate of the All-Female (XX) Rainbow Trout “Mal” Population

PubMed Central

Valdivia, Karina; Jouanno, Elodie; Volff, Jean-Nicolas; Galiana-Arnoux, Delphine; Guyomard, René; Helary, Louise; Mourot, Brigitte; Fostier, Alexis; Quillet, Edwige; Guiguen, Yann

2014-01-01

Salmonids are generally considered to have a robust genetic sex determination system with a simple male heterogamety (XX/XY). However, spontaneous masculinization of XX females has been found in a rainbow trout population of gynogenetic doubled haploid individuals. The analysis of this masculinization phenotype transmission supported the hypothesis of the involvement of a recessive mutation (termed mal). As temperature effect on sex differentiation has been reported in some salmonid species, in this study we investigated in detail the potential implication of temperature on masculinization in this XX mal-carrying population. Seven families issued from XX mal-carrying parents were exposed from the time of hatching to different rearing water temperatures ((8, 12 and 18°C), and the resulting sex-ratios were confirmed by histological analysis of both gonads. Our results demonstrate that masculinization rates are strongly increased (up to nearly two fold) at the highest temperature treatment (18°C). Interestingly, we also found clear differences between temperatures on the masculinization of the left versus the right gonads with the right gonad consistently more often masculinized than the left one at lower temperatures (8 and 12°C). However, the masculinization rate is also strongly dependent on the genetic background of the XX mal-carrying families. Thus, masculinization in XX mal-carrying rainbow trout is potentially triggered by an interaction between the temperature treatment and a complex genetic background potentially involving some part of the genetic sex differentiation regulatory cascade along with some minor sex-influencing loci. These results indicate that despite its rather strict genetic sex determinism system, rainbow trout sex differentiation can be modulated by temperature, as described in many other fish species. PMID:25501353

VIII Olimpíada Brasileira de Astronomia e Astronáutica

NASA Astrophysics Data System (ADS)

Garcia Canalle, João Batista; Villas da Rocha, Jaime Fernando; Wuensche de Souza, Carlos Alexandre; Pereira Ortiz, Roberto; Aguilera, Nuricel Villalonga; Padilha, Maria De Fátima Catta Preta; Pessoa Filho, José Bezerra; Soares Rodrigues, Ivette Maria

2007-07-01

Neste trabalho apresentamos as motivações pelas quais organizamos, em conjunto, pela primeira vez, a Olimpíada Brasileira de Astronomia incluindo a Astronáutica, em colaboração com a Agência Espacial Brasileira. Esta ampliação contribuiu para atrair ainda mais alunos, professores, escolas e patrocinadores para participarem desta Olimpíada. Em 2005 participaram da VIII Olimpíada Brasileira de Astronomia e Astronáutica (VIII OBA) 187.726 alunos distribuídos por 3.229 escolas, pertencentes a todos os estados brasileiros, incluindo o Distrito Federal. O crescimento em número de alunos participantes foi 52,4% maior do que em 2004. Em abril de 2005 organizamos, em Itapecerica da Serra, SP, um curso para os 50 alunos previamente selecionados e participantes da VII OBA e ao final selecionamos, dentre eles, uma equipe de 5 alunos, os quais representaram o Brasil na X Olimpíada Internacional de Astronomia, na China, em outubro de 2005. Ganhamos, pela primeira vez, uma medalha de ouro naquele evento. Em Agosto de 2005, organizamos a VIII Escola de Agosto para 50 alunos e respectivos professores, em Águas de Lindóia, SP, juntamente com a XXXI reunião anual da Sociedade Astronômica Brasileira (SAB). Em novembro de 2005 realizamos a I Jornada Espacial, em São José dos Campos, com 22 alunos e 22 professores selecionados dentre os participantes que melhores resultados obtiveram nas questões de Astronáutica da VIII OBA. Neste trabalho detalhamos os resultados da VIII OBA bem como as ações subseqüentes.

Independent degeneration of W and Y sex chromosomes in frog Rana rugosa.

PubMed

Miura, Ikuo; Ohtani, Hiromi; Ogata, Mitsuaki

2012-01-01

The frog Rana rugosa uniquely possesses two different sex-determining systems of XX/XY and ZZ/ZW, separately in the geographic populations. The sex chromosomes of both types share the same origin at chromosome 7, and the structural differences between X and Y or Z and W were evolved through two inversions. In order to ascertain the mechanisms of degeneration of W and Y chromosomes, we gynogenetically produced homozygous diploids WW and YY and examined their viability. Tadpoles from geographic group N (W(N)W(N)) containing three populations died of edema at an early developmental stage within 10 days after hatching, while tadpoles from the geographic group K (W(K)W(K)) that contained two populations died of underdeveloped growth at a much later stage, 40-50 days after fertilization. On the contrary, W(N)W(K) and W(K)W(N) hybrid embryos were viable, successfully passed the two lethal stages, and survived till the attainment of adulthood. The observed survival implies that the lethal genes of the W chromosomes are not shared by the two groups and thus demonstrates their independent degeneration histories between the local groups. In sharp contrast, a sex-linked gene of androgen receptor gene (AR) from the W chromosome was down-regulated in expression in both the groups, suggesting that inactivation of the W-AR allele preceded divergence of the two groups and appearance of the lethal genes. Besides, the YY embryos died of cardiac edema immediately after hatching. The symptom of lethality and the stage of developmental arrest differed from those for either of WW lethal embryos. We therefore conclude that the W and Y chromosomes involve no evolutionary common scenario for degeneration.

Chromosomal Context Affects the Molecular Evolution of Sex-linked Genes and Their Autosomal Counterparts in Turtles and Other Vertebrates.

PubMed

Radhakrishnan, Srihari; Valenzuela, Nicole

2017-10-30

Sex chromosomes evolve differently from autosomes because natural selection acts distinctly on them given their reduced recombination and smaller population size. Various studies of sex-linked genes compared with different autosomal genes within species support these predictions. Here, we take a novel alternative approach by comparing the rate of evolution between subsets of genes that are sex-linked in selected reptiles/vertebrates and the same genes located in autosomes in other amniotes. We report for the first time the faster evolution of Z-linked genes in a turtle (the Chinese softshell turtle Pelodiscus sinensis) relative to autosomal orthologs in other taxa, including turtles with temperature-dependent sex determination (TSD). This faster rate was absent in its close relative, the spiny softshell turtle (Apalone spinifera), thus revealing important lineage effects, and was only surpassed by mammalian-X linked genes. In contrast, we found slower evolution of X-linked genes in the musk turtle Staurotypus triporcatus (XX/XY) and homologous Z-linked chicken genes. TSD lineages displayed overall faster sequence evolution than taxa with genotypic sex determination (GSD), ruling out global effects of GSD on molecular evolution beyond those by sex-linkage. Notably, results revealed a putative selective sweep around two turtle genes involved in vertebrate gonadogenesis (Pelodiscus-Z-linked Nf2 and Chrysemys-autosomal Tspan7). Our observations reveal important evolutionary changes at the gene level mediated by chromosomal context in turtles despite their low overall evolutionary rate and illuminate sex chromosome evolution by empirically testing expectations from theoretical models. Genome-wide analyses are warranted to test the generality and prevalence of the observed patterns. © The American Genetic Association 2017. All rights reserved. For permissions, please e-mail: journals.permissions@oup.com.

Variability of nutritional and cooking quality in bean (Phaseolus vulgaris L) as a function of genotype.

PubMed

Saha, Supradip; Singh, Gyanendra; Mahajan, V; Gupta, H S

2009-06-01

Screening of natural biodiversity for the better quality traits are of prime importance for quality breeding programs. The objective of this investigation was to select candidate accession of bean having high concentrations of protein as well as macro and micro minerals with good cooking quality for use as parents in breeding programme for these compounds. Thirty-five accessions of bean (Phaseolus vulgaris L) were field grown and their seeds were analyzed for their cooking quality and nutritional composition. Wide variations were observed in most of the measurements e.g. protein (18.7-26.2%), iron (79.4-137.6 ppm) and hardness after cooking (4.65-9.88 Kg) suggesting that there are considerable levels of genetic diversity. Across all accessions the concentration of potassium was negatively correlated with protein (r = -0.43, P < 0.05). Concentrations of protein was significantly greater in accessions VIII, XIII and XIX compared to other accessions analyzed. Iron concentrations were greatest (137 ppm) in XIX and lowest (79 ppm) in XXVII. Lines with less cooking time were line III, X, XXVI, XXX and XXXI. Bean line XIX contains high protein (24.9%) with high zinc (33.3 ppm) and highest iron (137.6 ppm), but it has high hardness after cooking (7.32 kg). Four clusters were computed by cluster analysis that explained quite a good variation in the traits. The great variability for these attributes suggests that these selected accessions may be useful as parents in hybridization programs to produce bean with value-added traits. This information was also potentially useful for pulse breeders working on the development of new varieties.

CD24-Positive Cells from Normal Adult Mouse Liver Are Hepatocyte Progenitor Cells

PubMed Central

Qiu, Qiong; Hernandez, Julio Cesar; Dean, Adam M.; Rao, Pulivarthi H.

2011-01-01

The identification of specific cell surface markers that can be used to isolate liver progenitor cells will greatly facilitate experimentation to determine the role of these cells in liver regeneration and their potential for therapeutic transplantation. Previously, the cell surface marker, CD24, was observed to be expressed on undifferentiated bipotential mouse embryonic liver stem cells and 3,5-diethoxycarbonyl-1,4-dihydrocollidine-induced oval cells. Here, we describe the isolation and characterization of a rare, primary, nonhematopoietic, CD24+ progenitor cell population from normal, untreated mouse liver. By immunohistochemistry, CD24-expressing cells in normal adult mouse liver were colocalized with CK19-positive cholangiocytes. This nonhematopoietic (CD45−, Ter119−) CD24+ cell population isolated by flow cytometry represented 0.04% of liver cells and expressed several markers of liver progenitor/oval cells. The immunophenotype of nonhematopoietic CD24+ cells was CD133, Dlk, and Sca-1 high, but c-Kit, Thy-1, and CD34 low. The CD24+ cells had increased expression of CK19, epithelial cell adhesion molecule, Sox 9, and FN14 compared with the unsorted cells. Upon transplantation of nonhematopoietic CD24+ cells under the sub-capsule of the livers of Fah knockout mice, cells differentiated into mature functional hepatocytes. Analysis of X and Y chromosome complements were used to determine whether or not fusion of the engrafted cells with the recipient hepatocytes occurred. No cells were found that contained XXXY or any other combination of donor and host sex chromosomes as would be expected if cell fusion had occurred. These results suggested that CD24 can be used as a cell surface marker for isolation of hepatocyte progenitor cells from normal adult liver that are able to differentiate into hepatocytes. PMID:21361791

The VMC survey - XXXI. The spatially resolved star formation history of the main body of the Small Magellanic Cloud

NASA Astrophysics Data System (ADS)

Rubele, Stefano; Pastorelli, Giada; Girardi, Léo; Cioni, Maria-Rosa L.; Zaggia, Simone; Marigo, Paola; Bekki, Kenji; Bressan, Alessandro; Clementini, Gisella; de Grijs, Richard; Emerson, Jim; Groenewegen, Martin A. T.; Ivanov, Valentin D.; Muraveva, Tatiana; Nanni, Ambra; Oliveira, Joana M.; Ripepi, Vincenzo; Sun, Ning-Chen; van Loon, Jacco Th

2018-05-01

We recover the spatially resolved star formation history across the entire main body and Wing of the Small Magellanic Cloud (SMC), using fourteen deep tile images from the VISTA survey of the Magellanic Clouds (VMC), in the YJK_s filters. The analysis is performed on 168 subregions of size 0.143 deg2, covering a total contiguous area of 23.57 deg2. We apply a colour-magnitude diagram (CMD) reconstruction method that returns the best-fitting star formation rate SFR(t), age-metallicity relation, distance and mean reddening, together with their confidence intervals, for each subregion. With respect to previous analyses, we use a far larger set of VMC data, updated stellar models, and fit the two available CMDs (Y-K_s versus K_s and J-K_s versus K_s) independently. The results allow us to derive a more complete and more reliable picture of how the mean distances, extinction values, star formation rate, and metallicities vary across the SMC, and provide a better description of the populations that form its Bar and Wing. We conclude that the SMC has formed a total mass of (5.31 ± 0.05) × 108 M⊙ in stars over its lifetime. About two thirds of this mass is expected to be still locked in stars and stellar remnants. 50 per cent of the mass was formed prior to an age of 6.3 Gyr, and 80 per cent was formed between 8 and 3.5 Gyr ago. We also illustrate the likely distribution of stellar ages and metallicities in different parts of the CMD, to aid the interpretation of data from future astrometric and spectroscopic surveys of the SMC.

CD24-positive cells from normal adult mouse liver are hepatocyte progenitor cells.

PubMed

Qiu, Qiong; Hernandez, Julio Cesar; Dean, Adam M; Rao, Pulivarthi H; Darlington, Gretchen J

2011-12-01

The identification of specific cell surface markers that can be used to isolate liver progenitor cells will greatly facilitate experimentation to determine the role of these cells in liver regeneration and their potential for therapeutic transplantation. Previously, the cell surface marker, CD24, was observed to be expressed on undifferentiated bipotential mouse embryonic liver stem cells and 3,5-diethoxycarbonyl-1,4-dihydrocollidine-induced oval cells. Here, we describe the isolation and characterization of a rare, primary, nonhematopoietic, CD24+ progenitor cell population from normal, untreated mouse liver. By immunohistochemistry, CD24-expressing cells in normal adult mouse liver were colocalized with CK19-positive cholangiocytes. This nonhematopoietic (CD45-, Ter119-) CD24+ cell population isolated by flow cytometry represented 0.04% of liver cells and expressed several markers of liver progenitor/oval cells. The immunophenotype of nonhematopoietic CD24+ cells was CD133, Dlk, and Sca-1 high, but c-Kit, Thy-1, and CD34 low. The CD24+ cells had increased expression of CK19, epithelial cell adhesion molecule, Sox 9, and FN14 compared with the unsorted cells. Upon transplantation of nonhematopoietic CD24+ cells under the sub-capsule of the livers of Fah knockout mice, cells differentiated into mature functional hepatocytes. Analysis of X and Y chromosome complements were used to determine whether or not fusion of the engrafted cells with the recipient hepatocytes occurred. No cells were found that contained XXXY or any other combination of donor and host sex chromosomes as would be expected if cell fusion had occurred. These results suggested that CD24 can be used as a cell surface marker for isolation of hepatocyte progenitor cells from normal adult liver that are able to differentiate into hepatocytes.

Host-Pathogen Interactions : XXXII. A Fungal Glucan Preparation Protects Nicotianae against Infection by Viruses.

PubMed

Kopp, M; Rouster, J; Fritig, B; Darvill, A; Albersheim, P

1989-05-01

A glucan preparation obtained from the mycelial walls of the fungus Phytophthora megasperma f.sp. glycinea and known as an elicitor of phytoalexins in soybean was shown to be a very efficient inducer of resistance against viruses in tobacco. The glucan preparation protected against mechanically transmitted viral infections on the upper and lower leaf surfaces. Whether the glucan preparation was applied by injection, inoculation, or spraying, it protected the plants if applied before, at the same time as, or not later than 8 hours after virus inoculation. At concentrations ranging from 0.1 to 10 micrograms per milliliter, the glucan preparation induced protection ranging from 50 to 100% against both symptom production (necrotic local lesions, necrotic rings, or systemic mosaic) and virus accumulation in all Nicotiana-virus combinations examined. However, no significant protection against some of the same viruses was observed in bean or turnip. The host plants successfully protected included N. tabacum (9 different cultivars), N. sylvestris, N. glutinosa, and N. clevelandii. The viruses belonged to several taxonomic groups including tobacco mosaic virus, alfalfa mosaic virus, and tomato black ring virus. The glucan preparation did not act directly on the virus and did not interfere with virus disassembly; rather, it appeared to induce changes in the host plant that prevented infections from being initiated or recently established infections from enlarging. The induced resistance does not depend on induction of pathogenesis-related proteins, the phenylpropanoid pathway, lignin-like substances, or callose-like materials. We believe the induced resistance results from a mechanism that has yet to be described.

The HARPS search for southern extra-solar planets . XXXII. New multi-planet systems in the HARPS volume limited sample: a super-Earth and a Neptune in the habitable zone

NASA Astrophysics Data System (ADS)

Lo Curto, G.; Mayor, M.; Benz, W.; Bouchy, F.; Hébrard, G.; Lovis, C.; Moutou, C.; Naef, D.; Pepe, F.; Queloz, D.; Santos, N. C.; Segransan, D.; Udry, S.

2013-03-01

The vast diversity of planetary systems detected to date is defying our capability of understanding their formation and evolution. Well-defined volume-limited surveys are the best tool at our disposal to tackle the problem, via the acquisition of robust statistics of the orbital elements. We are using the HARPS spectrograph to conduct our survey of ≈850 nearby solar-type stars, and in the course of the past nine years we have monitored the radial velocity of HD 103774, HD 109271, and BD-061339. In this work we present the detection of five planets orbiting these stars, with msin (i) between 0.6 and 7 Neptune masses, four of which are in two multiple systems, comprising one super-Earth and one planet within the habitable zone of a late-type dwarf. Although for strategic reasons we chose efficiency over precision in this survey, we have the capability to detect planets down to the Neptune and super-Earth mass range as well as multiple systems, provided that enough data points are made available. Based on observations made with the HARPS instrument on the ESO 3.6 m telescope at La Silla (Chile), under the GTO program ID 072.C-0488 and the regular programs: 085.C-0019, 087.C-0831 and 089.C-0732. RV data are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/551/A59

Systemic lupus erythematosus in a multi-ethnic cohort (LUMINA) XXXII: [corrected] contributions of admixture and socioeconomic status to renal involvement.

PubMed

Alarcón, G S; Bastian, H M; Beasley, T M; Roseman, J M; Tan, F K; Fessler, B J; Vilá, L M; McGwin, G

2006-01-01

Renal involvement in systemic lupus erythematosus (SLE) is more frequent in minorities. We examined whether genetic or socioeconomic status (SES) explain these disparities in a large multiethnic (Hispanics from Texas and Puerto Rico, African Americans and Caucasians) SLE cohort. Renal involvement was defined as WHO Class II-V and/or proteinuria (> 0.5 g/24 h or 3+) attributable to SLE and/or abnormal urinary sediment, proteinuria 2+, elevated serum creatinine/ decreased creatinine clearance twice, 6 months apart present any time over the course of the disease. Ancestry informative markers (AIMS) were used to define the admixture proportions in each patient and group. Logistic regression models were examined to determine the percentage variance (R2) in renal involvement related to ethnicity that is explained by socio-economic status (SES) and admixture (adjusting for age, gender and disease duration, basic model). Four-hundred and fifty-nine (out of 575) patients were included; renal involvement occurred in 44.6% Texas Hispanics, 11.3% Puerto Rico Hispanics, 45.8% African Americans, 18.3% Caucasians. SES accounted for 14.5% of the variance due to ethnicity (after adjusting for basic model variables), admixture 36.8% and both, 12.2%; 45.9% of the variance remained unexplained. Alternative models for decreased glomerula filtration rate and end-stage renal disease were comparable in the distribution of the explanatory variables. Our data indicate that genetic factors appear to be more important than SES in explaining the ethnic disparities in the occurrence of renal involvement.

Ultrasound imaging for the rheumatologist. XXXII. Sonographic assessment of the foot in patients with psoriatic arthritis.

PubMed

Delle Sedie, A; Riente, L; Filippucci, E; Scirè, C A; Iagnocco, A; Meenagh, G; Gutierrez, M; Valesini, G; Montecucco, C; Grassi, W; Bombardieri, S

2011-01-01

Psoriatic arthritis (PsA) is an arthropathy associated with psoriasis, which is part of the spondyloarthropathy family, and which may present with various forms, from mono-oligoarthritis to symmetric polyarthritis mimicking rheumatoid arthritis. In longstanding disease, the symmetric polyarthritis is the most common pattern of PsA, involving the small joints of hands, feet (the involvement of which seems to be very common, ranging from 50 to 100% of patients), wrists, ankles and knees. Other common features are represented by the inflammation of enthesis and tendons. Its exact prevalence, in Italy, should be about 30% in psoriatic subjects or 0.42% when considering the general population. The aims of our study were to investigate, by US examination, the prevalence and the features of foot involvement in PsA and to describe their correlations with clinical findings. Ultrasound (US) examinations were performed using a Logiq 9 (General Electric Medical Systems, Milwaukee, WI) equipped with a multifrequency linear probe, working at 14 MHz. One hundred and eighty feet were investigated in a total of 101 patients. Prior to US assessment, all patients underwent a clinical examination by an expert rheumatologist who recorded the presence/absence of pain, tenderness (detected by palpation and/or active or passive mobilisation of the feet) and swelling. US finding indicative of metatarsophalangeal joint inflammation were obtained in 77 (76.2%) patients, while only 34 (33.7%) patients were positive to the clinical examination. This study demonstrates that US detected a higher number of inflamed joints with respect to clinical assessment in PsA patients.

Atomic data from the IRON Project. XXXII. On the accuracy of the effective collision strength for the electron impact excitation of the quadrupole transition in AR III

NASA Astrophysics Data System (ADS)

Galavís, M. E.; Mendoza, C.; Zeippen, C. J.

1998-12-01

Since te[Burgess et al. (1997)]{bur97} have recently questioned the accuracy of the effective collision strength calculated in the IRON Project for the electron impact excitation of the 3ssp23p sp4 \\ sp1 D -sp1 S quadrupole transition in Ar iii, an extended R-matrix calculation has been performed for this transition. The original 24-state target model was maintained, but the energy regime was increased to 100 Ryd. It is shown that in order to ensure convergence of the partial wave expansion at such energies, it is necessary to take into account partial collision strengths up to L=30 and to ``top-up'' with a geometric series procedure. By comparing effective collision strengths, it is found that the differences from the original calculation are not greater than 25% around the upper end of the common temperature range and that they are much smaller than 20% over most of it. This is consistent with the accuracy rating (20%) previously assigned to transitions in this low ionisation system. Also the present high-temperature limit agrees fairly well (15%) with the Coulomb-Born limit estimated by Burgess et al., thus confirming our previous accuracy rating. It appears that Burgess et al., in their data assessment, have overextended the low-energy behaviour of our reduced effective collision strength to obtain an extrapolated high-temperature limit that appeared to be in error by a factor of 2.

Chromosome Banding in Amphibia. XXXII. The Genus Xenopus (Anura, Pipidae).

PubMed

Schmid, Michael; Steinlein, Claus

2015-01-01

Mitotic chromosomes of 16 species of the frog genus Xenopus were prepared from kidney and lung cell cultures. In the chromosomes of 7 species, high-resolution replication banding patterns could be induced by treating the cultures with 5-bromodeoxyuridine (BrdU) and deoxythymidine (dT) in succession, and in 6 of these species the BrdU/dT-banded chromosomes could be arranged into karyotypes. In the 3 species of the clade with 2n = 20 and 4n = 40 chromosomes (X. tropicalis, X. epitropicalis, X. new tetraploid 1), as well as in the 3 species with 4n = 36 chromosomes (X. laevis, X. borealis, X. muelleri), the BrdU/dT-banded karyotypes show a high degree of homoeology, though differences were detected between these groups. Translocations, inversions, insertions or sex-specific replication bands were not observed. Minor replication asynchronies found between chromosomes probably involve heterochromatic regions. BrdU/dT replication banding of Xenopus chromosomes provides the landmarks necessary for the exact physical mapping of genes and repetitive sequences. FISH with an X. laevis 5S rDNA probe detected multiple hybridization sites at or near the long-arm telomeric regions in most chromosomes of X. laevis and X. borealis, whereas in X. muelleri, the 5S rDNA sequences are located exclusively at the long-arm telomeres of a single chromosome pair. Staining with the AT base pair-specific fluorochrome quinacrine mustard revealed brightly fluorescing heterochromatic regions in the majority of X. borealis chromosomes which are absent in other Xenopus species.

The evolutionary history of Drosophila buzzatii. XXXII. Linkage disequilibrium between allozymes and chromosome inversions in two colonizing populations.

PubMed

Betrán, E; Quezada-Díaz, J E; Ruiz, A; Santos, M; Fontdevila, A

1995-02-01

Chromosome polymorphism in Drosophila buzzatii is under selection but the genes responsible for the effect of the inversions of fitness are unknown. On the other hand, there is evidence for selection on several allozyme loci but the presence of paracentric inversions on the second chromosome, where most of the polymorphic loci are located, complicates the interpretation. Studies of the associations between allozymes and inversions are thus necessary to help understand the effect of selection at both the chromosomal and allozymic level. Until now this kind of information has only been available in D. buzzatii for two loci, Est-1 and Est-2, in Australian populations. Here we describe the genetic constitution of two Old World populations, Carboneras and Colera. Emphasis has been placed on the analysis of the linkage disequilibria between the second chromosome arrangements and three allozyme loci, Est-2, Pept-2 and Aldox, located on this chromosome. In addition, the recombination frequencies between the loci, and between the loci and the inversion breakpoints, have been estimated and a genetic map of the three loci has been produced. The two populations differ in allele and arrangement frequencies, as well as in the pattern of one-locus disequilibria. Est-2 and Aldox are associated with the second chromosome arrangements in both populations. On the other hand, Pept-2 is associated with the inversions in Colera but not in Carboneras. The gametic associations among the three loci are discussed taking into account the position of these loci on the chromosome map and the lack of recombination in the heterokaryotypes.

The Next Generation Virgo Cluster Survey (NGVS). XXXII. A Search for Globular Cluster Substructures in the Virgo Galaxy Cluster Core

NASA Astrophysics Data System (ADS)

Powalka, Mathieu; Puzia, Thomas H.; Lançon, Ariane; Longobardi, Alessia; Peng, Eric W.; Duc, Pierre-Alain; Alamo-Martínez, Karla; Blakeslee, John P.; Côté, Patrick; Cuillandre, Jean-Charles; Durrell, Patrick; Eigenthaler, Paul; Ferrarese, Laura; Guhathakurta, Puragra; Gwyn, S. D. J.; Hudelot, Patrick; Liu, Chengze; Mei, Simona; Muñoz, Roberto P.; Roediger, Joel; Sánchez-Janssen, Rubén; Toloba, Elisa; Zhang, Hongxin

2018-03-01

Substructure in globular cluster (GC) populations around large galaxies is expected in galaxy formation scenarios that involve accretion or merger events, and it has been searched for using direct associations between GCs and structure in the diffuse galaxy light, or with GC kinematics. Here, we present a search for candidate substructures in the GC population around the Virgo cD galaxy M87 through the analysis of the spatial distribution of the GC colors. The study is based on a sample of ∼1800 bright GCs with high-quality u, g, r, i, z, K s photometry, selected to ensure a low contamination by foreground stars or background galaxies. The spectral energy distributions of the GCs are associated with formal estimates of age and metallicity, which are representative of its position in a 4D color space relative to standard single stellar population models. Dividing the sample into broad bins based on the relative formal ages, we observe inhomogeneities that reveal signatures of GC substructures. The most significant of these is a spatial overdensity of GCs with relatively young age labels, of diameter ∼0.°1 (∼30 kpc), located to the south of M87. The significance of this detection is larger than about 5σ after accounting for estimates of random and systematic errors. Surprisingly, no large Virgo galaxy is present in this area that could potentially host these GCs. But candidate substructures in the M87 halo with equally elusive hosts have been described based on kinematic studies in the past. The number of GC spectra available around M87 is currently insufficient to clarify the nature of the new candidate substructure.

THE FURTHER SEPARATION OF TYPES AMONG THE PNEUMOCOCCI HITHERTO INCLUDED IN GROUP IV AND THE DEVELOPMENT OF THERAPEUTIC ANTISERA FOR THESE TYPES

PubMed Central

Cooper, Georgia; Rosenstein, Carolyn; Walter, Annabel; Peizer, Lenore

1932-01-01

The unclassified strains known as Group IV have been separated into twenty-nine types which are designated by the Roman numerals IV and XXXII. Only a small percentage of the pneumococcus strains isolated in New York City for this study were left unclassified. The majority of the types gave very slight cross-reactions, the exceptions being Types II and V, III and VIII, VII and XVIII and XV and XXX. In the series of cases studied, Types IV, V, VII and VIII were found more prevalent in the lobar pneumonia of adults and Types V, VI a and XIV in children. The majority of the types were also found in normal individuals and in persons having respiratory infections other than pneumonia. Types VI a and XIX were most prevalent in the limited number of strains studied by us. Fourteen of the types were found in pneumococcus meningitis; Type XVIII was found most often. Antisera suitable for clinical trial have been prepared for fourteen types. From the majority of the horses inoculated for more than a year, antisera having 500 to 1000 units per cc. were obtained. Antisera of lower potency were concentrated and preparations obtained equal to or stronger than high grade unconcentrated serum. Potent bivalent antisera have been prepared for types which were found to give marked cross-agglutination reactions. The results with each type as to prevalence, severity of cases, presence in normal individuals, and in spinal meningitis, potency of antisera produced for therapeutic trial and virulence of strains for mice have been considered under the different type headings. PMID:19870011

Genetics of Ustilago violacea. XXXII. Genetic evidence for transposable elements.

PubMed

Garber, E D; Ruddat, M

1994-12-01

Crosses between Ustilago violacea mutant strains with different color phenotypes that were derived from the 1.A1 and 2.A2 laboratory strains yielded, as expected, bisectored teliospore colonies with the parental colors as well as the a-1 and the a-2 mating-types. Generally, wild teliospore collections usually produced sporidia of both mating-types, providing two-mating-type (TMT) strains. Occasionally, however, sporidia with only one mating-type allele, a-1 or a-2, were obtained from teliospores, providing one-mating-type (OMT) strains. Crosses between OMT and laboratory strains with different color phenotypes gave (1) bisectored teliospore colonies with the parental colors or colonies with a parental color and a nonparental color and (2) nonsectored colonies with the nonparental color or with the parental color. The frequencies for the occurrence of non-parental color ranged from 41% to 93%, depending on the strain. The yield of teliospore colonies was usually reduced for these crosses. In many of these teliospore colonies, morphologically-altered sporidia (MAS phenotype) were observed. The morphology and the size of the sporidia with the MAS phenotype differed from those of teliospore colonies of the crosses between the laboratory strains. In addition, these sporidia did not form conjugants. A cross involving the TMT strains C449 yielded the MAS phenotype as well as a high incidence of tetrad colonies with a nonparental color. The high degree of instability of the parental color phenotypes, and the high frequency of the appearance of nonparental color phenotypes as well as the appearance of the MAS phenotype, are in accord with the presence of active and inactive transposable elements in the OMT strains, TMT strains, and laboratory strains.

Connective tissue activation. XXXII. Structural and biologic characteristics of mesenchymal cell-derived connective tissue activating peptide-V.

PubMed

Cabral, A R; Cole, L A; Walz, D A; Castor, C W

1987-12-01

Connective tissue activating peptide-V (CTAP-V) is a single-chain, mesenchymal cell-derived anionic protein with large and small molecular forms (Mr of 28,000 and 16,000, respectively), as defined by sodium dodecyl sulfate-polyacrylamide gel electrophoresis. The proteins have similar specific activities with respect to stimulation of hyaluronic acid and DNA formation in human synovial fibroblast cultures. S-carboxymethylation or removal of sialic acid residues did not modify CTAP-V biologic activity. Rabbit antibodies raised separately against each of the purified CTAP-V proteins reacted, on immunodiffusion and on Western blot, with each antigen and neutralized mitogenic activity. The amino-terminal amino acid sequence of the CTAP-V proteins, determined by 2 laboratories, confirmed their structural similarities. The amino-terminal sequence through 37 residues was demonstrated for the smaller protein. The first 10 residues of CTAP-V (28 kd) were identical to the N-terminal decapeptide of CTAP-V (16 kd). The C-terminal sequence, determined by carboxypeptidase Y digestion, was the same for both CTAP-V molecular species. The 2 CTAP-V peptides had similar amino acid compositions, whether residues were expressed as a percent of the total or were normalized to mannose. Reduction of native CTAP-V protein released sulfhydryl groups in a protein:disulfide ratio of 1:2; this suggests that CTAP-V contains 2 intramolecular disulfide bonds. Clearly, CTAP-V is a glycoprotein. The carbohydrate content of CTAP-V (16 kd) and CTAP-V (28 kd) is 27% and 25%, respectively. CTAP-V may have significance in relation to autocrine mechanisms for growth regulation of connective tissue cells and other cell types.

First Asteroid Spectrometric Observations with BTA: 3045 Alois

NASA Astrophysics Data System (ADS)

Busarev, V. V.; Burenkov, A. N.; Pramskij, A. G.

2001-11-01

BTA, Russian 6-m telescope, was mainly used for faint stars and extragalactic objects observations. We have firstly performed with the telescope spectrometric observations of a main belt asteroid, 3045 Alois, and are planning to use it for Centaurs and Kuiper Belt objects spectrometry. We have obtained some results of the observations. Spectra of Alois were recorded on two nights of March 2001 (29/30 and 30/31) with a long slit spectrograph (UAGS + CCD) in the .38-.80 um spectral range. HD105633 (G5) [1] considered as a solar analog was also observed, and the data were used for calculation the asteroid reflectance spectra. It was found that reflectance spectra of Alois obtained on different nights have various continuum slopes and absorption features. The reflectance spectrum on 29/30 March had a flat continuum in the range .44-.65 um and absorption bands at .5 um (ab. 7 % with respect to the continuum) similar to that found on the E-type asteroid 2035 Stearns [2], and at .80 um (ab. 25 %). Another one on 30/31 March had a red continuum in the range .40-.67 um and absorption bands at .43 um (ab. 6 %) resembling absorption features found on some C-, M- and S-type asteroids [3, 4], and at .80 um (ab. 17 %). From the data and taking into account the mean heliocentric distance of 3045 Alois (3.13 AU) we suppose that the asteroid having irregular spectral characteristics may be of M- or E-type and possibly hydrated. Unfortunately, its albedo and rotational period remain still unknown. [1] Mermilliod J.-C. (1994) Bull. Inf. CDS 45, 3. [2] Fornasier S. and Lazzarine M. (2001) Icarus 152, 127-133. [3] Vilas F. et al. (1993) Icarus 102, 225-231. [4] Busarev V. V. (2001) LPSC XXXII, abs. 1927.

Ribonucleoprotein organization of eukaryotic RNA. XXXII. U2 small nuclear RNA precursors and their accurate 3' processing in vitro as ribonucleoprotein particles.

PubMed

Wieben, E D; Nenninger, J M; Pederson, T

1985-05-05

Biosynthetic precursors of U2 small nuclear RNA have been identified in cultured human cells by hybrid-selection of pulse-labeled RNA with cloned U2 DNA. These precursor molecules are one to approximately 16 nucleotides longer than mature U2 RNA and contain 2,2,7-trimethylguanosine "caps". The U2 RNA precursors are associated with proteins that react with a monoclonal antibody for antigens characteristic of small nuclear ribonucleoprotein particles. Like previously described precursors of U1 and U4 small nuclear RNAs, the pre-U2 RNAs are recovered in cytoplasmic fractions, although it is not known if this is their location in vivo. The precursors are processed to mature-size U2 RNA when cytoplasmic extracts are incubated in vitro at 37 degrees C. Mg2+ is required but ATP is not. The ribonucleoprotein structure of the pre-U2 RNA is maintained during the processing reaction in vitro, as are the 2,2,7-trimethylguanosine caps. The ribonucleoprotein organization is of major importance, as exogenous, protein-free U2 RNA precursors are degraded rapidly in the in vitro system. Two lines of evidence indicate that the conversion of U2 precursors to mature-size U2 RNA involves a 3' processing reaction. First, the reaction is unaffected by a large excess of mature U2 small nuclear RNP, whose 5' trimethylguanosine caps would be expected to compete for a 5' processing activity. Second, when pre-U2 RNA precursors are first stoichiometrically decorated with an antibody specific for 2,2,7-trimethylguanosine, the extent of subsequent processing in vitro is unaffected. These results provide the first demonstration of a eukaryotic RNA processing reaction in vitro occurring within a ribonucleoprotein particle.

SEXCMD: Development and validation of sex marker sequences for whole-exome/genome and RNA sequencing.

PubMed

Jeong, Seongmun; Kim, Jiwoong; Park, Won; Jeon, Hongmin; Kim, Namshin

2017-01-01

Over the last decade, a large number of nucleotide sequences have been generated by next-generation sequencing technologies and deposited to public databases. However, most of these datasets do not specify the sex of individuals sampled because researchers typically ignore or hide this information. Male and female genomes in many species have distinctive sex chromosomes, XX/XY and ZW/ZZ, and expression levels of many sex-related genes differ between the sexes. Herein, we describe how to develop sex marker sequences from syntenic regions of sex chromosomes and use them to quickly identify the sex of individuals being analyzed. Array-based technologies routinely use either known sex markers or the B-allele frequency of X or Z chromosomes to deduce the sex of an individual. The same strategy has been used with whole-exome/genome sequence data; however, all reads must be aligned onto a reference genome to determine the B-allele frequency of the X or Z chromosomes. SEXCMD is a pipeline that can extract sex marker sequences from reference sex chromosomes and rapidly identify the sex of individuals from whole-exome/genome and RNA sequencing after training with a known dataset through a simple machine learning approach. The pipeline counts total numbers of hits from sex-specific marker sequences and identifies the sex of the individuals sampled based on the fact that XX/ZZ samples do not have Y or W chromosome hits. We have successfully validated our pipeline with mammalian (Homo sapiens; XY) and avian (Gallus gallus; ZW) genomes. Typical calculation time when applying SEXCMD to human whole-exome or RNA sequencing datasets is a few minutes, and analyzing human whole-genome datasets takes about 10 minutes. Another important application of SEXCMD is as a quality control measure to avoid mixing samples before bioinformatics analysis. SEXCMD comprises simple Python and R scripts and is freely available at https://github.com/lovemun/SEXCMD.

Increased number of sex chromosomes affects height in a nonlinear fashion: a study of 305 patients with sex chromosome aneuploidy.

PubMed

Ottesen, Anne Marie; Aksglaede, Lise; Garn, Inger; Tartaglia, Nicole; Tassone, Flora; Gravholt, Claus H; Bojesen, Anders; Sørensen, Kaspar; Jørgensen, Niels; Rajpert-De Meyts, Ewa; Gerdes, Tommy; Lind, Anne-Marie; Kjaergaard, Susanne; Juul, Anders

2010-05-01

Tall stature and eunuchoid body proportions characterize patients with 47,XXY Klinefelter syndrome, whereas patients with 45,X Turner syndrome are characterized by impaired growth. Growth is relatively well characterized in these two syndromes, while few studies describe the growth of patients with higher grade sex chromosome aneuploidies. It has been proposed that tall stature in sex chromosome aneuploidy is related to an overexpression of SHOX, although the copy number of SHOX has not been evaluated in previous studies. Our aims were therefore: (1) to assess stature in 305 patients with sex chromosome aneuploidy and (2) to determine the number of SHOX copies in a subgroup of these patients (n = 255) these patients and 74 healthy controls. Median height standard deviation scores in 46,XX males (n = 6) were -1.2 (-2.8 to 0.3), +0.9 (-2.2 to +4.6) in 47,XXY (n = 129), +1.3 (-1.8 to +4.9) in 47,XYY (n = 44), +1.1 (-1.9 to +3.4) in 48,XXYY (n = 45), +1.8 (-2.0 to +3.2) in 48,XXXY (n = 9), and -1.8 (-4.2 to -0.1) in 49,XXXXY (n = 10). Median height standard deviation scores in patients with 45,X (n = 6) were -2.6 (-4.1 to -1.6), +0.7 (-0.9 to +3.2) in 47,XXX (n = 40), -0.6 (-1.9 to +2.1) in 48,XXXX (n = 13), and -1.0 (-3.5 to -0.8) in 49,XXXXX (n = 3). Height increased with an increasing number of extra X or Y chromosomes, except in males with five, and in females with four or five sex chromosomes, consistent with a nonlinear effect on height. Copyright 2010 Wiley-Liss, Inc.

Increased Number of Sex Chromosomes Affects Height in a Nonlinear Fashion: A Study of 305 Patients With Sex Chromosome Aneuploidy

PubMed Central

Ottesen, Anne Marie; Aksglaede, Lise; Garn, Inger; Tartaglia, Nicole; Tassone, Flora; Gravholt, Claus H.; Bojesen, Anders; Sørensen, Kaspar; Jørgensen, Niels; Meyts, Ewa Rajpert-De; Gerdes, Tommy; Lind, Anne-Marie; Kjaergaard, Susanne; Juul, Anders

2017-01-01

Tall stature and eunuchoid body proportions characterize patients with 47,XXY Klinefelter syndrome, whereas patients with 45,X Turner syndrome are characterized by impaired growth. Growth is relatively well characterized in these two syndromes, while few studies describe the growth of patients with higher grade sex chromosome aneuploidies. It has been proposed that tall stature in sex chromosome aneuploidy is related to an overexpression of SHOX, although the copy number of SHOX has not been evaluated in previous studies. Our aims were therefore: (1) to assess stature in 305 patients with sex chromosome aneuploidy and (2) to determine the number of SHOX copies in a subgroup of these patients (n =255) these patients and 74 healthy controls. Median height standard deviation scores in 46,XX males (n =6) were −1.2 (−2.8 to 0.3), +0.9 (−2.2 to + 4.6) in 47,XXY (n =129), +1.3 (−1.8 to +4.9) in 47,XYY (n =44), +1.1 (−1.9 to +3.4) in 48,XXYY (n =45), +1.8 (−2.0 to +3.2) in 48,XXXY (n =9), and −1.8 (−4.2 to −0.1) in 49,XXXXY (n =10). Median height standard deviation scores in patients with 45,X (n =6) were −2.6 (−4.1 to −1.6), +0.7 (−0.9 to +3.2) in 47,XXX (n =−40), −0.6 (−1.9 to +2.1) in 48,XXXX (n =13), and −1.0 (−3.5 to −0.8) in 49,XXXXX (n =3). Height increased with an increasing number of extra X or Y chromosomes, except in males with five, and in females with four or five sex chromosomes, consistent with a nonlinear effect on height. PMID:20425825

Comparative study of mitotic chromosomes in two blowflies, Lucilia sericata and L. cluvia (Diptera, Calliphoridae), by C- and G-like banding patterns and rRNA loci, and implications for karyotype evolution

PubMed Central

Chirino, Mónica G.; Rossi, Luis F.; Bressa, María J.; Luaces, Juan P.; Merani, María S.

2015-01-01

Abstract The karyotypes of Lucilia cluvia (Walker, 1849) and Lucilia sericata (Meigen, 1826) from Argentina were characterized using conventional staining and the C- and G-like banding techniques. Besides, nucleolus organizer regions (NORs) were detected by fluorescent in situ hybridization (FISH) and silver staining technique. The chromosome complement of these species comprises five pairs of autosomes and a pair of sex chromosomes (XX/XY, female/male). The autosomes of both species have the same size and morphology, as well as C- and G-like banding patterns. The X and Y chromosomes of Lucilia cluvia are subtelocentric and easily identified due to their very small size. In Lucilia sericata, the X chromosome is metacentric and the largest of the complement, showing a secondary constriction in its short arm, whereas the Y is submetacentric and smaller than the X. The C-banding patterns reflect differences in chromatin structure and composition between the subtelocentric X and Y chromosomes of Lucilia cluvia and the biarmed sex chromosomes of Lucilia sericata. These differences in the sex chromosomes may be due to distinct amounts of constitutive heterochromatin. In Lucilia cluvia, the NORs are placed at one end of the long-X and of the long-Y chromosome arms, whereas one of the NORs is disposed in the secondary constriction of the short-X chromosome arm and the other on the long-Y chromosome arm in Lucilia sericata. Although the G-like banding technique does not yield G-bands like those in mammalian chromosomes, it shows a high degree chromosomal homology in both species because each pair of autosomes was correctly paired. This chromosome similarity suggests the absence of autosomal rearrangements during karyotype evolution in the two species studied. PMID:25893078

Chromosome evolution in Cophomantini (Amphibia, Anura, Hylinae).

PubMed

Ferro, Juan M; Cardozo, Dario E; Suárez, Pablo; Boeris, Juan M; Blasco-Zúñiga, Ailin; Barbero, Gastón; Gomes, Anderson; Gazoni, Thiago; Costa, William; Nagamachi, Cleusa Y; Rivera, Miryan; Parise-Maltempi, Patricia P; Wiley, John E; Pieczarka, Julio C; Haddad, Celio F B; Faivovich, Julián; Baldo, Diego

2018-01-01

The hylid tribe Cophomantini is a diverse clade of Neotropical treefrogs composed of the genera Aplastodiscus, Boana, Bokermannohyla, Hyloscirtus, and Myersiohyla. The phylogenetic relationships of Cophomantini have been comprehensively reviewed in the literature, providing a suitable framework for the study of chromosome evolution. Employing different banding techniques, we studied the chromosomes of 25 species of Boana and 3 of Hyloscirtus; thus providing, for the first time, data for Hyloscirtus and for 15 species of Boana. Most species showed karyotypes with 2n = 2x = 24 chromosomes; some species of the B. albopunctata group have 2n = 2x = 22, and H. alytolylax has 2n = 2x = 20. Karyotypes are all bi-armed in most species presented, with the exception of H. larinopygion (FN = 46) and H. alytolylax (FN = 38), with karyotypes that have a single pair of small telocentric chromosomes. In most species of Boana, NORs are observed in a single pair of chromosomes, mostly in the small chromosomes, although in some species of the B. albopunctata, B. pulchella, and B. semilineata groups, this marker occurs on the larger pairs 8, 1, and 7, respectively. In Hyloscirtus, NOR position differs in the three studied species: H. alytolylax (4p), H. palmeri (4q), and H. larinopygion (1p). Heterochromatin is a variable marker that could provide valuable evidence, but it would be necesserary to understand the molecular composition of the C-bands that are observed in different species in order to test its putative homology. In H. alytolylax, a centromeric DAPI+ band was observed on one homologue of chromosome pair 2. The band was present in males but absent in females, providing evidence for an XX/XY sex determining system in this species. We review and discuss the importance of the different chromosome markers (NOR position, C-bands, and DAPI/CMA3 patterns) for their impact on the taxonomy and karyotype evolution in Cophomantini.

Chromosome evolution in Cophomantini (Amphibia, Anura, Hylinae)

PubMed Central

Suárez, Pablo; Boeris, Juan M.; Blasco-Zúñiga, Ailin; Barbero, Gastón; Gomes, Anderson; Gazoni, Thiago; Costa, William; Nagamachi, Cleusa Y.; Rivera, Miryan; Parise-Maltempi, Patricia P.; Wiley, John E.; Pieczarka, Julio C.; Haddad, Celio F. B.; Faivovich, Julián; Baldo, Diego

2018-01-01

The hylid tribe Cophomantini is a diverse clade of Neotropical treefrogs composed of the genera Aplastodiscus, Boana, Bokermannohyla, Hyloscirtus, and Myersiohyla. The phylogenetic relationships of Cophomantini have been comprehensively reviewed in the literature, providing a suitable framework for the study of chromosome evolution. Employing different banding techniques, we studied the chromosomes of 25 species of Boana and 3 of Hyloscirtus; thus providing, for the first time, data for Hyloscirtus and for 15 species of Boana. Most species showed karyotypes with 2n = 2x = 24 chromosomes; some species of the B. albopunctata group have 2n = 2x = 22, and H. alytolylax has 2n = 2x = 20. Karyotypes are all bi-armed in most species presented, with the exception of H. larinopygion (FN = 46) and H. alytolylax (FN = 38), with karyotypes that have a single pair of small telocentric chromosomes. In most species of Boana, NORs are observed in a single pair of chromosomes, mostly in the small chromosomes, although in some species of the B. albopunctata, B. pulchella, and B. semilineata groups, this marker occurs on the larger pairs 8, 1, and 7, respectively. In Hyloscirtus, NOR position differs in the three studied species: H. alytolylax (4p), H. palmeri (4q), and H. larinopygion (1p). Heterochromatin is a variable marker that could provide valuable evidence, but it would be necesserary to understand the molecular composition of the C-bands that are observed in different species in order to test its putative homology. In H. alytolylax, a centromeric DAPI+ band was observed on one homologue of chromosome pair 2. The band was present in males but absent in females, providing evidence for an XX/XY sex determining system in this species. We review and discuss the importance of the different chromosome markers (NOR position, C-bands, and DAPI/CMA3 patterns) for their impact on the taxonomy and karyotype evolution in Cophomantini. PMID:29444174

Non-uniform thickness in Europa's icy shell: implications for astrobiology mission design

NASA Astrophysics Data System (ADS)

Fairén, A.; Amils, R.

The exploration of Europa's subsurface ocean is hardly constrained by the presence of an outer ice shell of unknown thickness: a somewhat thin crust would allow easier access to the ocean below. Current estimates for the thickness of Europa's icy surface range from a few km [1] to a few tens of km [2], the shell overlying a liquid water ocean up to 150 km thick [3,4,5]. The surface is believed to be young (mean age of 30-80 Myr [6]) and geologically active [7,8,9], as it is sparsely cratered. Here we report geological evidence indicating that the thickness of Europa's ice crust is actually a complex combination of thicker and thinner areas, highlighting the implications of such structure in the future exploration of the inner ocean. Detailed geologic mapping of impact craters, palimpsests and chaotic terrains distribution on Europa's surface, offers an initial approach to a comprehensive description of the thickness variation in the ice shell. Our analysis is based in: (1) Crater distribution, morphology, diameter and depth. Seminal work by Schenk [2] of transitions in crater shape/diameter suggested enhanced structural collapse of craters with diameter >27-33 km, that will consequently form multiring basins, due to weaker ice or a global ocean at depths >19-25 km. This being true, strictly can only be interpreted regionally: multiring basins indicate regions where the ice shell is thick; in those regions where the icy surface is thin, a bolide impact will breach the ice and leave neither crater nor multiring basin behind, but probably Ganymede's type palimpsests. (2) Palimpsest-type features distribution, indicating regions where the ice shell is too thin to support crater formation after big bolide impacts. In Ganymede, palimpsests are circular, low albedo and relief features formerly formed by impacts [10,11]. (3) Chaotic terrain distribution, considering features tens to hundreds of km across, that may be the evidence for very thin ice areas (from ˜ 2 km to zero shell thickness [12]) with liquid water at shallow depths [5], allowing for bolide penetration, diapirism and the extrusion of water to the surface. The heterogeneity in shell's thickness may be originated in spatial variations in tidal heating [13] and/or warm water upwellings from the silicate interior capable of melt-through the ice from below [12,14]. This thickness heterogeneity can be embedded in a general equatorward thickening trending, due to tidal dissipation and surface temperature variations [15]. A major constraint must be addressed at this point: the dynamism of ductile ice near the base of the shell may drive to decay in lateral thickness contrasts. But this effect has been examined both assuming ice as a Newtonian [16,17,18] and a non-Newtonian material [19], broadly reaching to similar conclusions: global shell thickness variations may survive for up to 100 Myr. In addition, lateral pressure gradients may not decay if they comprise only shallow depths [19]. Therefore, our results point to a dynamic non-uniform Europa's icy shell, displaying some regional and temporal heterogeneity in thickness. As thin/thick ice distribution is as time dependent as the surface ice features are (both are reshaped in periods ˜ 100 Myr), the analysis performed here offers an estimation of the current thickness distribution in the ice shell, estimation that cannot be extrapolated to ancient (e.g., >100 Myr) times. The astrobiological potential the shell and ocean below possess is highlighted by these results: a somewhere thin outer crust allows the possibility for some exogenous materials delivered by asteroids and comets to reach the inner liquid water ocean by breaching the brittle lithosphere [20], and so join to those generated in the interior of Europa via volcanic and hydrothermal activity [21]. In addition, pressure gradients driving the ductile ice at the base of the shell to flow laterally may help to redistribute such materials among the inner ice shell and/or ocean through time. Our results have a direct deal with the investigation of Europa's interior. Mission design will need to incorporate a drill system routine well suited to penetrate the ice shell tens of meters in the thinner areas, allowing to deep subsurface access and sampling. Landing and drilling targets should be selected among the zones where mapping indicates the presence of a thinner ice shell, as it may potentially suggest the existence of nutrient-rich hydrothermal plumes rising from the rocky interior and melting the ice from below, probably creating chaotic terrains [14]. Little-cratered, thin-crust areas would consequently be interpreted as key pacemakers to detect both the ice/ocean interface and the most complex environments under the ice shell. Additionally, drilling processes will be clearly easier in such zones. References: [1] Hoppa, G., et al. Science 285, 1899-1903 (1999). [2] Schenk, P.M. Nature 417, 419-421 (2002). [3] Anderson J.D. et al. Science 276, 1236-1239 (1997). [4] Anderson J.D. et al. Science 281, 2019-2022 (1998). [5] Carr, M.H., et al. Nature 391, 363-365 (1998). [6] Zahnle, K., et al. Icarus 163, 263-289 (2003). [7] Smith, B.A., et al. Science 206, 927-950 (1979). [8] Zahnle, K., et al. Icarus 136, 202-222 (1998). [9] Levison, H.F., et al. Icarus 143, 415-420 (2000). [10] Schenk, P.M. Lunar Planet. Sci. Conf. XXVII, #1137-1138 (1996). [11] Farrar, K.S. & Collins, G.C. Lunar Planet Sci. Conf. XXXIII, #1450 (2002). [12] Greenberg, R., et al. Icarus 141, 263-286 (1999). [13] Ojakangas, G.W. & Stevenson, D.J. Icarus 81, 220-241 (1989). [14] Collins, G.C. & Goodman, J.C. Europa's Icy Shell Conf., #7032 (2004). [15] Tobie, G., et al. J. Geophys. Res. 108, doi: 10.1029/2003JE002099 (2003). [16] Stevenson, D.J. Lunar Planet Sci. Conf. XXXI, #1506 (2000). [17] O'Brien, D.P., et al. Icarus 156, 152-161 (2002). [18] Buck, L., et al. Geophys. Res. Lett. 29, doi: 10.1029/2002GL016171 (2002). [19] Nimmo, F. Icarus in press (2004). [20] Pierazzo, E. and Chyba, C. F. Icarus 157, 120-127 (2002). [21] McCord, T.B. et al. Science 280, 1242-1245 (1998).

Can the Yarkovsky effect significantly influence the main-belt size distribution?

NASA Astrophysics Data System (ADS)

O'Brien, D. P.; Greenberg, R.

2001-11-01

It has been proposed that the size distribution of main-belt asteroids may be significantly modified by the Yarkovsky effect---a size-dependent radiation force which can sweep asteroids into resonances and out of the main belt. Bell [1] suggested that this effect could deplete the population of asteroids smaller than ~10 m by at least an order of magnitude, resulting in the lack of small craters observed on Eros. Others have hypothesized that the same effect could explain the steepness of the crater distribution on Gaspra [2]. We have explicitly included Yarkovsky removal in a numerical collisional evolution model. The algorithm uses recent calculations of the expected removal rates of different sized bodies from the main belt (David Vokrouhlicky, personal communication). We find that the rate of removal of bodies from the main belt by the Yarkovsky effect may be within an order of magnitude of the rate of collisional destruction for asteroids ~10 m in diameter, and negligible for larger or smaller asteroids. When Yarkovsky removal is incorporated into our numerical collisional evolution model, the numbers of bodies ~10 m in diameter is reduced by ~10-20%, and a wave propagates up the size distribution increasing the number of bodies ~300 m by ~10%. This `waviness' could conceivably be detected in the cratering records on asteroids. However, the uncertainties in crater counts on Ida, Gaspra, Malthide, and Eros are >10% for diameters >100 m (i. e. the craters made by impactors >10 m in diameter). Contrary to the earlier hypothesis, Yarkovsky removal of small asteroids cannot have substantially affected the overall slopes of the crater populations on these asteroids. Moreover, Yarkovsky removal cannot explain the lack of small (<10 m) craters on Eros, because the corresponding impactors (<1 m) are unaffected by the Yarkovsky effect. [1] Bell, J. F. (2001). LPSC XXXII abstract no. 1964. [2] Hartmann, W. K. and E. V. Ryan (1996). DPS 28, abstract no. 10.35.

Volcanic Eruption Classification on Io and Earth from Low Spatial Resolution Remote-Sensing Data

NASA Astrophysics Data System (ADS)

Davies, A. G.; Keszthelyi, L. P.

2005-08-01

Earth and Io exhibit high-temperature (silicate) active volcanism. While there are important differences in the eruptions on Earth and Io, in low-spatial-resolution data (corresponding to the bulk of available and foreseeable data of Io), similar styles of effusive and explosive volcanism yield similar thermal flux densities [1-3]. If, from observed thermal emission as a function of wavelength and change in thermal emission with time, the eruption style of an ionian volcano can be constrained, estimates of volumetric fluxes can be made and compared with terrestrial volcanoes using techniques derived for analysing terrestrial remotely-sensed data. We find that ionian volcanoes fundamentally differ from their terrestrial counterparts only in areal extent, with Io volcanoes covering larger areas, with higher volumetric fluxes. Even with the low-spatial resolution data available it is possible to sometimes constrain and classify eruption style both on Io and Earth from the integrated thermal emission spectrum, and how this changes temporally. Plotting 2 and 5 μm fluxes reveals the evolution of individual eruptions of different styles, as well as the relative intensity of eruptions, allowing comparison to be made from individual eruptions on both planets. For some Ionian volcanoes, low-resolution analyses are confirmed from observations obtained at high spatial resolution Of great importance, possibly more so than spatial resolution, is temporal resolution, as this has proven diagnostic in determining style of eruption at a number of volcanoes (e.g., Prometheus, Pele, Loki Patera, Pillan 1997) [1-3]. Active lava lakes, fire-fountains and insulated flows are identified using this methodology, and this allows comparison of individual eruptions on both planets. References: [1] Davies et al. (2001) JGR, 106, 33079-33,103. [2] Keszthelyi et al. (2001) LPSC XXXII Abstract 1523. [3] Davies (2003) JGR, 108, 10.1029/2001JE001509. This work was carried out at the Jet Propulsion Laboratory-California Institute of Technology, under contract to NASA.

The Solar Neighborhood. XXXII. The Hydrogen Burning Limit

NASA Astrophysics Data System (ADS)

Dieterich, Sergio B.; Henry, Todd J.; Jao, Wei-Chun; Winters, Jennifer G.; Hosey, Altonio D.; Riedel, Adric R.; Subasavage, John P.

2014-05-01

We construct a Hertzsprung-Russell diagram for the stellar/substellar boundary based on a sample of 63 objects ranging in spectral type from M6V to L4. We report newly observed VRI photometry for all 63 objects and new trigonometric parallaxes for 37 objects. The remaining 26 objects have trigonometric parallaxes from the literature. We combine our optical photometry and trigonometric parallaxes with 2MASS and WISE photometry and employ a novel spectral energy distribution fitting algorithm to determine effective temperatures, bolometric luminosities, and radii. Our uncertainties range from ~20 K to ~150 K in temperature, ~0.01 to ~0.06 in log (L/L ⊙) and ~3% to ~10% in radius. We check our methodology by comparing our calculated radii to radii directly measured via long baseline optical interferometry. We find evidence for the local minimum in the radius-temperature and radius-luminosity trends that signals the end of the stellar main sequence and the start of the brown dwarf sequence at T eff ~ 2075 K, log (L/L ⊙) ~ -3.9, and (R/R ⊙) ~ 0.086. The existence of this local minimum is predicted by evolutionary models, but at temperatures ~400 K cooler. The minimum radius happens near the locus of 2MASS J0523-1403, an L2.5 dwarf with V - K = 9.42. We make qualitative arguments as to why the effects of the recent revision in solar abundances accounts for the discrepancy between our findings and the evolutionary models. We also report new color-absolute magnitude relations for optical and infrared colors which are useful for estimating photometric distances. We study the optical variability of all 63 targets and find an overall variability fraction of 36^{+9}_{-7}% at a threshold of 15 mmag in the I band, which is in agreement with previous studies.

Buried Craters In Isidis Planitia, Mars

NASA Astrophysics Data System (ADS)

Seabrook, A. M.; Rothery, D. A.; Wallis, D.; Bridges, J. C.; Wright, I. P.

We have produced a topographic map of Isidis Planitia, which includes the Beagle 2 landing site, using interpolated Mars Orbiter Laser Altimeter (MOLA) data from the Mars Global Surveyor (MGS) spacecraft currently orbiting Mars. MOLA data have a vertical precision of 37.5 cm, a footprint size of 130 m, an along-track shot spacing of 330 m, and an across-track spacing that is variable and may be several kilometres. This has revealed subtle topographic detail within the relatively smooth basin of Isidis Planitia. Analysis of this map shows apparent wrinkle ridges that could be the volcanic basement to the basin and also several circular depressions with diameters of several to tens of kilometres which we interpreted as buried impact craters, comparable to the so-called stealth craters recognised elsewhere in the northern lowlands of Mars[1]. Stealth craters are considered to be impact craters subjected to erosion and/or burial. Some of these features in Isidis have depressions that are on the order of tens metres lower than their rims and are very smooth, and so are often not visible in MGS Mars Orbiter Camera (MOC) or Viking images of the basin. The Isidis stealth craters are not restricted to the Hesperian Vastitas Borealis formations like those detected elsewhere in the northern lowlands by Kreslavsky and Head [1], but are also found in a younger Amazonian smooth plains unit. It is generally believed that Isidis Planitia has undergone one or more episodes of sedi- ment deposition, and so these buried craters most likely lie on an earlier surface, which could be the postulated volcanic basement to the basin. Analysis of the buried craters may give some understanding of the thickness, frequencies and ages of sedimentation episodes within the basin. This information will be important in developing a context in which information from the Beagle 2 lander can be analysed when it arrives on Mars in December 2003. [1] Kreslavsky M. A. and Head J. W. (2001) LPS XXXII

Tides on Self-gravitating, Compressible Bodies

NASA Astrophysics Data System (ADS)

Hurford, T. A.; Greenberg, R.

2001-11-01

Most modern derivations of tidal amplitude follow the approach presented by Love [1]. Love's analysis for a homogeneous sphere assumed an incompressible material, which required introduction of a non-rigorously justified pressure term. We have solved the more general case of arbitrary compressibility, which allows for a more straightforward derivation [2,3]. We find the h2 love number of a body of radius R, density ρ , by solving the deformation equation [4], μ ∇ 2 u = ρ ∇U - (λ + μ ) ∇ (∇ ṡ u) where μ is the rigidity of the body and λ the Lamé constant. The potential U is the sum of (a) the tide raising potential, (b) the potential of surface mass shifted above or below the spherical surface, (c) potential due to the internal density changes and (d) the change in potential of each bit of volume due to its displacement u. A self-consistent solution can be obtained with U = \\sum_{q=0}^{\\infty} b_{(2+2q)} r^{(2+2q)} ( {3}/{2} \\cos2 \\theta - {1}/{2} ). In [1] and [3] only the r2 term was considered, which was valid only if compressibility is small or elasticity governs deformation (i.e. ρ g R << (λ + 2 μ )). The solution with only the r2 term reduces to Love's [1] solution in the limit of zero compressibility (λ = ∞ ). However, for rock μ ~ λ [4], in which case h2 is enhanced by ~ 3 %, and solutions for greater compressibility give up to 8 % enhancement of tidal amplitude. If ρ g R is significant, higher order r(2q+2) terms are important and even greater corrections are required to the classical tidal amplitude. [1] Love, A.E.H., New York Dover Publications, 1944 [2] Hurford, T.A. and R. Greenberg, Lunar Plan. Sci. XXXII 1741, 2001 [3] Hurford, T.A. and R. Greenberg, 2001 DDA meeting, Bull. Amer. Astron. Soc. in press [4] Kaula, W.M., John Wiley & Sons, Inc., 1968

The Lack of Small Craters on Eros is not due to the Yarkovsky Effect

NASA Astrophysics Data System (ADS)

O'Brien, David P.; Greenberg, R.

2007-10-01

Eros approaches saturation for craters larger than 200 m in diameter, but is significantly depleted in smaller craters [1]. It has been suggested that this could reflect a paucity of small impactors in the main belt, due to their removal by the Yarkovsky effect [1,2]. Here we present the results of a self-consistent collisional and dynamical evolution model for the main belt and NEAs, along with a model for the evolution of asteroid crater populations, that show that Eros' lack of small craters is not likely due to the depletion of small impactors by the Yarkovsky effect, or any other depletion mechanism. To produce a main-belt size distribution that is suitably depleted in small impactors to match Eros' small crater population requires a more extreme size-dependent removal rate than the Yarkovsky effect and Poynting-Robertson drag can provide. Using such an extreme removal rate introduces a wave into the model main-belt size distribution that propagates to large sizes, and is inconsistent with the observed main-belt population. Similarly, it introduces a wave in the model NEA population that is inconsistent with the observed NEAs. Eros is not alone in showing a depletion of small craters. Recent observations of the asteroid Itokawa by the Hyabusa spacecraft show relatively few craters, and Yarkovsky depletion of small impactors has again been suggested as a possible explanation [3]. Our work shows that a substantial depletion of small impactors from the main belt would have consequences at large sizes, inconsistent with observations of the actual main-belt and NEA size distributions. Other explanations for the depletion of small craters on asteroid surfaces must be explored [eg. 4,5]. References: [1] Chapman (2002), Icarus 155, p.104. [2] Bell (2001), LPSC XXXII, no.1964. [3] Saito (2006), Science 312, p.1341. [4] Richardson (2004), Science 306, p.1526. [5] Greenberg (2003), DPS 35, no.24.06.

"European" race-specific metacentrics in East Siberian common shrews (Sorex araneus): a description of two new chromosomal races, Irkutsk and Zima.

PubMed

Pavlova, Svetlana V; Borisov, Sergei A; Timoshenko, Alexander F; Sheftel, Boris I

2017-01-01

Karyotype studies of common shrews in the vicinity of Lake Baikal (Irkutsk Region, Eastern Siberia) resulted in the description of two new chromosomal races of Sorex araneus Linnaeus, 1758 (Lypotyphla, Mammalia), additional to 5 races formerly found in Siberia. In the karyotypes of 12 specimens from 3 locations, the polymorphism of metacentric and acrocentric chromosomes of the Robertsonian type was recorded and two distinct groups of karyotypes interpreted as the chromosomal races were revealed. They are geographically distant and described under the racial names Irkutsk (Ir) and Zima (Zi). Karyotypes of both races were characterized by species-specific (the same for all 74 races known so far) metacentric autosomes af, bc, tu and jl , and the typical sex chromosome system - XX/XY 1 Y 2 . The race-specific arm chromosome combinations include three metacentrics and four acrocentrics in the Irkutsk race ( gk, hi, nq, m, o, p, r ) and four metacentrics and two acrocentrics in the Zima race ( gm, hi, ko, nq, p, r ). Within the races, individuals with polymorphic chromosomes were detected ( g/m, k/o, n/q, p/r ). The presence of the specific metacentric gk allowed us to include the Irkutsk race into the Siberian Karyotypic Group (SKG), distributed in surrounding regions. The Zima race karyotype contained two metacentrics, gm and ko , which have been never found in the Siberian part of the species range, but appear as the common feature of chromosomal races belonging to the West European Karyotypic Group (WEKG). Moreover, the metacentrics of that karyotype are almost identical to the Åkarp race (except the heterozygous pair p/r ) locally found in the southern Sweden. One of two Siberian races described here for the first time, the Zima race, occurs in an area considerably distant from Europe and shares the common metacentrics ( gm, hi, ko ) with races included in WEKG. This fact may support a hypothesis of independent formation of identical arm chromosome combinations due to occurrence of the same centric fusions in different parts of the species range.

An extreme bias in the germ line of XY C57BL/6<->XY FVB/N chimaeric mice

PubMed Central

MacGregor, G. R.

2011-01-01

Chimaeric analysis is a powerful method to address questions about the cell-autonomous nature of defects in spermatogenesis. Symplastic spermatids (sys) mice have a recessive mutation that causes male sterility due to an arrest in germ-cell development during spermiogenesis. Chimaeric mice were generated by aggregation of eight-cell embryos from sys (FVB/N genetic background) and wild-type C57BL/6 (B6) mice to determine whether the male germ-cell defect is cell-autonomous. The resulting FVB/N<->B6 chimaeras (<-> denotes fusion of embryos) were mated with FVB/N mice and coat colour of offspring was used to identify transmission of FVB/N or B6 gametes. Regardless of the relative contribution of B6 to somatic tissues of the chimaeras, almost all (282 of 284; 99.3%) offspring of B6 XY<->XY FVB/N (+/+ or sys/+) males (n = 9) received a FVB/N-derived paternal gamete. After mating of female B6<->FVB/N chimaeras, 51 of 73 (69.9%) offspring received an FVB-derived maternal gamete. Southern blot analysis of different tissues from chimaeric males indicated that, despite the presence of balanced chimaerism in somatic tissues, the germ line in B6 XY<->XY FVB/N mice was essentially FVB/N in composition. Thus there is a strong selective advantage for FVB/N male germ cells over B6 male germ cells in B6<->FVB/N-aggregation chimaeras at some stage during development of the male germ line. Each of three male chimaeras that were either B6 XY<->XY FVB/N (sys/sys) or B6 XX<->XY FVB/N (sys/sys) in composition was sterile, and testis histology was essentially sys mutant. This finding indicates that the function of the gene(s) affected in the sys mutation may be required in the testis, although whether expression is required in germ cells, somatic cells or both remains unknown. The extreme bias in transmission of male gametes has implications for experimental design in studies that use chimaeric analysis to address questions regarding the cell-autonomous nature of germ-cell defects in mice. PMID:12201811

Sports injury and illness incidence in the Rio de Janeiro 2016 Olympic Summer Games: A prospective study of 11274 athletes from 207 countries.

PubMed

Soligard, Torbjørn; Steffen, Kathrin; Palmer, Debbie; Alonso, Juan Manuel; Bahr, Roald; Lopes, Alexandre Dias; Dvorak, Jiri; Grant, Marie-Elaine; Meeuwisse, Willem; Mountjoy, Margo; Pena Costa, Leonardo Oliveira; Salmina, Natalia; Budgett, Richard; Engebretsen, Lars

2017-09-01

To describe the pattern of injuries and illnesses sustained during the Games of the XXXI Olympiad, hosted by Rio de Janeiro from 5 to 21 August 2016. We recorded the daily incidence of athlete injuries and illnesses (1) through the reporting of all National Olympic Committee (NOC) medical teams and (2) in the polyclinic and medical venues by the Rio 2016 medical staff. In total, 11 274 athletes (5089 women, 45%; 6185 men, 55%) from 207 NOCs participated in the study. NOC and Rio 2016 medical staff reported 1101 injuries and 651 illnesses, equalling 9.8 injuries and 5.4 illnesses per 100 athletes over the 17-day period. Altogether, 8% of the athletes incurred at least one injury and 5% at least one illness. The injury incidence was highest in BMX cycling (38% of the athletes injured), boxing (30%), mountain bike cycling (24%), taekwondo (24%), water polo (19%) and rugby (19%), and lowest in canoe slalom, rowing, shooting, archery, swimming, golf and table tennis (0%-3%). Of the 1101 injuries recorded, 40% and 20% were estimated to lead to ≥1 and >7 days of absence from sport, respectively. Women suffered 40% more illnesses than men. Illness was generally less common than injury, with the highest incidence recorded in diving (12%), open-water marathon (12%), sailing (12%), canoe slalom (11%), equestrian (11%) and synchronised swimming (10%). Illnesses were also less severe; 18% were expected to result in time loss. Of the illnesses, 47% affected the respiratory system and 21% the gastrointestinal system. The anticipated problem of infections in the Rio Olympic Games did not materialise, as the proportion of athletes with infectious diseases mirrored that of recent Olympic Games (3%). Overall, 8% of the athletes incurred at least one injury during the Olympic Games, and 5% an illness, which is slightly lower than in the Olympic Summer Games of 2008 and 2012. © Article author(s) (or their employer(s) unless otherwise stated in the text of the article) 2017. All rights reserved. No commercial use is permitted unless otherwise expressly granted.

Spectroscopic Detection of Minerals in Martian Meteorites using Reflectance and Emittance Spectroscopy and Applications to Surface Mineralogy on Mars

NASA Astrophysics Data System (ADS)

Bishop, J. L.; Hamilton, V. E.

2001-12-01

Martian meteorites provide direct information about crustal rocks on Mars. In this study we are measuring reflectance and emittance spectra of multiple Martian meteorites in order to characterize the spectral properties of the minerals present and to develop comprehensive criteria for remote detection of rocks and minerals. Previous studies have evaluated mid-IR emittance spectra [Hamilton et al., 1997] and visible/IR reflectance spectra [Bishop et al., 1998a,b] of Martian meteorites independently. The current study includes comparisons of the visible/NIR and mid-IR spectral regions and also involves comparison of mid-IR spectra measured using biconical reflectance and thermal emission techniques. Combining spectral analyses of Martian meteorite chips and powders enables characterization of spectral bands for remote detection of potential source regions for meteorite-like rocks on the surface of Mars using both Thermal Emission Spectrometer (TES) datasets and visible/NIR datasets from past and future missions. Identification of alteration minerals in these meteorites also provides insights into the alteration processes taking place on Mars. Analysis of TES data on Mars has identified global regions of basaltic and andesitic surface material [e.g. Bandfield et al., 2000; Christensen et al., 2000]; however neither of these spectral endmembers corresponds well to the spectra of Martian meteorites. Some preliminary findings suggest that small regions on the surface of Mars may relate to meteorite compositions [e.g. Hoefen et al., 2000; Hamilton et al., 2001]. Part of the difficulty in identifying meteorite compositions on Mars may be due to surface alteration. We hope to apply the results of our spectroscopic analyses of Martian meteorites, as well as fresh and altered basaltic material, toward analysis of composition on Mars using multiple spectral datasets. References: Bandfield J. et al., Science 287, 1626, 2000. Bishop J. et al., MAPS 33, 699, 1998a. Bishop J. et al., MAPS 33, 693, 1998b. Christensen P., et al., JGR 105, 9609, 2000. Hamilton V. et al., JGR 102, 25593, 1997. Hamilton V. et al., LPSC XXXII, #2184, 2001. Hoefen T. et al., Bull. Am. Astron. Soc. 32, 1118, 2000.

High Precision Iron Isotope Compositions in Components From the Allende CV3 Meteorite by MC-ICP-MS

NASA Astrophysics Data System (ADS)

Mullane, E.; Russell, S. S.; Weiss, D.; Mason, T. F.; Gounelle, M.

2001-12-01

Four chondrules and one matrix sample of Allende were examined for Fe-isotope frac-tionation, using multi-collector inductively coupled plasma mass spectrometry (MC-ICPMS). Iron is the most volatile major constituent of chondrules and a recent study [1] suggested that solar system Fe was initially isotopically homogeneous. Thus, any isotopic variation is likely due to mass fractionation during nebular process-ing. The chondrule samples were split. One portion was subject to a standard acid dis-solution whilst the other was polished, ena-bling textural and compositional characteri-zation. Fe, Cu and Zn are separated from the remaining matrix elements [2], removing potential interfering ions from the solution. 100 % elemental recovery (within error) is achieved, ensuring that chromatographic fractionation does not occur [2]. Hydrogen is bled into the collision cell, minimising Ar polyatomic species interferences. Typical precisions of 0.1‰ (2σ ) for 54Fe/56Fe ratios are achieved for 75 replicates. Instrumental mass bias is assessed using (1) sample-standard brack-eting and (2) doping with Cu. A variation of 0.8‰ /amu is observed, which is approximately 18 times the analyti-cal uncertainty at the 2σ level. Our high precision data show that: (1) Allende chondrules and matrix exhibit clear isotopic variation in iron. (2) δ 54Fe val-ues appear to be correlated to the bulk FeO content, with the more iron rich samples enriched in the lighter 54Fe isotope. (3) δ 54Fe values appear to be unre-lated to texture, and consequently to the temperature of chondrule formation. Bulk Fe-content may be a proxy for the amount of volatilisation experienced, and volatilisation of Fe in chondrule precursor material has resulted in a residue of the heavier Fe isotopes. Chondrules are known to have often experienced several heating events, and their texture primarily reflects the nature of the last event. Thus, the lack of correlation between the δ 54Fe value and chondrule texture suggests that Fe-isotope composi-tion was derived from chondrule precursor material. [1] Zhu et al. (2001) Nature 412, p.311 [2] Mullane et al. (2001) LPS XXXII, No.1545.

Unique Spectral Features Search In The 20 - 35 Micron Range of Mgs Tes Data

NASA Astrophysics Data System (ADS)

Altieri, F.; Bellucci, G.

TES is the Thermal Emission Spectrometer aboard the NASA mission Mars Global Surveyor (MGS) orbiting around Mars since September 1997. It is collecting 6 - 50 micron thermal emission spectra and one of its principal purposes is to determine and map the Mars surface composition. Spectral features directly ascribable to sur- face minerals have been identified in the 20 - 35 micron spectral range: deposits of crystalline gray hematite have been localized in three regions, Sinus Meridiani, Aram Chaos and Valles Marineris [1, 2], and outcrops of olivines have been individuated in Nili Fossae [3]. The crystalline gray hematite areas have been interpreted to be formed by aqueous mineralization, indicating that liquid water was stable near the Mars sur- face for a long period of time in some limited regions. On the other hand there is no evidence in TES data for large scale occurrences (< 10 km) of moderate-grained (> 50 micron) carbonates exposed at the surface at a detection limit of 10 % [2]. Mars thermal emission spectra show, in general, significant variance between 20 and 35 mi- cron. This variance is not directly attributable to surface mineralogical components for the difficulty of discriminating the contribute of atmospheric components: CO2 and water vapour gas, dust and water ice aerosols. Moreover, the dust layer deposited on the soil has a spectral masking effect, obscuring superficial signature related to smaller mineral deposit and making difficult their identification. In this study we report some examples of single TES spectra with typical hematite and olivine bands and spectra with other unique features in the 20 - 35 micron range likely related to superficial components. For some of them we have analysed how the spectral features change in two different Mars seasons. These single TES pixels could be best investigated by instruments with an higher spatial resolution, as THEMIS and OMEGA. References: [1] Christensen P. R., et al., JGR, 105, 9623-9642, 2000. [2] Christensen P. R., et al., JGR,106, 23823-23871, 2001. [3] Hoefen T. M. and Clark R. N., LPS XXXII, 2049, 2001.

Mapping the sex determination locus in the hāpuku (Polyprion oxygeneios) using ddRAD sequencing.

PubMed

Brown, Jeremy K; Taggart, John B; Bekaert, Michaël; Wehner, Stefanie; Palaiokostas, Christos; Setiawan, Alvin N; Symonds, Jane E; Penman, David J

2016-06-10

Hāpuku (Polyprion oxygeneios) is a member of the wreckfish family (Polyprionidae) and is highly regarded as a food fish. Although adults grow relatively slowly, juveniles exhibit low feed conversion ratios and can reach market size in 1-2 years, making P. oxygeneios a strong candidate for aquaculture. However, they can take over 5 years to reach sexual maturity in captivity and are not externally sexually dimorphic, complicating many aspects of broodstock management. Understanding the sex determination system of P. oxygeneios and developing accurate assays to assign genetic sex will contribute significantly towards its full-scale commercialisation. DNA from parents and sexed offspring (n = 57) from a single family of captive bred P. oxygeneios was used as a template for double digestion Restriction-site Associated DNA (ddRAD) sequencing. Two libraries were constructed using SbfI - SphI and SbfI - NcoI restriction enzyme combinations, respectively. Two runs on an Illumina MiSeq platform generated 70,266,464 raw reads, identifying 19,669 RAD loci. A combined sex linkage map (1367 cM) was constructed based on 1575 Single Nucleotide Polymorphism (SNP) markers that resolved into 35 linkage groups. Sex-specific linkage maps were of similar size (1132 and 1168 cM for male and female maps respectively). A single major sex-determining locus, found to be heterogametic in males, was mapped to linkage group 14. Several markers were found to be in strong linkage disequilibrium with the sex-determining locus. Allele-specific PCR assays were developed for two of these markers, SphI6331 and SphI8298, and demonstrated to accurately differentiate sex in progeny within the same pedigree. Comparative genomic analyses indicated that many of the linkage groups within the P. oxygeneios map share a relatively high degree of homology with those published for the European seabass (Dicentrarchus labrax). P. oxygeneios has an XX/XY sex determination system. Evaluation of allele-specific PCR assays, based on the two SNP markers most closely associated with phenotypic sex, indicates that a simple molecular assay for sexing P. oxygeneios should be readily attainable. The high degree of synteny observed with D. labrax should aid further molecular genetic study and exploitation of hāpuku as a food fish.

Germ cells are not the primary factor for sexual fate determination in goldfish.

PubMed

Goto, Rie; Saito, Taiju; Takeda, Takahiro; Fujimoto, Takafumi; Takagi, Misae; Arai, Katsutoshi; Yamaha, Etsuto

2012-10-01

The presence of germ cells in the early gonad is important for sexual fate determination and gonadal development in vertebrates. Recent studies in zebrafish and medaka have shown that a lack of germ cells in the early gonad induces sex reversal in favor of a male phenotype. However, it is uncertain whether the gonadal somatic cells or the germ cells are predominant in determining gonadal fate in other vertebrate. Here, we investigated the role of germ cells in gonadal differentiation in goldfish, a gonochoristic species that possesses an XX-XY genetic sex determination system. The primordial germ cells (PGCs) of the fish were eliminated during embryogenesis by injection of a morpholino oligonucleotide against the dead end gene. Fish without germ cells showed two types of gonadal morphology: one with an ovarian cavity; the other with seminiferous tubules. Next, we tested whether function could be restored to these empty gonads by transplantation of a single PGC into each embryo, and also determined the gonadal sex of the resulting germline chimeras. Transplantation of a single GFP-labeled PGC successfully produced a germline chimera in 42.7% of the embryos. Some of the adult germline chimeras had a developed gonad on one side that contained donor derived germ cells, while the contralateral gonad lacked any early germ cell stages. Female germline chimeras possessed a normal ovary and a germ-cell free ovary-like structure on the contralateral side; this structure was similar to those seen in female morphants. Male germline chimeras possessed a testis and a contralateral empty testis that contained some sperm in the tubular lumens. Analysis of aromatase, foxl2 and amh expression in gonads of morphants and germline chimeras suggested that somatic transdifferentiation did not occur. The offspring of fertile germline chimeras all had the donor-derived phenotype, indicating that germline replacement had occurred and that the transplanted PGC had rescued both female and male gonadal function. These findings suggest that the absence of germ cells did not affect the pathway for ovary or testis development and that phenotypic sex in goldfish is determined by somatic cells under genetic sex control rather than an interaction between the germ cells and somatic cells. Copyright © 2012 Elsevier Inc. All rights reserved.

Renormalization of loop functions for all loops

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

Brandt, R.A.; Neri, F.; Sato, M.

1981-08-15

It is shown that the vacuum expectation values W(C/sub 1/,xxx, C/sub n/) of products of the traces of the path-ordered phase factors P exp(igcontour-integral/sub C/iA/sub ..mu../(x)dx/sup ..mu../) are multiplicatively renormalizable in all orders of perturbation theory. Here A/sub ..mu../(x) are the vector gauge field matrices in the non-Abelian gauge theory with gauge group U(N) or SU(N), and C/sub i/ are loops (closed paths). When the loops are smooth (i.e., differentiable) and simple (i.e., non-self-intersecting), it has been shown that the generally divergent loop functions W become finite functions W when expressed in terms of the renormalized coupling constant and multipliedmore » by the factors e/sup -K/L(C/sub i/), where K is linearly divergent and L(C/sub i/) is the length of C/sub i/. It is proved here that the loop functions remain multiplicatively renormalizable even if the curves have any finite number of cusps (points of nondifferentiability) or cross points (points of self-intersection). If C/sub ..gamma../ is a loop which is smooth and simple except for a single cusp of angle ..gamma.., then W/sub R/(C/sub ..gamma../) = Z(..gamma..)W(C/sub ..gamma../) is finite for a suitable renormalization factor Z(..gamma..) which depends on ..gamma.. but on no other characteristic of C/sub ..gamma../. This statement is made precise by introducing a regularization, or via a loop-integrand subtraction scheme specified by a normalization condition W/sub R/(C-bar/sub ..gamma../) = 1 for an arbitrary but fixed loop C-bar/sub ..gamma../. Next, if C/sub ..beta../ is a loop which is smooth and simple except for a cross point of angles ..beta.., then W(C/sub ..beta../) must be renormalized together with the loop functions of associated sets S/sup i//sub ..beta../ = )C/sup i//sub 1/,xxx, C/sup i//sub p/i) (i = 2,xxx,I) of loops C/sup i//sub q/ which coincide with certain parts of C/sub ..beta../equivalentC/sup 1//sub 1/. Then W/sub R/(S/sup i//sub ..beta../) = Z/sup i/j(..beta..)W(S/sup j//sub ..beta../) is finite for a suitable matrix Z/sup i/j(..beta..).« less

Application of Geographical Information System Arc/info Grid-Based Surface Hyrologic Modeling to the Eastern Hellas Region, Mars

NASA Astrophysics Data System (ADS)

Mest, S. C.; Harbert, W.; Crown, D. A.

2001-05-01

Geographical Information System GRID-based raster modeling of surface water runoff in the eastern Hellas region of Mars has been completed. We utilized the 0.0625 by 0.0625 degree topographic map of Mars collected by the Mars Global Surveyor Mars Orbiter Laser Altimeter (MOLA) instrument to model watershed and surface runoff drainage systems. Scientific interpretation of these models with respect to ongoing geological mapping is presented in Mest et al., (2001). After importing a region of approximately 77,000,000 square kilometers into Arc/Info 8.0.2 we reprojected this digital elevation model (DEM) from a Mars sphere into a Mars ellipsoid. Using a simple cylindrical geographic projection and horizontal spatial units of decimal degrees and then an Albers projection with horizontal spatial units of meters, we completed basic hydrological modeling. Analysis of the raw DEM to determine slope, aspect, flow direction, watershed and flow accumulation grids demonstrated the need for correction of single pixel sink anomalies. After analysis of zonal elevation statistics associated with single pixel sinks, which identified 0.8 percent of the DEM points as having undefined surface water flow directions, we filled single pixel sink values of 89 meters or less. This correction is comparable with terrestrial DEMs that contain 0.9 percent to 4.7 percent of cells, which are sinks (Tarboton et al., 1991). The fill-corrected DEM was then used to determine slope, aspect, surface water flow direction and surface water flow accumulation. Within the region of interest 8,776 watersheds were identified. Using Arc/Info GRID flow direction and flow accumulation tools, regions of potential surface water flow accumulation were identified. These networks were then converted to a Strahler ordered stream network. Surface modeling produced Strahler orders one through six. As presented in Mest et al., (2001) comparisons of mapped features may prove compatible with drainage networks and watersheds derived using this methodology. Mest, Scott C., Crown, David A., and Harbert, William, 2001, Highland drainage basins and valley networks in the eastern Hellas Region of Mars, Abstract 1419, Lunar and Planetary Science XXXII Meeting Houston (CDROM). Tarboton D. G., Bras, R. L., and Rodriguez-Iturbe, 1991, On the Extraction of Channel Networks from Digital Elevation Data, Hydrological Processes, v. 5, 81-100. http://viking.eps.pitt.edu

Artificial size frequency distribution indices in laboratory experiments: Implications for understanding the evolution of Itokawa

NASA Astrophysics Data System (ADS)

Noviello, Jessica; Barnouin, Olivier S.; Ernst, Carolyn M.; Daly, Michael

2014-11-01

Asteroid 25143 Itokawa is a near-Earth irregular asteroid 535 by 294 by 209 meters in size [1]. The surface topography can be divided into the smooth lowlands and the rocky highlands. The origins of these regions could be due to the surface flow of fines from high to low points of gravitational potential [2]. Previous block studies conducted by Michikami et al. [3] and Mazrouei et al. [4] reported average size frequency distribution (SFD) indices on blocks larger than 6 m in diameter to be -3.1 ± 0.1 and -3.5 ± 0.1, respectively. Noviello et al. [5] reported preliminary results showing that blocks from 0.1 to 6 m in diameter had significantly lower SFD indices. They also reported that SFDs created from lowland image analyses consistently yield indices of around -2.71 ± 0.01, while the SFDs from highland images yield indices of roughly -2.00 ± 0.01 at the same scale. There are a number of geologic processes that could be responsible for the observed differences in SFD indices between different topographical regions. To quantify the effects of seismic shaking on SFD indices, we conducted simple laboratory experiments. Blocks were placed in a bin and slowly covered with sand and gravel, and then subjected to periods of moderate shaking in 10-second increments. The same methods used in the observational study were then applied to the experimental blocks to quantify the change in SFD index as the blocks were first covered and subsequently revealed. The initial results are: 1) As blocks are covered, in general the indices decrease; 2) Seismic shaking restores the indices; and 3) Larger blocks reappear faster than smaller rocks after shaking. This has implications for interpreting results of block count studies (the brazil nut effect [6]) and sample return missions, while also providing details about the physical expression of certain geologic processes on small bodies. [1] Fujiwara, A. et al., (2006) Science, 312, 1330-1334. [2] Miyamoto, H. et al., (2007) Science, 316, 1011-1014. [3] Michikami, T. et al., (2008) Earth Planets Space, 60, 13-20. [4] Mazrouei, S. et al., (2014) Icarus 229, 181-189. [5] Noviello, J. L. et al., (2014) LPSC XLV, Abstract #1587. [6] Asphaug, E., et al. (2001) LPSC XXXII, Abstract #1708.

Why we need detailed visible-range spectral data on Kuiper belt objects?

NASA Astrophysics Data System (ADS)

Busarev, V. V.

2001-05-01

Our understanding of Kuiper belt objects (KBOs)' nature may be based on two general scenarios of their origin. First, they could result from early accretional phases of the Solar System ``in situ". Then they are probably the most primitive and unprocessed bodies among known and should be mostly icy, with a very low content of silicate component. Second, a considerable portion of them (if not a majority) might have been thrown by Jupiter and other giant planets from their zones of accumulation. If so, they could include much more silicates (possibly up to 40%). To check the suppositions we need high-resolution visible and near-infrared spectral data on Centaurs (as possible `fugitives' from the Kuiper belt) and the KBOs. Because of faintness of the objects their physicochemical properties remain still little-known. Visible-range observations of the bodies by means of a spacecraft approaching to the belt could much help in solving the problem. Visible-infrared spectrophotometric observations of the objects showed a considerable diversity among them (Jewitt D. & J. Luu, 1998, Astron. J., 115, 1667-1670). It hints at a diversity in content of their matter. Spectral features of ices could not probably dominate in the visible range spectra of silicate-bearing KBOs. Reflectance spectra of principal gases' frosts are mainly flat and featureless in the range (Wagner J. K. et al., 1987, Icarus, 69, 14-28). Besides, silicates of KBOs are probably oxidized and hydrated to a high extent. Highly hydrated main-belt C-class asteroids have absorption bands at 0.43 and 0.6-0.8 microns (up to about 5%) (Vilas F. & M. J. Gaffey, 1989, Science, 246, 790-792 and Vilas F. et al., 1993, Icarus, 102, 225-231). Similar spectral features attributed to oxidized and hydrated silicates were also found on many M- and S-asteroids (e. g., Busarev V. V., 2001, LPSC XXXII, abstract 1927). The absorption bands are interpreted as caused by electronic processes in a bulk of oxidized silicates and hydrated clay minerals including structural OH-groups. Thus, the absorption features may be considered as indicators of a presence of oxidized and/or hydrated silicates on a solid body regardless of its position in the Solar System. For these reasons we have started visible-range spectroscopic observations of Centaurs and the KBOs on Russian 6-m telescope.

Identification of a Spectrally and Thermophysically Unique Region in Northern Amazonis Planitia, Mars: Surface Analysis using TES and THEMIS Data

NASA Astrophysics Data System (ADS)

Rogers, D.; Christensen, P. R.

2002-12-01

An intermediate-albedo (0.23-0.24) region located in northeastern Amazonis Planitia (approximately 900 km2 in area, centered at 40§N, 150§W) has been discovered to have a unique combination of certain spectral and thermophysical properties. The range of thermal inertia values for this region is 40-150 J/m2Ks1/2. On Mars, these values are usually indicative of a thick deposit of very fine-grained material (<63 microns) [1]. However, unlike typical dust deposits on Mars, this region exhibits moderate spectral contrast, with surface emissivity values ranging from 0.94-0.97 near 1030 cm-1. These emissivity values are uncharacteristic of fine-grained material [e.g., 2]. The modal mineralogy obtained by linear deconvolution of selected emissivity spectra from at least four different orbits over this region is not different than that reported for the Acidalia Planitia andesitic surface [3], within the mineral abundance detection limit estimated for TES [4]. However, the atmospherically-corrected surface spectral shape is distinct from the surface spectra common to Acidalia Planitia [3], Syrtis Major [3, 4], Sinus Meridiani [5] and Nili Fossae [6]. A spectral index was developed that describes the shape of a concave-down portion of the surface spectrum near 900 cm-1. A global 4 pixel-per-degree map of this index shows that the spectral character is unique to this region on Mars. MOC and THEMIS visible images available for this area show a uniform geomorphology consisting of parallel sinuous features trending NW-SE. Finally, THEMIS IR images show a sharp temperature contact that corresponds with the boundary of this area in the spectral index map. There are likely to be other explanations for reconciling the low thermal inertia with high spectral feature depth, however a favored hypothesis for this anomalous surface is that it is composed of a consolidated but highly porous material. This and other interpretations for this region will be discussed. References: [1] Kieffer et al. 1977, JGR, 82, 4249-4291; [2] Moersch and Christensen, 1995, JGR, 100, 7465-7477; [3] Bandfield et al. 2000, Science, 287, 1626-1630; [4] Christensen et al. 2000, JGR, 105, 9609-9621; [5] Christensen et al. 2000, JGR, 105, 9623-9642; [6] Hamilton et al. 2001, LPSC XXXII Abstracts, abstract 2184

Seabed images from Southern Ocean shelf regions off the northern Antarctic Peninsula and in the southeastern Weddell Sea

NASA Astrophysics Data System (ADS)

Piepenburg, Dieter; Buschmann, Alexander; Driemel, Amelie; Grobe, Hannes; Gutt, Julian; Schumacher, Stefanie; Segelken-Voigt, Alexandra; Sieger, Rainer

2017-07-01

Recent advances in underwater imaging technology allow for the gathering of invaluable scientific information on seafloor ecosystems, such as direct in situ views of seabed habitats and quantitative data on the composition, diversity, abundance, and distribution of epibenthic fauna. The imaging approach has been extensively used within the research project DynAMo (Dynamics of Antarctic Marine Shelf Ecosystems) at the Alfred Wegener Institute, Helmholtz Centre for Polar and Marine Research Bremerhaven (AWI), which aimed to comparatively assess the pace and quality of the dynamics of Southern Ocean benthos. Within this framework, epibenthic spatial distribution patterns have been comparatively investigated in two regions in the Atlantic sector of the Southern Ocean: the shelf areas off the northern tip of the Antarctic Peninsula, representing a region with above-average warming of surface waters and sea-ice reduction, and the shelves of the eastern Weddell Sea as an example of a stable high-Antarctic marine environment that is not (yet) affected by climate change. The AWI Ocean Floor Observation System (OFOS) was used to collect seabed imagery during two cruises of the German research vessel Polarstern, ANT-XXIX/3 (PS81) to the Antarctic Peninsula from January to March 2013 and ANT-XXXI/2 (PS96) to the Weddell Sea from December 2015 to February 2016. Here, we report on the image and data collections gathered during these cruises. During PS81, OFOS was successfully deployed at a total of 31 stations at water depths between 29 and 784 m. At most stations, series of 500 to 530 pictures ( > 15 000 in total, each depicting a seabed area of approximately 3.45 m2 or 2.3 × 1.5 m) were taken along transects approximately 3.7 km in length. During PS96, OFOS was used at a total of 13 stations at water depths between 200 and 754 m, yielding series of 110 to 293 photos (2670 in total) along transects 0.9 to 2.6 km in length. All seabed images taken during the two cruises, including metadata, are available from the data publisher PANGAEA via the two persistent identifiers at https://doi.org/10.1594/PANGAEA.872719 (for PS81) and https://doi.org/10.1594/PANGAEA.862097 (for PS96).

PREFACE: Mini EURO Conference on Improving Healthcare: new challenges, new approaches

NASA Astrophysics Data System (ADS)

2015-05-01

The XXXI Euro Mini Conference on Improving Healthcare: new challenges, new approaches took place in Coimbra, Portugal, from the 30th March to the 1st April 2015. This volume contains 17 contributed papers, presented during the Conference. Recent advances in medicine allow us to live longer and healthier lives. These advances have been made possible through the joint contribution of very different scientific fields. Healthcare is nowadays better understood as a multidisciplinary field, with increasing number of challenges that can be better tackled by joint collaboration of researchers with different scientific backgrounds. The challenges that Healthcare is facing have not only to do with the ability of providing better services to all (treatments, preventive medicine, better diagnosis tools), with an increased focus on improved personalized treatment options, but also with the need to tackle an increased pressure felt by Healthcare systems: increased number of patients, some of them requiring expensive treatments, with a consequent increase in the workload for health institutions that most of the times have to deal with important budget restrictions. The Conference provided a forum in which researchers coming from different scientific disciplines discussed and shared their experience regarding methodological approaches to tackle different healthcare challenges. The Conference welcomed contributions from operational research, industrial engineering, medicine, medical physics, management, computational biology, bioinformatics and health economics, among others. The Conference had 93 enrolled participants, from 22 different nationalities: Australia, Belgium, Brazil, Canada, Hong Kong, Ireland, Israel, Italy, Lebanon, Poland, Portugal, Romania, Serbia, Singapore, South Africa, Spain, Sweden, Switzerland, The Netherlands, United Arab Emirates, United Kingdom and United States of America. These participants had very different academic backgrounds: operations research, medicine, medical physics, engineering, biomedicine, medicine, among others. Moreover, participants had also very different professional backgrounds: researchers from academia, researchers from private companies, clinicians, etc. This diversity contributed to the fulfillment of the Conference objectives. Among these participants there were 20 PhD students presenting their research work, many of them for the first time. The Conference Program was composed by a total of 70 talks, 4 of which invited talks. Our invited speakers were Alexandre Quintanilha, Ben Heijmen, David Craft and Sally Braislford. The conference was supported by EURO (the Association of European Operational Research Societies), ORAHS (EURO Working Group on Operational Research Applied to Health Services), APDIO (Portuguese Operational Research Society), Inesc-Coimbra, Faculty of Economics of University of Coimbra, FCT (Portuguese Science Foundation) and COMPETE under project grant PTDC/EIA-CCO/121450/2010.

Planck intermediate results: XXXIII. Signature of the magnetic field geometry of interstellar filaments in dust polarization maps

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

Ade, P. A. R.; Aghanim, N.; Alves, M. I. R.

2016-02-09

Planck observations at 353 GHz provide the first fully sampled maps of the polarized dust emission towards interstellar filaments and their backgrounds (i.e., the emission observed in the surroundings of the filaments). The data allow us to determine the intrinsic polarization properties of the filaments and therefore to provide insight into the structure of their magnetic field (B). In this paper, we present the polarization maps of three nearby (several parsecs long) star-forming filaments of moderate column density (N H about 10 22 cm -2): Musca, B211, and L1506. These three filaments are detected above the background in dust totalmore » and polarized emission. We use the spatial information to separate Stokes I, Q, and U of the filaments from those of their backgrounds, an essential step in measuring the intrinsic polarization fraction (p) and angle (ψ) of each emission component. We find that the polarization angles in the three filaments (ψ fil) are coherent along their lengths and not the same as in their backgrounds (ψ bg). The differences between ψ fil and ψ bg are 12° and 54° for Musca and L1506, respectively, and only 6° in the case of B211. These differences forMusca and L1506 are larger than the dispersions of ψ, both along the filaments and in their backgrounds. The observed changes of ψ are direct evidence of variations of the orientation of the plane of the sky (POS) projection of the magnetic field. As in previous studies, we find a decrease of several per cent in p with N H from the backgrounds to the crest of the filaments. We show that the bulk of the drop in p within the filaments cannot be explained by random fluctuations of the orientation of the magnetic field because they are too small (σ ψ< 10°). We recognize the degeneracy between the dust alignment efficiency (by, e.g., radiative torques) and the structure of the B-field in causing variations in p, but we argue that the decrease in p from the backgrounds to the filaments results in part from depolarization associated with the 3D structure of the B-field: both its orientation in the POS and with respect to the POS. We do not resolve the inner structure of the filaments, but at the smallest scales accessible with Planck (~0.2 pc), the observed changes of ψ and p hold information on the magnetic field structure within filaments. Finally, they show that both the mean field and its fluctuations in the filaments are different from those of their backgrounds, which points to a coupling between the matter and the B-field in the filament formation process.« less

Projected Zika Virus Importation and Subsequent Ongoing Transmission after Travel to the 2016 Olympic and Paralympic Games - Country-Specific Assessment, July 2016.

PubMed

Grills, Ardath; Morrison, Stephanie; Nelson, Bradley; Miniota, Jennifer; Watts, Alexander; Cetron, Martin S

2016-07-22

Zika virus belongs to the genus Flavivirus of the family Flaviviridae; it is transmitted to humans primarily through the bite of an infected Aedes species mosquito (e.g., Ae. aegypti and Ae. albopictus) (1). Zika virus has been identified as a cause of congenital microcephaly and other serious brain defects (2). As of June 30, 2016, CDC had issued travel notices for 49 countries and U.S. territories across much of the Western hemisphere (3), including Brazil, where the 2016 Olympic and Paralympic Games (Games of the XXXI Olympiad, also known as Rio 2016; Games) will be hosted in Rio de Janeiro in August and September 2016. During the Games, mosquito-borne Zika virus transmission is expected to be low because August and September are winter months in Brazil, when cooler and drier weather typically reduces mosquito populations (4). CDC conducted a risk assessment to predict those countries susceptible to ongoing Zika virus transmission resulting from introduction by a single traveler to the Games. Whereas all countries are at risk for travel-associated importation of Zika virus, CDC estimated that 19 countries currently not reporting Zika outbreaks have the environmental conditions and population susceptibility to sustain mosquito-borne transmission of Zika virus if a case were imported from infection at the Games. For 15 of these 19 countries, travel to Rio de Janeiro during the Games is not estimated to increase substantially the level of risk above that incurred by the usual aviation travel baseline for these countries. The remaining four countries, Chad, Djibouti, Eritrea, and Yemen, are unique in that they do not have a substantial number of travelers to any country with local Zika virus transmission, except for anticipated travel to the Games. These four countries will be represented by a projected, combined total of 19 athletes (plus a projected delegation of about 60 persons), a tiny fraction of the 350,000-500,000 visitors expected at the Games.* Overall travel volume to the Games represents a very small fraction (<0.25%) of the total estimated 2015 travel volume to Zika-affected countries,(†) highlighting the unlikely scenario that Zika importation would be solely attributable to travel to the Games. To prevent Zika virus infection and its complications among athletes and visitors to the Games and importation of Zika virus into countries that could sustain local transmission, pregnant women should not travel to the Games, mosquito bites should be avoided while traveling and for 3 weeks after returning home, and measures should be taken to prevent sexual transmission (Box).

Iron isotope signatures within chondrules from Allende and Chainpur as indicators of thermal history.

NASA Astrophysics Data System (ADS)

Mullane, E.; Russell, S. S.; Gounelle, M.; Mason, T. F. D.

2003-04-01

Introduction: We have studied the petrography and Fe-isotope composition of seven chondrules, four from Allende (CV3) and three from Chainpur (LL3.4). A range of textural-chemical chondrule types are represented, allowing us to examine the Fe-isotope signature in material with different thermal histories, with a view to constraing the chondrule forming process and elucidating the nature of chondrule precursor material. Analytical procedures are detailed elsewhere [1,2,3] Fe-isotope Fractionation: The overall variation in δ56Fe is 1.98 ppm and in δ57Fe is 2.87 ppm. EM-1 (non-porphyritic) is most isotopically heavy and EM-3 (porphyritic) is most isotopically light, with all other chondrules falling in a mass fractionation line between these two end-members. This line is defined by the equation δ57Fe = (1.450±0.050)δ56Fe - (0.009±0.016) (R^2 = 0.9995). Discussion: The Fe-fractionation exhibited here is less than would be expected during open system evaporation. This suggests that Rayleigh conditions were not fulfilled during chondrule melting. Chainpur chondrules exhibit less fractionation than Allende chondrules, a total of 0.46 ppm (δ56Fe) in contrast to 1.98 ppm (δ56Fe), respectively, suggesting that Chainpur may be more equilibrated than Allende. Chainpur Fe-isotopes may have been increasingly homogenised by later addition of Fe, either from the nebular reservoir or parent body alteration. Porphyritic and nonporphyritic chondrules have differing thermal histories. The former are a product of incomplete melting, whereas the latter derive from almost total/complete melting of precursor material. However, Fe-isotope fractionation does not appear to vary systematically with texture. We conclude that chondrule Fe-isotopic signatures represent that of the precursor material, with later equilibration of the Chainpur chondrules. Melting history may also influence the Fe-isotopic signature. The isotopically heaviest chondrules (e.g. EM-1 &EC-3) may derive from a melt which attained liquidus temperatures more than once. The precursor to EM-2 (isotopically lightest), may not have been subject to as many aggressive heating events. References: [1] Mullane et al. (2001) LPS XXXII, Abs. #1545. [2] Mullane et al. (2002) In: Plasma Source Mass Spec. Royal Soc. Chem. (in press). [3] Mullane et al. (2002) Met. Plan. Sci. 37, 105 Abs. [4] Alexander C.M.O'D. &Wang J. (2001) Met. Plan. Sci. 36, 419--428.

The Enigma of Io's Warm Polar Regions

NASA Astrophysics Data System (ADS)

Matson, D. L.; Veeder, G. J.; Davies, A. G.; Johnson, T. V.; Blaney, D. L.

Io's polar temperatures are higher than expected for any passive surface. Data from the Galileo Photopolarimeter (PPR) show that minimum nighttime temperatures are in the range of 90 -95 K virtually everywhere [1]. This is particularly striking at high latitudes, within the polar regions. Furthermore, the distribution of minimum night- time temperatures across the surface of Io (away from the sunset terminator) shows little variation with latitude and/or time of night [1,2,3,4]. We consider suggested mechanisms for this elevated-minimum-temperature effect: 1) Polar terrain is warmer than expected because it is rough, 2) Higher latitudes have lower albedos, 3) Thermal inertia increases with latitude, and 4) Cooling lava controls nighttime temperatures. We find that the passive mechanisms fail. This leads to the suggestion that most of Io is covered by cooling lavas. In this context, lava cools to the observed temperature range on time scales of ten to ten thousand years depending upon the nature of the eruption scenario(s). Separately, analysis of thermal anomalies reveals that the trend of the data (log-cumulative-surface-area versus log-temperature) extrapolated to the entire surface area of Io predicts large- scale, ambient, temperatures in the 90-95 K range. Recent Galileo observations showing a myriad of small volcanic hot spots [7] provide strong support for the paradigm of ubiquitous volcanic activity with global, cooling-lava fields on Io. While explaining the high nighttime polar temperatures, this model displaces the previous explaination for Io's anomalously low 20 micron daytime emission. Explaining this emission is an important focus for current work. Warm polar regions appear to require some heat flow through very large areas in addition to the small, hot anomalies already known. This has implications for raising Io's global heat flow. Presently, the heat flow is constrained between a lower bound of ~2.5 W m -2[5] and an upper bound of ~13 W m -2[3,4,6]. References: [1] Spencer J. R. et al. (2000) Science, 288, 1198-1201. [2] Rathbun J. A. et al. (2001) EOS Trans. AGU, 82, P11A-11. [3] Matson D. L. et al. (2001) LPSC XXXII, 1938. [4] Matson D. L. et al. (2001) JGR, in press [5] Veeder G. J. et al. (1994) JGR, 99, 17095- 17162. [6] Matson D. L. et al. (2000) EOS, 81, F788. [7] Lopes-Gautier R. et al. (2000) Science, 288, 1201-1204. This work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract to NASA.

Big climate data analysis

NASA Astrophysics Data System (ADS)

Mudelsee, Manfred

2015-04-01

The Big Data era has begun also in the climate sciences, not only in economics or molecular biology. We measure climate at increasing spatial resolution by means of satellites and look farther back in time at increasing temporal resolution by means of natural archives and proxy data. We use powerful supercomputers to run climate models. The model output of the calculations made for the IPCC's Fifth Assessment Report amounts to ~650 TB. The 'scientific evolution' of grid computing has started, and the 'scientific revolution' of quantum computing is being prepared. This will increase computing power, and data amount, by several orders of magnitude in the future. However, more data does not automatically mean more knowledge. We need statisticians, who are at the core of transforming data into knowledge. Statisticians notably also explore the limits of our knowledge (uncertainties, that is, confidence intervals and P-values). Mudelsee (2014 Climate Time Series Analysis: Classical Statistical and Bootstrap Methods. Second edition. Springer, Cham, xxxii + 454 pp.) coined the term 'optimal estimation'. Consider the hyperspace of climate estimation. It has many, but not infinite, dimensions. It consists of the three subspaces Monte Carlo design, method and measure. The Monte Carlo design describes the data generating process. The method subspace describes the estimation and confidence interval construction. The measure subspace describes how to detect the optimal estimation method for the Monte Carlo experiment. The envisaged large increase in computing power may bring the following idea of optimal climate estimation into existence. Given a data sample, some prior information (e.g. measurement standard errors) and a set of questions (parameters to be estimated), the first task is simple: perform an initial estimation on basis of existing knowledge and experience with such types of estimation problems. The second task requires the computing power: explore the hyperspace to find the suitable method, that is, the mode of estimation and uncertainty-measure determination that optimizes a selected measure for prescribed values close to the initial estimates. Also here, intelligent exploration methods (gradient, Brent, etc.) are useful. The third task is to apply the optimal estimation method to the climate dataset. This conference paper illustrates by means of three examples that optimal estimation has the potential to shape future big climate data analysis. First, we consider various hypothesis tests to study whether climate extremes are increasing in their occurrence. Second, we compare Pearson's and Spearman's correlation measures. Third, we introduce a novel estimator of the tail index, which helps to better quantify climate-change related risks.

WIYN Open Cluster Study. XXXII. Stellar Radial Velocities in the Old Open Cluster NGC 188

NASA Astrophysics Data System (ADS)

Geller, Aaron M.; Mathieu, Robert D.; Harris, Hugh C.; McClure, Robert D.

2008-06-01

We present the results of our ongoing radial-velocity (RV) survey of the old (7 Gyr) open cluster NGC 188. Our WIYN 3.5 m data set spans a time baseline of 11 years, a magnitude range of 12 <= V <= 16.5 (1.18-0.94 M sun), and a 1° diameter region on the sky. With the addition of a Domain Astrophysical Observatory data set we extend our bright limit to V = 10.8 and, for some stars, extend our time baseline to 35 years. Our magnitude limits include solar-mass main-sequence stars, subgiants, giants, and blue stragglers (BSs), and our spatial coverage extends radially to 17 pc (~13 core radii). For the WIYN data we present a detailed description of our data reduction process and a thorough analysis of our measurement precision of 0.4 km s-1 for narrow-lined stars. We have measured radial velocities for 1046 stars in the direction of NGC 188, and have calculated RV membership probabilities for stars with >=3 measurements, finding 473 to be likely cluster members. We detect 124 velocity-variable cluster members, all of which are likely to be dynamically hard-binary stars. Using our single member stars, we find an average cluster radial velocity of -42.36 ± 0.04 km s-1. We use our precise RV and proper-motion membership data to greatly reduce field-star contamination in our cleaned color-magnitude diagram, from which we identify six stars of note that lie far from a standard single-star isochrone. We present a detailed study of the spatial distribution of cluster-member populations, and find the binaries to be centrally concentrated, providing evidence for the presence of mass segregation in NGC 188. We observe the BSs to populate a bimodal spatial distribution that is not centrally concentrated, suggesting that we may be observing two populations of BSs in NGC 188, including a centrally concentrated distribution as well as a halo population. Finally, we find NGC 188 to have a global RV dispersion of 0.64 ± 0.04 km s-1, which may be inflated by up to 0.23 km s-1 from unresolved binaries. When corrected for unresolved binaries, the NGC 188 RV dispersion has a nearly isothermal radial distribution. We use this mean-corrected velocity dispersion to derive a virial mass of 2300 ± 460 M sun .

Planck 2013 results. XXXI. Consistency of the Planck data

NASA Astrophysics Data System (ADS)

Planck Collaboration; Ade, P. A. R.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Burigana, C.; Cardoso, J.-F.; Catalano, A.; Challinor, A.; Chamballu, A.; Chiang, H. C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Désert, F.-X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Keihänen, E.; Keskitalo, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J.-M.; Lasenby, A.; Lawrence, C. R.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maino, D.; Mandolesi, N.; Maris, M.; Martin, P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, D.; Pearson, T. J.; Perdereau, O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J.-L.; Rachen, J. P.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Ristorcelli, I.; Rocha, G.; Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Scott, D.; Stolyarov, V.; Sudiwala, R.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.

2014-11-01

The Planck design and scanning strategy provide many levels of redundancy that can be exploited to provide tests of internal consistency. One of the most important is the comparison of the 70 GHz (amplifier) and 100 GHz (bolometer) channels. Based on different instrument technologies, with feeds located differently in the focal plane, analysed independently by different teams using different software, and near the minimum of diffuse foreground emission, these channels are in effect two different experiments. The 143 GHz channel has the lowest noise level on Planck, and is near the minimum of unresolved foreground emission. In this paper, we analyse the level of consistency achieved in the 2013 Planck data. We concentrate on comparisons between the 70, 100, and 143 GHz channel maps and power spectra, particularly over the angular scales of the first and second acoustic peaks, on maps masked for diffuse Galactic emission and for strong unresolved sources. Difference maps covering angular scales from 8° to 15' are consistent with noise, and show no evidence of cosmic microwave background structure. Including small but important corrections for unresolved-source residuals, we demonstrate agreement (measured by deviation of the ratio from unity) between 70 and 100 GHz power spectra averaged over 70 ≤ ℓ ≤ 390 at the 0.8% level, and agreement between 143 and 100 GHz power spectra of 0.4% over the same ℓ range. These values are within and consistent with the overall uncertainties in calibration given in the Planck 2013 results. We also present results based on the 2013 likelihood analysis showing consistency at the 0.35% between the 100, 143, and 217 GHz power spectra. We analyse calibration procedures and beams to determine what fraction of these differences can be accounted for by known approximations or systematicerrors that could be controlled even better in the future, reducing uncertainties still further. Several possible small improvements are described. Subsequent analysis of the beams quantifies the importance of asymmetry in the near sidelobes, which was not fully accounted for initially, affecting the 70/100 ratio. Correcting for this, the 70, 100, and 143 GHz power spectra agree to 0.4% over the first two acoustic peaks. The likelihood analysis that produced the 2013 cosmological parameters incorporated uncertainties larger than this. We show explicitly that correction of the missing near sidelobe power in the HFI channels would result in shifts in the posterior distributions of parameters of less than 0.3σ except for As, the amplitude of the primordial curvature perturbations at 0.05 Mpc-1, which changes by about 1σ. We extend these comparisons to include the sky maps from the complete nine-year mission of the Wilkinson Microwave Anisotropy Probe (WMAP), and find a roughly 2% difference between the Planck and WMAP power spectra in the region of the first acoustic peak.

Near-infrared spectroscopy of 3:1 Kirkwood Gap asteroids III

NASA Astrophysics Data System (ADS)

Fieber-Beyer, Sherry K.; Gaffey, Michael J.

2015-09-01

The research is an integrated effort beginning with telescopic observations and extending through detailed mineralogical characterizations to provide constraints on the composition and meteorite affinities of a subset of fourteen asteroids in/near the 3:1 Kirkwood Gap. Eight asteroids were identified as having either one or two absorption features, while six were deemed featureless. The compositional analysis of Asteroids (355) Gabriella and (1447) Utra reveal Fs and Fa values which are consistent with values for the L-type ordinary chondrites (Fs19-22 and Fa22-26). The location of these two bodies with respect to each other and to the previously identified L-chondrite parent body Asteroid (1722) Goffin, suggests a small L-chondrite genetic family. These results support the model that the L-chondrites come from an asteroid family rather than from a single object. Asteroids (1368) Numidia, (1587) Kahrstadt, (1854) Skvortsov, (2497) Kulikovskij, and (5676) Voltaire were analyzed and determined to have "basaltic" silicate mineralogies similar to those of the HED (howardite-eucrite-diogenite) meteorite group. In particular, we found that the compositions of (1368), (1587) and (1854) are consistent with olivine-orthopyroxenitic diogenites, while (2497) and (5676)'s compositions are consistent with harzburgitic diogenites. The Band I and Band II absorption feature depths are much shallower than seen in diogenite spectra, typically ∼70% depth (Burbine, T.H. et al. [2000]. Forging asteroid-meteorite relationships through reflectance spectroscopy. Lunar Planet. Sci. XXXI. Abstract 1844). The nature of the weak features seen in the asteroid spectra when compared to measured band depths of in situ diogenite samples indicate an additional mechanism(s) acting to weaken the features, most likely space weathering. The aforementioned five asteroids are plausible sources for the olivine-orthopyroxenitic diogenites and harzburgitic diogenites, and very well may be fragments of Vesta. Asteroid (46) Hestia is an interesting object whose surface minerals may be consistent with a CR2 chondrite; however, the unique spectrum deserves further study in the future. Featureless Asteroids (248) Lameia, (1960) Guisan, (3345) Tarkovskij and (6212) 1993 MS1 surface materials are likely organic assemblages consistent with the Type 1 or 2 carbonaceous chondrite meteorite class; however specific terrestrial meteorite analog could not be identified. The spectra of Asteroids (3228) Pire and (3999) Aristarchus are consistent with each other and have been assigned to the Eulalia by Walsh et al. (Walsh, K.J. et al. [2013]. Icarus 225, 283-297). Spectrally they are similar to (495) in terms of blue-slope and albedo (Fieber-Beyer, S.K., et al. [2012]. Icarus 221, 593-602), thus increasing our confidence the three bodies are truly related dynamically and genetically. By extrapolation and due to their location adjacent to the 3:1 Kirkwood Gap, (3228) and (3999) are plausible sources of the CV3OXB carbonaceous chondrites.

Planck intermediate results: XXXII. The relative orientation between the magnetic field and structures traced by interstellar dust

DOE PAGES

Adam, R.; Ade, P. A. R.; Aghanim, N.; ...

2016-02-09

The role of the magnetic field in the formation of the filamentary structures observed in the interstellar medium (ISM) is a debated topic owing to the paucity of relevant observations needed to test existing models. The Planck all-sky maps of linearly polarized emission from dust at 353 GHz provide the required combination of imaging and statistics to study the correlation between the structures of the Galactic magnetic field and of interstellar matter over the whole sky, both in the diffuse ISM and in molecular clouds. The data reveal that structures, or ridges, in the intensity map have counterparts in themore » Stokes Q and/or U maps. In this paper, we focus our study on structures at intermediate and high Galactic latitudes, which cover two orders of magnitude in column density, from 10 20 to 10 22 cm -2. We measure the magnetic field orientation on the plane ofthe sky from the polarization data, and present an algorithm to estimate the orientation of the ridges from the dust intensity map. We use analytical models to account for projection effects. Comparing polarization angles on and off the structures, we estimate the mean ratio between the strengths of the turbulent and mean components of the magnetic field to be between 0.6 and 1.0, with a preferred value of 0.8. We find that the ridges are usually aligned with the magnetic field measured on the structures. This statistical trend becomes more striking for increasing polarization fraction and decreasing column density. There is no alignment for the highest column density ridges. We interpret the increase in alignment with polarization fraction as a consequence of projection effects. We present maps to show that the decrease in alignment for high column density is not due to a loss of correlation between the distribution of matter and the geometry of the magnetic field. In molecular complexes, we also observe structures perpendicular to the magnetic field, which, statistically, cannot be accounted for by projection effects. This first statistical study of the relative orientation between the matter structures and the magnetic field in the ISM points out that, at the angular scales probed by Planck, the field geometry projected on the plane of the sky is correlated with the distribution of matter. In the diffuse ISM, the structures of matter are usually aligned with the magnetic field, while perpendicular structures appear in molecular clouds. Finally, we discuss our results in the context of models and MHD simulations, which attempt to describe the respective roles of turbulence, magnetic field, and self-gravity in the formation of structures in the magnetized ISM.« less

Planck intermediate results. XXXII. The relative orientation between the magnetic field and structures traced by interstellar dust

NASA Astrophysics Data System (ADS)

Planck Collaboration; Adam, R.; Ade, P. A. R.; Aghanim, N.; Alves, M. I. R.; Arnaud, M.; Arzoumanian, D.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartolo, N.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bracco, A.; Burigana, C.; Butler, R. C.; Calabrese, E.; Cardoso, J.-F.; Catalano, A.; Chamballu, A.; Chiang, H. C.; Christensen, P. R.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Couchot, F.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Ferrière, K.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.; Ghosh, T.; Giard, M.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.; Guillet, V.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J.-M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Levrier, F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Oppermann, N.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat, M.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J.-L.; Rachen, J. P.; Reach, W. T.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ristorcelli, I.; Rocha, G.; Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Soler, J. D.; Spencer, L. D.; Stolyarov, V.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Wiesemeyer, H.; Yvon, D.; Zacchei, A.; Zonca, A.

2016-02-01

The role of the magnetic field in the formation of the filamentary structures observed in the interstellar medium (ISM) is a debated topic owing to the paucity of relevant observations needed to test existing models. The Planck all-sky maps of linearly polarized emission from dust at 353 GHz provide the required combination of imaging and statistics to study the correlation between the structures of the Galactic magnetic field and of interstellar matter over the whole sky, both in the diffuse ISM and in molecular clouds. The data reveal that structures, or ridges, in the intensity map have counterparts in the Stokes Q and/or U maps. We focus our study on structures at intermediate and high Galactic latitudes, which cover two orders of magnitude in column density, from 1020 to 1022 cm-2. We measure the magnetic field orientation on the plane ofthe sky from the polarization data, and present an algorithm to estimate the orientation of the ridges from the dust intensity map. We use analytical models to account for projection effects. Comparing polarization angles on and off the structures, we estimate the mean ratio between the strengths of the turbulent and mean components of the magnetic field to be between 0.6 and 1.0, with a preferred value of 0.8. We find that the ridges are usually aligned with the magnetic field measured on the structures. This statistical trend becomes more striking for increasing polarization fraction and decreasing column density. There is no alignment for the highest column density ridges. We interpret the increase in alignment with polarization fraction as a consequence of projection effects. We present maps to show that the decrease in alignment for high column density is not due to a loss of correlation between the distribution of matter and the geometry of the magnetic field. In molecular complexes, we also observe structures perpendicular to the magnetic field, which, statistically, cannot be accounted for by projection effects. This first statistical study of the relative orientation between the matter structures and the magnetic field in the ISM points out that, at the angular scales probed by Planck, the field geometry projected on the plane of the sky is correlated with the distribution of matter. In the diffuse ISM, the structures of matter are usually aligned with the magnetic field, while perpendicular structures appear in molecular clouds. We discuss our results in the context of models and MHD simulations, which attempt to describe the respective roles of turbulence, magnetic field, and self-gravity in the formation of structures in the magnetized ISM.

A Comparative Study Of Dust Devils

NASA Astrophysics Data System (ADS)

Lange, C. F.; Prieto, L. E.

2005-12-01

Spatial variations in the column of water vapour in the Martian near-surface are due to the combined effects of several process within water underground reservoirs and the atmosphere. Among these process, dust devils could be an important local factor in the water concentration levels. In fact, the apparently high occurrence of dust devils could potentially affect the mass transfer rate of water vapour from the Martian regolith. A detailed study of these atmospheric vortices may help to better understand the complex relation between the cycle of water and this Martian atmospheric event. Subsequently, field data are required to provide a close estimation of the dynamics presented in Martian surface. The upcoming Phoenix mission is being designed to investigate these natural events on Mars. However, field studies of dust devils are difficult because of their sporadic, unpredictable occurrence and distance. In contrast, laboratory simulations present a better physical insight into this complex swirling flow by consideration of a much simplified, and more controllable and reproducible model flow. The use of numerical simulations in addition to laboratory experiments can provide complementary information on flow properties in regions where measurements are difficult due to flow profiles. Computational models also allow for significant flexibility in the model layout and they are, therefore, ideally suited for a comparison of different types of model flows. A 3-D numerical study is presented for two different types of dust devil laboratory simulators (Ward, 1952 and Greeley et al., 2001). An initial numerical study was conducted to validate the simulation results with previous laboratory measurements (Lund and Snow, 1993). Secondly, a numerical comparison was carried out between the two tornado-like vortex representations based on kinematic similarities to provide a clear method to relate dust devils in several nature environments, laboratory simulations, and computational models. This was accomplished by examining features of the dust devils in the form of three main flow parameters: the ratio of the inflow layer height h to the updraft radius r_0 (aspect ratio), the radial Reynolds number characterizing the updraft zone, and the ratio of the tangential velocity to the mean radial velocity (swirl ratio) at the radius of the updraft zone, r_0. The detailed analysis of the numerical flow solutions led to a simple definition of h and r_0, valid for the types of model flows analyzed. This study is a necessary part of a larger effort to examine and compare both numerical and laboratory simulations of atmospheric vortices in terrestrial and Martian conditions. References [1] R. Greeley et al., XXXII Lunar and Planetary Science, 2001. [2] D. E. Lund and J. T. Snow, The Tornado: Its Structure, Dynamics, Prediction, and Hazards, 1993, p. 297--306. [3] N. B. Ward, J. Atmos. Sci., 1972, 1194--1204.

Planck intermediate results: XXXII. The relative orientation between the magnetic field and structures traced by interstellar dust

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

Adam, R.; Ade, P. A. R.; Aghanim, N.

The role of the magnetic field in the formation of the filamentary structures observed in the interstellar medium (ISM) is a debated topic owing to the paucity of relevant observations needed to test existing models. The Planck all-sky maps of linearly polarized emission from dust at 353 GHz provide the required combination of imaging and statistics to study the correlation between the structures of the Galactic magnetic field and of interstellar matter over the whole sky, both in the diffuse ISM and in molecular clouds. The data reveal that structures, or ridges, in the intensity map have counterparts in themore » Stokes Q and/or U maps. In this paper, we focus our study on structures at intermediate and high Galactic latitudes, which cover two orders of magnitude in column density, from 10 20 to 10 22 cm -2. We measure the magnetic field orientation on the plane ofthe sky from the polarization data, and present an algorithm to estimate the orientation of the ridges from the dust intensity map. We use analytical models to account for projection effects. Comparing polarization angles on and off the structures, we estimate the mean ratio between the strengths of the turbulent and mean components of the magnetic field to be between 0.6 and 1.0, with a preferred value of 0.8. We find that the ridges are usually aligned with the magnetic field measured on the structures. This statistical trend becomes more striking for increasing polarization fraction and decreasing column density. There is no alignment for the highest column density ridges. We interpret the increase in alignment with polarization fraction as a consequence of projection effects. We present maps to show that the decrease in alignment for high column density is not due to a loss of correlation between the distribution of matter and the geometry of the magnetic field. In molecular complexes, we also observe structures perpendicular to the magnetic field, which, statistically, cannot be accounted for by projection effects. This first statistical study of the relative orientation between the matter structures and the magnetic field in the ISM points out that, at the angular scales probed by Planck, the field geometry projected on the plane of the sky is correlated with the distribution of matter. In the diffuse ISM, the structures of matter are usually aligned with the magnetic field, while perpendicular structures appear in molecular clouds. Finally, we discuss our results in the context of models and MHD simulations, which attempt to describe the respective roles of turbulence, magnetic field, and self-gravity in the formation of structures in the magnetized ISM.« less

PREFACE: XXXIII Symposium on Nuclear Physics

NASA Astrophysics Data System (ADS)

Barrón-Palos, Libertad; Bijker, Roelof; Fossion, Ruben; Lizcano, David

2010-04-01

The attached PDF gives a full listing of contributors and organisation members. In the present volume of Journal of Physics: Conference Series we publish the proceedings of the "XXXIII Symposium on Nuclear Physics", that was held from January 5-8, 2010 at the Hacienda Cocoyoc, Morelos, Mexico. The proceedings contain the plenary talks that were presented during the conference. The abstracts of all contributions, plenary talks and posters, were published in the Conference Handbook. The Symposium on Nuclear Physics has a long and distinguished history. From the beginning it was intended to be a relatively small meeting designed to bring together some of the leading nuclear scientists in the field. Its most distinctive feature is to provide a forum for specialists in different areas of nuclear physics, both theorists and experimentalists, students, postdocs and senior scientists, in a relaxed and informal environment providing them with a unique opportunity to exchange ideas. After the first meeting in Oaxtepec in 1978, the Symposium was organized every year without interruption which makes the present one the 33rd in a row. This year's meeting was dedicated to the memory of Marcos Moshinsky, who passed away on April 1, 2009. Dr. Moshinsky was the most distinguished pioneer and promoter of nuclear physics in Mexico and Latin America and holds the record of 31 (out of 32) participations at the Symposium. In the inaugural session, Alejandro Frank (ICN-UNAM), Peter Hess (ICN-UNAM) and Jorge Flores (IF-UNAM) spoke in his honor and recalled the virtues that characterized him as a teacher, scientist, founder of schools and academic institutions, colleague and friend. His generosity, excellence and honesty were emphasized as the personal qualities that characterized both his personal and academic life. moshinksky_photo "Marcos Moshinsky (1921-2009)" The scientific program consisted of 26 invited talks and 20 posters on a wide variety of hot topics in contemporary nuclear physics, ranging from the traditional fields of nuclear structure and reactions to radioactive beams, nuclear astrophysics, hadronic physics, fundamental symmetries, ultrarelativistic heavy ions, cosmic rays and quantum chaos. The high quality of the talks, the prestige of the speakers and the broad spectrum of subjects covered in the meeting, shows that nuclear physics is a very active area at the frontier of scientific research which establishes bridges between many different disciplines. One of the exciting new areas in nuclear physics is that of radioactive beams. It provides a powerful tool not only to study exotic nuclei close to the proton and neutron drip lines to obtain important information about the nature of the nucleon-nucleon interaction in stable and unstable nuclei, but also to address questions of fundamental importance in nuclear astrophysics as well as in various applications like mass spectroscopy, the production of radioactive isotopes and medical applications (Galindo-Uribarri). There was a presentation on the FRIB project which is currently under construction in the USA and its relevance for nuclear astrophysics and the limits of stability (Sherrill and Schatz) In the session on nuclear structure, there were several talks on the nucleon-nucleon interaction in nuclei close to the proton and neutron drip lines, like neutron-proton pairing in nuclei with an equal number of protons and neutrons (Pittel), and studies of stable and unstable neutron-rich nuclei near the closed shells N = 82 and N = 50 using (d, p) transfer reactions and Coulomb excitation by means of radioactive beams (Cizewski and Padilla-Rodal). There were several talks on the importance of reaction rates for the excitation of spin-isospin resonances (Sakai), massive star evolution (Klapp) and nuclear synthesis and stellar evolution (Rolfs). In another presentation, the importance of rare isotopes for astrophysical processes was highlighted (Schatz). In addition, there were discussions about the importance of the Pauli exclusion principle and phase transitions in nuclear cluster models (Cseh and Hess) and an analysis of elastic scattering close to the Coulomb barrier in the framework of the optical model (Gómez-Camacho). Another important area is that of hadronic physics, the study of nucleons as composite systems of strongly interacting quarks and gluons. This field is situated on the borderline between nuclear and particle physics and presents a formidable challenge since the scale of the energies involved prohibits the use of the methods of perturbative QCD. In the session on hadronic physics, there were talks on chiral symmetry in non-perturbative QCD (Bietenholz), the structure of the nucleon in an unquenched quark model (Bijker), quark and meson degrees of freedom in Deeply Virtual Compton Scattering (Szczepaniak) and studies of hadronic structure by means of neutrino-induced pion production (Mariano). At ultrarelativistic energies, one can study the phase transition between hadronic matter and a new state of nuclear matter, the quark-gluon plasma. The Organizing Committee is proud to mention that the Cocoyoc 2010 meeting was one of first international conferences where the first scientific resuls from LHC were presented by the ALICE collaboration on proton-proton collisions at an energy of 900 GeV (Paic). In the session on cosmic rays, there was a talk on the origin of ultra high-energy cosmic rays (100 EeV = 1020 eV) as observed by the Pierre Auger Observatory (Medina-Tanco). Furthermore, there was a presentation of the project NuMoon which proposes to use the Moon's surface to detect cosmic rays that are out of the range of the Auger Observatory (Scholten). In addition, there was a review of the advances of the Mexican project HAWC, an observatory under construction in the Sierra Negra of Puebla (Sandoval) to study some of the most violentphenomena in the Universe through the detection of gamma rays with energies between hundreds of GeV and hundreds of TeV. At the other extreme of the energy scale is the field of the study of fundamental symmetries with novel experiments with ultra-cold neutrons. In this session, there were proposals by the NPDGamma collaboration (Gillis) and the abBA collaboration (Barr´on-Palos) to use polarized neutrons to study the weak hadronic interaction and neutron beta-decay, respectively. In another talk, there was a discussion on the measurement of the electric dipole moment of the neutron which is of fundamental importance to the standard model (Crawford). Finally, there was a session dedicated to quantum chaos where various proposals were discussed to identify chaotic behaviour in quantum systems, such as spectral fluctuations, time series and 1/f noise (Molina). Applications were presented to many-body systems in nuclear physics (Stránský) and the dripping-laser system as a quantum realization of the dripping faucet, one of the paradigms of classical chaos (Fossion). Many of the participants spent the free afternoon in the "magic village" of Tepoztlán to visit the arts and crafts market, the church, the convent or just to enjoy the good food. The most daring persons climbed the nearby cliff Tepozteco and the pyramid built on top of it to contemplate the spectacular view over the valley. As always, some of the participants of the conference prolonged their stay in Mexico to establish, to develop or to consolidate their collaborations with the local nuclear physics community. At the annual reunion of the Nuclear Physics Division which was held during the meeting, there was a long discussion on the future of the Symposium and, more generally, of the field of nuclear physics in Mexico and Latin America. Libertad Barr´on Palos, Roelof Bijker, Ruben Fossion and David Lizcano were re-elected as members of the Local Organizing Committee of the next Symposium which will be held at the Hacienda Cocoyoc from January 4-7, 2011, but now with Libertad as Chair. Libertad Barrón-Palos Roelof Bijker Ruben Fossion David Lizcano conference photo_photo

Searching for an Improved Spectral Match to TES and IRIS Sinus Meridiani Spectra: Coatings and Cemented Materials

NASA Astrophysics Data System (ADS)

Kirkland, L. E.; Herr, K. C.; Adams, P. M.

2001-05-01

A region on Mars within Sinus Meridiani has been interpreted as a surface partially covered by coarse-grained (gray) hematite, using spectra measured by the 1996 Global Surveyor Thermal Emission Spectrometer (TES) [Lane et al., 1999; Christensen et al., 2000]. The band strengths recorded by TES of this region are consistent with either coarse-grained hematite, or cemented poorly crystalline or cemented fine-grained hematite. The band strengths are inconsistent with unconsolidated, poorly crystalline or fine-grained hematite, including nanophase hematite dust [Christensen et al., 2000]. Currently the gray hematite interpretation is based on bands centered near 22 and 33 microns. TES also records a band centered near 18 microns that was used in early hematite interpretations [Lane et al., 1999]. However, it was noted [Kirkland et al., 1999a] that the 18 micron band is too narrow in both TES and the 1971 Mariner Mars IRIS spectra to be a good match to typical spectra of well-crystalline hematite [e.g. Salisbury et al., 1991]. The 18 micron band is near the very strong 15 micron atmospheric CO2 band, but if anything the nearby CO2 band should cause the 18 micron band to appear wider, not narrower. In addition, the higher spectral resolution of IRIS allows improved separation of the bands [Kirkland et al., 1999b]. More recent publications no longer show the TES 18 micron band [e.g. Lane et al., 2000; Christensen et al., 2000], which temporarily resolved the issue. However, we feel it is important to understand why TES and IRIS spectra exhibit an 18 micron band that is too narrow to match typical spectra of coarse-grained hematite. Smooth-surfaced cemented (e.g. ferricrete) or coated materials (e.g. desert varnish) have spectral contrast that is consistent with the observed IRIS and TES band contrast. On Mars, one possible source for cemented material or coatings would be the nanophase hematite dust. Cemented materials may occur in bulk (e.g. duricrust or ferricrete), or as a thin coating (e.g. desert varnish). We have investigated the signatures of naturally occurring cemented materials that contain hematite, and found samples that exhibit 22 and 33 micron bands that are consistent with coarse-grained hematite signatures, and yet also exhibit narrower 18 micron bands. We are continuing to study the materials more in-depth to examine the variations in spectral shape, and to determine the cause of varied 18 micron band width. References. Christensen, P. R. et al., JGR 105, 9632, 2000. Kirkland, L., K. Herr, P. Forney, and J. Salisbury, LPSC XXX, abs. 1693 and oral presentation, 1999a. Kirkland, L., K. Herr, and P. Forney, 5th Internat'l Conf. on Mars, abs. 6174, 1999b. Lane, M., R. Morris, and P. Christensen, LPSC XXX, abs. 1469, 1999. Lane, M., R. Morris, and P. Christensen, LPSC XXXI, abs. 1140, 2000. Salisbury, J., L. Walter, N. Vergo, D. D'Aria, Infrared (2.1-25 micron) Spectra of Minerals, Johns Hopkins UP, 1991.

Dense, gravity-driven granular-liquid flows down steep channels

NASA Astrophysics Data System (ADS)

Armanini, A.; Larcher, M.; Nucci, E.

2011-12-01

Debris flows are complex natural phenomena, characterized by a mixture of poorly sorted sediments and water driven by gravity. Depending on the size distribution, on the volume concentration of sediments and on the geometry and topography of the channel, flow conditions may be very different, ranging from very fast flows, dominated by granular collisions and by the turbulence on the liquid phase, to very slow and dense flows, dominated by the frictional contacts among the grains. To investigate the basic physics of debris flows, it is very useful to analyze the flow of a mixture of identical spherical particles saturated by water and driven by gravity down a steep channel in steady flow condition (Armanini et al. 2005). The flow presents three regions: an external one, near to the free surface, dominated by nearly instantaneous contacts among the particles (collisional regime), an internal region dominated by prolonged contacts among the particles (frictional regime) and a static bed in which the particles are immobile. The detailed vertical structure of this kind of flows was obtained by means of experiments carried out by Armanini et al. (2005) and Larcher et al. (2007). Armanini et al. (2009) analysed the stratification of rheological mechanisms inside the flow, focusing on the coexistence of frictional and collisional regimes, on the stress transmission inside the flow and on particles kinematics. In particular, it was observed that debris flows may show locally a typical intermittence of the flow regime, switching alternatively from frictional to collisional. While the rheology of the collisional layers is well described by the dense gas analogy (kinetic theory), a persuasive theoretical description of the frictional regime does not yet exist. A Coulombian scheme is often assumed, but this hypothesis is rather limitative because it requires a constant concentration or a distribution of particles concentration known a priori. An interesting scheme of this kind was recently proposed by GDR-Midi (2004), but this model does not contain a suitable formulation for the granular pressure (equation of state of the mixture). Following Armanini (2010), we propose a reinterpretation of the model, as weighted average of a pure Coulombian stress (dependent on the static friction angle at the static bed level) and of a dynamic stress, represented by a dynamic friction angle. Besides, a state relation is introduced for the granular pressure and the dynamic friction angle is derived from the kinetic theory. The proposed relations are finally successfully compared with the experimental data introduced above. REFERENCES A. Armanini, H. Capart, L. Fraccarollo, M. Larcher, 2005, J.F.M., 532, 269-319. A. Armanini, M. Larcher, L. Fraccarollo, Ph. Rev. E, 2009, 79, 051306. A. Armanini, 2010, Palermo, Proc. XXXII Conv. Naz. di Idr. e C.I. (in Italian) GDR MiDi, 2004. Eur. Phys. J. E, 14, 341-365 M. Larcher, L. Fraccarollo, A. Armanini, H. Capart, 2007, Journal Hydr. Res., 45, 59-71.

Spectra and structure of silicon containing compounds. XXXII. Raman and infrared spectra, conformational stability, vibrational assignment and ab initio calculations of n-propylsilane-d0 and Si-d3.

PubMed

Durig, James R; Pan, Chunhua; Guirgis, Gamil A

2003-03-15

The infrared (3100-40 cm(-1)) and Raman (3100-20 cm(-1)) spectra of gaseous and solid n-propylsilane, CH(3)CH(2)CH(2)SiH(3) and the Si-d(3) isotopomer, CH(3)CH(2)CH(2)SiD(3), have been recorded. Additionally, the Raman spectra of the liquids have been recorded and qualitative depolarization values obtained. Both the anti and gauche conformers have been identified in the fluid phases but only the anti conformer remains in the solid. Variable temperature (-105 to -150 degrees C) studies of the infrared spectra of n-propylsilane dissolved in liquid krypton have been recorded and the enthalpy difference has been determined to be 220+/-22 cm(-1) (2.63+/-0.26 kJ mol(-1)) with the anti conformer the more stable form. A similar value of 234+/-23 cm(-1) (2.80+/-0.28 kJ mol(-1)) was obtained for deltaH for the Si-d(3) isotopomer. At ambient temperature it is estimated that there is 30+/-2% of the gauche conformer present. The potential function governing the conformation interchange has been estimated from the far infrared spectral data, the enthalpy difference, and the dihedral angle of the gauche conformer, which is compared to the one predicted from ab initio MP2/6-31G(d) calculations. The barriers to conformational interchange are: 942, 970 and 716 cm(-1) for the anti to gauche, gauche to gauche, and gauche to anti conformers, respectively. Relatively complete vibrational assignments are proposed for both the n-propylsilane-d(0) and Si-d(3) molecules based on the relative infrared and Raman spectral intensities, infrared band contours, depolarization ratios, and normal coordinate calculations. The geometrical parameters, harmonic force constants, vibrational frequencies, infrared intensities, Raman activities and depolarization ratios, and energy differences have been obtained for the anti and gauche conformers from ab initio MP2/6-31G(d) calculations. Structural parameters and energy differences have also been obtained utilizing the larger 6-311 + G(d,p) and 6-311 + G(2d,2p) basis sets. From the isolated Si-H stretching frequency from the Si-d(2) isotopomer the r(0) distances of 1.484 and 1.485 A have been determined for the SiH(s) and SiH(a) bonds, respectively, for the anti conformer, and 1.486 A for the SiH bond for the gauche conformer. Utilizing previously reported microwave rotational constants for the anti conformer and the determined SiH distances along with ab initio predicted parameters 'adjusted r(0)' parameters have been obtained for the anti conformer. The results are discussed and compared to those obtained for some similar molecules. Copyright 2002 Elsevier Science B.V.

Spectra and structure of silicon containing compounds. XXXII. Raman and infrared spectra, conformational stability, vibrational assignment and ab initio calculations of n-propylsilane-d 0 and Si-d 3

NASA Astrophysics Data System (ADS)

Durig, James R.; Pan, Chunhua; Guirgis, Gamil A.

2003-03-01

The infrared (3100-40 cm -1) and Raman (3100-20 cm -1) spectra of gaseous and solid n-propylsilane, CH 3CH 2CH 2SiH 3 and the Si-d 3 isotopomer, CH 3CH 2CH 2SiD 3, have been recorded. Additionally, the Raman spectra of the liquids have been recorded and qualitative depolarization values obtained. Both the anti and gauche conformers have been identified in the fluid phases but only the anti conformer remains in the solid. Variable temperature (-105 to -150 °C) studies of the infrared spectra of n-propylsilane dissolved in liquid krypton have been recorded and the enthalpy difference has been determined to be 220±22 cm -1 (2.63±0.26 kJ mol -1) with the anti conformer the more stable form. A similar value of 234±23 cm -1 (2.80±0.28 kJ mol -1) was obtained for Δ H for the Si-d 3 isotopomer. At ambient temperature it is estimated that there is 30±2% of the gauche conformer present. The potential function governing the conformation interchange has been estimated from the far infrared spectral data, the enthalpy difference, and the dihedral angle of the gauche conformer, which is compared to the one predicted from ab initio MP2/6-31G(d) calculations. The barriers to conformational interchange are: 942, 970 and 716 cm -1 for the anti to gauche, gauche to gauche, and gauche to anti conformers, respectively. Relatively complete vibrational assignments are proposed for both the n-propylsilane-d 0 and Si-d 3 molecules based on the relative infrared and Raman spectral intensities, infrared band contours, depolarization ratios, and normal coordinate calculations. The geometrical parameters, harmonic force constants, vibrational frequencies, infrared intensities, Raman activities and depolarization ratios, and energy differences have been obtained for the anti and gauche conformers from ab initio MP2/6-31G(d) calculations. Structural parameters and energy differences have also been obtained utilizing the larger 6-311+G(d,p) and 6-311+G(2d,2p) basis sets. From the isolated SiH stretching frequency from the Si-d 2 isotopomer the r0 distances of 1.484 and 1.485 Å have been determined for the SiH s and SiH a bonds, respectively, for the anti conformer, and 1.486 Å for the SiH bond for the gauche conformer. Utilizing previously reported microwave rotational constants for the anti conformer and the determined SiH distances along with ab initio predicted parameters 'adjusted r0' parameters have been obtained for the anti conformer. The results are discussed and compared to those obtained for some similar molecules.

Terrestrial microbes in martian and chondritic meteorites

NASA Astrophysics Data System (ADS)

Airieau, S.; Picenco, Y.; Andersen, G.

2007-08-01

Introduction: The best extraterrestrial analogs for microbiology are meteorites. The chemistry and mineralogy of Asteroid Belt and martian (SNC) meteorites are used as tracers of processes that took place in the early solar system. Meteoritic falls, in particular those of carbonaceous chondrites, are regarded as pristine samples of planetesimal evolution as these rocks are primitive and mostly unprocessed since the formation of the solar system 4.56 billion years ago. Yet, questions about terrestrial contamination and its effects on the meteoritic isotopic, chemical and mineral characteristics often arise. Meteorites are hosts to biological activity as soon as they are in contact with the terrestrial biosphere, like all rocks. A wide biodiversity was found in 21 chondrites and 8 martian stones, and was investigated with cell culture, microscopy techniques, PCR, and LAL photoluminetry. Some preliminary results are presented here. The sample suite included carbonaceous chondrites of types CR, CV, CK, CO, CI, and CM, from ANSMET and Falls. Past studies documented the alteration of meteorites by weathering and biological activity [1]-[4]. Unpublished observations during aqueous extraction for oxygen isotopic analysis [5], noted the formation of biofilms in water in a matter of days. In order to address the potential modification of meteoritic isotopic and chemical signatures, the culture of microbial contaminating species was initiated in 2005, and after a prolonged incubation, some of the species obtained from cell culture were analyzed in 2006. The results are preliminary, and a systematic catalog of microbial contaminants is developing very slowly due to lack of funding. Methods: The primary method was cell culture and PCR. Chondrites. Chondritic meteorite fragments were obtained by breaking stones of approximately one gram in sterile mortars. The core of the rocks, presumably less contaminated than the surface, was used for the present microbial study, and the remaining fragments of the samples were used for amino acid and isotopic analyses [6]. Some samples were fragments of dried and wet meteorites isolated in centrifuge tubes after a 10-day water extraction. Sabouraud Dextrose (dilutions 1:10 and 1:1000), Bacto Agar, LB Broth Miller (dilutions 1:10 and 1:1000), and R2A agar (1:1 and 1:1000), were autoclaved and cooled in culture plates inside a clean hood for cell culture. Some controls retained sterile moist agar still adhering to the perimeter of the plates for up to 18 months, and validated the sterile technique. Cell culture, PCR and microscopy documented a diversity of archea, prokaryotes and eukaryotes in these samples [7]. The plates displaying microbial growth at room temperature after 6 weeks or less were used to produce streak plates and isolate colonies of individual species for long term freezing in Eppendorf tubes. Any plate with biological growth along the perimeter of the plate was discarded. The plates without microbial activity after 6 weeks were stored in a fridge for 18 months. Control plates, exposed to the clean hood, laboratory room, used gloves, and weighing paper used in the analyses, sustained the prolonged storage with no sign of microbial activity that could be related to the analysis method. Dust grains and water extracts from the meteorites were spread on agar surfaces in cell culture Petri dishes in a clean hood. SNC samples.In early 2005, the surface of SNC stones in the USNM curation facility were brushed with sterile swabs. Fallen dust grains were collected on weighing paper and isolated in sterile tubes. The sample suite included Zagami USNM 6545, Lafayette USNM 1505, Los Angeles USNM 7052, Shergotty USNM 321, Nakhla USNM 5892, Nakhla USNM 426 (117.4 g) and Nakhla USNM 426 (18.2 g), and Chassigny USNMMNHN 2524. The controls, worker's gloves, blank swabs, and weighing paper exhibited no microbial activity in subsequent months. The cell culture was conducted with Sabouraud Dextrose and R2A only, by deposition of dry grains onto the surface of agar in culture plates that were incubated at 20 Celsius 2 weeks, then at 35 Celsius 3 days, and finally at 4 Celsius for 18 months. Limulus Amoebocyte Lysate (LAL Assay) measurements of the swabs [7] revealed low biological activity in all SNCs, except in a small piece of Nakhla USNM 426 (18.2 g) (activity below detection limit) and Chassigny (data unavailable). The LAL technique assesses gram negative bacterial equivalents. Culture sample material was recovered from the agar plates using sterile pipette tips. The material was added to 100 uL sterile water. This material was boiled for 15 min. in a water bath to lyse the cells and inactivate enzymes. 10 uL of the boiled lysate was used as template in PCR. Universal bacterial primers (27F and 1492R) were used to amplify a major portion of the 16S rRNA gene. PCR product was purified using a Qiagen MinElute PCR Purification kit and then sent for sequencing. Results and Comments: GRA 95229. Biological growth out of dust grains deposited on the agar surface was visible with the naked eye, and occurred after incubation in a fridge for 10 months. Leoville. Biological growth occurred at the contact of a dust grain and the agar surface after 1 month. It continued to expand outside a dust grain deposited on Sabouraud Dextrose 1:1000, while stored at 20 Celsius for 12 months. The fan shaped outgrowth reached about 1 cm on either side of the meteorite grain and dried. DNA was recovered, and PCR products yielded sequences of a Bacillus spp. Bacillus is a common soil bacterial genus, and the close sequence relatives of this isolate were no exception. They were rock or soil Bacillus, and have been found in Allende [4]. EET 87770. Rock fragments were wet for 8 months (Millipore water) in a sterile centrifuge tube, and were used to make a spread plate that dried over a period of 10 months. The yellow dried colonies yielded good PCR product and the sequences were compared to other GenBank sequences using the BLAST program. The closest matches were in the genus Microbacterium. Soil and plant isolates were close relatives by sequence comparison. Los Angeles. After 11 months of incubation in a fridge, a yellow colony grew at the center of a culture plate of Los Angeles dust grains (1:1000 R2A). There was no cell activity in the other agars. A DNA extraction yielded no usable results [7]. Sequencing was not performed because the culture plate became contaminated with outside organisms that overtook the colony of interest. Conclusions: The sequences for EET 87770 and Leoville were of a good quality and the sequence reads were long, so the data are clear that these are typical soil and/or plant-related bacteria commonly found in Earth habitats. Microbial species present in a dozen chondritic samples from isolates are not yet identified, and the contaminant in Los Angeles needs to be recovered. In addition, isotopic analyses of samples with various amounts of microbial contamination could help quantified isotopic impact of microbes on protoplanetary chemistry in these rocks. References : [1] Gounelle, M. and Zolensky M. LPS, (2001) LPS XXXII, Abstract #999. [2] Fries, M. et al. (2005) Meteoritical Society Meeting 68, Abstract # 5201. [3] Burckle, L. H. and Delaney, J. S (1999) Meteoritics & Planet. Sci., 32, 475-478. [4] Whitby, C. et al. (2000) ) LPS XXXI, Abstract #1732. [5] Airieau, S. A. et al (2005) Geochim. Cosmochim. Acta, 69, 4166-4171. [6] Unpublished data, with H. J. Cleaves, A. Aubrey, J. Bada (Scripps Institution of Oceanography), M. Thiemens (UC San Diego) and M. Fogel (Carnegie Institution of Washington). [7] Unpublished data, with A. Steele (CIW), and N. Wainwright (Marine Biological Laboratory). Acknowledgements: Lisa Welleberger for access to SNC samples at USNM; Ralph Harvey for organizing ANSMET; Denise C. Thiry and Andrew Steele for long term storage of samples, NormWainwright for LAL measurements. A small portion of this work was funded with a NASA Cosmochemistry grant, ( P. I. Thiemens).

Geologic mapping of the saturnian satellites based on Cassini ISS images: objectives, methods, and results

NASA Astrophysics Data System (ADS)

Wagner, R.; Roatsch, T.; Giese, B.; Wolf, U.; Neukum, G.

Remote Sensing of the Earth and Planets, Freie Universitaet Berlin, Germany Data set and objectives: Since the Cassini Orbiter has been inserted into orbit around Saturn on July 1, 2004, image data of the major saturnian satellites were collected by the Cassini ISS narrow and wide angle cameras (NAC and WAC respectively) at resolutions up to 10 - 20 m/pxl [1]. Up to now, the surface of each one of these satellites was imaged at least once at distances less than 20000 km. The extended image coverage and much higher resolution compared to Voyager images from more than two decades ago help to define (1) the global distribution of geologic units at regional map scale (100 - 300 m/pxl), (2) to identify units of possibly cryovolcanic origin, (3) to map tectonic landforms in detail, and (4) to use the crater size-frequency distributions measured on geologic units for relative and absolute age dating. Also (5), the stratigraphic column for each satellite can be subdivided into time-stratigraphic systems by the combination of stratigraphy and crater frequency measurements. Methods: All geologic maps are produced on image base maps put together from images of various flybys at each satellite [2]. Geologic units are identified by their specific albedo and morphology. In some cases, topographic data and digital elevation models are available. Cratering chronology models are used to derive absolute model ages from crater size-frequency measurements [3]. Important stratigraphic markers (and their associated crater frequencies and ages) which can be used to subdivide the geological history of a specific satellite are (1) volcanic flows, (2) prominent tectonic landforms, (3) large impact features, such as basins, and (4) craters with extended ray systems. Results: In this paper we focus on regional geologic maps of Dione and Rhea, two neighbours in orbit, and of Enceladus. Dione and Rhea, 1124 and 1538 km in diameter, are characterized (a) by densely cratered plains, (b) smooth, less densely cratered plains, and (3) by tectonic features, mostly horst and graben structures [4][5][6]. Cratering model ages of the densely cratered plains are on the order of 4.2 Gyr [6]. The surface of Rhea appears to be more densely cratered and hence older than the one of Dione. Also, Rhea has a higher abundance of large impact features several 100 km in diameter while only one such basin was found on Dione [6][7]. Ray craters are not abundant at crater sizes larger than 20 km except for one feature found on Rhea. Enceladus (502 km in diameter) shows a wide range of geologic units and surface ages. Densely cratered plains with ages on the order of 4 Gyr are cut by tectonic bands of ridges and grooves with various model ages ranging from 1 to more than 3 Gyr [6]. In the south polar terrain, areas almost devoid of craters and with cratering model ages much less than 4 Myr 1 reveal on-going geologic processes which recently were confirmed by the discovery of cryovolcanic activity on this moon [6][8]. References: [1] Porco, C. C. et al., Space Sci. Rev. 115, 363-497, 2004. [2] Roatsch, T. et al., Planet. Space Sci., in press, 2006. [3] Neukum G. et al., 40th ESLAB Symposium, May 8-12, 2006, abstract book, 235, 2006. [4] Plescia, J., Icarus 56, 401-413, 1983. [5] Moore, J., Icarus 59, 205-220, 1984. [6] Wagner, R. et al., LPSC XXXVII, abstr. No. 1805 [CD-Rom], 2006. [7] Stooke, P. J., LPSC XXXIII, abstr. No. 1553 [CD-Rom], 2002. [8] Porco, C. C. et al., Science 311, 1393-1401, 2006. 2

Modeling of Ionosphere Effects of Geomagnetic Storm Sequence on September 9-14, 2005 in View of Solar Flares and Dependence of Model Input Parameters from AE-and Kp-indices

NASA Astrophysics Data System (ADS)

Klimenko, Maxim; Klimenko, Vladimir; Ratovsky, Konstantin; Goncharenko, Larisa

Earlier by Klimenko et al., 2009 under carrying out the calculations of the ionospheric effects of storm sequence on September 9-14, 2005 the model input parameters (potential difference through polar caps, field-aligned currents of the second region and particle precipitation fluxes and energy) were set as function of Kp-index of geomagnetic activity. The analyses of obtained results show that the reasons of quantitative distinctions of calculation results and observations can be: the use of 3 hour Kp-index at the setting of time dependence of model input parameters; the dipole approach of geomagnetic field; the absence in model calculations the effects of the solar flares, which were taken place during the considered period. In the given study the model input parameters were set as function of AE-and Kp-indices of geomagnetic activity according to different empirical models and morphological representations Feshchenko and Maltsev, 2003; Cheng et al., 2008; Zhang and Paxton, 2008. At that, we taken into account the shift of field-aligned currents of the second region to the lower latitudes as by Sojka et al., 1994 and 30 min. time delay of variations of the field-aligned currents of second region relative to the variations of the potential difference through polar caps at the storm sudden commencement phase. Also we taken into account the ionospheric effects of solar flares. Calculation of ionospheric effects of storm sequence has been carried out with use of the Global Self-Consistent Model of the Thermosphere, Ionosphere and Protonosphere (GSM TIP) developed in WD IZMIRAN (Nam-galadze et al., 1988). We carried out the comparison of calculation results with experimental data. This study is supported by RFBR grant 08-05-00274. References Cheng Z.W., Shi J.K., Zhang T.L., Dunlop M. and Liu Z.X. Relationship between FAC at plasma sheet boundary layers and AE index during storms from August to October, 2001. Sci. China Ser. E-Tech. Sci., 2008, Vol. 51, No. 7, 842-848. Feshchenko E.Yu., Maltsev Yu.P. Relations of the polar cap voltage to the geophysical activity. Physics of Auroral Phenomena: XXVI Annual Seminar (February 25-28, 2003): Proc./PGI KSC RAS. Apatity, 2003, 59-61. Klimenko M.V., Klimenko V.V., Ratovsky K.G., and Goncharenko L.P. Numerical modeling of ionospheric parameters during sequence of geomagnetic storms on September 9-14, 2005. Physics of Auroral Phenomena: XXXII Annual Seminar (March 3-6, 2009): Proc./PGI KSC RAS. Apatity, 2009, 162-165. Namgaladze A.A., Korenkov Yu.N., Klimenko V.V., Karpov I.V., Bessarab F.S., Surotkin V.A., Glushenko T.A., Naumova N.M. Global model of the thermosphere-ionosphere-protonosphere system. Pure and Applied Geophysics (PAGEOPH), 1988, Vol. 127, No. 2/3, 219-254. Sojka J.J., Schunk R.W., Denig W.F. Ionospheric response to the sustained high geomagnetic activity during the March '89 great storm. J. Geophys. Res., 1994, Vol. 99, No. A11, 21341-21352. Zhang Y., Paxton L.J. An empirical Kp-dependent global auroral model based on TIMED/GUVI FUV data. J. Atmos. Solar-Terr. Phys., 2008, Vol. 70, 1231-1242.

Online Citizen Science with Clickworkers & MRO HiRISE E/PO

NASA Astrophysics Data System (ADS)

Gulick, V. C.; Deardorff, G.; Kanefsky, B.; HiRISE Science Team

2010-12-01

The High-Resolution Imaging Science Experiment’s E/PO has fielded several online citizen science projects. Our efforts are guided by HiRISE E/PO’s philosophy of providing innovative opportunities for students and the public to participate in the scientific discovery process. HiRISE Clickworkers, a follow-on to the original Clickworkers crater identification and size diameter marking website, provides an opportunity for the public to identify & mark over a dozen landform feature types in HiRISE images, including dunes, gullies, patterned ground, wind streaks, boulders, craters, layering, volcanoes, etc. In HiRISE Clickworkers, the contributor views several sample images showing variations of different landforms, and simply marks all the landform types they could spot while looking at a small portion of a HiRISE image. Contributors then submit their work & once validated by comparison to the output of other participants, results are then added to geologic feature databases. Scientists & others will eventually be able to query these databases for locations of particular geologic features in the HiRISE images. Participants can also mark other features that they find intriguing for the HiRISE camera to target. The original Clickworkers website pilot study ran from November 2000 until September 2001 (Kanefsky et al., 2001, LPSC XXXII). It was among the first online Citizen Science efforts for planetary science. In its pilot study, we endeavored to answer two questions: 1) Was the public willing & able to help science, & 2) Can the public produce scientifically useful results? Since its inception over 3,500,000 craters have been identified, & over 350,000 of these craters have been classified. Over 2 million of these craters were marked on Viking Orbiter image mosaics, nearly 800,000 craters were marked on Mars Orbiter Camera (MOC) images. Note that these are not counts of distinct craters. For example, each crater in the Viking orbiter images was counted by about 50 contributors. In HiRISE Clickworkers, over a dozen different geologic features have been identified on over 57,000 image tiles. A key objective of Clickworkers has been to break up work into manageable chunks so that people can contribute a few minutes at a time and their work all adds up. Our HiRISE Student Image Challenges (http://quest.nasa.gov), another online citizen science project, provide educators and students a virtual science team experience. Registered participants are given access to HiWeb, the HiRISE team’s image suggestion facility to submit their image suggestions. Once the images are returned, students browse, pan and zoom through their acquired images online and at full resolution before they are released to the public (http://marsoweb.nas.nasa.gov/HiRISE/quest/). Students fill out a report form summarizing the key results of their image analysis and with the help of a HiRISE team member write a caption for their image. The image is posted on the HiRISE image release website along with the caption, with credit to the suggesting class and school. HiWish, HiRISE’s public image suggestion website (see McEwen et al., this mtg.), provides a simpler interface for the public at large to submit HiRISE images. HiWish also provides a list of recently submitted image requests.

Noble gas Records of Early Evolution of the Earth

NASA Astrophysics Data System (ADS)

Ozima, M.; Podoesk, F. A.

2001-12-01

Comparison between atmospheric noble gases (except for He) and solar (or meteoritic) noble gases clearly suggests that the Earth should have much more Xe than is present in air, and thus that up to about 90 percent of terrestrial Xe is missing from the Earth (1). In this report, we discuss implications of these observations on I-Pu chronology of the Earth and on the origin of terrestrial He3. Whetherill (2) first noted that an estimated I129/I127 ratio (3x10-6) in the proto-Earth was about two orders of magnitude smaller than values commonly observed in meteorites (10-4), and pointed out the possibility that Earth formation postdated meteorites by about 100Ma. Ozima and Podosek (1999) came to a similar conclusion on the basis of I129/I127-Pu244/U238 systematics (1). In this report, we reexamine I-Pu systematics with new data for crustal I content (295 ppb for a bulk crust, (3)). With imposition of an estimated value of 86 percent missing Xe as a constraint on terrestrial Xe inventory, we conclude that the best estimate for a formation age of the Earth is about 28Ma after the initial condensation of the solar nebula (at 4.57Ga). The formation age thus estimated is significantly later than the generally assumed age of meteorites. We also argue from the I-Pu systematics that the missing Xe became missing place about 120Ma after Earth formation. Assuming that the Earth is mostly degassed, the I-Pu formation age of the Earth can be reasonably assumed to represent a whole Earth event. Therefore, we interpret that the I-Pu age of the Earth represents the time when the Earth started to retain noble gases. More specifically, this may correspond to the time when the proto-Earth attained a sufficient size to exert the necessary gravitational force. A giant impact could be another possibility, but it remains to be seen whether or not a giant impact could quantitatively remove heavier noble gases from the Earth. It is interesting to speculate that missing Xe was sequestered in the core during core formation. Core formation time would then be related to the time of the missing Xe event. The above estimated missing Xe age is close to the core formation age suggested from Nb-Zr systematics (4) and from U-Pb systematics (5), but considerably later than that suggested from Hf-W systematics (6). From a comparison of relative elemental abundance of noble gases between the Earth and the solar composition, we show that terrestrial He3 may be totally unrelated to heavier noble gases. This requires independent origin of terrestrial He3 from heavy noble gases. 1.Ozima M. and Podosek F.A. (1999) JGR, 104(BII), 25493. 2.Whetherill G.W. (1975) Ann. Rev. Nuclear Science, 25, 283. 3.Muramatsu Y. and Wedepohl K.H. (1998) Chemical Geology, 147, 201. 4. Jacobsen S.B. and Yin Q.Z. (2001) Lunar Planetary Science, XXXII, 1961.pdf (abstract). 5.Galer S.J.G. and Goldstein S.L. (1995) in Geophysical Monograph 95, 75-98, AGU. 6.Halliday A.N., Lee D.-C. and Jacobsen S.B. (2000) in Origin of the Earth and Moon, 45-62, Univ. Arizona Press.

VizieR Online Data Catalog: Solar neighborhood. XXXIII. 45 M dwarfs (Riedel+, 2014)

NASA Astrophysics Data System (ADS)

Riedel, A. R.; Finch, C. T.; Henry, T. J.; Subasavage, J. P.; Jao, W.-C.; Malo, L.; Rodriguez, D. R.; White, R. J.; Gies, D. R.; Dieterich, S. B.; Winters, J. G.; Davison, C. L.; Nelan, E. P.; Blunt, S. C.; Cruz, K. L.; Rice, E. L.; Ianna, P. A.

2015-01-01

The sample of 45 star systems in this paper was drawn from the hundreds of targets in the Cerro Tololo Inter-American Observatory Parallax Investigation (CTIOPI) target list. This is the 13th paper publishing parallax results from the ongoing CTIOPI program (Jao et al., 2003AJ....125..332J; Jao et al., 2005AJ....129.1954J; Costa et al., 2005AJ....130..337C; Costa et al, 2006AJ....132.1234C; Henry et al., 2006AJ....132.2360H; Subasavage et al., 2009AJ....137.4547S; Riedel et al., 2010AJ....140..897R; Jao et al., 2011AJ....141..117J; Boyd et al. 2001, cat. J/AJ/142/10) at the CTIO 0.9m telescope. The targets in this paper are all nearby bright M dwarfs Among the 45 systems considered here, we have individual photometry and astrometry of 51 components, because six of our star systems contain binaries with separations more than 1''. All CTIOPI photometry is conducted with the CTIO 0.9m telescope, initially (1999-2003) under the NOAO Survey Programs grant; later (2003-present) via the SMARTS Consortium. Photometry is conducted in three filters (Tektronix 2 VRI), utilizing only the central quarter (6.8*6.8' FOV, 401mas/pixel) of the Tektronics 2046*2046 CCD. These values are then transformed to standard Johnson/Kron-Cousins VJRKCIKC (the central wavelengths for VJ, RKC, and IKC are 5475, 6425, and 8075Å, respectively) photometry. The resulting photometry can be found in Table 2. Further details of the observation and reduction procedures can be found in Jao et al. (2005AJ....129.1954J) and Winters et al. 2011 (cat. J/AJ/141/21). CTIOPI astrometry is carried out using the same telescope and camera configuration as that used for photometry but uses only one filter for each object. Between 2005 March and 2009 September, a different V-band filter was used for astrometric and photometric observations. Additional details of CTIOPI observing procedures can be found in Jao et al. (2005AJ....129.1954J; Paper XIII), Henry et al. (2006AJ....132.2360H; Paper XVII), and other papers in this series. Four of the objects in this paper (BD-21°1074BC, SCR 0613-2742AB, L 449-1AB, and SCR 2010-2801AB) were selected for their X-ray brightness and observed with the Hubble Space Telescope's (HST's) Fine Guidance Sensors (FGSs) in Cycle 16B, in proposal 11943/11944 ("Binaries at the Extremes of the H-R Diagram") using the F583W filter (the bandpass of the F583W filter is shown here: http://www.stsci.edu/hst/fgs/design/filters, checked 2013 June 4) with no pupil. Spectroscopic observations of all the resolved objects in this paper (except SCR 0613-2742AB) were carried out between 2003-2006 and 2009-2011 using the CTIO 1.5m telescope under the aegis of the SMARTS Consortium. The CTIO 1.5m Richey-Chretien Spectrograph (RCSpec) was used with the 32/I grating setting, covering 6000-9600Å at a resolution of 8Å. We obtained spectra of SCR 0613-2742AB with the CTIO 4.0m telescope's RCSpec on 2008 September 18 and 2008 September 19 using the KPGLF-1 (632g/mm) grating, which covers 4900-8050Å at a resolution of 1.9Å/pixel. One spectrum of SCR 0613-2742AB was taken with the FEROS spectrograph on the MPG 2.2m telescope at La Silla Observatory on 2013 February 18 as part of ESO program 090.C-0200(A). FEROS is an echelle spectrograph fed by two 2.0'' fibers and provides R~48000 spectra over a wavelength range of 3500-9200Å. SCR 1425-4113AB was observed on the Canada-France-Hawaii Telescope (CFHT) with the ESPaDOnS. ESPaDONs was used in the "star+sky" mode, to get a resolving power of R=68000 covering 3700-10500Å over 40 grating orders. (11 data files).

Syrtis Major, Mars: Geology, Morphology and Topography Based on new MOLA and MOC Data

NASA Astrophysics Data System (ADS)

Hiesinger, H.; Head, J. W.

2001-05-01

The circular shape of Syrtis Major has been interpreted to be impact related [1] but the topography of the structure is more consistent with a low shield volcano [2, 3]. The low relief of Syrtis Major is very different from other Martian shield volcanos (e.g., Tharsis) and may be related to changes in composition, differentiation history, eruptive styles or differences in crustal thickness [2]. Individual lava flows of Syrtis Major are among the thinnest on Mars (25-30 m; [3]), are up to 120-150 km long [2], and ISM data suggest a SNC-like [4] composition. Slopes of northern Syrtis Major are ~0.13°, to the south slopes are ~0.02°, and to the west are on the order of 0.4°. We observe steeper slopes of ~0.5 to the east. According to Schaber [2] and Hodges and Moore [5] Syrtis Major is ~1100 km in diameter and has an estimated maximum height of only 0.5 km. E-W profiles based on MOLA data show that the height of the shield is ~0.5 km, consistent with previous estimates. However, MOLA N-S profiles indicate a significantly higher edifice of ~1 km. Nili Patera (caldera C1 of [2]) and Meroe Patera (caldera C2 of [2]) are located within a complex large N-S elongated depression [2, 6] and their floors are at an elevation of ~100-200 m and 180-250 m, respectively. The caldera floors are at about the same elevation as the cratered highlands immediately north of Syrtis Major and at significantly lower elevation than the cratered highlands west and south of Syrtis Major. The highest point of the shield is NW of Nili Patera at about 2300 m. The terrain southwest, west and north of the calderas is noticeably higher ( ~2000-2300 m) than east of the calderas ( ~1500-1700 m), hence forming a crescent-like summit with steeper slopes into the summit depression and gentler slopes away from the summit. A MOLA map of kilometer-scale surface roughness shows that the Syrtis Major Formation is rougher at all wavelengths (0.6-19.2 km) compared to other investigated Martian volcanic units (e.g., Hr, At4, At5, Aop) [7]. Syrtis Major can be clearly distinguished from the surrounding cratered highlands by its smoother surface. Isidis Planitia is significantly smoother than Syrtis Major and this might be related to sedimentation within the impact basin [8, 9]. A map derived from MGS data does not show significant differences in crustal thickness underneath the Syrtis Major volcanic complex compared to adjacent cratered highland plains [10]. Cratered highlands and Syrtis Major both have a crustal thickness on the order of ~45-60 km. However, the crust is significantly thinner compared to the Tharsis area (>60 km). The new data also indicate that there is no evidence for a gravity anomaly associated with Syrtis Major, hence supporting an origin independent of an impact [2]. [1] Meyer and Grolier, 1977, USGS I-995; [2] Schaber, 1982, J. Geophys. Res. 87, 9852-9866; [3] Head et al., 1998, LPSC 29, 1322; [4] Mustard et al., 1997, J. Geophys. Res. 102, 25605-25615; [5] Hodges and Moore, 1994, USGS Prof. Paper 1534, 152-153; [6] Crumpler et al., 1996, in: Volcano Instability on the Earth and other planets, 307-348; [7] Kreslavsky and Head, 2000, J. Geophys. Res. 105, 26695-26711; [8] Head and Bridges, 2001, LPSC XXXII, 1236; [9] Grizzaffi and Schultz, 1989, Icarus 77, 358-381; [10] Zuber et al., 2000, Science 287, 1788-1793.

A Clementine Derived Control Network and Topographic Model - The Unified Lunar Control Network 2005

NASA Astrophysics Data System (ADS)

Archinal, B. A.; Rosiek, M. R.; Kirk, R. L.; Redding, B. L.

2006-08-01

U. S. Geological Survey, Astrogeology Team, Flagstaff, AZ, United States Introduction: We have completed a new general unified lunar control network and lunar topographic model based on Clementine images. It includes the determination, in the lunar mean Earth/polar axis system, of the 3-D positions of 272,931 points on the lunar surface and the correction of the camera angles for 43,866 Clementine images, using 546,126 tie point measurements. The solution RMS is 0.9 pixels in the image plane, with the largest residual of 6.4 pixels. We are now documenting our solution and plan to release the solution results soon, initially as a USGS Open File report. ULCN 2005 Features: The new network is a combination of the Unified Lunar Control Network (ULCN), derived from the Apollo, Mariner 10, and Galileo missions, and Earth-based photographs, [1] and the Clementine Lunar Control Network (CLCN) [2], both derived from (mostly 750-nm) Clementine images, by M. Davies and T. Colvin at RAND. The primary difference between our new network and the previous ones is that we solve for the radii of the control points. This avoids (~7 km) distortion of horizontal positions present in the CLCN. The expected precision of such information is on the order of several hundred m, and compatible with Clementine LIDAR [3]. Thus, a by-product of this network is a global lunar topographic model that is denser than that provided by LIDAR and of similar accuracy, and denser than any other lunar topography information except that provided in limited areas ([4-7]). This is the only lunar topographic model positioning where both heights and horizontal positions are estimated in a globally-consistent system. Other features of the ULCN 2005 are that the camera angles to their values as measured during the mission, supposedly with an accuracy of 0.03º [8], and we have identified a majority of the original ULCN points on Clementine images. Future Work: The Lunar Orbiter (LO) digital mosaics now being generated [9] will be registered to the ULCN 2005. We will also further improve this network through the addition of Mariner 10, Galileo, and LO image measurements, and Clementine stereo [10], and by adding ties to the current absolute LLR and ALSEP network [11]. Although unfunded, the Clementine mosaics could also be regenerated in this system. It will be absolutely essential to further update and improve this network with data from future missions. This is necessary so that these new datasets can be compared to the prior data, particularly the LO and Clementine multispectral products. References: [1] Davies, M. E. et al. (1994) JGR, 99, E11, 23,211-23,214. [2] Edwards, et al. (1996), LPS XXVII, 335-336. [3] Smith, D. E. et al. (1997), JGR, 102, E1, 1591-1611. [4] Cook, A. C. et al. (2000), JGR, 105, E5, 12,023-12,033. [5] Rosiek, M. R. et al. (1998), LPS XXX, Abstract #1853. Rosiek, M. R., and Aeschliman, R. A. (2001) LPS XXXII, Abstract #1943. [6] Margot, J-L. C. (1999), PhD Thesis, Cornell University. [7] Wu, S. S. C. and Doyle, F. J. (1990), in Planetary Mapping, R. Greeley and R.M. Batson, eds., CUP, 169-207. [8] Nozette, S., et al. (1994), Science, 266, 1835-1839. [9] Weller, L., et al. (2006), LPS XXXVII, Abstract #2143. [10] Cook, A. C. et al. (2002), AGU Fall Meeting, Abstract #P22D-09. [11] Davies, M. E. and Colvin, T. R. (2000), JGR, 105, E8, 20,277-20,280.

High-resolution mapping of elemental abundances of the lunar regolith

NASA Astrophysics Data System (ADS)

Wöhler, Christian; Berezhnoy, Alexey; Evans, Richard

Many attempts have been made to derive elemental abundances of the lunar surface from mul-tispectral images (cf. e.g. [1]). The gamma ray spectrometer on board the Lunar Prospector spacecraft (LP GRS) provided the first "direct" global measurements of lunar elemental abun-dances including Fe, Th (15 km surface resolution), Ti, K, Sm (60 km), Al, O, Si, Mg, Ca, and U (150 km). In this study we rely on the elemental abundance estimation method intro-duced in [2], which is based on spectral features derived from the Clementine UVVIS+NIR data set and estimates the abundances of Ca, Al, Fe, Mg, Ti, and O by applying a second order polynomial regression model with the corresponding LP GRS abundances as "ground truth". The regarded spectral features are the continuum slope, the FWHM of the ferrous absorption trough near 1000 nm after continuum division, and the absorption wavelengths and relative absorption depths (cf. [2,3] for details). A petrographic analysis is performed based on the abundances of the key elements Al, Fe, and Mg [4]. The relative abundances of the endmem-bers mare basalt, Mg-rich rock, and ferroan anorthosite are estimated using Fe-Mg and Al-Mg diagrams, where the endmember compositions are determined based on the three-endmember plane fitted in Al-Fe-Mg space to the elemental abundances at 150 km resolution obtained with the regression model. The root-mean-square deviation from the three-endmember plane is only 0.3 wt percent. Our petrographic map shows Mg-rich rocks in the Mare Frigoris region, on the edges of large maria, in the South Pole Aitken basin, and in some cryptomaria such as the Schiller-Schickard basin. The presence of Mg-rich rocks in Mare Frigoris explains the Fe and Ti depletion discussed in [5]. Furthermore, our analysis confirms that the basalts of eastern mare Frigoris have an atypically high Al content [6]. The region south of Lichtenberg and around Seleucus and Briggs in northwestern Oceanus Procellarum is characterised by comparably large deviations from the three-endmember plane in Al-Fe-Mg space of 1 wt percent and more. These anomalous basalts have low ages of 1.7-2.8 Ga [7]. They are characterised by secondary absorption features near 1100 nm and high 2000/1500 spectral ratios, indicating a high olivine content. Anomalous material in lunar craters is generally interpreted as being excavated during crater formation from the lower lunar crust or upper mantle (cf. e.g. [8]). For the highland crater Tycho, our method reveals mafic units in the northern crater wall and in the central peaks and Mg-rich rock in the southwestern crater wall and distributed throughout the crater floor. This material is interpreted in [9] as anorthositic gabbro with a low Fe content and a mafic mineral assemblage dominated by high-Ca pyroxene. Our petrographic map of Copernicus shows the central peaks as small regions composed of the mare basalt endmember (interpreted as gabbroic material) with admixed troctolite (western peak) and mainly troctolite (eastern peak), respectively [8]. For the central peaks of the crater Bullialdus, our technique clearly reveals the Mg-rich rock component, which is interpreted as norite in [10]. We present very high resolution petrographic maps derived from newly released Selene multi-spectral data of the central peaks of Copernicus and Bullialdus. For the pyroclastic deposits (LPDs) on the floor of Alphonsus, our technique indicates high Mg/Al ratios between 1.4 (eastern LPDs) and 2.5 (western LPD) [11]. The secondary absorption near 1100 nm and the high 2000/1500 ratio suggest the presence of a major olivine component. As a general result, we show that our regression-based elemental abundance estimation method allows the detection of the main lunar terrain classes and rock types on small spatial scales based on multispectral imagery in the visible and near-infrared domain. [1] Lucey et al. (2000), JGR 105(E8), 20297-20306. [2] Wühler et al. (2009), EPSC 2009, 263. [3] Evans et al. (2009) LPSC XXXX, 1093. [4] Berezhnoy et al. (2005), PSS 53, 1097-1108. [5] Taylor et al. (1996), LPSC XXVII, 1317-1318. [6] Kramer et al. (2009), LPSC XXXX, 2369. [7] Hiesinger et al. (2003), JGR 108(E7), 5065-5091. [8] Pieters and Tompkins (1999), LPSC XXX, 1286. [9] Lucey et al. (2002), LPSC XXXIII, 1056. [10] Tompkins et al. (1994), Icarus 110(2), 261-274. [11] Schonfeld and Bielefeld (1978), LPSC V, 3037-3048.

Experimental evaluation of ALS point cloud ground extraction over different land cover in the Malopolska Province

NASA Astrophysics Data System (ADS)

Korzeniowska, Karolina; Mandlburger, Gottfried; Klimczyk, Agata

2013-04-01

The paper presents an evaluation of different terrain point extraction algorithms for Airborne Laser Scanning (ALS) point clouds. The research area covers eight test sites in the Małopolska Province (Poland) with varying point density between 3-15points/m² and surface as well as land cover characteristics. In this paper the existing implementations of algorithms were considered. Approaches based on mathematical morphology, progressive densification, robust surface interpolation and segmentation were compared. From the group of morphological filters, the Progressive Morphological Filter (PMF) proposed by Zhang K. et al. (2003) in LIS software was evaluated. From the progressive densification filter methods developed by Axelsson P. (2000) the Martin Isenburg's implementation in LAStools software (LAStools, 2012) was chosen. The third group of methods are surface-based filters. In this study, we used the hierarchic robust interpolation approach by Kraus K., Pfeifer N. (1998) as implemented in SCOP++ (Trimble, 2012). The fourth group of methods works on segmentation. From this filtering concept the segmentation algorithm available in LIS was tested (Wichmann V., 2012). The main aim in executing the automatic classification for ground extraction was operating in default mode or with default parameters which were selected by the developers of the algorithms. It was assumed that the default settings were equivalent to the parameters on which the best results can be achieved. In case it was not possible to apply an algorithm in default mode, a combination of the available and most crucial parameters for ground extraction were selected. As a result of these analyses, several output LAS files with different ground classification were achieved. The results were described on the basis of qualitative and quantitative analyses, both being in a formal description. The classification differences were verified on point cloud data. Qualitative verification of ground extraction was made on the basis of a visual inspection of the results (Sithole G., Vosselman G., 2004; Meng X. et al., 2010). The results of these analyses were described as a graph using weighted assumption. The quantitative analyses were evaluated on a basis of Type I, Type II and Total errors (Sithole G., Vosselman G., 2003). The achieved results show that the analysed algorithms yield different classification accuracies depending on the landscape and land cover. The simplest terrain for ground extraction was flat rural area with sparse vegetation. The most difficult were mountainous areas with very dense vegetation where only a few ground points were available. Generally the LAStools algorithm gives good results in every type of terrain, but the ground surface is too smooth. The LIS Progressive Morphological Filter algorithm gives good results in forested flat and low slope areas. The surface-based algorithm from SCOP++ gives good results in mountainous areas - both forested and built-up because it better preserves steep slopes, sharp ridges and breaklines, but sometimes it fails to remove off-terrain objects from the ground class. The segmentation-based algorithm in LIS gives quite good results in built-up flat areas, but in forested areas it does not work well. Bibliography: Axelsson, P., 2000. DEM generation from laser scanner data using adaptive TIN models. International Archives of the Photogrammetry, Remote Sensing and Spatial Information Sciences XXXIII (Pt. B4/1), 110- 117 Kraus, K., Pfeifer, N., 1998. Determination of terrain models in wooded areas with airborne laser scanner data. ISPRS Journal of Photogrammetry & Remote Sensing 53 (4), 193-203 LAStools website http://www.cs.unc.edu/~isenburg/lastools/ (verified in September 2012) Meng, X., Currit, N., Zhao, K., 2010. Ground Filtering Algorithms for Airborne LiDAR Data: A Review of Critical Issues. Remote Sensing 2, 833-860 Sithole, G., Vosselman, G., 2003. Report: ISPRS Comparison of Filters. Commission III, Working Group 3. Department of Geodesy, Faculty of Civil Engineering and Geosciences, Delft University of technology, The Netherlands Sithole, G., Vosselman, G., 2004. Experimental comparison of filter algorithms for bare-Earth extraction form airborne laser scanning point clouds. ISPRS Journal of Photogrammetry & Remote Sensing 59, 85-101 Trimble, 2012 http://www.trimble.com/geospatial/aerial-software.aspx (verified in November 2012) Wichmann, V., 2012. LIS Command Reference, LASERDATA GmbH, 1-231 Zhang, K., Chen, S.-C., Whitman, D., Shyu, M.-L., Yan, J., Zhang, C., 2003. A progressive morphological filter for removing non-ground measurements from airborne LIDAR data. IEEE Transactions on Geoscience and Remote Sensing, 41(4), 872-882

The Saturnian Moon Iapetus and the Cassini Targeted Flyby on September 10, 2007

NASA Astrophysics Data System (ADS)

Denk, T.; Roatsch, Th.; Giese, B.; Wagner, R.; Schmedemann, N.; Neukum, G.

2007-08-01

The ISS camera onboard the Cassini Spacecraft orbiting Saturn has observed the enigmatic moon Iapetus for over three years now, but always from great distance. The sofar closest approach occurred at New-Year's Eve 2005 when a range of 124000 km was achieved. Numerous discoveries have been made so far [e.g., 1,2,3]: The equatorial ridge on the leading and anti-Saturn side, a latitude dependence of the characteristics of the dark terrain, an unusually high number of giant impact basins, the latitudinal dependence of bright and dark crater rims, a global color dichotomy that shows different boundaries than the more obvious brightness dichotomy, the true (crater) nature of the "moat" feature, and so on. Earlier discoveries from Voyager data [4,5] such as the irregular boundary between the bright and the dark hemispheres, the giant bright mountains on the anti- and sub-Saturn side ("Voyager" mountains), the ellipsoidal shape of the whole moon, impact craters within the dark terrain, the reddish color of the dark terrain, etc., have been confirmed. Promising attempts were made to explain the formations of the brightness and color dichotomies [6,7] and the ellipsoidal shape [8]. Besides many unanswered questions, a major missing piece is a very close-up view on the surface. This is planned for the targeted flyby on Sept. 10, 2007. Our Cassini group at FU and DLR in Berlin has the responsibility for the imaging observation planning. The spacecraft will approach Iapetus over the mainly unlit, very-low albedo Saturnfacing hemisphere. Closest approach will occur at 1600 km altitude over the anti- Saturn side. This area is close to the (as far as we know) highest parts of the ridge. On the outbound trajectory, Cassini will look back on the as-yet only poorly imaged bright trailing side of Iapetus at low phase angle. A spacecraft trajectory tweak to significantly improve the observation conditions [9] was approved by the project in early 2007. There will be many scientific highlights during the flyby. A few examples are: Spatial resolution down to 10 m/pxl with the ISS narrow angle camera; ridge imaging at high and low phase angles; a large mosaic of the equatorial transition zone; global mapping of the trailing side at˜400 m/pxl; the only SAR observation of an icy satellite (RADAR); a star occultation to look for a tenuous atmosphere (UVIS); very highresolution thermal observations (CIRS); best-ever examination of outer-solar system dark material (VIMS); and much more. A small subset of questions that might be addressed with these data are: What is the geologic nature and origin of the ridge and the bright "Voyager" mountains? How far does the ridge extend into the trailing side? What is the thickness of the dark terrain blanket? Does it harbor small bright "holes" due to recent small impacts? What is the chemical and mineralogical nature of the dark material? How is the distribution of the dark material on the trailing side? What is the overall cause for the existence of the tremendous brightness dichotomy, the color dichotomy, the complex brightness patterns on the transition zones? References: [1] Porco, C.C., et al. (2005): Cassini Imaging Science: Initial Results on Phoebe and Iapetus. Science 307, 1237-1242. [2] Denk, T., et al. (2005): LPSC XXXVI, abstracts #2262 and #2268. [3] Giese et al. (2007): The Topography of Iapetus' Leading Side. Icarus, in press. [4] Morrison et al. (1986): The Satellites of Saturn. In: Satellites, UofA Press, 764-801. [5] Denk et al. (2000) LPSC XXXI, abstract #1596. [6] Spencer, J.R. et al. (2005), 37th DPS, abstract #39.08. [7] Denk et al. (2006) 38th DPS Conference, abstract #69.07. [8] Castillo-Rogez et al. (2007): Iapetus' Geophysics: Rotation Rate, Shape, and Equatorial Ridge. Icarus, doi:10.1016/j.icarus.2007.02.018. [9] Pelletier, F.J. (2006): Cassini Iapetus-1 Flyby Variations. JPL IOM-343J-06-049.

Periglacial landforms on Mars as evidence of undersurface ice

NASA Astrophysics Data System (ADS)

Sik, A.

1. Introduction By the methods of comparative planetology we can acquire new information not only from other planets, but from the Earth as well. The purpose of my research is to compare the periglacial environment of Mars and Earth, their forms and geomorphological processes. Hereby we might could refine our understanding of the paleoclimatic changes on these two planets, the history of near-surface water on Mars and the possibility of Martian life. I used the high resolution narrow angle images of Mars Global Surveyor's Mars Oriber Camera [1] to define landforms and the profiles of Mars Oriber Laser Altimeter [2] to characterize the relief on the examined terrains. Because of the "difficulties" of real field work on the surface of Mars, I obtained these kind of data during a periglacial research expedition of my university, carried out in the summer of 2000. 2. Short history of water on Mars After the formation of the planet, Mars had a stable and thick atmosphere, probably dominated by carbon-dioxide, water-vapour and nitrogen. So during the first part of its history, called "wet Mars period", planet Mars had active water-cycle and as a part of it, water-related erosion landforms had taken shape. This can be the explanation of the seashore-like, regionally identical altitude lines which separates different surface regions, the river channels and the inner crater pond sediments widely general on the surface. But as a result of more mechanisms, about 3,5 billion years ago this era ended. The main reasons probably were some giant impact events, produced a kind of atmospheric blow-off and resulted huge impact forms, like Hellas- and Argyre- basins. Another factor of it was the loss of global magnetic field, so the charged particles of solar wind was able to erode the outer part of the atmosphere. Besides, the low escape velocity caused by the small mass of the planet enabled gas molecules of the Martian atmosphere to leave for the interplanetary space. For all these reasons the quantity and pressure of the Martian atmosphere decreased, the previously generated green house effect became weaker and the surface temperature fallen down. From this time the volatiles frozen out and water was not stable on the surface in liquid form any more. So polar ice caps was formed and the pores in the thick regolith-mantle of the surface was filled with ice, resulting in a permafrost-like global cryosphere [3]. 3. Periglacial environment The periglacial regions most exactly can be defined by the temporary presence of ice under the surface. This often produce an ever-frozen, ice-saturated section of the ground, called permafrost, which is the reason of the most periglacial mechanisms and forms. The climate of these regions fluctuates round about 0°C in the year because it is needed to establish the conditions of ice-melting. The surface materials are also an important factor of the periglacial processes because most of these are related to rock debris covered surfaces. Well, it seems to be a complex environmental system and all these compounds are required to build- up a real periglacial landscape. These complex systems are very sensitive to the smallest environmental changes and because of their dynamic character (in comparison with other morpho-climatological regions) the reaction for any changing comes very quickly after that. In addition, if the observed terrain has significant relief, the mass movements are particularly important. 4. Rock glaciers on Earth As Earth-analogies, I collected data directly in two study area: 1) in a ruins of the former caldera of Erciyas Mountain in Anatolia, Turkey (38,5°N, 35,3°E) and 2) in a northwest-facing valley in Aladaglar Mountains of Anatolia, Turkey (37,7°N, 35°E). These locations are approximately 3100 m above sea level. The results of our expedition are high scale topographic and geomorphologic maps, microclimatic measurements and a huge number of photographs. At the first area there are some middle-sized rock glaciers formed from the gravitational talus regions of the inner walls of the caldera. The most typical form is a young and active, lobate-shaped rock glacier bordered by steep side- and front slopes and with well-defined transversal furrows-and-ridges pattern on its surface. The second location is more isolated, in the Pleistocene it was a cirque-region of a normal glacier. Recently there is only one rock glacier in the area, so that is very well bordered. The geomorpological map of this form shows curvilinear pattern, as a result of plastic deformation of inner ice lens. The lower end of this rock glacier has bigger units and deeper troughs between them. Perhaps it is resulted from changing active and less active periods of movement, in connection with temperature oscillations. 5. Debris aprons on Mars From Viking Orbiter images fretted terrains of Mars has known as high-relief transition zones between the young, northern low-lying plains and the old, southern highlands of the planet [4]. Here the isolated highland-mesas are surrounded by plastic, skirt-like forms of rock debris: these are called debris aprons. Their formation is supported by the global cryosphere. Other morphological evidences of this latitude-specific ice-rich layer are the rampart craters, relief relaxation phenomena, poligon-shaped surface matrix, thermokarst-like features and indirectly the formation of outflow channels [5]. These debris aprons can extend to 15-25 km long, they have a convex shape, steep frontal- and side slopes and they are differs from gravitational talus or fluvial aprons, respectively. The source of their rock debris is the intensive physical weathering, and their ice emanates from the underlying layers, from the mesa's material or condense from the atmosphere [6]. Primarily the ice content-related mass movement mechanisms (continuous creep and episodic sliding) are responsible for the plastic appearance of these forms [7]. The detailed analysis of three Martian debris aprons on MOC image M02-04416 and their corresponding MOLA profiles show morphological similarities to terrestrial rock glaciers. The source zone of the aprons seems like a gravitational talus formed on the weathering free rock face, with longitudinal lineaments on it. Downhill the surface of the aprons breaks up and changes from knobby to more disturbed character, furthermore tongue-shaped units can be separated, like girlands on Earth. In the middle part, where the plastic deformation causes the strongest extension, larger mass movements occur, with curvilinear fronts. 6. Conclusions On the basis of all the above mentioned things, truly the rock glaciers are the best terrestrial analogies of Martian periglacial debris aprons. They occur in similar environmental conditions, show analogous morphology and perhaps their movement mechanisms are the same as well. The most important difference is the temporal variety of the periglacial environments of Mars and Earth, because our planet is more dynamic. For this reason, the same mechanisms acting on the two planets can resulted in different landscape, considering the importance of time of form-evolution [8]. By Idrisi geoinformatic software I compared Martian images from the same location, which were taken minimum one Martian year time difference. There are only a few image-pair, but based on these no sign of seasonal changes can be found on the aprons. Nevertheless from longer period alteration no sure statement can be claimed, because the time expired since our first usable observations is very short. Though the detailed analysis of crater-density and crater erosion status provide more accurate time-information about the aprons, indicate that these are the relatively youngest landforms in their surface environment. 7. Implication of life on Mars If ice is present in the surface layers of Mars, it can be hopeful for the case of Martian life. Because the climate oscillation of the planet can cause warmer periods on short timescale when the partial melting of the ice content can not be ruled out and so a specially adapted organism can survive the frozen state in spore form and after revive in liquid water. If this conception is correct, recently Mars is in frozen state and we have to wait for the discovery of Martian life until a warmer period begin. 8. Proposal for future research We are planning to model these forms in the environment of our Hunveyor experimental space probe [9], but the best Earth-analogies (for its lithology, climate and orography as well) of these terrains are the McMurdo Dry Valleys of Antarctica [10]. So the new theories in connection with the topic of Martian periglacial environments should be tested there in the future. By doing so, and by a better understanding of correlation between morphology of terrestrial rock glaciers and climatic oscillation, we will able to refine our view of near-surface water-history and paleoclimate of Mars. References [1] www.msss.com; [2] lptwww.gsfc.nasa.gov/tharsis/mola.html; [3] Kereszturi, Á. and Sik, A. (2000) LPSC XXXI., #1216; [4] Squyres, S. W. et al. (1992) in Kieffer, H. H. et. al.: Mars, University of Arizona Press, Tucson, 523-554; [5] Carr, M. H. and Schaber, G. G. (1977) JGR, 82, 4039-4054; [6] Mangold, N. et. al. (2000) LPSC XXXI., #1131; [7] Vitek, J. D. (1987) in J. R. Giardino et. al.: Rock glaciers, Allen and Unwin, London, 239-264; [8] Humlum, O. (2000) Geomorphology, 35, 41-67; [9] Bérczi, Sz. et. al. (1999) LPSC XXX., #1332; [10] Nagy, B. and Szalai, Z.: Study of periglacial mass movements at King George Island (Southern Shetland Islands, Western Antarctica), Geographical Proceedings, in press.

Major water-related episodes on the lowlands of Mars

NASA Astrophysics Data System (ADS)

Fairén, A. G.; Dohm, J. M.; Baker, V. R.

2003-04-01

Throughout the recorded history of Mars, liquid water has distinctly shaped its landscape, including the prominent circum-Chryse and the northwestern slope valleys outflow channel systems (Dohm et al., 2001), and the extremely flat northern plains topography at the distal reaches of these outflow channel systems. Paleotopographic reconstructions of the Tharsis magmatic complex reveal the existence of an Europe-sized Noachian drainage basin and subsequent aquifer system in eastern Tharsis. This basin is proposed to source the magmatic-triggered outburst floods that sculpted the circum-Chryse and NSVs outflow channel systems (Dohm, et al., 2001), entrained boulders, rock, and sediment during passage, and ponded to form sequentially through time various hypothesized oceans, seas, and lakes in the northern plains (Parker et al., 1993; Baker et al., 1991; Scott et al., 1995; Head et al., 1999) and glaciers and rock glaciers and lacustrine environments such as in the southern hemisphere (Baker, 2001). The floodwaters decreased in volume with time due to inadequate groundwater recharge of the Tharsis aquifer system. Basing on the ideas of episodic greenhouse atmosphere and water stability on the lowlands of Mars (Baker et al., 1991), a conceptual scheme for water evolution and associated geomorphologic features on the northern plains can be proposed. This model highlights Tharsis-triggered flood inundations and their direct impact on shaping the northern plains, as well as making possible the existence of fossil and/or extant life. Martian topography, as observed from the Mars Orbiter Laser Altimeter, corresponds well to these ancient flood inundations, including the approximated shorelines that have been proposed for the northern plains (Parker et al., 1993). Stratigraphy, geomorphology, and topography record at least one great Noachian/early Hesperian northern plains ocean (Fairén and De Pablo, 2002), best portrayed by the martian dichotomy boundary or Contact 1, but in Arabia Terra, where the initial shoreline might have been as far south as Sinus Meridani (Edgett and Parker, 1997), forming an almost equipotential line (total elevation differences are ˜2 km) that we name Contact 0, which is also consistent with the location of the boundary in crustal thickness dichotomy, as deduced from topography and gravity data (Zuber et al., 2000), and with the locus of debouch of almost every valley network in Arabia (Edgett and Parker, 1997; Carr, 2002); a Late Hesperian sea, which would have extended over the deeper areas in the lowlands inset within the boundary of the first great ocean, and so portrayed by Contact 2; and a number of widely distributed minor lakes that may represent a reduced Late Hesperian sea, or ponded waters in the deepest reaches of the northern plains related to minor Tharsis (e.g., Anderson et al., 2001) and Elysium (Skinner and Tanaka, 2001) induced Amazonian flooding. Possible biologic evolution throughout the resulting different climatic and hydrologic conditions would account for very distinct metabolic pathways for hypothesized organisms capable of surviving and perhaps evolving in each aqueous environment, those that existed in the dry and cold periods between the flood inundations, and those organisms that could survive both extremes. Terrestrial microbiota, chemolithotrophic and heterotrophic bacteria, provide exciting analogues for such potential extremophile existence in Mars, especially where long-lived, magmatic-driven hydrothermal activity is indicated (Farmer and Des Marais, 1999). Such Martian environments and related materials and life forms may have been excavated to the surface by catastrophic outflows making targets readily available for sampling and in-deep analyses. References Anderson, R. C. et al.: Primary centers and secondary concentrations of tectonic activity through time in western hemisphere of Mars. J. Geophys. Res. 106, 20 563--20 585, 2001. Baker, V.R., et al.: Ancient oceans, ice sheets and the hydrological cycle on Mars. Nature, 352, 589--594, 1991. Baker, V. R.: Water and the martian landscape. Nature, 412, 228--236, 2001. Carr, M. H.: Elevations of water-worn features on Mars: Implications for circulation of groundwater, J. Geophys. Res., 107, 5131, doi:10.1029/2002JE001845, 2002. Dohm, J.M., et al.: Ancient drainage basin of the Tharsis region, Mars: Potential source for outflow channel systems and putative oceans or paleolakes. J. Geophys. Res., 106, 32 943--32 958, 2001. Edgett, K.S. and Parker, T.J.: Water on early Mars: Possible subaqueous sedimentary deposits covering ancient cratered terrain in western Arabia and Sinus Meridani. Geophys. Res. Lett., 24, 2897--2900, 1997. Farmer, J.D. and Des Marais, D.J.: Exploring for a record of ancient martian life. J. Geophys. Res., 104, 26 977--26 995, 1999. Fairén, A.G. and de Pablo, M.A.: An evolutionary timescale for the water on Mars. Lunar Planet. Sci. Conf., XXXIII, #1013 (abstract) [CD-ROM], 2002. Head, J.W., et al.: Possible ancient oceans on Mars: Evidence from Mars Orbiter laser altimeter data. Science, 286, 2134--2137, 1999. Parker, T.J., et al.: Coastal geomorphology of the Martian northern plains. J. Geophys. Res., 98, 11 061--11 078, 1993. Scott, D.H., et al.: Map of Mars showing channels and possible paleolake basins. U.S. Geol. Surv. Misc. Invest. Ser. MAP I-2461, 1995. Skinner, J.A. and Tanaka, K.L.: Long-lived hydrovolcanism of Elysium. Eos. Trans. AGU 82(47), Fall Meet. Suppl., Abstract P31B-07, 2001. Zuber, M. T., et al.: Internal structure and early thermal evolution of Mars from Mars Global Surveyor topography and gravity. Science, 287, 1788--1793, 2000.

Books Noted

NASA Astrophysics Data System (ADS)

Walsh, Edward J.

1999-10-01

The Colloidal Domain: Where Physics, Chemistry, Biology, and Technology Meet, 2nd edition

D. Fennell Evans and Hakan Wennerstroem. Advances in Interfacial Engineering Series. Wiley-VCH: New York, 1999. xl + 632 pp. ISBN 0-471-24247-0. 89.95.

Commercial Nuclear Power: Assuring Safety for the Future

Charles B. Ramsey and Mohammed Modarres. Wiley-Interscience: New York, 1998. xxviii + 508 pp. ISBN 0-471-29186-2. 79.95.

Advances in Medicinal Chemistry, Vol. 4

Bruce E. Maryanoff and Allen B. Reitz, Eds. JAI Press: Stamford, CT, 1999. ISBN 1-7623-0064-7. 109.50.

Advances in Strained and Interesting Organic Molecules, Vol. 7

Brian Halton, Ed. JAI Press: Stamford, CT, 1999. xii + 259 pp. ISBN 0-7623-0530-4. 109.50.

Advances in Electron Transfer Chemistry, Vol. 6

Patrick S. Mariano, Ed. JAI Press: Stamford, CT, 1999. x + 171 pp. ISBN 0-7623-0213-5. 109.50.

Automating Science and Engineering Laboratories with Visual Basic

Mark F. Russo and Martin M. Echols. Wiley-Interscience Series on Laboratory Automation. Wiley-Interscience: New York, 1999. xx + 355 pp. ISBN 0-471-25493-2. 49.95.

Plantwide Process Control

Kelvin T. Erickson and John L. Hedrick. Wiley Series in Chemical Engineering. Wiley-Interscience: New York, 1999. xii + 547 pp. ISBN 0-471-17835-7. 89.95.

Heme Peroxidases

H. Brian Dunford. Wiley-VCH: New York, 1999. xiii + 507 pp. ISBN 0-471-24244-6. 195.00.

Industrial Ecology: Environmental Chemistry and Hazardous Wastes

Stanley E. Manahan. Lewis: Boca Raton, FL, 1999. 318 pp. ISBN 1-56670-381-6. 69.95.

Reviews in Computational Chemistry, Vol. 13

Kenny B. Lipkowitz and Donald B. Boyd. Wiley-VCH: New York, 1999. xxxiii + 426 pp. ISBN 0-471-33135-x. 135.00.

Surfaces, Interfaces, and Colloids: Principles and Applications, 2nd edition

Drew Myers. Wiley-VCH: New York, 1999. xx + 501 pp. ISBN 0-471-33060-4. 94.95.

Onium Ions

George A. Olah, Kenneth K. Laali, Qi Wang, and G. K. Surya Prakash. Wiley-Interscience: New York, 1998. xv + 509 pp. ISBN 0-471-14877-6. 110.00.

Environmental Soil and Water Chemistry: Principles and Applications V. P. Evangelou. Wiley-Interscience: New York, 1998. xix + 564 pp. ISBN 0-471-16515-8. 79.95.

1001 Chemicals in Everyday Products, 2nd edition

Grace Ross Lewis. Wiley-Interscience: New York, 1999. x + 388 pp. ISBN 0-471-29212-5. 39.95.

Organic Coatings: Science and Technology, 2nd edition

Zeno W. Wicks Jr., Frank N. Jones, and S. Peter Pappas. Wiley-Interscience: New York, 1999. xxi + 630 pp. ISBN 0-471-24507-0. 125.00.

Progress in Inorganic Chemistry, Vol. 48

Kenneth D. Karlin, Ed. Wiley-Interscience: New York, 1999. vi + 603 pp. ISBN 0-471-32623-2. 145.00.

Occupational Biomechanics, 3rd edition

Don B. Chaffin, Gunnar B. Andersson, and Bernard J. Martin. Wiley-Interscience: New York, 1999. xvii + 579 pp. ISBN 0-471-24697-2. 69.95.

Advances in Photochemistry, Vol. 25

Douglas C. Neckers, David H. Volman, and Gunther Von Bünau. Wiley-Interscience: New York, 1999. xi + 238 pp. ISBN 0-471-32708-5. 110.00.

Distillation

Johann G. Stichlmair and James R. Fair. Wiley-VCH: New York, 1998. xiii + 524 pp. ISBN 0-471-25241-7. 94.95.

Ammonia - Principles and Industrial Practice

Maz Appl. Wiley-VCH: New York, 1999. ix + 301 pp. ISBN 3-527-29593-3. 160.00.

Precursor-Derived Ceramics: Synthesis, Structure, and High-Temperature Mechanical Properties

Fritz Aldinger, Fumihiro Wakai, and Joachim Bill, Eds. Wiley-VCH: New York, 1999. xv + 298 pp. ISBN 3-527-29814-2. 180.00.

Advances in Sonochemisty, Vol. 5

Timothy J. Mason. JAI Press: Stamford, CT, 1999. xi + 311 pp. ISBN 0-7623-0331-x. 109.50.

Fluid Metals: The Liquid-Vapor Transition of Metals

Friedrich Hensel and William W. Warren Jr. Princeton University Press: Princeton, NJ. 1999. xvii + 243 pp. ISBN 0-691-05830-x. 69.50.

Direct Phasing in Crystallography: Fundamentals and Applications

Carmelo Giacovazzo. Oxford University Press: New York, 1999. xxiii + 767 pp. ISBN 0-19-850072-6. 140.00.

Practical Environmental Analysis

M. Radojevic and V. N. Bashkin. Royal Society of Chemistry: Cambridge, UK. 1999. xx + 466 pp. ISBN 0-85404-594-5. £32.00.

Advances in Dendritic Macromolecules, Vol. 4 George R. Newkome, Ed. JAI Press: Stamford, CT, 1999. x + 207 pp. ISBN 0-7623-0347-6. 109.50.

Advances in Quantitative Structure-Property Relationships, Vol. 2

Marvin Charton. JAI Press: Stamford, CT, 1999. ix + 257 pp. ISBN 0-7623-0067-1. 109.50.

Pesticide Residues in Foods: Methods, Techniques, and Regulations

W. George Fong, H. Anson Moye, James N. Seiber, and John P. Toth. Chemical Analysis, Vol. 151.Wiley-Interscience: New York, 1999. xiv + 358 pp. ISBN 0-471-57400-7. $84.95.

Cycles of edifice growth and destruction at Tharsis Tholus, Mars

NASA Astrophysics Data System (ADS)

Platz, T.; McGuire, P. C.; Münn, S.; Cailleau, B.; Dumke, A.; Neukum, G.; Procter, J. N.

2009-04-01

Tharsis Tholus, approx. 800 km to the ENE of Ascraeus Mons, is unique among Martian volcanoes as it is structurally divided into sectors suggesting a complex volcano-tectonic evolution [1-3]. The objective of this study was 1) to identify cycles of edifice growth and destruction and causes of instability, 2) to estimate the mineralogical composition of rocks and loose deposits, 3) to provide a time frame of volcanic activity, and 4) to characterize eruptive styles at Tharsis Tholus. The edifice has a planar extension of 155 km (NW-SE) by 125 km (NE-SW) with an elevation up to 9000 m on the west flank. The volcano exhibits a strong relief and can be subdivided into five major sectors: north flank, west flank, east flank, south flank, and the central caldera. The slopes vary from <1° up to 27°. The volcano is partly buried by lava flows, presumably originating from the Tharsis Montes. As a result, the original basement surface is unknown. However, to the east of the volcano, the tips of a large buried impact-crater rim are still preserved. Using the approximate extension of 41×47 km of the impact-crater rim, a rim height of about 500 m results [4], with the basement being at 500 m altitude. The visible edifice volume is approximately 31.1×10³ km³, however, if a basal horizontal plane at 500 m is assumed, an edifice volume of >50×10³ km³ results. The structure of the edifice indicates at least four large deformation events. The central and most prominent structure of the volcano is its central caldera. It is bordered by a well-preserved system of concentric normal faults. The maximum subsidence of the caldera floor is 3000 m; the collapse volume is calculated at approx. 2160 km³. The caldera (36.7×38.9 km) has an elliptic shape oriented NW-SE. The flanks of the volcano are characterized by four large scarps oriented radially from the central caldera. The arcuate shapes of the scarps and their orientations suggest voluminous collapses of the western and eastern volcano flanks. On the southern flank, a further caldera structure is displayed by an arcuate scarp and a plateau-like plain. Due to a large impact event, most of the caldera structure is now concealed. Large parts of the volcano are cut by parallel normal faults forming grabens. These grabens post-date the large collapse structures at the volcano's flanks. All graben structures are oriented in the NE-SW direction. Minimum and maximum graben widths are 0.47 km and 4.36 km, respectively. Multiple areas of volcanic activity at Tharsis Tholus were identified: 1) flank eruptions associated with graben formation, 2) fissure eruptions, and 3) a satellite vent at the foot of the west flank forming a strato-cone. This satellite volcano has a nearly perfect conical shape and rises 1168 m above the surrounding lava plain. The visible volume is about 5.7 km³. There are currently no indications for volcanic activity prior to or after the formation of the central caldera. First results of crater counting indicate that the oldest parts of the edifice were constructed at around 3.82 Ga (late Noachian). The west flank appears to be ca. 3.73 Ga old whereas the east flank shows an age of ca. 1.08 Ga (Middle Amazonian). A fissure eruption on the south flank produced a lava flow at around 196 Ma (Late Amazonian). The existence of two main loci of activity, the central caldera and the subordinate southern caldera, indicate a multipart magma storage system. Changes in lava rheology are observed (shield volcano vs. strato-cone), which indicates magma differentiation within the plumbing system of the volcano during phases of activity. The lifetime of the volcano spans more than 3.6 Gyrs starting prior to 3.82 Ga. Hence, the fissure eruption at around 196 Ma may not represent the final volcanic activity at Tharsis Tholus. Scarps on the western and eastern flanks are interpreted to be structurally related to at least two large sector collapses. Their arcuate shape can be fitted by ellipses suggesting more or less sub-vertical caldera-like collapses, with the major portion of the upper flanks collapsing into the centre of the volcano and minor portions of the lower flanks collapsing laterally forming debris avalanches. Graben formations across the edifice reflect a regional-tectonic deformation superimposed on the local volcano-tectonic pattern of Tharsis Tholus. The least compressive stress of this regional stress field is oriented NW-SE which agrees with the direction of ellipticity of the central caldera and fitted ellipses to the flank scarps. The geometry of the central caldera indicates a shallow magma storage region, probably at the base of the volcano. References: [1] F. Maciejak et al. 1995. LPS XXVI, 881-882. [2] J. B. Plescia 2001. LPS XXXII, 1090-1091. [3] J. B. Plescia 2003. Icarus, 165, 223-241. [4] D. H. Scott and K. L. Tanaka 1986. US Geol. Survey. Miscellaneous Investigations Map I-1802A.

The Age of the Medusae Fossae Formation

NASA Astrophysics Data System (ADS)

Kerber, L.; Head, J. W.

2008-09-01

Introduction The Medusae Fossae Formation (MFF) is a complicated and discontinuous formation located in the southern parts of Elysium Planitia and Amazonis Planitia (130°-230°E and 12°S-12°N), covering an area of approximately 2.1 x 106 km2 and having an estimated volume of 1.4 x 106 km3 [1]. It is thought to have been deposited during the Amazonian period [2,3]. However, much of the cratering record may have been erased as friable units were eroded and long-buried terrains exhumed [4-6]. The formation is characterized by large accumulations of fine-grained, friable deposits and evidence of large amounts of erosion. There are many theories regarding the emplacement of this formation; recently the literature has focused on three possibilities: ignimbrites, ash fall, and aeolian dust. Some modified and inverted fluvial channels have been found within the deposit [7,8], (Fig. 1), indicating that there was some fluvial activity during or after the emplacement of the MFF. If the MFF is among the youngest surficial deposits on Mars [9], it is implied that meandering, channelized flow must have extended into the Amazonian, a significant constraint when considering the atmospheric evolution of the planet through time. Because of the wide implications that these findings have for the evolution of Mars and the Martian atmosphere, it is instructive to re-examine the evidence for the Amazonian age of the MFF. The initial conclusion comes from two main arguments: the relatively few superposed craters on the unit, and the superposition of the MFF on young lowland lava deposits [1, 9]. Using new high resolution data, we reexamine the relationships both within the MFF and with respect to adjacent units. Cratering Record The cratering record of the MFF and other easily eroded units has often been deemed unreliable [4, 10, 12], but it continues to be cited as evidence for the formation's young age. Throughout the MFF, pedestal craters, inverted craters, and remnant knobs can be found which trace the progression of crater erosion and suggest that a large number of craters originally superposed on the unit have been erased or degraded beyond recognition (Fig. 2). Stratigraphy Because lava units are emplaced in a geologically short period of time, cease to evolve after emplacement, and are relatively resistant to erosion, they are useful age markers for adjacent units such as the MFF which are more difficult to date. Early descriptions noted that lowland lava flows embay the formation in places [12], but later works have placed the MFF at the top of the stratigraphic column because it overlies lowland lavas [9]. We have observed that Cerberus lavas embay the formation in Northern Aeolis Planum and Zephyria Planum, though eroded Medusae Fossae Formation has been blown out onto the lava where it collects as sand dunes. In other places direct contacts are lacking, but ancient contacts may be recognized where lava units embayed the MFF after which the MFF was eroded from these areas, leaving irregular depressions and negative yardang patterns in the embaying lava units (Fig. 3). These boundaries are found in most places where there is a contact with a lava unit, including northwestern Aeolis Planum, north and east of Eumenides Dorsum, and in north-eastern Gordii Dorsum. In between Eumenides Dorsum and Amazonis Planum, several lobes of lava from Arsia Mons, mapped as Late Hesperian/Early Amazonian (AHt3) by [2], end abruptly in a negative yardang pattern, in close proximity to an eroding patch of MFF. Additionally, the large fan on the southeastern flank of Apollinaris Patera appears to embay the MFF yardangs at its base (Fig. 4). Discussion The Medusae Fossae Formation is a mobile unit which both erases craters on its own surface as well as sheltering nearby units from incoming projectiles, resulting in a misleadingly young age. The MFF appears to continuously erode into yardangs and reaccumulate as dunes and massive deposits. If it comes to a rest, the unconsolidated material gradually becomes indurated (perhaps through compression or interaction with the atmosphere) until it reaches a point where it can begin eroding into yardangs again. Lava flows, which remain relatively stable through time, make useful chronological markers for where the unit is and where it used to be. Recognition of remnant contacts between MFF and lava units is helpful in unravelling relationships between the MFF and lava units where direct contacts are not available. Lava unit contacts suggest that parts of the MFF may be older than previously hypothesized, perhaps Hesperian. This conclusion is consistent with the presence of fluvial channels within the deposit and relaxes the time constraint on its emplacement. References [1] Bradley, B.A. and Sakimoto, S.E.H. (2002) JGR, 107, E8. [2] Scott, D.H. and Tanaka, K.L. (1986) USGS Misc. Invest. Ser. Map I-1802-A. [3] Greeley, R. and Guest, J. (1987) USGS Misc. Inv. Series Map I-1802-B. [4] Schultz, P.H. and Lutz, A.B. (1988) Icarus 73, 91-141 [5] Schultz, P.H. (2006) Plan. Chron. Workshop, Abs. 6024. [6] Schultz, P.H. (2007) Science 318, 1080-1081. [7] Zimbelman, J.R. (2000) GSA Abs. Prog., 32(7), A303. [8] Edgett K.S. and Williams R.M.E. (2006) LPSC XXXVI, Abs. 1099. [9] Bradley, B.A. and Sakimoto, S.E.H. (2001) LPSC XXXII, Abs. 1335. [10] Tanaka, K.L. (2000) Icarus 144(2), 254-266. [11] Greeley et al. (2001) Space Sci. Rev. 96(1-4), 393-404. [12] Scott, D.H. and Tanaka, K.L. (1982) JGR 87(B2), 1179-1190.

Morphology of cone-fields in SW Elysium Planitia - Traces of hydrothermal venting on Mars?

NASA Astrophysics Data System (ADS)

Lanz, J. K.; Saric, M. B.

2008-09-01

Introduction Small cone-shaped features with summit pits can be found in several regions on Mars; mainly in Isidis Planitia; Elysium Planitia; Amazonis Planitia; Acidalia Planitia; in the Cydonia Region; in Cerberus Planum; the Phlegra Montes and on several volcanic flanks. They vary greatly in size and morphology and have been compared to terrestrial features of various origins; namely (1) cinder cones (e.g. [1]), (2) tuff cones or tuff rings (e.g. [2]), (3) rootless cones (pseudocraters) (e.g. [3], [4]), (4) pingos (e.g. [5], [6]) and (5) mud volcanoes (e.g. [7]). They are often found near volcanic centers and large lava fields or cluster in regions where the volatile content of the Martian regolith was/is supposedly high. This has led to the assumption that (ground-) water or ground ice was a trigger or driving force of cone formation. They could therefore, be an important indicator of the history of water on the planet. We have studied an area in western Elysium Planitia, bordering the Aeolis Planum plateau, which exhibits a large number of pitted cones, ridges and dome-like structures. Their distribution and morphology differs strongly from pitted cones elsewhere in Elysium Planitia, which have mainly been interpreted as hydrovolcanic rootless cones, and from other regions on Mars. Based on our observations, we present an alternative model for cone formation in the study area that might hint towards hydrothermal processes in the Aeolis Planum region and possibly young igneous activity. Aeolis Planum Cones The Aeolis Planum pitted cones (referred to as APCs from now on) cluster along the southern edges of the broad shallow valley that borders the Aeolis Planum Formation (APF) to the north. Cones along the northern edges of the valley are rare and can only be found in association with APF remnants where they strongly resemble the cones in the south. Along the southern border the cone coverage is almost continuous, describing a narrow band approximately 2 to 3 km wide. There are distinct morphological changes both within the band from north to south and along the band from east to west (Fig. 2). The cones are mostly circular but elongated, irregular forms are common. They are of varying size with basal diameters ranging from 20 to 200 meters, though most (single) cones have basal diameters below 100 meters. The heights of the cones are difficult to determine as their sizes are far below the resolution limits of either MOLA or HRSC stereo data, yet photoclinometric calculations have given approximate heights between ~ 10 up to several dozens of meters. Often the cones show hardly any elevation above the surroundings (e.g. Fig. 2c, e or f). Most of the APCs have steep convex flanks and large summit pits with diameters at least half as wide as their bases. The overall morphology of the cones changes from S to N with distance from the APF and from E to W along the edges of the APF. Toward the south, close to the strongly eroded borders of the APF, broad ridges and elongated domes are dominant. They form a narrow band approximately 2 km wide. The ridges and domes are a few dozen to several hundred meters long and between 10 to 50 meters wide and show numerous cracks and fissures. They are often topped by small cones, elongated pits and remnants of APF sediments. Further north follows a rather abrupt transition from the ridged area to more cone-dominated regions. Here single cones are prevalent with a more random distribution. Their number decreases rapidly with increasing distance from the APF and approximately 3 km off the southern edge of the APF no further cones are found. Hydrothermal venting on Mars? Morphology and stratigraphic relationships indicate that the cones are young and that they have, at least in places, developed inside the APF complex. APF remnants can be found covering the central pits of cones and APF units have been tilted and eroded by coneforming processes. Furthermore, cones are mainly found inside a narrow band 2-3 km wide along the APF-lava contact. A connection between APF-lava interaction and cone-forming processes is therefore likely. We propose that a combination of contact metamorphosis and associated hydrothermal venting comparable to hydrothermal vent complexes on Earth could have been the driving force of cone-formation in the study area based on the assumption of a high volatile content of the APF. The processes might then have proceeded as follows: Phase 1: The flooding of the study area by lava caused initial explosive reactions along the lava-APF-boundary forming clusters of pseudocraters. Pseudocraters are only visible towards the edges of the depression where the lava cover is thinnest. Towards the center the thick lava coverage prevented pseudocrater formation or quickly reburied forming cones. Phase 2: The heat of the cooling lava, which could be as thick as 500 m based on the diameters of flooded craters, causes contact metamorphosis and the mobilization of volatiles in the surrounding APF-sediments. Similar to hydrothermal vent complexes on Earth, this may have caused hydrofracturing of the sediments and the formation of sediment pipes and dikes that transport the volatiles to the surface. Pre-existing fissures would have served as additional pathways. At the surface rapid decompression causes phreatic explosions and the formation of small cones. Phase 3: Close to the lava-body mobilization of volatiles (e.g. by dehydratation of hydrated minerals, mobilization of ground- or pore ice or even juvenile waters and other volatiles from the lava itself) was strongest. In combination with lower sediment thickness and shorter pathways to the surface, phreatic explosion were more violent and conduits may have been repeatedly active. The lower atmospheric pressure and lower gravity on Mars would have further enhanced the explosive activity. While the lower gravity leads to a faster ascent of the volatile-sediment-phase, thereby preventing early degassing, the lower atmospheric pressure causes stronger decompression and expansion of gases. With increasing distance and increasing APF-thickness the surface manifestation of the processes weakens and phreatic explosive activity decreases. The cracked domes and elongated ridges may then be the surface expression of sediment pipes and dikes that have cooled and degassed before reaching the surface. The flow structures surrounding many cones and ridges could be interpreted in this context as fluidized sediment as lava would not have been discharged from the vents. This kind of sediment volcanism took place after the erosion of the APF and marks the end of the hydrothermal activity. Phase 4: Erosion of the APF, enhanced by the cone-forming processes themselves, later exhumed deeper parts of the vents and the brecciated sediment cores, leaving remnants of APF sediments in central pits and on top of cones, ridges and domes. References: [1] Plescia J. B. (1980) NASA Tech. Memo., 82385, 263-265. [2] Bridges J. C. et al. (2003) JGR, 180(E1), 5001, doi:10.1029/2001JE001820. [3] Fagents S. A. (2002) LPSC XXXIII, Abstract #1594. [4] Bruno B. C. (2004) JGR, 109, doi:1029/2004JE002273. [5] Theilig E. and Greeley R. (1979) J. Geophys. Res., 84, 7994-8010. [6] Page and Murray (2006) Icarus, 183, 46-54. [7] Skinner J. A. and Tanaka K. L. (2006) Icarus, 186, 41-59. [7] Watters T. R. et al. (2007) Sciencexpress, science. 1148112, 10.1126.

Astrobiology - The New Synthesis

NASA Astrophysics Data System (ADS)

Sik, A.; Simon, T.

Background In connection with the complex planetology-education in Hungary [1] we have compiled an Astrobiology coursebook - as a base of its teaching in universities and perhaps in secondary schools as well. We tried to collect and assemble in a logical and thematical order the scientific breakthroughs of the last years, that made possible the fast improvement of astrobiology. The followings are a kind of summary of these. Introduction - The ultimate science Astrobiology is a young science, that search for the possibility, forms and places of extraterrestrial life. But it is not SETI, because do not search for intelligent life, just for living organisms, so SETI is a part of astrobiology. and an extremely important statement: we can search for life-forms that similar to terrestrial life in physiology so we can recognize it as life. Astrobiology is one of the most dynamical-developing sciences of the 21st century. To determine its boundaries is difficult because the complex nature of it: astrobiology melt into itself lot of other sciences, like a kind of ultimate science. The fundamental questions are very simple [2]: When, where and how converted the organic matter into life?; How does life evolve in the Universe?; Has it appeared on other planets?; How does it spread in time and space?; and What is the future of terrestrial life? However, trying to find the answers is quite difficult. So an astrobiologist has to be aware of the basics of astronomy, space research, earth and planetary sciences, and life sciences (mainly ecology, genetics, molecular and evolution biology). But it is not enough - the newest results of these at least as important as the basic knowledge. Part I. - Astro 1. Exoplanets 1995 was a particular year in astronomy: we have found the first planet out of the Solar System. Since that time the discovery of exoplanets progress fast: nowdays more than 80 examples are known and just 6 years passed [3]. The detailed analysis of these distant objects has verified and solidified our theo- ries of planet-formation. The places of this process are contacting clouds of gas and dust, like the Orion Nebula. In these star-birth clouds we can observe clusters of mat- ter in which the temperature and pressure reach a limit and a new-born star begin to "function", or rather radiate. Around the star, the remnant matter settle into a plane, 1 forming a protoplanetary disk. It has different zones: heavy elements nearer to the star, light elements farther from it. The planets are taking shape from these zones - perhaps rocky types and gas giants as well. To see so much example we can state that planetary system-formation is an absolutely normal, everyday process in the Universe. As a consequence there are a lot of planetary system near to our Earth, with planets orbiting around stars. Though, the known exoplanets are not too Earth-like objects. Most of them seems to be lonely gas giants (with mass bigger than our Jupiter) nearer to their star then rocky planets to our Sun (the only known multiple exoplanet sys- tem is around Upsilon Andromedae [4]). Probable the reason of this difference is the weak capability of our instrument and not the speciality of our system. By using ad- vanced methods and instruments (like Next Generation Space Telescope or Terrestrial Planet Finder spacecraft, planned to launch in 5 years [5]) rocky-like planets will be found as well. 2. Water in the Solar System Looking closer, the knowledge of our Solar System has increased intensively during the last years of the 20th century - due to the planetary spacecraft missions, like Lunar Prospector, Mars Pathfinder, Mars Global Surveyor, Galileo and NEAR-Shoemaker. The most important discovery, that liquid water is quite general in our local cosmic environment. and as we know this is the most important condition of life. First and foremost, the most important is Planet Mars. By reconstructing the surface evolution of our outer neighbor it seems that in the past, more billion years ago it had global ocean, the depressions were filled with seas and lakes and rivers had carved channel-systems. Though in the present the sur- face dry and cold, the pressure is very low so H2O is stable only in ice or gas form [6]. A significant amount of water had been blown off or escaped, the remnant of the ancient water-reserve is freezed out at the poles or into the megaregolith's pores, re- spectively [7]. Well, it is possible that life began on the red planet in the past and after these dramatical ecological changes became extinct. Or it might survived and exists today but we were unable to find it. If this is the case, 2004 is the next time, when 3 lander (and 2 orbiter) arrives to Planet Mars, searching for the sings of life. An other hopeful object is Europa, moon of Jupiter. Based on its drifting ice-like surface mor- phology and the electromagnetic measurements of Galileo spacecraft it is accepted that under the icy crust there is a water-ocean (or at least a slushy layer of H2O). and other Galilei-moons, Ganymedes and Callisto seems to have similar inner structure as well. So the Europa Orbiter will be an exciting mission, planned within 10 years [8]. Saturn's moon Titan is also an interesting target. It is the only moon with signifi- cant atmosphere, mainly composed from nitrogen and a small amount of methane [9]. This reductive conditions are similar to the young Earth's ecology where life had be- gan approximately 3,8 billion years ago. We will know more about this environment in 2004, when the Cassini-Huygens spacecraft will arrive to Saturn and the Huygens probe will land on Titan's surface [10]. Water can be found in the icy cores of comets 2 as well. Sometimes they called dirty snowballs because of their material and structure. Besides the matter of comets is very ancient because they were created few after the birth of the Solar System and a comet's core did not take part in any planet-forming process. Finally, complex organic molecules have been found in the interstellar mat- ter, signing that chemical evolution can start without solid surface. So the first steps of the path leading to life perhaps can be done in the space as well. 3. Meteorites from Mars Back to Planet Mars, the most popular topic of astrobiology was the ALH84001 Martian meteorite in the past five years. Since 1996, when researchers announced that they found sings of ancient, primitive, microbiological Martian life in a meteorite here on Earth, intensive research has started and arguments has arisen for and against it as well [11]. But the final word will be said not earlier than 2004, after the arrival of the new spacecrafts to Planet Mars. (An interesting relation of this discovery is with panspermia-theory. Its essence that life, for example in the form of bacterium- spores, can travel between planets, so bring life from one to an other. So the findings in ALH84001 can be the evidence of this theory which can have important influence on the origin of terrestrial and/or Martian life [12].) Part II. - Bio 1. The champions of bearing: extremophile organisms The other parts of recent breakthroughs in astrobiology come not from space but from the Earth it- self. Terrestrial life namely proves more persistent, flexible and adaptable than previ- ously thought. Places that were considered unbearable for life some years ago recently known as home of a diverse ecosystem - mainly primitive, bacterial life forms. The organisms, that prefer the extreme ecological conditions of these niches called ex- tremophiles. These life forms can be found in thermal springs, hydrothermal vents and black smokers, in the water of isolated lakes under polar ice sheets, in the frozen soils of permafrost terrains, in chemically special places and - most surprisingly - they flourish in rocks as well, deep below the surface. However some extremophile species have known for more then 50 years, the list of them longer and longer from year to year. They research intensified for more reason: by analyzing their biochemistry and genetics we can get closer the understanding of formation and early evolution of life; their special enzymes ("extremozymes") have more and more significant scien- tific and industrial applications [13]; and terrestrial extremophile-analogies can help to understand the possible extreme ecosystems of other planets or moons. Most of the extremophiles are bacteria (eubacteria and archaea-bacteria as well) but in some extreme ecosystems eukaryotes also can be found. The base of their classification is the environmental factor that is tolerated extremely. - Thermophiles and hyperther- mophiles: the best known group and probably the most important in the understand- ing of life. Mainly prokaryotes that tolerate temperatures higher than 45C (if this is higher than 80C, the organism is hyperthermophile). The first species with higher optimum than 70C, Thermus aquaticus, an eubacterium was found in the thermal 3 springs of Yellowstone National Park (DNA polymerase enzyme was produced from it, which has revolutionized many aspects of genetics through the Polymerase Chain Reaction). However the first hyperthermophile was an archaea-bacteria (Sulfolobus acidocaldarius). After 1970 a lot of other species was found near to black smokers, so today approximately 50 hyperthermophiles are known. The record is 121C (Pyrod- ictium occultum) and the upper limit of tolerable temperature-range is not uncertain, 150C is the estimated value. - Psychrofiles: they can live in the polar ice layers, in glacier-ice and in permafrost soils also. - Acidophiles: pH-tolerance between value 5-2, lot of them are hyperthermophiles as well and lives in black smokers. The most ancient genome sequences are from these organisms signing that the first terrestrial organisms were acidophiles- hyperthermophiles. - Alkaliphiles: life functions above 9 pH value, general in soda-lakes. Together with the acidophiles they way of life is not to let acids and alkalis into their cells. - Halophiles: these species are identified from salt lakes, salt mines and salt crystals (some of these are 250 million years old). The salt concentration of their cytoplasm is extreme high so the outer salt can not enter. 2. Extremophiles and evolution Jelentősek az extremofilek evolúciós evolution as- pects vonatkozásai, mivel igen sok ősbaktériumot archaea találunk közöttük. A hagyományos nézet, mely szerint az élővilág a baktériumok bacteria és eukar- ióták eukaryotes birodalmára osztható, a 70-es évek végén (Woese et al), 80-as évek elején (Fox et al) ingott meg, amikor a 16S rRNS (az élővilág egyik legkonz- ervatívabb molekuláris szerkezete molecular structure) összehasonlító szekvenciav- izsgálatai comparative sequence analysis alapján kiderült: az ősbaktériumok különválasztása a legmagasabb rendszertani taxonomy level szinten is indokolt, tehát külön birodalmat separate domain képeznek. Az eddigi genomtérképezések genome sequencing során kiderült, hogy az ősbaktériumok egyes génjei csak eukar- iótákban találhatók meg, nagyobb részük pedig teljesen egyedi [14]. Újabb elméletek szerint az eubaktériumok és ősbaktériumok közös őstől származ- nak, az eukarióták pedig az ősbaktériumokból fejlődhettek ki [15]. Az ősbaktériumok az egyetemes őshöz (LUCA - "last universal common ancestor") legközelebb álló élő kövületek living fossils lehetnek. Luca: az RNS-világ RNS world, a ribo-organizmusok ribo organisms utáni első orga- nizmus, amelyben már kialakult a fehérjék proteins és a DNS DNS mai szerepe. Az ősbaktériumok tanulmányozásával tehát a közel 4 milliárd évvel ezelőtti földi körülményekre következtethetünk. Az utóbbi években a földkéregben felfedezett gazdag extremofil-társulások alapján megdőlni látszik az a hagyományos nézet, mely szerint Luca egy meleg felszíni pocsolyában tenyészett, s divatossá vált sötétebb helyekre való költöztetése: mélyen a föld alá helyezik, a forró vulkáni kőzetek hasadékaiba, ahol bőségesen találhatott magának ként, vasat, hidrogént és szenet. A genetikai bizonyítékok alapján a hő- és mélységkedvelők es- 4 nek legközelebb az egyetemes őshöz. [16]. The synthesis Mindezek alapján a földi extremofilek vizsgálata során deríthetjük ki, hogy más égitesteken (egyelőre a Naprendszerben) hol kell keresnünk az életet, és mit kell keresnünk a planetológiai kutatások során egyre jobban megismert szélsőséges környezetekben. Segítségükkel megtudhatjuk, melyek azok az alak- tani, geokémiai, esetleg biokémiai jegyek, amelyek életre utalhatnak; melyek az élet azon alapvető jellemzői, amelyek elég általánosak és biztonsággal kimu- tathatók, milyen műszerekkel kell felszerelnünk a jövő űrszondáit, milyen módszereket kell alkalmaznunk, hogy sikerrel kutathassunk a Földön kívüli élet után. References [1] H. Hargitai et. al., XXXIII. LPSC (2002), Houston, #1261; [2] Origins Roadmap, 2000, JPL; [3] http://www.obspm.fr/encycl/catalog.html [4] http://www.physics.sfsu.edu/~gmarcy/planetsearch/ upsand/upsand.html [5] http://tpf.jpl.nasa.gov/ [6] A. Kereszturi, and A. Sik, XXXI. LPSC (2000), Houston, #1216; [7] S. W. Squyres et. al. (1992) in H. H. Kieffer, et. al.: Mars, University of Arizona Press, Tucson, 523-554; [8] http://www.jpl.nasa.gov/europaorbiter/ [9] www.nineplanets.org [10] http://www.jpl.nasa.gov/cassini/ [11] http://www- curator.jsc.nasa.gov/curator/antmet/ marsmets/alh84001/sample.htm [12] P. Davies: The fifth miracle - The search for the origin of life (1998), Orion; [13] M. T. Madigan and B. L. Marrs: Extremophiles, Scientific American (1997), 276, 82-87; [14] J. A. Lake et al.: Methanococcus Genome, Science (1996), 274, 901-905; [15] N. C. Kyrpides and G. J. Olsen: Archaeal and bacterial hyperthermophiles: Horizontal gene exchange or common ancestry?, Trends in Genetics (1999), 15, 298-299; [16] Takai, K. and K. Horikoshi. 1999. Genetic diversity of archaea in deep-sea hydrothermal vent environments. Genetics 152:1285-1297. 5

X-ray Fluorescence Observations of the Moon by SMART-1/D-CIXS

NASA Astrophysics Data System (ADS)

Grande, Manuel; Swinyard, B.; Joy, K. H.; Kellett, Barry J.; Crawford, Ian A.; Howe, Chris J.

2008-09-01

Introduction The SMART-1 mission to the Moon included in its payload D-CIXS, a compact X-ray spectrometer [1], [2] SMART-1 was a technology evaluation mission, and D-CIXS was the first of a new generation of planetary X-ray spectrometers. Novel technologies enabled new capabilities for measuring the fluorescent yield of a planetary surface or atmosphere which is illuminated by solar X-rays. During the extended SMART-1 cruise phase, observations of the Earth showed strong argon emission, providing a good source for calibration and demonstrating the potential of the technique. At the Moon, observations showed a first unambiguous remote sensing of calcium in the lunar regolith (Grande et al 2007) (Fig 1). Data obtained were broadly consistent with current understanding of mare and highland composition. Ground truth was provided by the returned Apollo and Luna sample sets. We have extended our observations to comparisons of Lunar near and farside, and by careful analysis enabled new elemental lines to be observed. Observations: In March, 2005, the SMART-1 spacecraft reached its nominal lunar orbit, and we began full commissioning for lunar operations. During the pre-commissioning period in mid-January, 2005, observations of the lunar surface were made which coincided with the occurrence of several major M and X class flares. This opportunity provided an excellent chance to observe spatially localized fluorescence from the lunar surface. X-ray fluorescent elemental lines from the lunar surface are detected by all three facets of D-CIXS while the XSM instrument observes the input solar spectrum. At the end of this interval, a long duration M-class solar flare began at 06:00 UTC on the 15th of January, 2005. The flare lasted for more than 1 hour but only ~30 minutes corresponded to D-CIXS observations. At this time SMART-1 was orbiting over the Moon's near-side eastern limb from about the equator, traveling northwards. As SMART-1 flew north, its altitude was also increasing from around 2100 km at 06:00 to ~3100 km at 06:35. Due to the nature of SMART-1's orbit and thermal dynamics, the spacecraft was performing a mid-orbit slew (rotation), and so D-CIXS's three facets had different surface ground tracks during the observation of interest. However, this variability in footprints was very fortuitous as the instrument FOVs included areas of both mare basalt and highland lithologies, which have different and recognizable elemental signatures. Facet 1 (thin Al-filter, 12º FOV) was oriented throughout the observation toward highland areas to the northeast of Mare Crisium. Facet 3 (Mg-filter, 12º FOV) had a ground track that crossed Mare Crisium. Due to the 12º FOV and the 2100 km altitude, the facet 3 footprint always contains a mixture of mare and highland regions. The footprint of facet 2 (thin Alfilter, 8º FOV) encompassed the regions between the two facets shown and covered a mixture of mare and highland regions but with a smaller signal due to its narrower FOV. Fig. 1 shows the particle background corrected spectra from summed data of the 3 D-CIXS facets for the interval 06:00 UTC to 06:35 UTC. Separate facet spectra have been derived by co-adding data from detectors. Essentially, elemental lines seen in the three different facet spectra represent an averaged geochemical signature from the areas covered by the D-CIXS ground tracks. The spectra shown in figure 5 indicate that lowenergy lines (Mg: 1.25 keV, Al; 1.49 keV and Si: 1.74 keV) are observed in detectors from Facet 1 and 2 (Alfilter). Detectors in Facet 3 are covered by a Magnesium filter which was designed to attenuate the signal from Al and Si X-rays, and so in the Facet 3 spectrum Mg is the only significant low-energy peak detected. Data taken from the Facet 3 spectrum also show a clear Fe peak at around 6.4 keV which is interpreted to be related to fluorescence from Mare Crisium (see below). All three facets clearly show the detection of a Ca emission peak at ~3.69 keV. Although inferences about the distribution of Ca in the lunar crust have been made indirectly from neutron and gamma ray measurements [3], this observation represents the first ever unambiguous remote sensing of Ca on the Moon. Discussion: The areas of the lunar surface observed during the flare of January 15 include Mare Crisium, and highlands to the north and east. The basaltic lavas of Mare Crisium, which appear dark in, are iron-rich owing to high modal abundances of mafic minerals (principally pyroxene). In contrast, the adjacent highlands are expected to be anorthositic (i.e., composed largely of the mineral plagioclase), and thus iron poor but relatively enriched in calcium and aluminium. Some `ground truth' is provided by samples collected at the Luna 20 and 24 landing sites, both of which were located within the footprint of facet 3 during these observations . Remote sensing by Clementine [4] and Lunar Prospector [5] suggests that the Soviet Luna 24 and Luna 20 iron abundances are reasonably representative of the Mare Crisium basalts, and the adjacent highlands, respectively. These remote sensing data also suggest that the highlands north and east of Crisium, are more anorthositic (i.e. poorer in Fe and richer in Ca) than those immediately adjacent to the Crisium basin and which were sampled by Luna 20. These expectations are confirmed by the D-CIXS data shown in Figure 1, when facet 3 was over the centre of Crisium and facet 1 was observing the highlands approximately 900 km to the north (material apparently similar to that of the highlands of the Luna 20 landing site). As expected, the Fe flux is strongly enhanced over Crisium, while Ca is somewhat enhanced over the highlands. Moreover, although there is strictly no ground truth available for the facet 1 footprint, the greater variability of Fe relative to Ca between mare and highland regions apparent in Fig. 6 is explicable in terms of the Luna 20 and 24 results presented in Table 2: while Fe is almost three times as abundant in the Crisium basalts than in the adjacent highlands, the Ca abundance is only some 20% less. Essentially the same trend is obtained by comparing the Fe and Ca Lunar Prospector data [3], which imply a factor of 2 difference in Fe, but less than a 10% difference in Ca, between these two footprints. Figure 2 shows a comparison of a spectrum obtained close to the Apollo 12 site, with a modelled spectrum, derived from averaged Apollo 12 soil compositions [6]. The match between data (black line) and model (grey) is reasonable, with the exception of the low energy continuum, where the model clearly needs refinement. We have extended our observations to comparison of Lunar near and farside, and by careful analysis enabled new elemental lines to be observed (Swinyard et al 2008)[8]. Conclusions: The instrument demonstrates the capability of this method to perform X-ray fluorescence measurements of the Moon. A number of rock forming elements have been successfully detected from the Moon during solar flare events, and we have made the first unambiguous remote detection of Calcium from the lunar surface. For more detail see Grande et al 2007 [7].All of this has been achieved during solar minimum and proves that the technique will be highly suitable for the upcoming Chandrayaan- 1 mission [9]), when the mission will take place during the rising phase of the solar cycle, and for which it forms part of the core payload. Acknowledgements We acknowledge the contributions of the entire DCIXS team (M. Grande, J. Huovelin, B. Kellett, R Browning, C. Howe, B. Swinyard, C. H. Perry, S. Dunkin, N. Waltham, B. Kent, D. Parker, I. Crawford, K. Joy, J. Guest, S. Russell, M. Grady, A. Christou, H. Alleyne, D. Hughes, C. D. Murray, S. Maurice C. L. Duston , O. Gasnaut, N. Bhandari, R. Lundin, S. Barabash, D Lawrence, V. Fernandes, I. Casanova, M. Kato, T. Okada, P. Clark, B. Foing, D. Heather, M. Wieczorek). We acknowledge the SMART-1 teams from ESA/ESTEC project, industrial teams, STOC Science and Technology Operations Centre and ESOC spacecraft operations, SMART-1 Science and Technology Working Team. The D-CIXS instrument development was supported with SMART-1 funding from ESA Science and Technology Research Programmes, and funding sources (BNSC, RAL, PPARC/STFC). Additional hardware was provided by CESR, Toulouse, University of Helsinki observatory and IRF Kiruna, Sweden. References [1] Grande, (2001) Earth Moon And Planets, Vol 85-6, pp 143-152). [2] Grande et al., (2003), Planet. & Sp. Sci., 51 (6), 427. [3] Prettyman et al, 33rd LPS XXXIII #2012. [4] Bussey & Spudis (2000), JGR- Planets, 105, 4235- 4243. [5] Lawrence et al (2002) JGRPlanets, 107, (#E12), 5130, 10.1029/2001JE001530, 2002. [6] Haskin and Warren. 1991. The Lunar Sourcebook. Eds. Heiken [7] Grande et al (2007), in press Planet. & Sp. Sci 2006 [8] Swinyard et al 2008 submitted Science [9] Grande et al., (2008), Submitted Planet. & Sp. Sci.,

A report on the Unified Lunar Control Network 2005 and lunar topographic model

NASA Astrophysics Data System (ADS)

Archinal, B.; Rosiek, M.; Kirk, R.; Redding, B.

Introduction: We have finished a new general unified lunar control network and lunar topographic model based on Clementine images. This photogrammetric network solution is the largest planetary control network ever completed. It includes the determination of the 3-D positions of 272,931 points on the lunar surface and the correction of the camera angles for 43,866 Clementine images, using 546,126 tie point measurements. The solution RMS is 20 µm (= 0.9 pixels) in the image plane, with the largest residual of 6.4 pixels. We are now documenting our solution [1] and plan to release the solution results soon [2]. Previous Networks: In recent years there have been two generally accepted lunar control networks. These are the Unified Lunar Control Network (ULCN) and the Clementine Lunar Control Network (CLCN), both derived by M. Davies and T. Colvin at RAND. The original ULCN was described in the last major publication about a lunar control network [3]. Images for this network are from the Apollo, Mariner 10, and Galileo missions, and Earth-based photographs. The CLCN was derived from Clementine images and measurements on Clementine 750-nm images. The purpose of this network was to determine the geometry for the Clementine Base Map [4]. The geometry of that mosaic was used to produce the Clementine UVVIS digital image model [5] and the Near-Infrared Global Multispectral Map of the Moon from Clementine [6]. Through the extensive use of these products, they and the underlying CLCN in effect define the generally accepted current coordinate system for reporting and describing the location of lunar features. The CLCN is described in print only briefly [7]. See [8] for ULCN and CLCN files. Our efforts have merged these two networks into an improved ULCN. ULCN 2005 Features: The primary difference between our new network and the previous ones is that we solve for the radii of the control points. This avoids distortion of horizontal positions (of about 7 km average, and up to 15 km or more [9-11]) present in the CLCN primarily due to its points being constrained to the surface of a sphere of radius 1736.7 km. This is possible since the overlapping Clementine images provide stereo information. The expected precision of such information is on the order of several hundred m, but these data appear to be compatible with Clementine LIDAR ([12], previously the most accurate elevation data); the mean absolute difference between 1 the our values and a reference surface derived from the LIDAR values is 137 m with a standard deviation of 219 m. This shows that radii are being recovered at that level or better. Thus, a by-product of this network is a global lunar topographic model that is denser than that provided by LIDAR and of similar accuracy, and denser than any other lunar topography information except that provided in limited areas ([10, 13-15]). This radius information is also defined in a consistent, full, absolute, 3D system. This is the only lunar topographic model positioning where both heights and horizontal positions are estimated in a globally-consistent system. A second significant feature of the ULCN 2005 is that we have constrained the camera angles to their values as measured during the mission, supposedly with an accuracy of 0.03o [16]. We have used a constraint of 1o , with angles that show changes of more than 0.6o allowed to change freely, on the assumption they are from angle measurement blunders (a few angles change by up to ˜25o , probably due to unaccounted for spacecraft operations). We believe this provides significant improvement in the horizontal accuracy of the network (and therefore improves the vertical accuracy, which is coupled), because from an average altitude of 640 km, the implied horizontal position accuracy due to this 0.03o a priori information is 335 m. Since 99% of the angles change less than 0.45o , this and the 640 km altitude would also imply that even if the a priori angles were perfect, the 3σ horizontal error introduced by our solution is 5.1 km. This also assumes that the spacecraft positions - which we do not adjust - are perfectly accurate. Obviously this is not the case, but the cited errors [17] in the orbit positions (at least radially) are ˜100 m, which when RSS added to the pointing errors, would still cause a maximum of a few hundred m additional errors. A third feature is that we identified a majority of the original ULCN points on Clementine images and included measurements of them in the new ULCN 2005. 1261 points are measured, with 754 of them having two or more measurements. This therefore allows for the direct incorporation of the ULCN into the new ULCN 2005. We have done so by weighting the ULCN points appropriately (0.18-5 km horizontally, 2-6 km vertically) for the accuracies as described in [3]. 124 ULCN points, which had particularly high residuals, were interpreted as misidentified points or points where the original ULCN was in error and weighted the same as non-ULCN points (2° and 10 km, effectively free). This tie to the ULCN and the use of Clementine a priori spacecraft data in the mean Earth/polar axis system also places our solution in the same system (see [3]). Future Work: We now plan to finish the analysis of our ULCN 2005 solution, publish a paper describing it, and release the solution data on the web ([8]). Although difficult, given the lack of any higher accuracy data, we will attempt to quantify the horizontal 2 and vertical accuracy of this network. We will provide the topographic information in various formats, and also provide information for converting CLCN coordinates and CLCN registered images to the new system. The Lunar Orbiter digital mosaics now being generated [18] will also be registered to this system. Finally, we plan to continue to improve this network by the addition of the direct use of Mariner 10, Galileo, and Lunar Orbiter image measurements, and Clementine stereo [10]. We will also add ties to the current absolute LLR and ALSEP network [19]. It will be essential to further update and improve this network with data from future missions. This is necessary so that these new datasets can be compared to the prior data, particularly the Lunar Orbiter and Clementine multispectral products. References: [1] Archinal, B. A., et al. (2006). In preparation. [2] Archinal, B. A, et al. (2006). USGS Open File Report. In preparation. [3] Davies, M. E. et al. (1994) JGR, 99, E11, 23,211-23,214. [4] USGS (1997) Clementine Basemap Mosaic, USA_NASA_PDS_CL_30xx, NASA PDS. [5] USGS (1999) Clementine UVVIS Mosaic, USA_NASA_PDS_CL_40xx, NASA PDS. Eliason, E. M. et al. (1999), LPS XXX, Abstract #1933. [6] USGS, in publication. Eliason, E. (2003), LPS XXXIV, Abstract #2093. [7] Edwards, et al. (1996), LPS XXVII, 335-336. [8] http://astrogeology.usgs.gov/Projects/ControlNetworks/. [9] Malin, M. and M. Ravine (1998), Clementine High Resolution Camera Mosaicking Project, TR, Malin Space Science Systems San Diego. [10] Cook, A. C. et al. (2000), JGR, 105, E5, 12,023-12,033. [11] Cook, A. C. et al. (2002), AGU Fall Meeting, Abstract #P22D- 09. [12] Smith, D. E. et al. (1997), JGR, 102, E1, 1591-1611. [13] Rosiek, M. R. et al. (1998), LPS XXX, Abstract #1853. Rosiek, M. R., and Aeschliman, R. A. (2001) LPS XXXII, Abstract #1943. Rosiek, M. R. et al. (2001), Planetary Mapping 2001, ISPRS WG IV/9, http://astrogeology.usgs.gov/Projects/ISPRS/MEETINGS/. [14] Margot, J-L. C. (1999), PhD Thesis, Cornell University. [15] Wu, S. S. C. and Doyle, F. J. (1990), in Planetary Mapping, R. Greeley and R.M. Batson, eds., CUP, 169-207. [16] Nozette, S., et al. (1994), Science, 266, 1835-1839. [17] Zuber, M. T., et al. (1994) Science, 266, 1839-1843. [18] Weller, L., et al. (2006), LPS XXXVII, Abstract #2143. Also http://astrogeology.usgs.gov/Projects/LunarOrbiterDigitization/. [19] Davies, M. E. and Colvin, T. R. (2000), JGR, 105, E8, 20,277-20,280. 3