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Sample records for grb follow-up observations

  1. Prompt GRB optical follow-up experiments

    SciTech Connect

    Park, H-S; Williams, G; Ables, E; Band, D; Barthelmy, S; Bionta, R; Cline, T; Gehrels, N; Hartmann, D; Hurley, K; Kippen, M; Nemiroff, R; Pereira, W; Porrata, R

    2000-11-13

    Gamma Ray Bursts (GRBs) are brief, randomly located, releases of gamma-ray energy from unknown celestial sources that occur almost daily. The study of GRBs has undergone a revolution in the past three years due to an international effort of follow-up observations of coordinates provided by Beppo/SAX and IPN GRB. These follow-up observations have shown that GRBs are at cosmological distances and interact with surrounding material as described by the fireball model. However, prompt optical counterparts have only been seen in one case and are therefore very rare or much dimmer than the sensitivity of the current instruments. Unlike later time afterglows, prompt optical measurements would provide information on the GRB progenitor. LOTIS is the very first automated and dedicated telescope system that actively utilizes the GRB Coordinates Network (GCN) and it attempts to measure simultaneous optical light curve associated with GRBs. After 3 years of running, LOTIS has responded to 75 GRB triggers. The lack of any optical signal in any of the LOTIS images places numerical limits on the surrounding matter density, and other physical parameters in the environment of the GRB progenitor. This paper presents LOTIS results and describes other prompt GRB follow-up experiments including the Super-LOTIS at Kitt Peak in Arizona.

  2. Radio and Optical Follow-Up Observations and Improved IPN Position of GRB 970111

    NASA Technical Reports Server (NTRS)

    Galama, T. J.; Groot, P. J.; Strom, R. G.; vanParadijs, J.; Hurley, K.; Kouveliotou, C.; Fishman, G. J.; Meegan, C. A.; Heise, J.; intZand, J. J. M.

    1997-01-01

    We report on Westerbork 840 MHz, 1.4 and 5 GHz radio observations of the improved IPN-WFC error box of the gamma ray burst GRB 970111, between 26.4 hours and 120 days after the event onset. In the approximately 16 sq arcmin area defined by the IPN (BATSE and Ulysses) annulus and the published refined BeppoSAX Wide Field Camera (WFC) error box we detected no steady sources brighter than 0.56 mJy (4sigma), and no varying radio emission, down to 1.0 mJy (4sigma). We also report on B, V, R and I band observations of the error box with the 4.2 m William Herschel Telescope at La Palma. Subject headings: gamma rays: bursts - gamma rays: individual (GRB 9701 1 1)

  3. Exploring the first stars with rapid GRB follow-up observations

    NASA Astrophysics Data System (ADS)

    Cucchiara, Antonino; Cenko, Stephen; Schmidt, Brian; Perley, Daniel; Berger, Edo; Fox, Derek; Fruchter, Andrew; Bloom, Joshua; Prochaska, Jason X.; Lopez, Sebastian; Cobb, Bethany; Roth, Kathy; Levan, Andrew; Tanvir, Nial; Rapoport, Sharon; Yuan, Fang; Chornock, Ryan; Wen-Fai, Fong; Morgan, Adam; Wiersema, Klaas

    2013-02-01

    GRBs provide a unique window on exotic, highly relativistic physics. Our discovery of cosmic explosions like GRB090423 at z=8.2, breaking the record for the most distant known object, also demonstrates the power of using GRBs as lighthouses visible into the epoch of re-ionization, pinpointing the earliest stars and galaxies. Therefore, we intend (i) to observe GRBs at very high-z, in order to explore the IGM during reionization and place fundamental constraints on the early epochs of star-formation; (ii) to study in detail the class of short-duration bursts, especially their electromagnetic signatures in relation to gravitational-wave sources; (iii) to observe exceptionally energetic bursts, such as detected by the Fermi-LAT satellite in order to test theories of quantum gravity; (iv) continue our quest for low-z GRBs associated with supernovae, which, in conjunction with a larger sample of GRB afterglow spectra will provide unique insights into the stellar progenitors and explosion sites of these intriguing phenomena. Gemini, with its flexible schedule and instrumentation suite, represents a cornerstone facility of global GRB research and we will continue to use it in combination with a large network of other facilities.

  4. Rapid UBVRI Follow-up of the Highly Collimated Optical Afterglow of GRB 010222

    NASA Astrophysics Data System (ADS)

    Stanek, Krzysztof Z.; Garnavich, Peter M.; Jha, Saurabh; Kilgard, Roy E.; McDowell, Jonathan C.; Bersier, David; Challis, Peter M.; Falco, Emilio; Quinn, Jason L.

    2001-12-01

    We present the earliest optical observations of the optical counterpart to the gamma-ray burst (GRB) 010222, obtained with the Fred L. Whipple Observatory 1.2 m telescope in UBVRI passbands, starting 3.64 hr after the burst (0.4 hr after public notification of the burst localization). We also present late R-band observations of the afterglow obtained with the 1.8 m Vatican Advanced Technology Telescope ~25 days after the burst. The temporal analysis of our data joined with published data indicates a steepening decay, independent of wavelength, asymptotically approaching Fν~t-0.80+/-0.05 at early times (t<<1 day) and Fν~t-1.30+/-0.05 at late times, with a sharp break at tb=0.72+/-0.10 days. This is the second earliest observed break of any afterglow (after GRB 980519), which clearly indicates the importance of rapid multiband follow-up for GRB afterglow research. The optical spectral energy distribution, corrected for small Galactic reddening, can be fitted fairly well by a single power law with Fν~ν-1.07+/-0.09. However, when we fit using our BVRI data only, we obtain a shallower slope of -0.88+/-0.10, in excellent agreement with the slope derived from our low-resolution spectrum (-0.89+/-0.03). The spectral slope and light-curve decay slopes we derive are not consistent with a jet model despite the presence of a temporal break. Significant host dust extinction with a starburst reddening law would flatten the spectral index to match jet predictions and still be consistent with the observed spectral energy distribution. We derive an opening angle of 2.1d, smaller than any listed in the recent compilation of Frail et al. The total beamed energy corrected for the jet geometry is 4×1050 ergs, very close to the ``standard'' value of 5×1050 ergs found by Frail et al. for a number of other bursts with light-curve breaks. Based on observations collected at the FLWO 1.2 m telescope and the 1.8 m VATT.

  5. Six years of GRB follow up with MITSuME Okayama Telescope

    SciTech Connect

    Yanagisawa, Kenshi; Kuroda, Daisuke; Shimizu, Yasuhiro; Nagayama, Shogo; Toda, Hiroyuki; Yoshida, Michitoshi; Ohta, Kouji; Kawai, Nobuyuki

    2010-10-15

    MITSuME Okayama Telescope is an autonomous telescope with a diameter of 50 cm dedicated primarily to follow-up {gamma}-ray bursts. The telescope has successfully been in operation since 2004. We have made 131 observations of {gamma}-ray bursts and submitted 47 reports to GCN circulars. In this article, we present an overview of the instrumentation and scientific results obtained so far.

  6. The Discovery and Broadband Follow-Up of the Transient Afterglow of GRB 980703

    NASA Technical Reports Server (NTRS)

    Bloom, J. S.; Frail, D. A.; Kulkarni, S. R.; Djorgovski, S. G.; Halpern, J. P.; Marzke, R. O.; Patton, D. R.; Oke, J. B.; Horne, K. D.; Gomer, R.; Goodrich, R.; Campbell, R.; Moriarity-Schieven, G. H.; Redman, R. O.; Feldman, P. A.; Costa, E.; Masetti, N.

    1998-01-01

    We report on the discovery of the radio, infrared, and optical transient coincident with an X-ray transient proposed to be the afterglow of GRB 980703. At later times when the transient has faded below detection, we see an underlying galaxy with R = 22.6; this galaxy is the brightest host galaxy (by nearly 2 mag) of any cosmological gamma-ray burst (GRB) thus far. In keeping with an established trend, the GRB is not significantly offset from the host galaxy. Interpreting the multiwavelength data in the framework of the popular fireball model requires that the synchrotron cooling break was between the optical and X-ray bands on 1998 July 8.5 UT and that the intrinsic extinction of the transient is A(sub v) = 0.9. This is somewhat higher than the extinction for the galaxy as a whole, as estimated from spectroscopy.

  7. Goddard Robotic Telescope - Optical Follow-up of GRBs and Coordinated Observations of AGNs

    NASA Technical Reports Server (NTRS)

    Sakamoto, T.; Wallace, C. A.; Donato, D.; Gehrels, N.; Okajima, T.; Ukwatta, T. N.

    2010-01-01

    Since it is not possible to predict when a Gamma-Ray Burst (GRB) will occur or when Active Galactic Nucleus (AGN) flaring activity starts, follow-up/monitoring ground telescopes must be located as uniformly as possible all over the world in order to collect data simultaneously with Fermi and Swift detections. However, there is a distinct gap in follow-up coverage of telescopes in the eastern U.S. region based on the operations of Swift. Motivated by this fact, we have constructed a 14" fully automated optical robotic telescope, Goddard Robotic Telescope (GRT), at the Goddard Geophysical and Astronomical Observatory. The aims of our robotic telescope are 1) to follow-up Swift/Fermi GRBs and 2) to perform the coordinated optical observations of Fermi Large Area Telescope (LAT) AGN. Our telescope system consists of off-the-shelf hardware. With the focal reducer, we are able to match the field of view of Swift narrow instruments (20' x 20'). We started scientific observations in mid-November 2008 and GRT has been fully remotely operated since August 2009. The 3(sigma) upper limit in a 30-second exposure in the R filter is approx.15.4 mag; however, we can reach to approx.18 mag in a 600-second exposures. Due to the weather condition at the telescope site. our observing efficiency is 30-40%, on average.

  8. Afterglow Population Studies from Swift Follow-Up Observations of Fermi LAT GRBs

    NASA Technical Reports Server (NTRS)

    Racusin, Judith L.; Oates, S. R.; McEnery, J.; Vasileiou, V.; Troja, E.; Gehrels, N.

    2010-01-01

    The small population of Fermi LAT detected GRBs discovered over the last year has been providing interesting and unexpected clues into GRB prompt and afterglow emission mechanisms. Over the last 5 years, it has been Swift that has provided the robust data set of UV/optical and X-ray afterglow observations that opened many windows into other components of GRB emission structure. We explore the new ability to utilize both of these observatories to study the same GRBs over 10 orders of magnitude in energy, although not always concurrently. Almost all LAT GRBs that have been followed-up by Swift within 1-day have been clearly detected and carefully observed. We will present the context of the lower-energy afterglows of this special subset of GRBs that has > 100 MeV emission compared to the hundreds in the Swift database that may or may not have been observed by LAT, and theorize upon the relationship between these properties and the origin of the high energy gamma-ray emission.

  9. Prompt, early and afterglow optical observations of five γ-ray bursts: GRB 100901A, GRB 100902A, GRB 100905A, GRB 100906A and GRB 101020A

    NASA Astrophysics Data System (ADS)

    Gorbovskoy, E. S.; Lipunova, G. V.; Lipunov, V. M.; Kornilov, V. G.; Belinski, A. A.; Shatskiy, N. I.; Tyurina, N. V.; Kuvshinov, D. A.; Balanutsa, P. V.; Chazov, V. V.; Kuznetsov, A.; Zimnukhov, D. S.; Kornilov, M. V.; Sankovich, A. V.; Krylov, A.; Ivanov, K. I.; Chvalaev, O.; Poleschuk, V. A.; Konstantinov, E. N.; Gress, O. A.; Yazev, S. A.; Budnev, N. M.; Krushinski, V. V.; Zalozhnich, I. S.; Popov, A. A.; Tlatov, A. G.; Parhomenko, A. V.; Dormidontov, D. V.; Senik, V.; Yurkov, V. V.; Sergienko, Yu. P.; Varda, D.; Kudelina, I. P.; Castro-Tirado, A. J.; Gorosabel, J.; Sánchez-Ramírez, R.; Jelinek, M.; Tello, J. C.

    2012-04-01

    We present the results of the prompt, early and afterglow optical observations of five γ-ray bursts (GRBs): GRB 100901A, GRB 100902A, GRB 100905A, GRB 100906A and GRB 101020A. These observations were made with the Mobile Astronomical System of TElescope-Robots in Russia (MASTER-II Net), the 1.5-m telescope of the Sierra Nevada Observatory and the 2.56-m Nordic Optical Telescope. For two sources, GRB 100901A and GRB 100906A, we detected optical counterparts and obtained light curves starting before the cessation of γ-ray emission, at 113 and 48 s after the trigger, respectively. Observations of GRB 100906A were conducted in two polarizing filters. Observations of the other three bursts gave the upper limits on the optical flux; their properties are briefly discussed. A more detailed analysis of GRB 100901A and GRB 100906A, supplemented by Swift data, provides the following results and indicates different origins for the prompt optical radiation in the two bursts. The light-curve patterns and spectral distributions suggest that there is a common production site for the prompt optical and high-energy emission in GRB 100901A. The results of the spectral fits for GRB 100901A in the range from optical to X-ray favour power-law energy distributions and a consistent value of the optical extinction in the host galaxy. GRB 100906A produced a smoothly peaking optical light curve, suggesting that the prompt optical radiation in this GRB originated in a front shock. This is supported by a spectral analysis. We have found that the Amati and Ghirlanda relations are satisfied for GRB 100906A. We obtain an upper limit on the value of the optical extinction on the host of GRB 100906A.

  10. Status of the BOOTES-IR Project at OSN for GRB near-IR follow-up

    NASA Astrophysics Data System (ADS)

    Cunniffe, R.; Castro-Tirado, A. J.; Jelínek, M.; Gorosabel, J.; Moliné, B.; García-Segura, F.

    2013-07-01

    Bootes-IR (Castro-Tiradoet al. 2005) is a robotic observatory based around a 60 cm alt-az telescope (dubbed T60) that can slew rapidly while carrying heavy instrumentation at the Nasmyth foci. Initially commissioned with an optical camera, with which the optical afterglow to GRB 060707 (http://gcn.gsfc.nasa.gov/gcn3/5290.gcn3) was discovered, we have concentrated our efforts on the near-IR (0.8-2.5 μm) camera (BIRCAM) for which the telescope was specifically designed. The telescope is installed at the Observatorio de Sierra Nevada near Granada in Spain, at an altitude of 3000 m and in an area of very low humidity. The telescope, dome, camera and liquid nitrogen generation and refilling systems have all been recently brought back into operation, and routine observations are expected to begin within the next few months.

  11. High Resolution Active Optics Observations from the Kepler Follow-up Observation Program

    NASA Astrophysics Data System (ADS)

    Gautier, Thomas N.; Ciardi, D. R.; Marcy, G. W.; Hirsch, L.

    2014-01-01

    The ground based follow-up observation program for candidate exoplanets discovered with the Kepler observatory has supported a major effort for high resolution imaging of candidate host stars using adaptive optics wave-front correction (AO), speckle imaging and lucky imaging. These images allow examination of the sky as close as a few tenths of an arcsecond from the host stars to detect background objects that might be the source of the Kepler transit signal instead of the host star. This poster reports on the imaging done with AO cameras on the Keck, Palomar 5m and Shane 3m (Lick Observatory) which have been used to obtain high resolution images of over 500 Kepler Object of Interest (KOI) exoplanet candidate host stars. All observations were made at near infrared wavelengths in the J, H and K bands, mostly using the host target star as the AO guide star. Details of the sensitivity to background objects actually attained by these observations and the number of background objects discovered are presented. Implications to the false positive rate of the Kepler candidates are discussed.

  12. Follow-up after acute poisoning by substances of abuse: a prospective observational cohort study

    PubMed Central

    Vallersnes, Odd Martin; Jacobsen, Dag; Ekeberg, Øivind; Brekke, Mette

    2016-01-01

    Objective To chart follow-up of patients after acute poisoning by substances of abuse, register whether patients referred to specialist health services attended, and whether patients contacted a general practitioner (GP) after the poisoning episode. Design Observational cohort study. Setting A primary care emergency outpatient clinic in Oslo, Norway. Subjects Patients ≥12 years treated for acute poisoning by substances of abuse were included consecutively from October 2011 to September 2012. Main outcome measures Follow-up initiated at discharge, proportion of cases in which referred patients attended within three months, and proportion of cases in which the patient consulted a GP the first month following discharge. Results There were 2343 episodes of acute poisoning by substances of abuse. In 391 (17%) cases the patient was hospitalised, including 49 (2%) in psychiatric wards. In 235 (10%) cases the patient was referred to specialist health services, in 91 (4%) advised to see their GP, in 82 (3%) to contact social services, in 74 (3%) allotted place in a homeless shelter, and in 93 (4%) other follow-up was initiated. In 1096 (47%) cases, the patient was discharged without follow-up, and in a further 324 (14%), the patient self-discharged. When referred to specialist health services, in 200/235 (85%) cases the patient attended within three months. Among all discharges, in 527/1952 (27%) cases the patient consulted a GP within one month. When advised to see their GP, in 45/91 (49%) cases the patient did. Conclusion Attendance was high for follow-up initiated after acute poisoning by substances of abuse. Key Points Despite poor long-term prognosis, patients treated for acute poisoning by substances of abuse are frequently not referred to follow-up.Nearly all patients referred to specialist health services attended, indicating the acute poisoning as an opportune moment for intervention.Advising patients to contact their GP was significantly associated with

  13. SWIFT FOLLOW-UP OBSERVATIONS OF CANDIDATE GRAVITATIONAL-WAVE TRANSIENT EVENTS

    SciTech Connect

    Evans, P. A.; Osborne, J. P.; Beardmore, A.; Fridriksson, J. K.; Homan, J.; Gehrels, N.; Siegel, M.; Gelbord, J.; Kennea, J. A.; Smith, M.; Zhu, Q.; Handbauer, P.; Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M.; Accadia, T.; Collaboration: LIGO Scientific Collaboration and Virgo Collaboration; and others

    2012-12-15

    We present the first multi-wavelength follow-up observations of two candidate gravitational-wave (GW) transient events recorded by LIGO and Virgo in their 2009-2010 science run. The events were selected with low latency by the network of GW detectors (within less than 10 minutes) and their candidate sky locations were observed by the Swift observatory (within 12 hr). Image transient detection was used to analyze the collected electromagnetic data, which were found to be consistent with background. Off-line analysis of the GW data alone has also established that the selected GW events show no evidence of an astrophysical origin; one of them is consistent with background and the other one was a test, part of a 'blind injection challenge'. With this work we demonstrate the feasibility of rapid follow-ups of GW transients and establish the sensitivity improvement joint electromagnetic and GW observations could bring. This is a first step toward an electromagnetic follow-up program in the regime of routine detections with the advanced GW instruments expected within this decade. In that regime, multi-wavelength observations will play a significant role in completing the astrophysical identification of GW sources. We present the methods and results from this first combined analysis and discuss its implications in terms of sensitivity for the present and future instruments.

  14. Swift Follow-Up Observations of Candidate Gravitational-Wave Transient Events

    NASA Technical Reports Server (NTRS)

    Evans, P. A.; Fridriksson, J. K.; Gehrels, N.; Homan, J.; Osborne, J. P.; Siegel, M.; Beardmore, A.; Handbauer, P.; Gelbord, J.; Kennea, J. A.; Smith, M.; Zhu, Q.; Aasi, J.; Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M.; Accadia, T.; Acernese, F.; Adams, C.; Adams, T.; Blackburn, J. K.; Camp, J. B.; Kanner, J. B.

    2012-01-01

    We present the first multi-wavelength follow-up observations of two candidate gravitational-wave (GW) transient events recorded by LIGO and Virgo in their 2009-2010 science run. The events were selected with low latency by the network of GW detectors (within less than 10 minutes) and their candidate sky locations were observed by the Swift observatory (within 12 hr). Image transient detection was used to analyze the collected electromagnetic data, which were found to be consistent with background. Off-line analysis of the GW data alone has also established that the selected GW events show no evidence of an astrophysical origin; one of them is consistent with background and the other one was a test, part of a "blind injection challenge." With this work we demonstrate the feasibility of rapid follow-ups of GW transients and establish the sensitivity improvement joint electromagnetic and GW observations could bring. This is a first step toward an electromagnetic follow-up program in the regime of routine detections with the advanced GW instruments expected within this decade. In that regime, multi-wavelength observations will play a significant role in completing the astrophysical identification of GW sources. We present the methods and results from this first combined analysis and discuss its implications in terms of sensitivity for the present and future instruments.

  15. Comparison of the Two Follow-up Observation Strategies for Gravitational Microlensing Planet Searches

    NASA Astrophysics Data System (ADS)

    Han, Cheongho; Kim, Yong-Gi

    2001-01-01

    There are two different strategies of follow-up observations for the detection of planets by using microlensing. One is detecting the light-curve anomalies affected by the planetary caustic from continuous monitoring of all events detected by microlensing survey programs (type I strategy), and the other is detecting anomalies near the peak amplification affected by the central caustic from intensive monitoring of high-amplification events (type II strategy). It was shown by Griest & Safizadeh that the type II strategy yields high planet detection efficiency per event. However, it is not known whether the planet detection rate by this strategy can make up a substantial fraction of the total rate. In this paper, we estimate the relative planet detection rates expected under the two follow-up observation strategies. From this estimation, we find that the rate under the type II strategy is substantial and will comprise ~1/4-1/2 of the total rate. We also find that compared to the type I strategy the type II strategy is more efficient in detecting planets located outside of the lensing zone. We determine the optimal monitoring frequency of the type II strategy to be ~20 times per night, which can be easily achieved by the current microlensing follow-up programs even with a single telescope.

  16. GRB Prompt Optical Observations by Master and Lomonosov

    NASA Astrophysics Data System (ADS)

    Gorbovskoy, Evgeny

    We present the results of the prompt, early and afterglow optical observations of five γ-ray bursts (GRBs): GRB 100901A, GRB 100902A, GRB 100905A, GRB 100906A and GRB 101020A. These observations were made with the Mobile Astronomical System of TElescope-Robots in Russia (MASTER-II Net), the 1.5-m telescope of the Sierra Nevada Observatory and the 2.56-m Nordic Optical Telescope. For two sources, GRB 100901A and GRB 100906A, we detected optical counterparts and obtained light curves starting before the cessation of γ-ray emission, at 113 and 48 s after the trigger, respectively. Observations of GRB 100906A were conducted in two polarizing filters. Observations of the other three bursts gave the upper limits on the optical flux; their properties are briefly discussed. A more detailed analysis of GRB 100901A and GRB 100906A, supplemented by Swift data, provides the following results and indicates different origins for the prompt optical radiation in the two bursts. The light-curve patterns and spectral distributions suggest that there is a common production site for the prompt optical and high-energy emission in GRB 100901A. The results of the spectral fits for GRB 100901A in the range from optical to X-ray favour power-law energy distributions and a consistent value of the optical extinction in the host galaxy. GRB 100906A produced a smoothly peaking optical light curve, suggesting that the prompt optical radiation in this GRB originated in a front shock. This is supported by a spectral analysis. We have found that the Amati and Ghirlanda relations are satisfied for GRB 100906A. We obtain an upper limit on the value of the optical extinction on the host of GRB 100906A. Also we consider prompt observation of dark gamma ray bursts for which on very widefield cameras MASTER-VWF and MASTER-II telescopes upper limits were received. We represent SHOCK experiment onboard the spacecraft Lomonosov.

  17. High-precision follow-up observations of Near-Earth Objects

    NASA Astrophysics Data System (ADS)

    Ramanjooloo, Yudish; Tholen, David J.; Fohring, Dora; Hung, Denise

    2016-10-01

    We present the latest results of ongoing high-precision astrometric follow-up observations of Near-Earth Objects (NEOs) using the University of Hawaii 2.24 metre telescope (currently 7.5 arcmin FOV), the Canada-France-Hawaii Telescope (CFHT; 1 degree FOV) with MegaPrime, and the Subaru Hyper Suprime-Cam (1.5 degree FOV). The combination of excellent observing conditions at Maunakea, and the use of no filter to maximise our throughput efficiency, allows us to recover targets having V < 24, and sometimes V < 25 under ideal conditions. We frequently achieve astrometric accuracy limited by the reference catalog and plan to improve on this capability with the implementation of the GAIA catalog. This work is funded by NASA grant NXX13AI64G.

  18. Swift/XRT follow-up observations of unidentified INTEGRAL sources

    NASA Astrophysics Data System (ADS)

    Maiorano, E.; Landi, R.; Parisi, P.; Masetti, N.; Bassani, L.; Malizia, A.; Bazzano, A.; Ubertini, P.; Bird, A. J.; Jimenez-Bailon, E.; Chavushyan, V.; Galaz, G.; Minniti, D.; Morelli, L.

    2010-10-01

    We report on X-ray follow-up observations performed with Swift/XRT of 3 unidentified INTEGRAL sources listed in the fourth IBIS Survey Catalogue (Bird et al. 2010, ApJS, 186, 1). IGR J08190-3835 Within the IBIS uncertainty XRT detects one source with a statistical significance of 5.8 sigma in the energy range 0.3-10 keV and 5.6 sigma above 3 keV. This object, located at RA(J2000) = 08h 19m 11.3s and Dec(J2000) = -38d 33m 09s (5 arcsec uncertainty), is associated with a 2MASS extended object (2MASX J08191136-3833104) classified as a galaxy in the NED archive and is positionally coincident with radio source NVSS J081910-383307.

  19. Owens Valley Interferometric Observations of the Gamma-Ray Bursts GRB 970228 and GRB 970508

    NASA Astrophysics Data System (ADS)

    Shepherd, D. S.; Frail, D. A.; Kulkarni, S. R.; Metzger, M. R.

    1998-04-01

    We have obtained new observations of the gamma-ray bursts GRB 970228 and GRB 970508 with the Owens Valley Radio Observatory. GRB 970228 was observed in the 1 and 3 mm continuum bands. The field was centered on the position of the optical counterpart approximately 17 days after the initial GRB burst. GRB 970228 was not detected at either wavelength, which places 3 σ upper limits of 2.16 mJy at 92.7 GHz and 38.1 mJy at 242.4 GHz. GRB 970508 was observed in the 3 mm continuum band, centered first on the position of the X-ray source SAX J0653.8+7916 and then on the position of the optical counterpart and the transient source detected by the Very Large Array. A series of five observations were made from 1997 May 10 (~2 days after initial burst detection) to 1997 May 16 (~8 days after burst). GRB 970508 was not detected during any observation. We combine data from May 12 to May 16 to place a solid 3 σ upper limit of 3.0 mJy at 86.8 GHz. Assuming the gamma-ray burst can be modeled by a cosmological fireball, our nondetection supports the interpretation by Frail and coworkers that large fluctuations seen in the centimeter-wave radio fluxes during this time are not due to changes in the source itself but are instead due to interstellar scintillation when the early fireball is nearly a point source.

  20. Loss to follow-up in the Australian HIV Observational Database

    PubMed Central

    McManus, Hamish; Petoumenos, Kathy; Brown, Katherine; Baker, David; Russell, Darren; Read, Tim; Smith, Don; Wray, Lynne; Giles, Michelle; Hoy, Jennifer; Carr, Andrew; Law, Matthew

    2015-01-01

    Background Loss to follow-up (LTFU) in HIV-positive cohorts is an important surrogate for interrupted clinical care which can potentially influence the assessment of HIV disease status and outcomes. After preliminary evaluation of LTFU rates and patient characteristics, we evaluated the risk of mortality by LTFU status in a high resource setting. Methods Rates of LTFU were measured in the Australian HIV Observational Database for a range of patient characteristics. Multivariate repeated measures regression methods were used to identify determinants of LTFU. Mortality by LTFU status was ascertained using linkage to the National Death Index. Survival following combination antiretroviral therapy initiation was investigated using the Kaplan-Meier (KM) method and Cox proportional hazards models. Results Of 3,413 patients included in this analysis, 1,632 (47.8%) had at least one episode of LTFU after enrolment. Multivariate predictors of LTFU included viral load (VL)>10,000 copies/ml (Rate ratio (RR) 1.63 (95% confidence interval (CI):1.45–1.84) (ref ≤400)), time under follow-up (per year) (RR 1.03 (95% CI: 1.02–1.04)) and prior LTFU (per episode) (RR 1.15 (95% CI: 1.06–1.24)). KM curves for survival were similar by LTFU status (p=0.484). LTFU was not associated with mortality in Cox proportional hazards models (univariate hazard ratio (HR) 0.93 (95% CI: 0.69–1.26) and multivariate HR 1.04 (95% CI: 0.77–1.43)). Conclusions Increased risk of LTFU was identified amongst patients with potentially higher infectiousness. We did not find significant mortality risk associated with LTFU. This is consistent with timely re-engagement with treatment, possibly via high levels of unreported linkage to other health care providers. PMID:25377928

  1. Multi-observation PET image analysis for patient follow-up quantitation and therapy assessment

    PubMed Central

    David, Simon; Visvikis, Dimitris; Roux, Christian; Hatt, Mathieu

    2011-01-01

    In Positron Emission Tomography (PET) imaging, an early therapeutic response is usually characterized by variations of semi-quantitative parameters restricted to maximum SUV measured in PET scans during the treatment. Such measurements do not reflect overall tumour volume and radiotracer uptake variations. The proposed approach is based on multi-observation image analysis for merging several PET acquisitions to assess tumour metabolic volume and uptake variations. The fusion algorithm is based on iterative estimation using stochastic expectation maximization (SEM) algorithm. The proposed method was applied to simulated and clinical follow-up PET images. We compared the multi-observation fusion performance to threshold-based methods, proposed for the assessment of the therapeutic response based on functional volumes. On simulated datasets, the adaptive threshold applied independently on both images led to higher errors than the ASEM fusion and on the clinical datasets, it failed to provide coherent measurements for four patients out of seven due to aberrant delineations. The ASEM method demonstrated improved and more robust estimation of the evaluation leading to more pertinent measurements. Future work will consist in extending the methodology and applying it to clinical multi-tracers datasets in order to evaluate its potential impact on the biological tumour volume definition for radiotherapy applications. PMID:21846937

  2. Changes observed in diabetic retinopathy: eight-year follow-up of a Spanish population

    PubMed Central

    Romero-Aroca, Pedro; de la Riva-Fernandez, Sofia; Valls-Mateu, Aida; Sagarra-Alamo, Ramon; Moreno-Ribas, Antonio; Soler, Nuria

    2016-01-01

    Background/aims To determine the changes in the incidence of diabetic retinopathy (DR), diabetic macular oedema (DMO) and their risk factors in a population-based study of patients with diabetes mellitus (DM) referred to our 16 Primary Health Care Areas (HCAs). Methods Prospective population-based study of a total of 15 396 Caucasian patients with DM, who represent 86.53% of the total patients with DM in our HCAs, were studied over an 8-year follow-up period. All patients were screened with a mean follow-up of 3.18±1.11 times for each patient over the 8 years. Results The yearly mean value of any DR was 8.37±2.19% (8.09%–8.99%); of advanced DR yearly mean value of 0.46±0.22% (0.03–0.78); and of DMO a yearly mean value of 2.19±0.18% (2%–2.49%). A clear increase was observed in the last 3 years, any DR increased from 8.09% in 2007 to 8.99% in 2014, and DMO from 2% in 2007 to 2.49% in 2014. These increases were more evident in some age groups. For patients with any DR aged 41–50 and 51–60 and for patients with advanced DR aged 41–50, 51–60 and 61–70, the increase was more marked, related to an increase in HbA1c values or to patients treated with insulin. Conclusions An increase in the incidence of DR and DMO was observed, especially in the younger patients aged between 31 and 70 years. This is linked to bad metabolic control of DM. Our results suggest a greater number of ocular complications in the near future, such as neovascular glaucoma, if these current findings are not addressed. PMID:26769672

  3. Photometric Follow-Up Observations of the Transiting Neptune-Mass Planet GJ 436b

    NASA Astrophysics Data System (ADS)

    Shporer, Avi; Mazeh, Tsevi; Pont, Frederic; Winn, Joshua N.; Holman, Matthew J.; Latham, David W.; Esquerdo, Gilbert A.

    2009-04-01

    This paper presents multiband photometric follow-up observations of the Neptune-mass transiting planet GJ 436b, consisting of five new ground-based transit light curves obtained in 2007 May. Together with one already published light curve, we have at hand a total of six light curves, spanning 29 days. The analysis of the data yields an orbital period P = 2.64386 ± 0.00003 days, midtransit time Tc [HJD] = 2454235.8355 ± 0.0001, planet mass Mp = 23.1 ± 0.9 M ⊕ = 0.073 ± 0.003 M Jup, planet radius Rp = 4.2 ± 0.2 R ⊕ = 0.37 ± 0.01 R Jup, and stellar radius Rs = 0.45 ± 0.02 R sun. Our typical precision for the midtransit timing for each transit is about 30 s. We searched the data for a possible signature of a second planet in the system through transit timing variations (TTV) and variation of the impact parameter. The analysis could not rule out a small, of the order of a minute, TTV and a long-term modulation of the impact parameter, of the order of +0.2 yr-1.

  4. X-ray follow-up observations of unidentified VHE {gamma}-ray sources

    SciTech Connect

    Puehlhofer, Gerd

    2008-12-24

    A large fraction of the recently discovered Galactic Very High Energy (VHE) source population remains unidentified to date. VHE {gamma}-ray emission traces high energy particles in these sources, but for example in case of hadronic processes also the gas density at the emission site. Moreover, the particles have sufficiently long lifetimes to be able to escape from their acceleration sites. Therefore, the {gamma}-ray sources or at least the areas of maximum surface brightness are in many cases spatially offset from the actual accelerators. A promising way to identify the objects in which the particles are accelerated seems to be to search for emission signatures of the acceleration process (like emission from shock-heated plasma). Also the particles themselves (through primary or secondary synchrotron emission) can be traced in lower wavebands. Those signatures are best visible in the X-ray band, and current X-ray observatories are well suited to conduct such follow-up observations. Some aspects of the current status of these investigations are reviewed.

  5. Systematic Errors in Low-latency Gravitational Wave Parameter Estimation Impact Electromagnetic Follow-up Observations

    NASA Astrophysics Data System (ADS)

    Littenberg, Tyson B.; Farr, Ben; Coughlin, Scott; Kalogera, Vicky

    2016-03-01

    Among the most eagerly anticipated opportunities made possible by Advanced LIGO/Virgo are multimessenger observations of compact mergers. Optical counterparts may be short-lived so rapid characterization of gravitational wave (GW) events is paramount for discovering electromagnetic signatures. One way to meet the demand for rapid GW parameter estimation is to trade off accuracy for speed, using waveform models with simplified treatment of the compact objects’ spin. We report on the systematic errors in GW parameter estimation suffered when using different spin approximations to recover generic signals. Component mass measurements can be biased by \\gt 5σ using simple-precession waveforms and in excess of 20σ when non-spinning templates are employed. This suggests that electromagnetic observing campaigns should not take a strict approach to selecting which LIGO/Virgo candidates warrant follow-up observations based on low-latency mass estimates. For sky localization, we find that searched areas are up to a factor of ∼ 2 larger for non-spinning analyses, and are systematically larger for any of the simplified waveforms considered in our analysis. Distance biases for the non-precessing waveforms can be in excess of 100% and are largest when the spin angular momenta are in the orbital plane of the binary. We confirm that spin-aligned waveforms should be used for low-latency parameter estimation at the minimum. Including simple precession, though more computationally costly, mitigates biases except for signals with extreme precession effects. Our results shine a spotlight on the critical need for development of computationally inexpensive precessing waveforms and/or massively parallel algorithms for parameter estimation.

  6. Optical Follow-Up Observations of PTF10qts, a Luminous Broad-Lined Type Ic Supernova Found by the Palomar Transient Factory

    NASA Technical Reports Server (NTRS)

    Walker, E. S.; Mazzali, P. A.; Pian, E.; Hurley, K.; Arcavi, I.; Cenko, S. B.; Gal-Yam, A.; Horesh, A.; Kasliwal, M.; Poznanski, D.; Silverman, J. M.; Barthelmy, S.

    2014-01-01

    We present optical photometry and spectroscopy of the broad-lined Type Ic supernova (SN Ic-BL) PTF10qts, which was discovered as part of the Palomar Transient Factory. The supernova was located in a dwarf galaxy of magnitude r = 21.1 at a redshift z = 0.0907.We find that the R-band light curve is a poor proxy for bolometric data and use photometric and spectroscopic data to construct and constrain the bolometric light curve. The derived bolometric magnitude at maximum light is Mbol = -18.51 +/- 0.2 mag, comparable to that of SN1998bw (Mbol = -18.7 mag) which was associated with a gamma-ray burst (GRB). PTF10qts is one of the most luminous SN Ic-BL observed without an accompanying GRB. We estimate the physical parameters of the explosion using data from our programme of follow-up observations, finding that it produced a larger mass of radioactive nickel compared to other SNeIc-BL with similar inferred ejecta masses and kinetic energies. The progenitor of the event was likely a approximately 20 solar mass star.

  7. Follow-up observations of extremely metal-poor stars identified from SDSS

    NASA Astrophysics Data System (ADS)

    Aguado, D. S.; Allende Prieto, C.; González Hernández, J. I.; Carrera, R.; Rebolo, R.; Shetrone, M.; Lambert, D. L.; Fernández-Alvar, E.

    2016-08-01

    Context. The most metal-poor stars in the Milky Way witnessed the early phases of formation of the Galaxy, and have chemical compositions that are close to the pristine mixture from Big Bang nucleosynthesis, polluted by one or few supernovae. Aims: Only two dozen stars with ([Fe/H] < -4) are known, and they show a wide range of abundance patterns. It is therefore important to enlarge this sample. We present the first results of an effort to identify new extremely metal-poor stars in the Milky Way halo. Methods: Our targets have been selected from low-resolution spectra obtained as part of the Sloan Digital Sky Survey, and followed-up with medium resolution spectroscopy on the 4.2 m William Herschel Telescope and, in a few cases, at high resolution on the 9.2 m Hobby-Eberly Telescope. Stellar parameters and the abundances of magnesium, calcium, iron, and strontium have been inferred from the spectra using classical model atmospheres. We have also derived carbon abundances from the G band. Results: We find consistency between the metallicities estimated from SDSS and those from new data at the level of 0.3 dex. The analysis of medium resolution data obtained with ISIS on the WHT allows us to refine the metallicities and in some cases measure other elemental abundances. Our sample contains 11 new metal-poor stars with [Fe/H] < -3.0, one of them with an estimated metallicity of [Fe/H] ~ -4.0. We also discuss metallicity discrepancies of some stars in common with previous works in the literature. Only one of these stars is found to be C-enhanced at about [C/Fe] ~ + 1, whereas the other metal-poor stars show C abundances at the level of [C/Fe] ~ + 0.45. Based on observations obtained with the Hobby-Eberly Telescope, which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen.The reduced spectra as FITS files are only available at

  8. The 80 Ms follow-up of the X-ray afterglow of GRB 130427A challenges the standard forward shock model

    NASA Astrophysics Data System (ADS)

    De Pasquale, M.; Page, M. J.; Kann, D. A.; Oates, S. R.; Schulze, S.; Zhang, B.; Cano, Z.; Gendre, B.; Malesani, D.; Rossi, A.; Troja, E.; Piro, L.; Boër, M.; Stratta, G.; Gehrels, N.

    2016-10-01

    GRB 130427A was the brightest gamma-ray burst detected in the last 30 yr. With an equivalent isotropic energy output of 8.5 × 1053 erg and redshift z = 0.34, it uniquely combined very high energetics with a relative proximity to Earth. As a consequence, its X-ray afterglow has been detected by sensitive X-ray observatories such as XMM-Newton and Chandra for a record-breaking baseline longer than 80 million seconds. We present the X-ray light curve of this event over such an interval. The light curve shows a simple power-law decay with a slope α = 1.309 ± 0.007 over more than three decades in time (47 ks-83 Ms). We discuss the consequences of this result for a few models proposed so far to interpret GRB 130427A, and more in general the significance of this outcome in the context of the standard forward shock model. We find that this model has difficulty in explaining our data, in both cases of constant density and stellar-wind circumburst media, and requires far-fetched values for the physical parameters involved.

  9. Using the 2-MASS photometric redshift survey to optimize LIGO follow-up observations

    NASA Astrophysics Data System (ADS)

    Antolini, Elisa; Heyl, Jeremy S.

    2016-10-01

    The initial discovery of Laser Interferometer Gravitational-Wave Observatory (LIGO) on 2015 September 14 was the inspiral merger and ring-down of the black hole binary at a distance of about 500 Mpc or a redshift of about 0.1. The search for electromagnetic counterparts for the inspiral of binary black holes is impeded by coarse initial source localizations and a lack of a compelling model for the counterpart; therefore, rapid electromagnetic follow-up is required to understand the astrophysical context of these sources. Because astrophysical sources of gravitational radiation are likely to reside in galaxies, it would make sense to search first in regions where the LIGO-Virgo probability is large and where the density of galaxies is large as well. Under the assumption that the probability of a gravitational-wave event from a given region of space is proportional to the density of galaxies within the probed volume, one can calculate an improved localization of the position of the source simply by multiplying the LIGO-Virgo skymap by the density of galaxies in the range of redshifts. We propose using the 2-MASS photometric redshift galaxy catalogue for this purpose and demonstrate that using it can dramatically reduce the search region for electromagnetic counterparts.

  10. [Results from the X-ray and Optical Follow-up Observations of the Swift BAT AGN Survey

    NASA Technical Reports Server (NTRS)

    Mushotzky, R.

    2008-01-01

    I will present results from the x-ray and optical follow-up observations of the Swift BAT ACN survey. I will discuss the nature of obscuration in these objects, the relationship to optical properties and the change of properties with luminosity and galaxy type and how they will influence the design of XO.

  11. WIDGET: System Performance and GRB Prompt Optical Observations

    NASA Astrophysics Data System (ADS)

    Urata, Yuji; Tashiro, Makoto S.; Tamagawa, Toru; Usui, Fumihiko; Kuwahara, Makoto; Lin, Hungmiao; Kageyama, Shoichi; Iwakiri, Wataru; Sugasahara, Takako; Takahara, Kazuki; Kodaka, Natsuki; Abe, Keiichi; Masuno, Keisuke; Onda, Kaori

    2011-02-01

    The WIDeField telescope for Gamma-ray burst Early Timing (WIDGET) is used for a fully automated, ultra-wide-field survey aimed at detecting the prompt optical emission associated with Gamma-ray Bursts (GRBs). WIDGET surveys the HETE-2 and Swift/BAT pointing directions, covering a total field of view of 62° × 62° every 10 secounds using a unfiltered system. This monitoring survey allows the exploration of optical emission before the γ-ray trigger. The unfiltered magnitude is well converted to the SDSS r' system at a 0.1 mag level. Since 2004, WIDGET has made a total of ten simultaneous and one pre-trigger GRB observations. The efficiency of synchronized observations with HETE-2 is four-times better than that of Swift. There has been no bright optical emission similar to that from GRB 080319B. A statistical analysis implies that GRB 080319B is a rare event. This paper summarizes the design and operation of the WIDGET system and the simultaneous GRB observations obtained with this instrument.

  12. Probing a GRB Progenitor at a Redshift of z=2: A Comprehensive Observing Campaign of the Afterglow of GRB 030226l

    NASA Technical Reports Server (NTRS)

    Klose, S.; Greiner, J.; Rau, A.; Henden, A. A.; Hartmann, D. H.; Zeh, A.; Ries, C.; Masetti, N.; Malesani, D.; Guenther, E.

    2004-01-01

    We report results from a comprehensive optical/near-infrared follow-up observing campaign of the afterglow of GRB 030226, including VLT spectroscopy and polarimetry, supplemented by Chandra X-ray and BOOTES-1 rapid response observations. First observations at ESO started 0.2 days after the burst when the afterglow was at a magnitude of R approx. 19. The multi-color light curve of the afterglow, with a break around 1 day after the burst, is achromatic within the observational uncertainties even during episodes of short-term fluctuations. Close to the break time the degree of linear polarization of the afterglow light was less than 1.1%, consistent with low intrinsic polarization observed in other afterglows. VLT spectra show a foreground absorber of Mg II at a redshift z=1.042 and two absorption line systems at redshifts z=1.962+/-0.001 and at z=1.986+/-0.001, placing the lower limit for the redshift of the GRB close to 2. The kinematics and the composition of the absorbing clouds is very similar to those observed in the afterglow of GRB 021004, supporting the view that at least some GRBs are physically related to the explosion of a Wolf-Rayet star.

  13. MASTER follow up observation of IceCube 160731A event

    NASA Astrophysics Data System (ADS)

    Lipunov, V.; Gorbovskoy, E.; Tyurina, N.; Kornilov, V.; Balanutsa, P.; Kuznetsov, A.; Kuvshinov, D.; Gorbunov, I.; Tlatov, A.; Senik, V.; Parhomenko, A. V.; Dormidontov, D.; Buckley, D.; Potter, S.; Kniazev, A.; Kotze, M.; Rebolo, R.; Serra, M.; Lodieu, N.; Israelian, G.; Podesta, R.; Lopez, C.; Podest, F.; Levato, H.; Saffe, C.; Gres, O.; Ivanov, K.; Yazev, S.; Budnev, N.; Poleshchuk, V.; Yurkov, V.; Sergienko, Yu.; Gabovich, A.

    2016-08-01

    MASTER Global robotic Net (MASTER-Net: http://observ.pereplet.ru , Lipunov et al., Advances in Astronomy, 2010, 30L ) received IceCube HESE event IceCube-160731A (AMON ICECUBE HESE 128290 6888376) at 2016-07-31 01:55:34.5 UT (30s after the EHE_event_time).

  14. The photometric follow-up observations for transiting exoplanet XO-2b

    NASA Astrophysics Data System (ADS)

    Gu, Sheng-hong; Collier Cameron, Andrew; Wang, Xiao-bin; Fang, Xiang-song; Cao, Dong-tao; Zhang, Li-yun

    2011-11-01

    Four new transit light curves of XO-2b obtained in 2008 and 2009, are analyzed by using MCMC algorithm, and the system parameters are derived. The result demonstrates that the orbital period of the system obtained from new observations is almost the same as Burke et al.'s one (2007), which does not confirm the result of Fernandez et al. (2009).

  15. Target Charaterization and Follow-Up Observations in Support of the Kepler Mission

    NASA Technical Reports Server (NTRS)

    Latham, David W.

    2004-01-01

    This report covers work carried out at the Smithsonian Astrophysical Observatory during the period 1 December 2003 to 30 November 2004 to support efforts to prepare the Kepler Input Catalog. The Catalog will be used to select the targets observed for planetary transits by Kepler.

  16. The University of Arizona Astronomy Club Follow-up Observations of Known Exoplanets

    NASA Astrophysics Data System (ADS)

    Small, Lindsay; Pearson, K.; Turner, J.; Biddle, L. I.; Nguyen, C.; Watson, Z.; Mango, D.; Romine, J. M.; Hume, J.; Sinor, K.; Amaya, H.; Stanford-Jones, C.; Qu, D.; Liu, Y.

    2014-01-01

    We observed the primary transits of GJ-1214b and Kelt-1b using the I and R photometric filters on the Kuiper 61" telescope. GJ-1214b is a super earth and Kelt-1b is a hot Jupiter. GJ-1214b has a flat transmission spectrum, which is most likely due to clouds in tis atmosphere. Kelt-1b was the first planet discovered by the KELT survey, and it also has a brown dwarf companion. Because of this, we can expect to observe a timing transit variation. A major component of this project is to give students a learning experience beyond the classroom by getting them involved in an introductory astronomy project. Undergraduates have the opportunity to gain hands-on experience doing data reduction and analysis while still being able to contribute updated planetary parameters for both these systems.

  17. The University of Arizona Astronomy Club Follow-up Observations of Known Exoplanets

    NASA Astrophysics Data System (ADS)

    Jones, Christen; Turner, J.; Cates, I.; Cook, K.; Crawford, B.; Guvenen, B.; Hardegree-Ullman, K.; McGraw, A. M.; Nguyen, C.; Pearson, K.; Robertson, A.; Sanford, B.; Small, L.; Smith, C.; Teske, J.; Tombleson, R.; Towner, A. P.; Walker-LaFollette, A.; Richardson, L.

    2013-01-01

    The University of Arizona Astronomy Club observed the transits of a series of extrasolar planets using the Steward Observatory 61” Kuiper Telescope. Observations of WASP-35b, WASP-43b, WASP-44b, WASP-48b, HAT-P-20b, and HAT-P-36b were taken in the Harris-R or Bessell-U filter. All of the selected planets are previously discovered hot Jupiters or hot Neptunes, but have not been studied extensively. Several have incomplete data and only partial light curves. We intend to confirm or improve upon published values for each planet's mass, radius, density, surface gravity, Safronov number, equilibrium temperature, orbital distance, and orbital inclination. Another goal is to obtain more complete light curves to look for transit timing variations. This project is also a way to familiarize undergraduate students with data reduction through the use of IRAF beyond in-class instruction.

  18. Spitzer Follow-up of HST Observations of Star Formation in H II Regions

    NASA Astrophysics Data System (ADS)

    Hester, Jeff; Bally, John; Desch, Steve; Healy, Kevin; Snider, Keely

    2005-06-01

    Images of regions of star formation taken with HST have given us an extraordinary view of young stellar objects and their natal environments. These views differ tremendously between low-mass YSOs seen in regions of isolated low-mass star formation such as Taurus-Auriga, and the proplyds, EGGs, and other structures seen in regions of massive star formation. While YSOs in Taurus spend their adolescence buried in the dark interiors of molecular clouds, YSOs near massive stars quickly find themselves overrun by ionization fronts and exposed to the intense UV radiation from nearby massive stars. This difference in environment has a profound effect on the way in which the protoplanetary disk around a star evolves -- a fact that is of great importance to us, given the strength of the evidence suggesting that the Sun formed near a massive star. But HST while HST can inform us about the evolution of YSOs in HII region environments once they are overrun by ionization fronts, it cannot show us the birth of the stars themselves. These remain hidden in the dense molecular material beyond the ionized volumes of these regions. Only Spitzer can show us the properties of the YSOs that lie hidden in the dark shadows of HST images of HII regions, and only Spitzer can provide us with information about PDRs, warm dust, and other tracers of the interaction of massive stars with their surroundings. The combination of HST and Spitzer observations of star forming regions is far greater than the sum of its parts. If we are to build a complete picture of low-mass star formation and the evolution of disks near massive stars, we need to combine HST and Spitzer observations of the same regions. In this proposal we request time to obtain both IRAC and MIPS 24 micron images of each HII region that has been observed by HST, but has yet to be observed with Spitzer. Together with previous images obtained from the archives, this will comprise an indispensible data set for testing hypotheses about

  19. Follow-Up Chandra Observations of Three Candidate Tidal Disruption Events

    NASA Astrophysics Data System (ADS)

    Halpern, J. P.; Gezari, S.; Komossa, S.

    2004-04-01

    Large-amplitude, high-luminosity soft X-ray flares were detected by the ROSAT All-Sky Survey in several galaxies with no evidence of Seyfert activity in their ground-based optical spectra. These flares had the properties predicted for a tidal disruption of a star by a central supermassive black hole. We report Chandra observations of three of these galaxies taken a decade after their flares that reveal weak nuclear X-ray sources that are from 240 to 6000 times fainter than their luminosities at peak, supporting the theory that these were special events and not ongoing active galactic nucleus (AGN) variability. The decline of RX J1624.9+7554 by a factor of 6000 is consistent with the (t-tD)-5/3 decay predicted for the fallback phase of a tidal disruption event, but only if ROSAT was lucky enough to catch the event exactly at its peak in 1990 October. RX J1242.6-1119A has declined by a factor of 240, also consistent with (t-tD)-5/3. In the H II galaxy NGC 5905 we find only resolved, soft X-ray emission that is undoubtedly associated with starburst activity. When accounting for the starburst component, the ROSAT observations of NGC 5905, as well as the Chandra upper limit on its nuclear flux, are consistent with a (t-tD)-5/3 decay by at least a factor of 1000. Although we found weak Seyfert 2 emission lines in Hubble Space Telescope spectra of NGC 5905, indicating that a low-luminosity AGN was present prior to the X-ray flare, we favor a tidal disruption explanation for the flare itself.

  20. Spectroscopic Observations of the Bright Afterglow of GRB021004

    NASA Astrophysics Data System (ADS)

    Harrison, Fiona

    2001-09-01

    One of the holy grails of gamma-ray burst research is to detect X-ray line signatures from an afterglow with high statistical significance. Of all possible observations, this perhaps offers the best chance of constraining the GRB mechanism and environment, and could provide the "smoking gun" signature connecting GRBs to massive stellar deaths. In order to accomplish this, we know long observations within one day of the event are necessary.

  1. Results of optical follow-up observations of advanced LIGO triggers from O1 in the southern hemisphere

    NASA Astrophysics Data System (ADS)

    Beroiz, Martin; Colazo, Carlos; Diaz, Mario; Dominguez, Mariano; Garcia Lambas, Diego; Gurovich, Sebastian; Lares, Marcelo; Macri, Lucas; Penuela, Tania; Rodriguez, Horacio; Sanchez, Bruno; Toros Collaboration

    2016-03-01

    We report on observations related to the follow-up of LIGO VIRGO collaboration triggers released to participating astronomers during the First Observation Run 1 (O1) from September 18, 2015 to January 12, 2016, performed by the TOROS collaboration. The Transient Optical Robotic Observatory of the South (TOROS) collaboration operated telescopes located in two different sites in Argentina: one at the Estación Astrofísica Bosque Alegre in Cordoba, and the other one located in Cordón Macón, Salta. In this communication we describe the main characteristics of the campaign sustained during O1 and the plans for continuing observation in the future.

  2. The XXL Survey. I. Scientific motivations - XMM-Newton observing plan - Follow-up observations and simulation programme

    NASA Astrophysics Data System (ADS)

    Pierre, M.; Pacaud, F.; Adami, C.; Alis, S.; Altieri, B.; Baran, N.; Benoist, C.; Birkinshaw, M.; Bongiorno, A.; Bremer, M. N.; Brusa, M.; Butler, A.; Ciliegi, P.; Chiappetti, L.; Clerc, N.; Corasaniti, P. S.; Coupon, J.; De Breuck, C.; Democles, J.; Desai, S.; Delhaize, J.; Devriendt, J.; Dubois, Y.; Eckert, D.; Elyiv, A.; Ettori, S.; Evrard, A.; Faccioli, L.; Farahi, A.; Ferrari, C.; Finet, F.; Fotopoulou, S.; Fourmanoit, N.; Gandhi, P.; Gastaldello, F.; Gastaud, R.; Georgantopoulos, I.; Giles, P.; Guennou, L.; Guglielmo, V.; Horellou, C.; Husband, K.; Huynh, M.; Iovino, A.; Kilbinger, M.; Koulouridis, E.; Lavoie, S.; Le Brun, A. M. C.; Le Fevre, J. P.; Lidman, C.; Lieu, M.; Lin, C. A.; Mantz, A.; Maughan, B. J.; Maurogordato, S.; McCarthy, I. G.; McGee, S.; Melin, J. B.; Melnyk, O.; Menanteau, F.; Novak, M.; Paltani, S.; Plionis, M.; Poggianti, B. M.; Pomarede, D.; Pompei, E.; Ponman, T. J.; Ramos-Ceja, M. E.; Ranalli, P.; Rapetti, D.; Raychaudury, S.; Reiprich, T. H.; Rottgering, H.; Rozo, E.; Rykoff, E.; Sadibekova, T.; Santos, J.; Sauvageot, J. L.; Schimd, C.; Sereno, M.; Smith, G. P.; Smolčić, V.; Snowden, S.; Spergel, D.; Stanford, S.; Surdej, J.; Valageas, P.; Valotti, A.; Valtchanov, I.; Vignali, C.; Willis, J.; Ziparo, F.

    2016-06-01

    Context. The quest for the cosmological parameters that describe our universe continues to motivate the scientific community to undertake very large survey initiatives across the electromagnetic spectrum. Over the past two decades, the Chandra and XMM-Newton observatories have supported numerous studies of X-ray-selected clusters of galaxies, active galactic nuclei (AGNs), and the X-ray background. The present paper is the first in a series reporting results of the XXL-XMM survey; it comes at a time when the Planck mission results are being finalised. Aims: We present the XXL Survey, the largest XMM programme totaling some 6.9 Ms to date and involving an international consortium of roughly 100 members. The XXL Survey covers two extragalactic areas of 25 deg2 each at a point-source sensitivity of ~5 × 10-15 erg s-1 cm-2 in the [0.5-2] keV band (completeness limit). The survey's main goals are to provide constraints on the dark energy equation of state from the space-time distribution of clusters of galaxies and to serve as a pathfinder for future, wide-area X-ray missions. We review science objectives, including cluster studies, AGN evolution, and large-scale structure, that are being conducted with the support of approximately 30 follow-up programmes. Methods: We describe the 542 XMM observations along with the associated multi-λ and numerical simulation programmes. We give a detailed account of the X-ray processing steps and describe innovative tools being developed for the cosmological analysis. Results: The paper provides a thorough evaluation of the X-ray data, including quality controls, photon statistics, exposure and background maps, and sky coverage. Source catalogue construction and multi-λ associations are briefly described. This material will be the basis for the calculation of the cluster and AGN selection functions, critical elements of the cosmological and science analyses. Conclusions: The XXL multi-λ data set will have a unique lasting legacy

  3. Follow-up Observations of a Sample of Stars in the MOTESS-GNAT MG1 Variable Star Catalog

    NASA Astrophysics Data System (ADS)

    Tucker, Roy A.; Craine, Eric R.; Flurchick, Kenneth M.; Kraus, Adam L.; Griego, Benjamin F.

    2013-05-01

    The MOTESS-GNAT variable star survey catalogs are producing large numbers of previously unknown and unstudied variable stars of a wide range of types. These stars include everything from well recognized archetypes to very unusual and interesting stars with presently unpredictable behavior. In most cases these stars are in need of more intensive follow-up observation. Such observation initially involves expanded photometric observing programs to better characterize variability. This may be because of short period systems that show aliased periods, it may be longer period systems that show superposed trends of period variations, it may be irregular systems that are recognized but poorly characterized. In some instances, the stars exhibit interesting, but wholly erratic and unpredictable behavior. In this paper we show how to find interesting stars in the survey data, discuss the necessary follow-up observations, and show numerous examples of some of the stars studied to date. We encourage SAS members to consider joining us in characterizing these stars.

  4. Implications for the Origin of GRB 051103 from LIGO Observations

    NASA Technical Reports Server (NTRS)

    Bizouard, M. A.; Dietz, A.; Guidi, G. M.; Was, M.; Camp, J. B.; Cannizzo, J.; Stroeer, A. S.; Blackburn, L.

    2012-01-01

    We present the results of a LIGO search for gravitational waves (GWs) associated with GRB 051103, a short-duration hard-spectrum gamma-ray burst whose electromagnetically determined sky position is coincident with the spiral galaxy M81, which is 3.6Mpc from Earth. Possible progenitors for short-hard GRBs include compact object mergers and soft gamma repeater (SGR) giant flares. A merger progenitor would produce a characteristic GW signal that should be detectable at the distance of M81, while GW emission from an SGR is not expected to be detectable at that distance. We found no evidence of a GW signal associated with GRB 051103. Assuming weakly beamed gamma-ray emission with a jet semi-angle of 30. we exclude a binary neutron star merger in M81 as the progenitor with a confidence of 98%. Neutron star-black hole mergers are excluded with > 99% confidence. If the event occurred in M81 our findings support the hypothesis that GRB 051103 was due to an SGR giant flare, making it the most distant extragalactic magnetar observed to date.

  5. [Diagnosis and follow-up observation of granulosa cell tumor of the ovary are becoming more precise].

    PubMed

    Färkkilä, Anniina; Unkila-Kallio, Leila

    2016-01-01

    Granulosa cell tumor of the ovary is a rare, hormonally active ovarian cancer, typical symptoms of which include various gynecological bleeding disorders. Adult granulosa cell tumor is most commonly detected at stage I, whereupon the prognosis is good. The disease, however, recurs in one third of stage I patients and leads to death in half of these. Conventional cytotoxic agents may be ineffective in the treatment of relapsed tumors. Inhibin B and anti-Müllerian hormone have proven to be sensitive and accurate markers. Knowledge about the disease mechanisms has improved the diagnostics and follow-up observation of the patients. PMID:27400589

  6. The Detection of a Type IIn Supernova in Optical Follow-up Observations of IceCube Neutrino Events

    NASA Astrophysics Data System (ADS)

    Aartsen, M. G.; Abraham, K.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Altmann, D.; Anderson, T.; Archinger, M.; Arguelles, C.; Arlen, T. C.; Auffenberg, J.; Bai, X.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Becker Tjus, J.; Becker, K.-H.; Beiser, E.; BenZvi, S.; Berghaus, P.; Berley, D.; Bernardini, E.; Bernhard, A.; Besson, D. Z.; Binder, G.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Bohm, C.; Börner, M.; Bos, F.; Bose, D.; Böser, S.; Botner, O.; Braun, J.; Brayeur, L.; Bretz, H.-P.; Brown, A. M.; Buzinsky, N.; Casey, J.; Casier, M.; Cheung, E.; Chirkin, D.; Christov, A.; Christy, B.; Clark, K.; Classen, L.; Coenders, S.; Cowen, D. F.; Cruz Silva, A. H.; Daughhetee, J.; Davis, J. C.; Day, M.; de André, J. P. A. M.; De Clercq, C.; Dembinski, H.; De Ridder, S.; Desiati, P.; de Vries, K. D.; de Wasseige, G.; de With, M.; DeYoung, T.; Díaz-Vélez, J. C.; Dumm, J. P.; Dunkman, M.; Eagan, R.; Eberhardt, B.; Ehrhardt, T.; Eichmann, B.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fahey, S.; Fazely, A. R.; Fedynitch, A.; Feintzeig, J.; Felde, J.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Flis, S.; Fuchs, T.; Glagla, M.; Gaisser, T. K.; Gaior, R.; Gallagher, J.; Gerhardt, L.; Ghorbani, K.; Gier, D.; Gladstone, L.; Glüsenkamp, T.; Goldschmidt, A.; Golup, G.; Gonzalez, J. G.; Góra, D.; Grant, D.; Gretskov, P.; Groh, J. C.; Gross, A.; Ha, C.; Haack, C.; Haj Ismail, A.; Hallgren, A.; Halzen, F.; Hansmann, B.; Hanson, K.; Hebecker, D.; Heereman, D.; Helbing, K.; Hellauer, R.; Hellwig, D.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Holzapfe, K.; Homeier, A.; Hoshina, K.; Huang, F.; Huber, M.; Huelsnitz, W.; Hulth, P. O.; Hultqvist, K.; In, S.; Ishihara, A.; Jacobi, E.; Japaridze, G. S.; Jero, K.; Jurkovic, M.; Kaminsky, B.; Kappes, A.; Karg, T.; Karle, A.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kemp, J.; Kheirandish, A.; Kiryluk, J.; Kläs, J.; Klein, S. R.; Kohnen, G.; Koirala, R.; Kolanoski, H.; Konietz, R.; Koob, A.; Köpke, L.; Kopper, C.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Krings, K.; Kroll, G.; Kroll, M.; Kunnen, J.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lesiak-Bzdak, M.; Leuermann, M.; Leuner, J.; Lünemann, J.; Madsen, J.; Maggi, G.; Mahn, K. B. M.; Maruyama, R.; Mase, K.; Matis, H. S.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Meli, A.; Menne, T.; Merino, G.; Meures, T.; Miarecki, S.; Middell, E.; Middlemas, E.; Miller, J.; Mohrmann, L.; Montaruli, T.; Morse, R.; Nahnhauer, R.; Naumann, U.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Obertacke, A.; Olivas, A.; Omairat, A.; O'Murchadha, A.; Palczewski, T.; Pandya, H.; Paul, L.; Pepper, J. A.; Pérez de los Heros, C.; Pfendner, C.; Pieloth, D.; Pinat, E.; Posselt, J.; Price, P. B.; Przybylski, G. T.; Pütz, J.; Quinnan, M.; Rädel, L.; Rameez, M.; Rawlins, K.; Redl, P.; Reimann, R.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.; Richter, S.; Riedel, B.; Robertson, S.; Rongen, M.; Rott, C.; Ruhe, T.; Ryckbosch, D.; Saba, S. M.; Sabbatini, L.; Sander, H.-G.; Sandrock, A.; Sandroos, J.; Sarkar, S.; Schatto, K.; Scheriau, F.; Schimp, M.; Schmidt, T.; Schmitz, M.; Schoenen, S.; Schöneberg, S.; Schönwald, A.; Schukraft, A.; Schulte, L.; Seckel, D.; Seunarine, S.; Shanidze, R.; Smith, M. W. E.; Soldin, D.; Spiczak, G. M.; Spiering, C.; Stahlberg, M.; Stamatikos, M.; Stanev, T.; Stanisha, N. A.; Stasik, A.; Stezelberger, T.; Stokstad, R. G.; Stössl, A.; Strahler, E. A.; Ström, R.; Strotjohann, N. L.; Sullivan, G. W.; Sutherland, M.; Taavola, H.; Taboada, I.; Ter-Antonyan, S.; Terliuk, A.; Tešić, G.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Tosi, D.; Tselengidou, M.; Turcati, A.; Unger, E.; Usner, M.; Vallecorsa, S.; van Eijndhoven, N.; Vandenbroucke, J.; van Santen, J.; Vanheule, S.; Veenkamp, J.; Vehring, M.; Voge, M.; Vraeghe, M.; Walck, C.; Wallraff, M.; Wandkowsky, N.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whelan, B. J.; Whitehorn, N.; Wichary, C.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.; Wissing, H.; Wolf, M.; Wood, T. R.; Woschnagg, K.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yanez, J. P.; Yodh, G.; Yoshida, S.; Zarzhitsky, P.; Zoll, M.; IceCube Collaboration; Ofek, Eran O.; Kasliwal, Mansi M.; Nugent, Peter E.; Arcavi, Iair; Bloom, Joshua S.; Kulkarni, Shrinivas R.; Perley, Daniel A.; Barlow, Tom; Horesh, Assaf; Gal-Yam, Avishay; Howell, D. A.; Dilday, Ben; PTF Collaboration; Evans, Phil A.; Kennea, Jamie A.; Swift Collaboration; Burgett, W. S.; Chambers, K. C.; Kaiser, N.; Waters, C.; Flewelling, H.; Tonry, J. L.; Rest, A.; Smartt, S. J.; Pan-STARRS1 Science Consortium

    2015-09-01

    The IceCube neutrino observatory pursues a follow-up program selecting interesting neutrino events in real-time and issuing alerts for electromagnetic follow-up observations. In 2012 March, the most significant neutrino alert during the first three years of operation was issued by IceCube. In the follow-up observations performed by the Palomar Transient Factory (PTF), a Type IIn supernova (SN IIn) PTF12csy was found 0.°2 away from the neutrino alert direction, with an error radius of 0.°54. It has a redshift of z = 0.0684, corresponding to a luminosity distance of about 300 Mpc and the Pan-STARRS1 survey shows that its explosion time was at least 158 days (in host galaxy rest frame) before the neutrino alert, so that a causal connection is unlikely. The a posteriori significance of the chance detection of both the neutrinos and the SN at any epoch is 2.2σ within IceCube's 2011/12 data acquisition season. Also, a complementary neutrino analysis reveals no long-term signal over the course of one year. Therefore, we consider the SN detection coincidental and the neutrinos uncorrelated to the SN. However, the SN is unusual and interesting by itself: it is luminous and energetic, bearing strong resemblance to the SN IIn 2010jl, and shows signs of interaction of the SN ejecta with a dense circumstellar medium. High-energy neutrino emission is expected in models of diffusive shock acceleration, but at a low, non-detectable level for this specific SN. In this paper, we describe the SN PTF12csy and present both the neutrino and electromagnetic data, as well as their analysis.

  7. The Sloan Digital Sky Survey-II Supernova Survey:Search Algorithm and Follow-up Observations

    SciTech Connect

    Sako, Masao; Bassett, Bruce; Becker, Andrew; Cinabro, David; DeJongh, Don Frederic; Depoy, D.L.; Doi, Mamoru; Garnavich, Peter M.; Craig, Hogan, J.; Holtzman, Jon; Jha, Saurabh; Konishi, Kohki; Lampeitl, Hubert; Marriner, John; Miknaitis, Gajus; Nichol, Robert C.; Prieto, Jose Luis; Richmond, Michael W.; Schneider, Donald P.; Smith, Mathew; SubbaRao, Mark; /Chicago U. /Tokyo U. /Tokyo U. /South African Astron. Observ. /Tokyo U. /Apache Point Observ. /Seoul Natl. U. /Apache Point Observ. /Apache Point Observ. /Tokyo U. /Seoul Natl. U. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ. /Apache Point Observ.

    2007-09-14

    The Sloan Digital Sky Survey-II Supernova Survey has identified a large number of new transient sources in a 300 deg2 region along the celestial equator during its first two seasons of a three-season campaign. Multi-band (ugriz) light curves were measured for most of the sources, which include solar system objects, Galactic variable stars, active galactic nuclei, supernovae (SNe), and other astronomical transients. The imaging survey is augmented by an extensive spectroscopic follow-up program to identify SNe, measure their redshifts, and study the physical conditions of the explosions and their environment through spectroscopic diagnostics. During the survey, light curves are rapidly evaluated to provide an initial photometric type of the SNe, and a selected sample of sources are targeted for spectroscopic observations. In the first two seasons, 476 sources were selected for spectroscopic observations, of which 403 were identified as SNe. For the Type Ia SNe, the main driver for the Survey, our photometric typing and targeting efficiency is 90%. Only 6% of the photometric SN Ia candidates were spectroscopically classified as non-SN Ia instead, and the remaining 4% resulted in low signal-to-noise, unclassified spectra. This paper describes the search algorithm and the software, and the real-time processing of the SDSS imaging data. We also present the details of the supernova candidate selection procedures and strategies for follow-up spectroscopic and imaging observations of the discovered sources.

  8. RoboNet-II: Follow-up observations of microlensing events with a robotic network of telescopes

    NASA Astrophysics Data System (ADS)

    Tsapras, Y.; Street, R.; Horne, K.; Snodgrass, C.; Dominik, M.; Allan, A.; Steele, I.; Bramich, D. M.; Saunders, E. S.; Rattenbury, N.; Mottram, C.; Fraser, S.; Clay, N.; Burgdorf, M.; Bode, M.; Lister, T. A.; Hawkins, E.; Beaulieu, J. P.; Fouqué, P.; Albrow, M.; Menzies, J.; Cassan, A.; Dominis-Prester, D.

    2009-01-01

    RoboNet-II uses a global network of robotic telescopes to perform follow-up observations of microlensing events in the Galactic Bulge. The current network consists of three 2 m telescopes located in Hawaii and Australia (owned by Las Cumbres Observatory) and the Canary Islands (owned by Liverpool John Moores University). In future years the network will be expanded by deploying clusters of 1 m telescopes in other suitable locations. A principal scientific aim of the RoboNet-II project is the detection of cool extra-solar planets by the method of gravitational microlensing. These detections will provide crucial constraints to models of planetary formation and orbital migration. RoboNet-II acts in coordination with the PLANET microlensing follow-up network and uses an optimization algorithm (``web-PLOP'') to select the targets and a distributed scheduling paradigm (eSTAR) to execute the observations. Continuous automated assessment of the observations and anomaly detection is provided by the ARTEMiS system.

  9. Four Years of Observations of GRB Localizations with TAROT

    SciTech Connect

    Boeer, M.; Thiebaud, C.; Atteia, J.-L.; Malina, R.; Freitas Pacheco, J. de; Pedersen, H.; Klotz, A

    2004-09-28

    We present a summary of the observations performed with the Telescope a Action Rapide pour les Objets Transitoires (TAROT - Rapid Action Telescope for Transient Objects) performed over the period 1999 - 2003. Seventeen GRB localization observations where performed shortly after the burst (10s - 90min.), and in at least one case, even while the source was still active in gamma-rays. During this period CGRO. HETE-2 and INTEGRAL were in operation. Though no alert was missed, no source was detected, to a magnitude limit between R = 15 and R = 20. Future plans are also presented, featuring the duplication of TAROT at ESO - La Silla.

  10. Observations of GRB 990123 by the Compton Gamma Ray Observatory

    NASA Technical Reports Server (NTRS)

    Briggs, M. S.; Band, D. L.; Kippen, R. M.; Preece, R. D.; Kouveliotou, C.; vanParadijs, J.; Share, G. H.; Murphy, R. J.; Matz, S. M.; Connors, A.

    1999-01-01

    GRB 990123 was the first burst from which simultaneous optical, X-ray, and gamma-ray emission was detected; its afterglow has been followed by an extensive set of radio, optical, and X-ray observations. We have studied the gamma-ray burst itself as observed by the Compton Gamma Ray Observatory detectors. We find that gamma-ray fluxes are not correlated with the simultaneous optical observations and that the gamma-ray spectra cannot be extrapolated simply to the optical fluxes. The burst is well fitted by the standard four-parameter GRB function, with the exception that excess emission compared with this function is observed below approx. 15 keV during some time intervals. The burst is characterized by the typical hard-to-soft and hardness-intensity correlation spectral evolution patterns. The energy of the peak of the vf (sub v), spectrum, E (sub p), reaches an unusually high value during the first intensity spike, 1470 plus or minus 110 keV, and then falls to approx. 300 keV during the tail of the burst. The high-energy spectrum above approx. 1 MeV is consistent with a power law with a photon index of about -3. By fluence, GRB 990123 is brighter than all but 0.4% of the GRBs observed with BATSE (Burst and Transient Source Experiment), clearly placing it on the -3/2 power-law portion of the intensity distribution. However, the redshift measured for the afterglow is inconsistent with the Euclidean interpretation of the -3/2 power law. Using the redshift value of greater than or equal to 1.61 and assuming isotropic emission, the gamma-ray energy exceeds 10 (exp 54) ergs.

  11. Radio observations of GRB 100418a: Test of an energy injection model explaining long-lasting GRB afterglows

    SciTech Connect

    Moin, A.; Wang, Z.; Chandra, P.; Miller-Jones, J. C. A.; Tingay, S. J.; Reynolds, C.; Taylor, G. B.; Frail, D. A.; Phillips, C. J.

    2013-12-20

    We present the results of our radio observational campaign of gamma-ray burst (GRB) 100418a, for which we used the Australia Telescope Compact Array, the Very Large Array, and the Very Long Baseline Array. GRB 100418a was a peculiar GRB with unusual X-ray and optical afterglow profiles featuring a plateau phase with a very shallow rise. This observed plateau phase was believed to be due to a continued energy injection mechanism that powered the forward shock, giving rise to an unusual and long-lasting afterglow. The radio afterglow of GRB 100418a was detectable several weeks after the prompt emission. We conducted long-term monitoring observations of the afterglow and attempted to test the energy injection model advocating that the continuous energy injection is due to shells of material moving at a wide range of Lorentz factors. We obtained an upper limit of γ < 7 for the expansion rate of the GRB 100418a radio afterglow, indicating that the range-of-Lorentz factor model could only be applicable for relatively slow-moving ejecta. A preferred explanation could be that continued activity of the central engine may have powered the long-lasting afterglow.

  12. Follow-up observations of Comet 17P/Holmes after its extreme outburst in brightness end of October 2007

    NASA Astrophysics Data System (ADS)

    Mugrauer, M.; Hohle, M. M.; Ginski, C.; Vanko, M.; Freistetter, F.

    2009-05-01

    We present follow-up observations of comet 17/P Holmes after its extreme outburst in brightness, which occurred end of October 2007. We obtained 58 V-band images of the comet between October 2007 and February 2008, using the Cassegrain-Teleskop-Kamera (CTK) at the University Observatory Jena. We present precise astrometry of the comet, which yields its most recent Keplerian orbital elements. Furthermore, we show that the comet's coma expands quite linearly with a velocity of about 1650 km/s between October and December 2007. The photometric monitoring of comet 17/P Holmes shows that its photometric activity level decreased by about 5.9 mag within 105 days after its outburst. Based on observations obtained with telescopes of the University Observatory Jena, which is operated by the Astrophysical Institute of the Friedrich-Schiller-University.

  13. INTEGRAL and XMM-Newton observations of GRB 040106

    NASA Astrophysics Data System (ADS)

    Moran, L.; Mereghetti, S.; Götz, D.; Hanlon, L.; von Kienlin, A.; McBreen, B.; Tiengo, A.; Preece, R.; Williams, O. R.; Bennett, K.; Kippen, R. M.; McBreen, S.; McGlynn, S.

    2005-03-01

    On January 6th 2004, the IBAS burst alert system triggered the 8th gamma-ray burst (GRB) to be located by the INTEGRAL satellite. The position was determined and publicly distributed within 12 s, prompting ESA's XMM-Newton to execute a ToO observation just 5 h later, during which an X-ray afterglow was detected. The GRB had a duration ~52 s with two distinct pulses separated by ~42 s. Here we present the results of imaging and spectral analyses of the prompt emission from INTEGRAL data and the X-ray afterglow from XMM-Newton data. The γ-ray spectrum is consistent with a single power-law of photon index -1.72 ± 0.15. The fluence (20-200 keV) was 8.2 × 10-7 erg cm-2. The X-ray afterglow (Fν(t) ∝ ν-β_X t-δ) was extremely hard with βX = 0.47 ± 0.01 and δ = 1.46 ± 0.04. The 2-10 keV flux 11 h after the burst was 1.1 × 10-12 erg cm-2 s-1. The time profile of the GRB is consistent with the observed trends from previous analysis of BATSE GRBs. We find that the X-ray data are not well-fit by either a simple spherical fireball or by a speading jet, expanding into a homogeneous medium or a wind environment. Based on previously determined correlations between GRB spectra and redshift, we estimate a redshift of ~0.9+0.5-0.4 (1σ) and a lower limit on the isotropic radiated energy of ~5 × 1051 erg in this burst. Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, Spain), Czech Republic and Poland, and with the participation of Russia and the USA.

  14. Ground-based Submm/mm Follow-up Observations For Wise Selected Hyper-luminous Galaxies

    NASA Astrophysics Data System (ADS)

    Wu, Jingwen; Tsai, C.; Benford, D.; Bridge, C.; Eisenhardt, P.; Blain, A.; Sayers, J.; Petty, S.; WISE Team

    2012-01-01

    One of the major objectives of NASA's Wide-field Infrared Survey Explorer (WISE) mission is to search for the most luminous galaxies in the universe. The most productive method so far to select hyper luminous galaxies from WISE is to select targets that undetectable by WISE at 3.4 and 4.6 microns, while clearly detected at 12 and 22 microns, the so called W12 dropout galaxies. We have used the Caltech Submillimeter Observatory to follow-up these high-z (z=1.6-4.6) galaxies with SHARC-II at 350 to 850 microns, and BOLOCAM at 1.1 mm. Based on Spitzer 3.3 and 4.7 microns follow-ups, WISE W3, W4, and CSO observations, we constructed the SEDs and estimate the infrared luminosity and dust temperature for these W12 dropout galaxies. The inferred infrared luminosities are at least 10^13 to 10^14 solar luminosities, making them one of the most luminous population. The typical SEDs of these galaxies are flat from mid-IR to submillimeter, peaking at shorter wavelengths than other infrared luminous galaxies, indicating hotter dust temperature than known populations. Their SEDs can not be well fitted with existing templates, suggesting they may be a distinct new population. They may be extreme cases of Dust-Obsecured Galaxies (DOGs) with very high luminosities and dust temperature, and tracing a short transiting phase with booming luminosity at the peak epoch of AGN/starburst galaxy evolution.

  15. Fermi-LAT Observations of the Gamma-Ray Burst GRB 130427A

    NASA Technical Reports Server (NTRS)

    Ackermann, M.; Ajello, M.; Asano, K.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Gehrels, Cornelis

    2013-01-01

    The observations of the exceptionally bright gamma-ray burst (GRB) 130427A by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope provide constraints on the nature of these unique astrophysical sources. GRB 130427A had the largest fluence, highest-energy photon (95 GeV), longest gamma-ray duration (20 hours), and one of the largest isotropic energy releases ever observed from a GRB. Temporal and spectral analyses of GRB 130427A challenge the widely accepted model that the nonthermal high-energy emission in the afterglow phase of GRBs is synchrotron emission radiated by electrons accelerated at an external shock.

  16. Fermi-LAT Observations of the Gamma-Ray Burst GRB 130427A

    NASA Astrophysics Data System (ADS)

    Ackermann, M.; Ajello, M.; Asano, K.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Bissaldi, E.; Bonamente, E.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Burgess, J. Michael; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Cecchi, C.; Chaplin, V.; Charles, E.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Chiaro, G.; Ciprini, S.; Claus, R.; Cleveland, W.; Cohen-Tanugi, J.; Collazzi, A.; Cominsky, L. R.; Connaughton, V.; Conrad, J.; Cutini, S.; D'Ammando, F.; de Angelis, A.; DeKlotz, M.; de Palma, F.; Dermer, C. D.; Desiante, R.; Diekmann, A.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Finke, J.; Fitzpatrick, G.; Focke, W. B.; Franckowiak, A.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gehrels, N.; Germani, S.; Gibby, M.; Giglietto, N.; Giles, M.; Giordano, F.; Giroletti, M.; Godfrey, G.; Granot, J.; Grenier, I. A.; Grove, J. E.; Gruber, D.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Horan, D.; Hughes, R. E.; Inoue, Y.; Jogler, T.; Jóhannesson, G.; Johnson, W. N.; Kawano, T.; Knödlseder, J.; Kocevski, D.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Mayer, M.; Mazziotta, M. N.; McEnery, J. E.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nemmen, R.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orienti, M.; Paneque, D.; Pelassa, V.; Perkins, J. S.; Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Pivato, G.; Porter, T. A.; Racusin, J. L.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Ritz, S.; Roth, M.; Ryde, F.; Sartori, A.; Parkinson, P. M. Saz; Scargle, J. D.; Schulz, A.; Sgrò, C.; Siskind, E. J.; Sonbas, E.; Spandre, G.; Spinelli, P.; Tajima, H.; Takahashi, H.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Tinivella, M.; Torres, D. F.; Tosti, G.; Troja, E.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Winer, B. L.; Wood, K. S.; Yamazaki, R.; Younes, G.; Yu, H.-F.; Zhu, S. J.; Bhat, P. N.; Briggs, M. S.; Byrne, D.; Foley, S.; Goldstein, A.; Jenke, P.; Kippen, R. M.; Kouveliotou, C.; McBreen, S.; Meegan, C.; Paciesas, W. S.; Preece, R.; Rau, A.; Tierney, D.; van der Horst, A. J.; von Kienlin, A.; Wilson-Hodge, C.; Xiong, S.; Cusumano, G.; La Parola, V.; Cummings, J. R.

    2014-01-01

    The observations of the exceptionally bright gamma-ray burst (GRB) 130427A by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope provide constraints on the nature of these unique astrophysical sources. GRB 130427A had the largest fluence, highest-energy photon (95 GeV), longest γ-ray duration (20 hours), and one of the largest isotropic energy releases ever observed from a GRB. Temporal and spectral analyses of GRB 130427A challenge the widely accepted model that the nonthermal high-energy emission in the afterglow phase of GRBs is synchrotron emission radiated by electrons accelerated at an external shock.

  17. GRB 050117: Simultaneous Gamma-ray and X-ray Observations with the Swift Satellite

    NASA Technical Reports Server (NTRS)

    Hill, J. E.; Morris, D. C.; Sakamoto, T.; Sato, G.; Burrows, D. N.; Angelini, L.; Pagani, C.; Moretti, A.; Abbey, A. F.; Barthelmy, S.

    2005-01-01

    The Swift Gamma-Ray Burst Explorer performed its first autonomous, X-ray follow-up to a newly detected GRB on 2005 January 17, within 193 seconds of the burst trigger by the Swift Burst Alert Telescope. While the burst was still in progress, the X-ray Telescope obtained a position and an image for an un-catalogued X-ray source; simultaneous with the gamma-ray observation. The XRT observed flux during the prompt emission was 1.1 x 10(exp -8) ergs/sq cm/s in the 0.5-10 keV energy band. The emission in the X-ray band decreased by three orders of magnitude within 700 seconds, following the prompt emission. This is found to be consistent with the gamma-ray decay when extrapolated into the XRT energy band. During the following 6.3 hours, the XRT observed the afterglow in an automated sequence for an additional 947 seconds, until the burst became fully obscured by the Earth limb. A faint, extremely slowly decaying afterglow, alpha=-0.21, was detected. Finally, a break in the lightcurve occurred and the flux decayed with alpha<-1.2. The X-ray position triggered many follow-up observations: no optical afterglow could be confirmed, although a candidate was identified 3 arcsecs from the XRT position.

  18. GRT: Goddard Robotic Telescope, Optical Follow-up of the GRBs and Optical Coordinated Observation of the AGNs

    NASA Astrophysics Data System (ADS)

    Okajima, Takashi; Sakamoto, T.; Donato, D.; Gehrels, N.; Ukwatta, T.; Urata, Y.

    2008-03-01

    We are constructing the 14" fully automated optical robotic telescope, Goddard Robotic Telescope (GRT), at the Goddard Geophysical and Astronomical Observatory. The aims of our robotic telescope is 1) to follow-up the Swift/GLAST GRBs and 2) to perform the coordinated optical observations of the GLAST AGNs. Our telescope system consists of the 14" Celestron OTA, the Astro-Physics 1200GTO mount, the Apogee U47 CCD camera, the JIM's electronic focuser, and the Finger Lake Instrumentation's color filter wheel with U, B, V, R, and I filters. With the focal reducer, 18' x 18' field of view has been achieved. The observatory dome is the Astro Haven's 7ft clam-shell dome. We will start the scientific observations on April 2008. While not observing our primary targets (GRBs and AGNs), we are planning to open our telescope time to the public for having a wider use of our telescope in both a different research field and an educational purpose.

  19. Follow-up spectroscopic observations of HD 107148 B: A new white dwarf companion of an exoplanet host star

    NASA Astrophysics Data System (ADS)

    Mugrauer, M.; Dinçel, B.

    2016-07-01

    We report on our follow-up spectroscopy of HD 1071478 B, a recently detected faint co-moving companion of the exoplanet host star HD 107148 A. The companion is separated from its primary star by about 35 arcsec (or 1790 AU of projected separation) and its optical and near infrared photometry is consistent with a white dwarf, located at the distance of HD 107148 A. In order to confirm the white dwarf nature of the co-moving companion, we obtained follow-up spectroscopic observations of HD 107148 B with CAFOS at the CAHA 2.2 m telescope. According to our CAFOS spectroscopy HD 107148 B is a DA white dwarf with an effective temperature in the range between 5900 and 6400 K. The properties of HD 107148 B can further be constrained with the derived effective temperature and the known visual and infrared photometry of the companion, using evolutionary models of DA white dwarfs. We obtain for HD 107148 B a mass of 0.56±0.05 M_⊙, a luminosity of (2.0±0.2)×10-4 L_⊙, log g [cm s-2])=7.95±0.09, and a cooling age of 2100±270 Myr. With its white dwarf companion the exoplanet host star HD 107148 A forms an evolved stellar system, which hosts at least one exoplanet. So far, only few of these evolved systems are known, which represent only about 5 % of all known exoplanet host multiple stellar systems. HD 107148 B is the second confirmed white dwarf companion of an exoplanet host star with a projected separation to its primary star of more than 1000 AU. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC).

  20. Follow-up spectroscopic observations of HD 107148 B: A new white dwarf companion of an exoplanet host star

    NASA Astrophysics Data System (ADS)

    Mugrauer, M.; Dinçel, B.

    2016-07-01

    We report on our follow-up spectroscopy of HD 1071478 B, a recently detected faint co-moving companion of the exoplanet host star HD 107148 A. The companion is separated from its primary star by about 35 arcsec (or 1790 AU of projected separation) and its optical and near infrared photometry is consistent with a white dwarf, located at the distance of HD 107148 A. In order to confirm the white dwarf nature of the co-moving companion, we obtained follow-up spectroscopic observations of HD 107148 B with CAFOS at the CAHA 2.2 m telescope. According to our CAFOS spectroscopy HD 107148 B is a DA white dwarf with an effective temperature in the range between 5900 and 6400 K. The properties of HD 107148 B can further be constrained with the derived effective temperature and the known visual and infrared photometry of the companion, using evolutionary models of DA white dwarfs. We obtain for HD 107148 B a mass of 0.56±0.05 M_ȯ, a luminosity of (2.0±0.2)×10-4 L_ȯ, log g [cm s-2])=7.95±0.09, and a cooling age of 2100±270 Myr. With its white dwarf companion the exoplanet host star HD 107148 A forms an evolved stellar system, which hosts at least one exoplanet. So far, only few of these evolved systems are known, which represent only about 5 % of all known exoplanet host multiple stellar systems. HD 107148 B is the second confirmed white dwarf companion of an exoplanet host star with a projected separation to its primary star of more than 1000 AU. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC).

  1. The status of the AGILE GRB observations and the noticeable case of GRB 080514B

    SciTech Connect

    Del Monte, E.; Costa, E.; Donnarumma, I.; Lapshov, I.; Lazzarotto, F.; Pacciani, L.; Soffitta, P.; Argan, A.; Feroci, M.; Pucella, G.; Trois, A.; Vittorini, V.; Evangelista, Y.; Fornari, F.; Giuliani, A.; Mereghetti, S.; Vercellone, S.; Caraveo, P.; Chen, A.; Pellizzoni, A.

    2009-05-25

    Since Summer 2007, the AGILE mission is successfully detecting and localizing Gamma Ray Bursts by using its wide-field hard X-ray monitor SuperAGILE (17-60 keV) and its CsI Minicalorimeter (0.3-20 MeV). Moreover, all the events with a known localization in the field of view of the Gamma Ray Imaging Detector are searched for in the 30 MeV-50 GeV energy range. Among the several bursts occurred in the field of view of the Gamma Ray Imaging Detector during more than one year of operations, at the time of writing the remarkable GRB 080514B is detected at high significance and GRB 080721 and GRB 081001 are detected at low significance. GRB 080514B is the first Gamma Ray Burst showing a significant emission above 20 MeV after EGRET, and the first ever associated with an afterglow, measured at X-rays and in the IR/Optical/UV. Significant upper limits are derived for the other GRBs. In this paper we report about the status and the scientific performances of the AGILE instrumentation in the study of GRBs and we discuss the properties of GRB 080514B in the context of the long Gamma Ray Bursts.

  2. ROSAT Imaging of GRB920525 and GRB930118

    NASA Technical Reports Server (NTRS)

    McNamara, Bernie

    1997-01-01

    For this effort we requested ROSAT images of two small gamma-ray burst (GRB) error boxes. Our goal was to search for sources that might be associated with the quiescent site of a GRB. More than 1000 GRBs have been detected in the twenty five years since their discovery, yet their origin remains a mystery. No real-time or quiescent counterparts at any wavelength have been identified as sources of GRBs despite considerable follow-up efforts. Ground based campaigns to examine GRB error boxes shortly after the bursts have revealed no transient, or highly variable objects at optical and radio wavelengths in the time period of more than 7 hours after the burst. Due to the heavy demand on X-ray satellite time, and the difficulty of re-scheduling observations, rapid follow-up observations at high energies have not been obtained as quickly as the ground based-efforts. In fact, X-ray images of GRB error boxes are normally obtained months-years after burst detection. The current fastest X-ray response time is over two weeks. Deep imaging of GRB error boxes at X-ray wavelengths is an additional observational approach that can be used to constrain models of the origin of GRBs. We combined the results of our investigation of the GRB920525 error box with that of a prior ROSAT PSPC observation of GRB910814 and submitted them for publication. We conclude that based upon our efforts and those of others, deep X-ray observations obtained long after the GRB are not likely to yield further productive results until smaller GRB error boxes become available. It may be possible to obtain such small error boxes in the near future from XTE, HETE and an augmented IPN.

  3. Gaia-FUN-SSO: a network for ground-based follow-up observations of Solar System Objects

    NASA Astrophysics Data System (ADS)

    Thuillot, W.; Carry, B.; Berthier, J.; David, P.; Hestroffer, D.; Rocher, P.

    2014-12-01

    Gaia-FUN-SSO (shortly described at https://www.imcce.fr/gaia-fun-sso/) is a ground-based network of observatories set up in the framework of the Gaia consortium (DPAC-CU4) for the follow-up of critical Solar System objects to be discovered from space by the Gaia satellite. Its goal is to retrieve from the ground a newly detected object and to complement the astrometry measurements carried out by Gaia to determine its heliocentric orbit. Data from both Gaia and the ground-based network will be sent to the Minor Planet Center, used to determine the orbit and thus to update the database of minor planet orbits, which is subsequently used by Gaia for the identification of moving objects. We are expecting the detection of many asteroids, mainly from the main belt, and also new near-Earth objects (NEO) at low solar elongation. Owing to the specific conditions of Gaia observations, we even expect the detection of objects whose orbit is fully contained within Earth's orbit (called inner-Earth or Atira asteroids). Several training campaigns have already been organized with the network and it is now able to enter in an operating mode when alerts will be triggered. We describe here the expected number of discoveries, the network, its activity, and the data processing of the central node of the network set in place for the operating mode.

  4. Low False Positive Rate of Kepler Candidates Estimated From A Combination Of Spitzer And Follow-Up Observations

    NASA Astrophysics Data System (ADS)

    Désert, Jean-Michel; Charbonneau, David; Torres, Guillermo; Fressin, François; Ballard, Sarah; Bryson, Stephen T.; Knutson, Heather A.; Batalha, Natalie M.; Borucki, William J.; Brown, Timothy M.; Deming, Drake; Ford, Eric B.; Fortney, Jonathan J.; Gilliland, Ronald L.; Latham, David W.; Seager, Sara

    2015-05-01

    NASA’s Kepler mission has provided several thousand transiting planet candidates during the 4 yr of its nominal mission, yet only a small subset of these candidates have been confirmed as true planets. Therefore, the most fundamental question about these candidates is the fraction of bona fide planets. Estimating the rate of false positives of the overall Kepler sample is necessary to derive the planet occurrence rate. We present the results from two large observational campaigns that were conducted with the Spitzer Space Telescope during the the Kepler mission. These observations are dedicated to estimating the false positive rate (FPR) among the Kepler candidates. We select a sub-sample of 51 candidates, spanning wide ranges in stellar, orbital, and planetary parameter space, and we observe their transits with Spitzer at 4.5 μm. We use these observations to measures the candidate’s transit depths and infrared magnitudes. An authentic planet produces an achromatic transit depth (neglecting the modest effect of limb darkening). Conversely a bandpass-dependent depth alerts us to the potential presence of a blending star that could be the source of the observed eclipse: a false positive scenario. For most of the candidates (85%), the transit depths measured with Kepler are consistent with the transit depths measured with Spitzer as expected for planetary objects, while we find that the most discrepant measurements are due to the presence of unresolved stars that dilute the photometry. The Spitzer constraints on their own yield FPRs between 5% and depending on the Kepler Objects of Interest. By considering the population of the Kepler field stars, and by combining follow-up observations (imaging) when available, we find that the overall FPR of our sample is low. The measured upper limit on the FPR of our sample is 8.8% at a confidence level of 3σ. This observational result, which uses the achromatic property of planetary transit signals that is not investigated

  5. Swift Observations of the X-Ray-Bright GRB 050315

    NASA Astrophysics Data System (ADS)

    Vaughan, S.; Goad, M. R.; Beardmore, A. P.; O'Brien, P. T.; Osborne, J. P.; Page, K. L.; Barthelmy, S. D.; Burrows, D. N.; Campana, S.; Cannizzo, J. K.; Capalbi, M.; Chincarini, G.; Cummings, J. R.; Cusumano, G.; Giommi, P.; Godet, O.; Hill, J. E.; Kobayashi, S.; Kumar, P.; La Parola, V.; Levan, A.; Mangano, V.; Mészáros, P.; Moretti, A.; Morris, D. C.; Nousek, J. A.; Pagani, C.; Palmer, D. M.; Racusin, J. L.; Romano, P.; Tagliaferri, G.; Zhang, B.; Gehrels, N.

    2006-02-01

    This paper discusses Swift observations of the γ-ray burst GRB 050315 (z=1.949) from 80 s to 10 days after the onset of the burst. The X-ray light curve displayed a steep early decay (t-5) for ~200 s and several breaks. However, both the prompt hard X-ray/γ-ray emission (observed by the BAT) and the first ~300 s of X-ray emission (observed by the XRT) can be explained by exponential decays, with similar decay constants. Extrapolating the BAT light curve into the XRT band suggests that the rapidly decaying, early X-ray emission was simply a continuation of the fading prompt emission; this strong similarity between the prompt γ-ray and early X-ray emission may be related to the simple temporal and spectral character of this X-ray-rich GRB. The prompt (BAT) spectrum was steep down to ~15 keV and appeared to continue through the XRT bandpass, implying a low peak energy, inconsistent with the Amati relation. Following the initial steep decline, the X-ray afterglow did not fade for ~1.2×104 s, after which time it decayed with a temporal index of α~0.7, followed by a second break at ~2.5×105 s to a slope of α~2. The apparent ``plateau'' in the X-ray light curve, after the early rapid decay, makes this one of the most extreme examples of the steep-flat-steep X-ray light curves revealed by Swift. If the second afterglow break is identified with a jet break, then the jet opening angle was θ0~5deg, implying Eγ>~1050 ergs.

  6. EARLY-TIME VLA OBSERVATIONS AND BROADBAND AFTERGLOW ANALYSIS OF THE FERMI/LAT DETECTED GRB 130907A

    SciTech Connect

    Veres, Péter; Corsi, Alessandra; Frail, Dale A.; Cenko, S. Bradley; Perley, Daniel A.

    2015-09-01

    We present multi-wavelength observations of the hyper-energetic gamma-ray burst (GRB) 130907A, a Swift-discovered burst with early radio observations starting at ≈4 hr after the γ-ray trigger. GRB 130907A was also detected by the Fermi/LAT instrument and at late times showed a strong spectral evolution in X-rays. We focus on the early-time radio observations, especially at >10 GHz, to attempt to identify reverse shock signatures. While our radio follow-up of GRB 130907A ranks among the earliest observations of a GRB with the Karl G. Jansky Very Large Array, we did not see an unambiguous signature of a reverse shock. While a model with both reverse and forward shock can correctly describe the observations, the data is not constraining enough to decide upon the presence of the reverse-shock component. We model the broadband data using a simple forward-shock synchrotron scenario with a transition from a wind environment to a constant density interstellar medium (ISM) in order to account for the observed features. Within the confines of this model, we also derive the underlying physical parameters of the fireball, which are within typical ranges except for the wind density parameter (A{sub *}), which is higher than those for bursts with wind-ISM transition, but typical for the general population of bursts. We note the importance of early-time radio observations of the afterglow (and of well-sampled light curves) for unambiguously identifying the potential contribution of the reverse shock.

  7. VI-Band Follow-Up Observations of Ultra-Long-Period Cepheid Candidates in M31

    NASA Astrophysics Data System (ADS)

    Ngeow, Chow-Choong; Lee, Chien-Hsiu; Ting-Chang Yang, Michael; Lin, Chi-Sheng; Hsiao, Hsiang-Yao; Cheng, Yu-Chi; Lin, Zhong-Yi; Lin, I.-Ling; Kanbur, Shashi M.; Ip, Wing-Huen

    2015-02-01

    The ultra-long-period Cepheids (ULPCs) are classical Cepheids with pulsation periods exceeding ≈ 80 days. The intrinsic brightness of ULPCs are ˜ 1 to ˜ 3 mag brighter than their shorter period counterparts. This makes them attractive in future distance scale work to derive distances beyond the limit set by the shorter period Cepheids. We have initiated a program to search for ULPCs in M31, using the single-band data taken from the Palomar Transient Factory, and identified eight possible candidates. In this work, we presented the VI-band follow-up observations of these eight candidates. Based on our VI-band light curves of these candidates and their locations in the color-magnitude diagram and the Period-Wesenheit diagram, we verify two candidates as being truly ULPCs. The six other candidates are most likely other kinds of long-period variables. With the two confirmed M31 ULPCs, we tested the applicability of ULPCs in distance scale work by deriving the distance modulus of M31. It was found to be {{μ }M31,ULPC}=24.30+/- 0.76 mag. The large error in the derived distance modulus, together with the large intrinsic dispersion of the Period-Wesenheit (PW) relation and the small number of ULPCs in a given host galaxy, means that the question of the suitability of ULPCs as standard candles is still open. Further work is needed to enlarge the sample of calibrating ULPCs and reduce the intrinsic dispersion of the PW relation before re-considering ULPCs as suitable distance indicators.

  8. VI-band follow-up observations of ultra-long-period Cepheid candidates in M31

    SciTech Connect

    Ngeow, Chow-Choong; Yang, Michael Ting-Chang; Lin, Chi-Sheng; Hsiao, Hsiang-Yao; Cheng, Yu-Chi; Lin, Zhong-Yi; Lin, I-Ling; Ip, Wing-Huen; Lee, Chien-Hsiu; Kanbur, Shashi M.

    2015-02-01

    The ultra-long-period Cepheids (ULPCs) are classical Cepheids with pulsation periods exceeding ≈80 days. The intrinsic brightness of ULPCs are ∼1 to ∼3 mag brighter than their shorter period counterparts. This makes them attractive in future distance scale work to derive distances beyond the limit set by the shorter period Cepheids. We have initiated a program to search for ULPCs in M31, using the single-band data taken from the Palomar Transient Factory, and identified eight possible candidates. In this work, we presented the VI-band follow-up observations of these eight candidates. Based on our VI-band light curves of these candidates and their locations in the color–magnitude diagram and the Period–Wesenheit diagram, we verify two candidates as being truly ULPCs. The six other candidates are most likely other kinds of long-period variables. With the two confirmed M31 ULPCs, we tested the applicability of ULPCs in distance scale work by deriving the distance modulus of M31. It was found to be μ{sub M31,ULPC}=24.30±0.76 mag. The large error in the derived distance modulus, together with the large intrinsic dispersion of the Period–Wesenheit (PW) relation and the small number of ULPCs in a given host galaxy, means that the question of the suitability of ULPCs as standard candles is still open. Further work is needed to enlarge the sample of calibrating ULPCs and reduce the intrinsic dispersion of the PW relation before re-considering ULPCs as suitable distance indicators.

  9. VizieR Online Data Catalog: Follow-up observations of SNIa ASASSN-14lp (Shappee+, 2016)

    NASA Astrophysics Data System (ADS)

    Shappee, B. J.; Piro, A. L.; Holoien, T.-S.; Prieto, J. L.; Contreras, C.; Itagaki, K.; Burns, C. R.; Kochanek, C. S.; Stanek, K. Z.; Alper, E.; Basu, U.; Beacom, J. F.; Bersier, D.; Brimacombe, J.; Conseil, E.; Danilet, A. B.; Dong, S.; Falco, E.; Grupe, D.; Hsiao, E. Y.; Kiyota, S.; Morrell, N.; Nicolas, J.; Phillips, M. M.; Pojmanski, G.; Simonian, G.; Stritzinger, M.; Szczygiel, D. M.; Taddia, F.; Thompson, T. A.; Thorstensen, J.; Wagner, M. R.; Wozniak, P. R.

    2016-09-01

    The All-sky Automated Survey for SuperNovae (ASAS-SN, or "Assassin"; Shappee et al. 2014ApJ...788...48S) scans the entire extragalactic sky in both the northern and southern hemispheres roughly once every 2-3 nights in the V band to depths of 16.5-17.3mag depending on lunation (Shappee et al. 2016, in preparation). We discovered a new source (ASASSN-14lp; V~14.9mag) on 2014 December 9.61 (JDtdisc=2457001.112) at RA=12:45:09.10, DE=-00:27:32.5 (J2000). There are no pre-explosion images of this site available in the Hubble Space Telescope (HST) Archive. Previous observations were obtained by ASAS-SN 1.25, 7.98, 10.98, 11.97, 15.96, and 18.96 days before discovery (see Table 1 and Figure 1 for details). The second set of prediscovery images were obtained by K. Itagaki from 2014 November 13 to 2015 January 09 at the Itagaki Astronomical Observatory, Japan. After the detection of ASASSN-14lp, we began a multiwavelength, ground- and space-based follow-up campaign from the X-ray to the near-infrared (NIR) wavelengths. Swift/UVOT observations were obtained in V (5468Å), B (4392Å), U (3465Å), UVW1 (2600Å), UVM2 (2246Å), and UVW2 (1928Å). These observations span more than 30days. Optical ground-based images were obtained with the LCOGT 1m network of telescopes (gri), the 2m Liverpool telescope (LT) (gri), and the 40-inch Swope telescope (ugri) as part of the Carnegie Supernova Project II (CSPII; Hsiao et al. 2013ApJ...766...72H). We obtained an extensive sample of low- and medium-resolution optical spectra of ASASSN-14lp spanning more than 3 months between 2014 December 10 and 2015 March 16 (see table 2). (2 data files).

  10. Homeopathic treatment of patients with chronic sinusitis: A prospective observational study with 8 years follow-up

    PubMed Central

    Witt, Claudia M; Lüdtke, Rainer; Willich, Stefan N

    2009-01-01

    Background An evaluation of homeopathic treatment and the outcomes in patients suffering from sinusitis for ≥12 weeks in a usual care situation. Methods Subgroup analysis including all patients with chronic sinusitis (ICD-9: 473.9; ≥12 weeks duration) of a large prospective multicentre observational study population. Consecutive patients presenting for homeopathic treatment were followed-up for 2 years, and complaint severity, health-related quality of life (QoL), and medication use were regularly recorded. We also present here patient-reported health status 8 years post initial treatment. Results The study included 134 adults (mean age 39.8 ± 10.4 years, 76.1% women), treated by 62 physicians. Patients had suffered from chronic sinusitis for 10.7 ± 9.8 years. Almost all patients (97.0%) had previously been treated with conventional medicine. For sinusitis, effect size (effect divided by standard deviation at baseline) of complaint severity was 1.58 (95% CI 1.77; 1.40), 2.15 (2.38; 1.92), and 2.43 (2.68; 2.18) at 3, 12, and 24 months respectively. QoL improved accordingly, with SF-36 changes in physical component score 0.27 (0.15; 0.39), 0.35 (0.19; 0.52), 0.44 (0.23; 0.65) and mental component score 0.66 (0.49; 0.84), 0.71 (0.50; 0.92), 0.65 (0.39; 0.92), 0.74 (0.49; 1.00) at these points. The effects were still present after 8 years with SF-36 physical component score 0.38 (0.10; 0.65) and mental component score 0.74 (0.49; 1.00). Conclusion This observational study showed relevant improvements that persisted for 8 years in patients seeking homeopathic treatment because of sinusitis. The extent to which the observed effects are due to the life-style regulation and placebo or context effects associated with the treatment needs clarification in future explanatory studies. PMID:19635154

  11. Spectral lag features of GRB 060814 from swift bat and Suzaku observations

    SciTech Connect

    Roychoudhury, Arundhati; Sarkar, Samir K.; Bhadra, Arunava E-mail: samirksarkar@rediffmail.com

    2014-02-20

    This work reports a study on the spectral lag of the prompt emission spectrum of a multi-pulse gamma-ray burst (GRB) GRB 060814 (z = 0.84) using the observations of the Swift Burst Alert Telescope and the Suzaku Wide Area Monitor. We found that the spectral lag for GRB 060814 is positive for the first two and the fourth pulses, while the third pulse exhibits negative lag. However, the time variation of the E {sub peak} of all the stated pulses shows a similar trend. The leading models for spectral lags in GRBs are thus found inadequate to explain the observed spectral lag features of GRB 060814. Probable causes of the spectral lag characteristics of GRB 060814 are discussed.

  12. Implications for the Origin of GRB 070201 from LIGO Observations

    NASA Astrophysics Data System (ADS)

    Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith, P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain, M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.; Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.; Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue, L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington, A.; Bunkowski, A.; Buonanno, A.; Burmeister, O.; Busby, D.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas, L.; Castaldi, G.; Cepeda, C.; Chalkley, E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini, F.; Christensen, N.; Clark, J.; Cochrane, P.; Cokelaer, T.; Coldwell, R.; Conte, R.; Cook, D.; Corbitt, T.; Coyne, D.; Creighton, J. D. E.; Croce, R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; DeBra, D.; Degallaix, J.; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandhar, S.; Díaz, M.; Dickson, J.; Di Credico, A.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.; Dumas, J.-C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.; Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.; Goggin, L. M.; González, G.; Gossler, S.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer, D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito, M.; Itoh, Y.; Ivanov, A.; Johnson, B.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim, C.; King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leiner, J.; Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.; Longo, M.; Lormand, M.; Lubinski, M.; Lück, H.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.; Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason, K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McWilliams, S.; Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger, C. J.; Meyers, D.; Mikhailov, E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi, K.; MowLowry, C.; Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.; Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton, G.; Nishizawa, A.; Numata, K.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi, M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab, F.; Rabeling, D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Ramsunder, M.; Ray-Majumder, S.; Re, V.; Rehbein, H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi, M.; Sancho de la Jordana, L.; Sandberg, V.; Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.; Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K.-X.; Sung, M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Taylor, R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; Van Den Broeck, C.; Varvella, M.; Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.; Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M.; zur Mühlen, H.; Zweizig, J.; LIGO Scientific Collaboration; Hurley, K. C.

    2008-07-01

    We analyzed the available LIGO data coincident with GRB 070201, a short-duration, hard-spectrum γ-ray burst (GRB) whose electromagnetically determined sky position is coincident with the spiral arms of the Andromeda galaxy (M31). Possible progenitors of such short, hard GRBs include mergers of neutron stars or a neutron star and a black hole, or soft γ-ray repeater (SGR) flares. These events can be accompanied by gravitational-wave emission. No plausible gravitational-wave candidates were found within a 180 s long window around the time of GRB 070201. This result implies that a compact binary progenitor of GRB 070201, with masses in the range 1 M⊙ < m1 < 3 M⊙ and 1 M⊙ < m2 < 40 M⊙, located in M31 is excluded at >99% confidence. If the GRB 070201 progenitor was not in M31, then we can exclude a binary neutron star merger progenitor with distance D < 3.5 Mpc, assuming random inclination, at 90% confidence. The result also implies that an unmodeled gravitational-wave burst from GRB 070201 most probably emitted less than 4.4 × 10-4 M⊙c2 (7.9 × 1050 ergs) in any 100 ms long period within the signal region if the source was in M31 and radiated isotropically at the same frequency as LIGO's peak sensitivity (f ≈ 150 Hz). This upper limit does not exclude current models of SGRs at the M31 distance.

  13. LATE-TIME OBSERVATIONS OF GRB 080319B: JET BREAK, HOST GALAXY, AND ACCOMPANYING SUPERNOVA

    SciTech Connect

    Tanvir, N. R.; O'Brien, P. T.; Wiersema, K.; Starling, R. L. C.; Rol, E.; Levan, A. J.; Svensson, K.; Fruchter, A. S.; Granot, J.; Jakobsson, P.; Fynbo, J.; Hjorth, J.; Curran, P. A.; Burrows, D. N.; Genet, F.

    2010-12-10

    The Swift-discovered GRB 080319B was by far the most distant source ever observed at naked-eye brightness, reaching a peak apparent magnitude of 5.3 at a redshift of z = 0.937. We present our late-time optical (Hubble Space Telescope, Gemini, and Very Large Telescope) and X-ray (Chandra) observations, which confirm that an achromatic break occurred in the power-law afterglow light curve at {approx}11 days post-burst. This most likely indicates that the gamma-ray burst (GRB) outflow was collimated, which for a uniform jet would imply a total energy in the jet E{sub jet} {approx}> 10{sup 52} erg. Our observations also show a late-time excess of red light, which is well explained if the GRB was accompanied by a supernova (SN), similar to those seen in some other long-duration GRBs. The latest observations are dominated by light from the host and show that the GRB took place in a faint dwarf galaxy (r(AB) {approx} 27.0, rest frame M{sub B} {approx} -17.2). This galaxy is small even by the standards of other GRB hosts, which is suggestive of a low-metallicity environment. Intriguingly, the properties of this extreme event-a small host and bright SN-are entirely typical of the very low luminosity bursts such as GRB 980425 and GRB 060218.

  14. Late-time Observations of GRB 080319B: Jet Break, Host Galaxy, and Accompanying Supernova

    NASA Astrophysics Data System (ADS)

    Tanvir, N. R.; Rol, E.; Levan, A. J.; Svensson, K.; Fruchter, A. S.; Granot, J.; O'Brien, P. T.; Wiersema, K.; Starling, R. L. C.; Jakobsson, P.; Fynbo, J.; Hjorth, J.; Curran, P. A.; van der Horst, A. J.; Kouveliotou, C.; Racusin, J. L.; Burrows, D. N.; Genet, F.

    2010-12-01

    The Swift-discovered GRB 080319B was by far the most distant source ever observed at naked-eye brightness, reaching a peak apparent magnitude of 5.3 at a redshift of z = 0.937. We present our late-time optical (Hubble Space Telescope, Gemini, and Very Large Telescope) and X-ray (Chandra) observations, which confirm that an achromatic break occurred in the power-law afterglow light curve at ~11 days post-burst. This most likely indicates that the gamma-ray burst (GRB) outflow was collimated, which for a uniform jet would imply a total energy in the jet E jet >~ 1052 erg. Our observations also show a late-time excess of red light, which is well explained if the GRB was accompanied by a supernova (SN), similar to those seen in some other long-duration GRBs. The latest observations are dominated by light from the host and show that the GRB took place in a faint dwarf galaxy (r(AB) ≈ 27.0, rest frame MB ≈ -17.2). This galaxy is small even by the standards of other GRB hosts, which is suggestive of a low-metallicity environment. Intriguingly, the properties of this extreme event—a small host and bright SN—are entirely typical of the very low luminosity bursts such as GRB 980425 and GRB 060218.

  15. The Wasilewski sample of emission-line galaxies - Follow-up CCD imaging and spectroscopic and IRAS observations

    NASA Technical Reports Server (NTRS)

    Bothun, Gregory D.; Schmitz, Mark; Halpern, Jules P.; Lonsdale, Carol J.; Impey, Chris

    1989-01-01

    The results of an extensive imaging and spectroscopic follow-up of the objective prism-selected emission line galaxy (ELG) sample of Wasilewski (1982) are presented. Fluxes at 12, 25, 60, and 100 microns were also obtained from the coadded IRAS survey data. ELGs found by objective prism surveys are found to be generally small and underluminous galaxies which usually have higher than average optical surface brightness. The Seyfert detection rate in objective prism surveys is roughly 10 percent and the ratio of the space densities of Seyfert 2 to Seyfert 1 galaxies is significantly larger than unity. Most of the galaxies selected by objective prism surveys are star-forming, late-type spirals which often show disturbed morphology. About 25 percent of the galaxies detected by the surveys are faint, high-excitation metal-poor compact H II regions.

  16. Risk factors for long-term posttraumatic stress reactions in unarmed UN military observers: a four-year follow-up study.

    PubMed

    Mehlum, Lars; Koldsland, Bjorn O; Loeb, Mitchell E

    2006-10-01

    Follow-up data from 187 male Norwegian veteran officers from unarmed UN military observer missions were compared with follow-up data from 211 male veteran officers from Norwegian contingents of the UNIFIL peacekeeping mission in South Lebanon on stress exposure, posttraumatic stress symptoms, level of alcohol consumption, and problems with social adaptation after redeployment from the mission. Observer mission veterans reported exposure to significantly higher levels of war zone stressors than veterans from peacekeeping units did. Observer veterans also reported significantly more posttraumatic stress symptoms at follow-up, higher alcohol consumption levels during service and at follow-up, and more problems with social adaptation to their lives at home in the years after their UN military service. All of these difficulties were most prominent in observers having served in missions with high-intensity stress exposure. Multivariate analyses demonstrated stress exposure during the mission and problems with social adaptation after homecoming to predict posttraumatic stress symptoms at follow-up. PMID:17041295

  17. Implications for the Origin of GRB 070201 from LIGO Observations

    SciTech Connect

    Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Anderson, S. B.; Araya, M.; Armandula, H.; Ballmer, S.; Barish, B. C.; Ajith, P.; Allen, B.; Amin, R.; Anderson, W. G.; Arain, M.; Ashley, M.; Aston, S.; Aufmuth, P.; Aulbert, C.; Babak, S.; Bantilan, H.

    2008-07-10

    We analyzed the available LIGO data coincident with GRB 070201, a short-duration, hard-spectrum {gamma}-ray burst (GRB) whose electromagnetically determined sky position is coincident with the spiral arms of the Andromeda galaxy (M31). Possible progenitors of such short, hard GRBs include mergers of neutron stars or a neutron star and a black hole, or soft {gamma}-ray repeater (SGR) flares. These events can be accompanied by gravitational-wave emission. No plausible gravitational-wave candidates were found within a 180 s long window around the time of GRB 070201. This result implies that a compact binary progenitor of GRB 070201, with masses in the range 1 M{sub sun} < m{sub 1} < 3 M{sub sun} and 1 M{sub sun} < m{sub 2} < 40 M{sub sun}, located in M31 is excluded at >99% confidence. If the GRB 070201 progenitor was not in M31, then we can exclude a binary neutron star merger progenitor with distance D < 3.5 Mpc, assuming random inclination, at 90% confidence. The result also implies that an unmodeled gravitational-wave burst from GRB 070201 most probably emitted less than 4.4 x 10{sup -4} M{sub sun}c{sup 2} (7.9 x 10{sup 50} ergs) in any 100 ms long period within the signal region if the source was in M31 and radiated isotropically at the same frequency as LIGO's peak sensitivity (f {approx} 150 Hz). This upper limit does not exclude current models of SGRs at the M31 distance.

  18. Probing a Gamma-Ray Burst Progenitor at a Redshift of z = 2: A Comprehensive Observing Campaign Campaign of the Afterglow of GRB 030226

    NASA Technical Reports Server (NTRS)

    Klose, S.; Greiner, J.; Rau, A.; Henden, A. A.; Hartmann, D. H.; Zeh, A.; Ries, C.; Masetti, N.; Malesani, D.; Guenther, E.

    2004-01-01

    We report results from a comprehensive follow-up observing campaign of the afterglow of GRB 030226 including VLT spectroscopy, VLT polarimetry, and Chandra X-ray observations. In addition, we present BOOTES-1 wide-field observations at the time of the occurrence of the burst. First observations at ESO started 0.2 days after the event when the gamma ray burst (GRB) afterglow was at a magnitude of R approximately 19 and continued until the afterglow had faded below the detection threshold (R greater than 26). No underlying host galaxy was found. The optical light curve shows a break around 0.8 days after the burst, which is achromatic within the observational errors, supporting the view that it was due to a jetted explosion. Close to the break time the degree of linear polarization of the afterglow light was less than 1.1%, which favors a uniform-jet model rather than a structured one. VLT spectra show two absorption line systems at redshifts z = 1.962 plus or minus 0.001 and 1.986 plus or minus 0.001, placing the lower limit for the redshift of the GRB close to 2. We emphasize that the kinematics and the composition of the absorbing clouds responsible for these line systems are very similar to those observed in the afterglow of GRB 021004. This corroborates the picture in which at least some GRBs are physically related to the explosion of a Wolf-Rayet star.

  19. Fermi Observations of High-energy Gamma-ray Emission from GRB 080825C

    NASA Astrophysics Data System (ADS)

    Abdo, A. A.; Ackermann, M.; Asano, K.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Band, D. L.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cecchi, C.; Chaplin, V.; Chekhtman, A.; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Cominsky, L. R.; Connaughton, V.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Gibby, L.; Giebels, B.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Goldstein, A.; Granot, J.; Grenier, I. A.; Grondin, M.-H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kerr, M.; Knödlseder, J.; Kocevski, D.; Komin, N.; Kouveliotou, C.; Kuehn, F.; Kuss, M.; Latronico, L.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McBreen, S.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Preece, R.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, O.; Reposeur, T.; Ritz, S.; Rochester, L. S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F.-W.; Sanchez, D.; Sander, A.; Saz Parkinson, P. M.; Scargle, J. D.; Sgrò, C.; Siskind, E. J.; Smith, D. A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T. L.; van der Horst, A. J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.

    2009-12-01

    The Fermi Gamma-ray Space Telescope has opened a new high-energy window in the study of gamma-ray bursts (GRBs). Here we present a thorough analysis of GRB 080825C, which triggered the Fermi Gamma-ray Burst Monitor (GBM), and was the first firm detection of a GRB by the Fermi Large Area Telescope (LAT). We discuss the LAT event selections, background estimation, significance calculations, and localization for Fermi GRBs in general and GRB 080825C in particular. We show the results of temporal and time-resolved spectral analysis of the GBM and LAT data. We also present some theoretical interpretation of GRB 080825C observations as well as some common features observed in other LAT GRBs.

  20. Agomelatine versus Sertraline: An Observational, Open-labeled and 12 Weeks Follow-up Study on Efficacy and Tolerability

    PubMed Central

    Akpınar, Esma; Cerit, Cem; Talas, Anıl; Tural, Ümit

    2016-01-01

    Objective In this open-labeled, 12 weeks follow-up study, we aimed to compare the efficacy and tolerability of agomelatine with sertraline Methods The outpatients of adult psychiatry clinic who have a new onset of depression and diagnosed as ‘major depressive episode’ by clinician according to the Diagnostic and Statistical Manual of Mental Disorders 4th edition and prescribed agomelatine (25 mg/day) or sertraline (50 mg/day) were included in the study. Results The decline of mean Montgomery-Asberg Depression Rating Scale (MADRS) scores of agomelatine group was significantly higher than the sertraline group at the end of 2nd week; however, the difference was not significant at the end of 3 months. Mean Clinical Global Impression-Improvement scale (CGI-I) scores of agomelatine group was lower than sertraline group at first week. Mean CGI-Severity scale and CGI-I scores were favour to sertraline group at the end of the study. Remission rates were 46.7% for sertraline group and 33.3% for agomelatine group while response rates were 76.7% for both groups. Any patient from agomelatine group dropped-out due to adverse effects. The amount of side effects was also less with agomelatine. Conclusion Agomelatine has a rapid onset efficacy on depressive symptoms and this can be beneficial for some critical cases. Considering MADRS scores, agomelatine seems to have similar efficacy with sertraline but we also point the need for long term studies since CGI scores were favour to sertraline group at the end of the study. Agomelatine has a favourable tolerability profile both in terms of discontinuation and the amount of side effects compared to sertraline. PMID:27776387

  1. Follow-up Observations and Analysis of V530 Andromedae: A Totally Eclipsing Shallow Contact Solar Type Binary

    NASA Astrophysics Data System (ADS)

    Chamberlain, Heather; Samec, Ronald G.; Caton, Daniel B.; Faulkner, Danny R.; Clark, Jeremy; Shebs, Travis

    2015-01-01

    We follow up on early, single coverage, UBVRcIc light curves (2013) and analyses. These early curves were taken in September 27 and 29 2011. Our present, BVRcIc, but full coverage light curves were taken on 6 nights: October 1,2,9, November 4,5, 2013 and January 4, 2014 by RGS, DBC, JDC, TS with the Dark Sky Observatory 0.81-m reflector of Appalachian State University and a (-40ºC) 2KX2K Apogee Alta CCD. Our present curves reveal V530 Andromedae as a totally eclipsing, shallow contact solar type binary rather than semidetached, near contact one. The newly determined times of minima include:HJD MinI = 2456566.84275 ±0.00007HJD MinII = 2456598.881995±0.0004, 24556600.6111±0.0002, 2456601.76665±0.00046.Using a new method of obtaining minima from earlier patrol light curves, in this case, NSVS, nine low weight timings of minimum light were added to the period study. Including these additional timings, we uncovered a period change. In our now, extended, period study over 9000 epochs, a 14.25 year interval, we find that the period is decreasing. This fits the scenario of magnetic breaking for solar type binaries. The temperatures of the primary and secondary components are estimated at 7000 and 6300 K, respectively, a large temperature difference for a contact binary. The fill-out, however, is a mere 4%. (Our earlier scant light curves modeled very nearly in contact.) The mass ratio, M2/M1, was found to be 0.385, almost identical with our first curves solution. The two star spots, probably magnetic in origin, were determined. A hot spot was modeled by the iterative process on the polar region of the smaller star. A cool spot is on the larger star facing the smaller star. The spot parameters have changed appreciably over the course of the two intervening years. We believe the binary has recently come into contact and thermal contact has not yet been achieved.

  2. Optical polarimetric observations of GRB prompt emissions by MASTER robots-telescopes net.

    NASA Astrophysics Data System (ADS)

    Gorbovskoy, Evgeny; Lipunov, Vladimir; Kornilov, Victor; Shatskij, Nikolaj; Kuvshi-Nov, Dmitry; Tyurina, Nataly; Belinski, Alexander; Krylov, Alexander; Balanutsa, Pavel; Chazov, Vadim; Kuznetsov, Artem; Zimnuhov, Dmitry; Balanutsa, Pavel; Kortunov, Petr; Sankovich, Anatoly; Tlatov, An-Drey; Parkhomenko, A.; Krushinsky, Vadim; Zalozhnyh, Ivan; Popov, A.; Kopytova, Taisia; Ivanov, Kirill; Yazev, Sergey; Yurkov, Vladimir

    The main goal of the MASTER-Net project is to produce a unique fast sky survey with all sky observed over a single night down to a limiting magnitude of 19 -20mag. Such a survey will make it possible to address a number of fundamental problems: search for dark energy via the discovery and photometry of supernovas (including SNIa), search for exoplanets, microlensing effects, discovery of minor bodies in the Solar System and space-junk monitoring. All MASTER telescopes can be guided by alerts, and we plan to observe prompt optical emission from gamma-ray bursts synchronously in several filters and in several polarization planes. Observations on telescopes capable to observ polarisation of GRB prompt emission have been begun in the summer of 2009. Since summer of 2009 an observations of several GRB have been made. In particular for GRB0910 and GRB091127 optical polarisation has been measured. So, for GRB091127 which supervision have begun all through 91 sec polarisation at level of several tens percent has been registered. (GCN 10231, GCN 10052, GCN 10203)

  3. Adaptive Optics and planned HST follow-up observations of the strongly lensed SNIa iPTF16geu

    NASA Astrophysics Data System (ADS)

    Goobar, Ariel; Amanullah, Rahman; Kulkarni, Shri; Steidel, Charles; Law, David

    2016-10-01

    Adaptive optics (AO) observations of iPTF16geu (ATel #9603) were carried out on October 11 with NACO in Natural Guide Star (NGS) mode on VLT. A bright star 30" SE of the SN position provided for the AO corrections.

  4. OPTICAL SPECTROSCOPIC OBSERVATIONS OF GAMMA-RAY BLAZAR CANDIDATES. IV. RESULTS OF THE 2014 FOLLOW-UP CAMPAIGN

    SciTech Connect

    Ricci, F.; Massaro, F.; Landoni, M.; D’Abrusco, R.; Milisavljevic, D.; Paggi, A.; Smith, Howard A.; Stern, D.; Masetti, N.; Tosti, G.

    2015-05-15

    The extragalactic γ-ray sky is dominated by the emission arising from blazars, one of the most peculiar classes of radio-loud active galaxies. Since the launch of Fermi several methods were developed to search for blazars as potential counterparts of unidentified γ-ray sources (UGSs). To confirm the nature of the selected candidates, optical spectroscopic observations are necessary. In 2013 we started a spectroscopic campaign to investigate γ-ray blazar candidates selected according to different procedures. The main goals of our campaign are: (1) to confirm the nature of these candidates, and (2) whenever possible, determine their redshifts. Optical spectroscopic observations will also permit us to verify the robustness of the proposed associations and check for the presence of possible source class contaminants to our counterpart selection. This paper reports the results of observations carried out in 2014 in the northern hemisphere with Kitt Peak National Observatory and in the southern hemisphere with the Southern Astrophysical Research telescopes. We also report three sources observed with the Magellan and Palomar telescopes. Our selection of blazar-like sources that could be potential counterparts of UGSs is based on their peculiar infrared colors and on their combination with radio observations both at high and low frequencies (i.e., above and below ∼1 GHz) in publicly available large radio surveys. We present the optical spectra of 27 objects. We confirm the blazar-like nature of nine sources that appear to be potential low-energy counterparts of UGSs. Then we present new spectroscopic observations of 10 active galaxies of uncertain type associated with Fermi sources, classifying all of them as blazars. In addition, we present the spectra for five known γ-ray blazars with uncertain redshift estimates and three BL Lac candidates that were observed during our campaign. We also report the case for WISE J173052.85−035247.2, candidate counterpart of the

  5. Swift Follow up observation of the transient source Fermi J1654-1055 (PMN J1632-1052)

    NASA Astrophysics Data System (ADS)

    Ajello, M.; Kocevski, D.; Buson, S.; Buehler, R.; Giomi, M.

    2016-02-01

    On February 25, 2016, Swift carried out a 2ks target of opportunity observation of the transient Fermi J1654-1055 (see ATel #8721). Only one source is clearly detected, within the LAT error circle, by the Swift X-ray telescope (XRT) at RA, Dec= 16h 32m 49.9s, -10d 52' 30.1" (J2000) with a 90 % uncertainty radius of 6.3 arcsec.

  6. Ground-Based BVRI Time-Series Follow-Up Observations for the RR Lyrae stars in Kepler Field

    NASA Astrophysics Data System (ADS)

    Jeon, Young-Beom; Ngeow, Chow-Choong; Nemec, James M.

    2015-09-01

    Time series observations for the 41 RR Lyrae stars in Kepler's fields were carried out in 2010 to 2013 using a number of meter class (or smaller) telescopes. These telescopes include the 1-m and 41-cm telescopes of Lulin Observatory (LOT and SLT respectively, Taiwan), the 81-cm telescope of Tenagra-II Observatory (TNG, Arizona, USA), the 1-m telescope at the Mt. Lemmon Optical Astronomy Observatory (LOAO, Arizona, USA), the 1.8-m and 15-cm telescopes at the Bohyunsan Optical Astronomy Observatory (BOAO, Korea), and the 61-cm telescope at the Sobaeksan Optical Astronomy Observatory (SOAO, Korea). All of these telescopes were equipped with commercial available CCD imagers, and the observations were done in standard BVRI filters. Photometric calibration of the RR Lyrae light curves was done with standard stars listed in Landolt standard stars [1]. Observations of selected Landolt standard stars (centered on SA 107-456 & SA 110-232) in Johnson-Kron-Cousins BVRI filters, spanning three distinct airmasses, were done with the 81-cm Tenagra II telescope on 25 June 2011. Raw imaging data were reduced with IRAF in the same manner as in the case of the RR Lyrae, and astrometric calibrated with astrometry.net [2]. We calibrated BVRI magnitudes for 40 RR Lyrae stars.

  7. Follow-up observations of the Crab pulsar with MAGIC and re-analysis of archival data

    NASA Astrophysics Data System (ADS)

    Saito, T. Y.; Dazzi, F.; Giavitto, G.; Hirotani, K.; Klepser, S.; Lopez, M.; Nakajima, D.; Schweizer, T.; Zanin, R.; MAGIC Collaboration

    2012-12-01

    The discovery of the extension of the Crab pulsar spectrum up to 400 GeV has challenged conventional pulsar theories and led to generation of new ones. In order to verify or rule out these new models, one would need to reduce the systematic and statistical errors in the spectra and light curves at these energies. For this reason, MAGIC is working on the upgrade of its telescopes and the improvement of the analysis methods. We report on the future prospects of the re-analysis of archival data and the observations with the upgraded system.

  8. Constraining GRB as Source for UHE Cosmic Rays through Neutrino Observations

    NASA Astrophysics Data System (ADS)

    Chen, P.

    2013-07-01

    The origin of ultra-high energy cosmic rays (UHECR) has been widely regarded as one of the major questions in the frontiers of particle astrophysics. Gamma ray bursts (GRB), the most violent explosions in the universe second only to the Big Bang, have been a popular candidate site for UHECR productions. The recent IceCube report on the non-observation of GRB induced neutrinos therefore attracts wide attention. This dilemma requires a resolution: either the assumption of GRB as UHECR accelerator is to be abandoned or the expected GRB induced neutrino yield was wrong. It has been pointed out that IceCube has overestimated the neutrino flux at GRB site by a factor of ~5. In this paper we point out that, in addition to the issue of neutrino production at source, the neutrino oscillation and the possible neutrino decay during their flight from GRB to Earth should further reduce the detectability of IceCube, which is most sensitive to the muon-neutrino flavor as far as point-source identification is concerned. Specifically, neutrino oscillation will reduce the muon-neutrino flavor ratio from 2/3 per neutrino at GRB source to 1/3 on Earth, while neutrino decay, if exists and under the assumption of normal hierarchy of mass eigenstates, would result in a further reduction of muon-neutrino ratio to 1/8. With these in mind, we note that there have been efforts in recent years in pursuing other type of neutrino telescopes based on Askaryan effect, which can in principle observe and distinguish all three flavors with comparable sensitivities. Such new approach may therefore be complementary to IceCube in shedding more lights on this cosmic accelerator question.

  9. Automated rapid follow-up of Swift gamma-ray burst alerts at 15 GHz with the AMI Large Array

    NASA Astrophysics Data System (ADS)

    Staley, T. D.; Titterington, D. J.; Fender, R. P.; Swinbank, J. D.; van der Horst, A. J.; Rowlinson, A.; Scaife, A. M. M.; Grainge, K. J. B.; Pooley, G. G.

    2013-02-01

    We present 15-GHz follow-up radio observations of 11 Swift gamma-ray burst (GRB) sources, obtained with the Arcminute Microkelvin Imager Large Array (AMI-LA). The initial follow-up observation for each source was made in a fully automated fashion; as a result four observations were initiated within 5 min of the GRB alert time stamp. These observations provide the first millijansky-level constraints on prolonged radio emission from GRBs within the first hour post-burst. While no radio emission within the first six hours after the GRB is detected in this preliminary analysis, radio afterglow is detected from one of the GRBs (GRB 120326A) on a time-scale of days. The observations were made as part of an ongoing programme to use AMI-LA as a systematic follow-up tool for transients at radio frequencies. In addition to the preliminary results, we explain how we have created an easily extensible automated follow-up system, describing new software tools developed for astronomical transient alert distribution, automatic requesting of target-of-opportunity observations and robotic control of the observatory.

  10. Astrometric follow-up observations of directly imaged sub-stellar companions to young stars and brown dwarfs

    NASA Astrophysics Data System (ADS)

    Ginski, C.; Schmidt, T. O. B.; Mugrauer, M.; Neuhäuser, R.; Vogt, N.; Errmann, R.; Berndt, A.

    2014-11-01

    The formation of massive planetary or brown dwarf companions at large projected separations from their host star is not yet well understood. In order to put constraints on formation scenarios, we search for signatures in the orbit dynamics of the systems. We are specifically interested in the eccentricities and inclinations since those parameters might tell us about the dynamic history of the systems and where to look for additional low-mass sub-stellar companions. For this purpose, we utilized VLT/NACO to take several well-calibrated high-resolution images of six target systems and analyse them together with available literature data points of those systems as well as Hubble Space Telescope archival data. We used a statistical least-squares Monte Carlo approach to constrain the orbit elements of all systems that showed significant differential motion of the primary star and companion. We show for the first time that the GQ Lup system shows significant change in both separation and position angle. Our analysis yields best-fitting orbits for this system, which are eccentric (e between 0.21 and 0.69), but cannot rule out circular orbits at high inclinations. Given our astrometry, we discuss formation scenarios of the GQ Lup system. In addition, we detected an even fainter new companion candidate to GQ Lup, which is most likely a background object. We also updated the orbit constraints of the PZ Tel system, confirming that the companion is on a highly eccentric orbit with e > 0.62. Finally, we show with a high significance, that there is no orbital motion observed in the cases of the DH Tau, HD 203030 and 1RXS J160929.1-210524 systems, and give the most precise relative astrometric measurement of the UScoCTIO 108 system to date.

  11. GRB 150101B/ Swift J123205.1-105602: Second epoch Chandra observations

    NASA Astrophysics Data System (ADS)

    Levan, A. J.; Hjorth, J.; Tanvir, N. R.; van der Horst, A. J.

    2015-02-01

    We obtained a second epoch of observations of the very short GRB 150101B/ Swift J123205.1-105602 (Cummings et al. GCN 17267) with Chandra. Observations began on 10 Feb 2015, 39 days after the burst, and 32 days after the first epoch of observations.

  12. Simultaneous observations of gamma-ray bursts with Phebus/Granat and Ulysses GRB

    NASA Technical Reports Server (NTRS)

    Atteia, J.-L.; Barat, C.; Boer, M.; Dezalay, J.-P.; Niel, M.; Talon, R.; Vedrenne, G.; Hurley, K.; Sommer, M.; Kuznetsov, A.

    1994-01-01

    We compare the characteristics of 35 gamma-ray bursts (GRBs) detected simultaneously by Phebus aboard Granat and the Ulysses GRB experiment. Phebus observes a medium to high energy range (100 keV - 100 MeV), while the Ulysses GRB detector is sensitive to lower energy photons (25 - 150 keV). Comparison of the peak counts recorded by these two instruments shows that the variation in burst intensities is more extended for Phebus (above approximately 150 keV) than for Ulysses GRB. This result confirms similar observations from other instruments (Atteia et al. 1991; Mitrofanov et al. 1992; Belli 1992). We discuss the consequences of this behavior for the statistical properties of GRBs, and for the searches for a possible cosmological redshift.

  13. Chandra Observations of the X-ray Environs of SN 1998bw/GRB 980425

    NASA Technical Reports Server (NTRS)

    Kouveliotou, C.; Woosley, S. E.; Patel, S. K.; Levan, A.; Blandford, R.; Ramirez-Ruiz, E.; Wijers, R. A. M. J.; Weisskopf, M. C.; Tennant, A.; Pian, E.

    2004-01-01

    We report X-ray studies of the environs of SN 1998bw and GRB 980425 using the Chandra X-Ray Observatory 1281 days after the gamma-ray burst (GRB). Eight X-ray point sources were localized, three and five each in the original error boxes, S1 and S2, assigned for variable X-ray counteparts to the GRB by BeppoSAX. The sum of the discrete X-ray sources plus continuous emission in S2 observed by Chandra on day 1281 is within a factor of 1.5 of the maximum and the upper limits seen by BeppoSAX. We conclude that S2 is the sum of several variable sources that have not disappeared and therefore is not associated with the GRB. Within S1, clear evidence is seen for a decline of approximately a factor of 12 between day 200 and day 1281. One of the sources in S 1, S 1 a, is coincident with the well-determined radio location of SN 1998bw and is certainly the remnant of that explosion. The nature of the other sources is also discussed. Combining our observation of the supernova with others of the GRB afterglow, a smooth X-ray light curve, spanning approx. 1400 days, is obtained by assuming that the burst and supernova were coincident at 35.6 Mpc. When this X-ray light curve is compared with those of the X-ray af "erglows" of ordinary GRBs, X-ray flashes, and ordinary supernovae, evidence emerges for at least two classes of light curves, perhaps bounding a continuum. By 3-10 yr, all these phenomena seem to converge on a common X-ray luminosity, possibly indicative of the supernova underlying them all. This convergence strengthens the conclusion that SN 1998 bw aid GRB 980425 took place in the same object.One possible explanation for the two classes is that a (nearly) standard GRB was observed at different angles, in which case X-ray afterglows with intermediate luminosities should eventually be discovered. Finally, we comment on the contribution of GRB afterglows to the ultraluminous X-ray source population.

  14. Fermi Observations of High-energy Gamma-ray Emission from GRB 090217A

    NASA Astrophysics Data System (ADS)

    Ackermann, M.; Ajello, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Connaughton, V.; Conrad, J.; Cutini, S.; Dermer, C. D.; de Angelis, A.; de Palma, F.; Digel, S. W.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Granot, J.; Grenier, I. A.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hadasch, D.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Kuss, M.; Lande, J.; Latronico, L.; Lee, S.-H.; Llena Garde, M.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McBreen, S.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Mehault, J.; Mészáros, P.; Michelson, P. F.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakajima, H.; Nakamori, T.; Naumann-Godo, M.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Okumura, A.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Porter, T. A.; Preece, R.; Racusin, J. L.; Rainò, S.; Rando, R.; Rau, A.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Ripken, J.; Roth, M.; Ryde, F.; Sadrozinski, H. F.-W.; Sander, A.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uehara, T.; Usher, T. L.; Vandenbroucke, J.; van der Horst, A. J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wood, K. S.; Wu, X. F.; Yamazaki, R.; Yang, Z.; Ylinen, T.; Ziegler, M.; Fermi LAT Collaboration; Fermi GBM Collaboration

    2010-07-01

    The Fermi observatory is advancing our knowledge of gamma-ray bursts (GRBs) through pioneering observations at high energies, covering more than seven decades in energy with the two on-board detectors, the Large Area Telescope (LAT) and the Gamma-ray Burst Monitor (GBM). Here, we report on the observation of the long GRB 090217A which triggered the GBM and has been detected by the LAT with a significance greater than 9σ. We present the GBM and LAT observations and on-ground analyses, including the time-resolved spectra and the study of the temporal profile from 8 keV up to ~1 GeV. All spectra are well reproduced by a Band model. We compare these observations to the first two LAT-detected, long bursts GRB 080825C and GRB 080916C. These bursts were found to have time-dependent spectra and exhibited a delayed onset of the high-energy emission, which are not observed in the case of GRB 090217A. We discuss some theoretical implications for the high-energy emission of GRBs.

  15. GROND observations of GRB 160622A/SNR RCW 103/SGR 1617-5103

    NASA Astrophysics Data System (ADS)

    Schady, P.; Kann, D. A.; Greiner, J.

    2016-06-01

    We observed the field of GRB 160622A/SNR RCW 103/SGR 1617-5103 (Swift trigger 700791; D'Ai et al., GCN #19547. ATel #9180) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile).

  16. J-GEM follow-up observations to search for an optical counterpart of the first gravitational wave source GW150914

    NASA Astrophysics Data System (ADS)

    Morokuma, Tomoki; Tanaka, Masaomi; Asakura, Yuichiro; Abe, Fumio; Tristram, Paul J.; Utsumi, Yousuke; Doi, Mamoru; Fujisawa, Kenta; Itoh, Ryosuke; Itoh, Yoichi; Kawabata, Koji S.; Kawai, Nobuyuki; Kuroda, Daisuke; Matsubayashi, Kazuya; Motohara, Kentaro; Murata, Katsuhiro L.; Nagayama, Takahiro; Ohta, Kouji; Saito, Yoshihiko; Tamura, Yoichi; Tominaga, Nozomu; Uemura, Makoto; Yanagisawa, Kenshi; Yatsu, Yoichi; Yoshida, Michitoshi

    2016-08-01

    We present our optical follow-up observations to search for an electromagnetic counterpart of the first gravitational wave source GW150914 in the framework of the Japanese collaboration for Gravitational wave ElectroMagnetic follow-up (J-GEM), which is an observing group utilizing optical and radio telescopes in Japan, as well as in New Zealand, China, South Africa, Chile, and Hawaii. We carried out a wide-field imaging survey with the Kiso Wide Field Camera (KWFC) on the 1.05 m Kiso Schmidt telescope in Japan and a galaxy-targeted survey with Tripole5 on the B&C 61 cm telescope in New Zealand. Approximately 24 deg2 regions in total were surveyed in i-band with KWFC and 18 nearby galaxies were observed with Tripole5 in g-, r-, and i-bands 4-12 days after the gravitational wave detection. Median 5 σ depths are i ˜ 18.9 mag for the KWFC data and g ˜ 18.9 mag, r ˜ 18.7 mag, and i ˜ 18.3 mag for the Tripole5 data. The probability for a counterpart to be in the observed area is 1.2% in the initial skymap and 0.1% in the final skymap. We do not find any transient source associated to an external galaxy with spatial offset from its center, which is consistent with the local supernova rate.

  17. REM observations of GRB 060418 and GRB 060607A: the onset of the afterglow and the initial fireball Lorentz factor determination

    NASA Astrophysics Data System (ADS)

    Molinari, E.; Vergani, S. D.; Malesani, D.; Covino, S.; D'Avanzo, P.; Chincarini, G.; Zerbi, F. M.; Antonelli, L. A.; Conconi, P.; Testa, V.; Tosti, G.; Vitali, F.; D'Alessio, F.; Malaspina, G.; Nicastro, L.; Palazzi, E.; Guetta, D.; Campana, S.; Goldoni, P.; Masetti, N.; Meurs, E. J. A.; Monfardini, A.; Norci, L.; Pian, E.; Piranomonte, S.; Rizzuto, D.; Stefanon, M.; Stella, L.; Tagliaferri, G.; Ward, P. A.; Ihle, G.; Gonzalez, L.; Pizarro, A.; Sinclaire, P.; Valenzuela, J.

    2007-07-01

    Context: Gamma-ray burst (GRB) emission is believed to originate in highly relativistic fireballs. Aims: Currently, only lower limits were securely set to the initial fireball Lorentz factor Γ_0. We aim to provide a direct measure of Γ_0. Methods: The early-time afterglow light curve carries information about Γ_0, which determines the time of the afterglow peak. We have obtained early observations of the near-infrared afterglows of GRB 060418 and GRB 060607A with the REM robotic telescope. Results: For both events, the afterglow peak could be clearly singled out, allowing a firm determination of the fireball Lorentz of Γ_0˜ 400, fully confirming the highly relativistic nature of GRB fireballs. The deceleration radius was inferred to be R_dec ≈ 1017 cm. This is much larger than the internal shocks radius (believed to power the prompt emission), thus providing further evidence for a different origin of the prompt and afterglow stages of the GRB. Tables 2 and 3 are only available in electronic form at http://www.aanda.org

  18. Chandra Observations of the X-ray Environs of SN 1998bw/GRB 980425

    NASA Technical Reports Server (NTRS)

    Kouveliotou, C.; Woosley, S. E.; Patel, S. K.; Levan, A.; Blandford, R.; Ramirez-Ruiz, E.; Wijers, R. A. M. J.; Weisskopf, M. C.; Tennant, A.; Pian, E.

    2004-01-01

    We report X-ray studies of the environs of SN 1998bw and GRB 980425 using the Chandra X-Ray Observatory 1281 days after the GRB. Eight X-ray point sources were localized, three and five each in the original error boxes - S1 and S2 - assigned for variable X-ray counterparts to the GRB by BeppoSAX. The sum of the discrete X-ray sources plus continuous emission in S2 observed by CXO on day 1281 is within a factor of 1.5 of the maximum and the upper limits seen by BeppoSAX. We conclude that S2 is the sum of several variable sources that have not disappeared, and therefore is not associated with the GRB. Within S1, clear evidence is seen for a decline of approximately a factor of 12 between day 200 and day 1281. One of the sources in S1, Sla, is coincident with the well-determined radio location of SN 1998bw, and is certainly the remnant of that explosion. The nature of the other sources is also discussed. Combining our observation of the supernova with others of the GRB afterglow, a smooth X-ray light curve, spanning approximately 1300 days, is obtained by assuming the burst and supernova were coincident at 35.6 Mpc. When this X-ray iight curve is compared with those of the X-ray afterglows of ordinary GRBs, X-ray Flashes, and ordinary supernovae, evidence emerges for at least two classes of lightcurves, perhaps bounding a continuum. By three to ten years, all these phenomena seem to converge on a common X-ray luminosity, possibly indicative of the supernova underlying them all. This convergence strengthens the conclusion that SN 1998bw and GRB 980425 took place in the same object. One possible explanation for the two classes is a (nearly) standard GRB observed at different angles, in which case X-ray afterglows with intermediate luminosities should eventually be discovered. Finally, we comment on the contribution of GRBs to the ULX source population.

  19. REAL-TIME DETECTION AND RAPID MULTIWAVELENGTH FOLLOW-UP OBSERVATIONS OF A HIGHLY SUBLUMINOUS TYPE II-P SUPERNOVA FROM THE PALOMAR TRANSIENT FACTORY SURVEY

    SciTech Connect

    Gal-Yam, Avishay; Arcavi, Iair; Green, Yoav; Yaron, Ofer; Ben-Ami, Sagi; Xu Dong; Sternberg, Assaf; Kasliwal, Mansi M.; Quimby, Robert M.; Kulkarni, Shrinivas R.; Ofek, Eran O.; Walters, Richard; Nugent, Peter E.; Poznanski, Dovi; Bloom, Joshua S.; Cenko, S. Bradley; Filippenko, Alexei V.; Li Weidong; Silverman, Jeffrey M.; Walker, Emma S.

    2011-08-01

    The Palomar Transient Factory (PTF) is an optical wide-field variability survey carried out using a camera with a 7.8 deg{sup 2} field of view mounted on the 48 inch Oschin Schmidt telescope at Palomar Observatory. One of the key goals of this survey is to conduct high-cadence monitoring of the sky in order to detect optical transient sources shortly after they occur. Here, we describe the real-time capabilities of the PTF and our related rapid multiwavelength follow-up programs, extending from the radio to the {gamma}-ray bands. We present as a case study observations of the optical transient PTF10vdl (SN 2010id), revealed to be a very young core-collapse (Type II-P) supernova having a remarkably low luminosity. Our results demonstrate that the PTF now provides for optical transients the real-time discovery and rapid-response follow-up capabilities previously reserved only for high-energy transients like gamma-ray bursts.

  20. Towards understanding magnetic field generation in relativistic shocks with GRB afterglow observations and the GRB radiation mechanism with photospheric simulations and the X-ray flare radiation mechanism

    NASA Astrophysics Data System (ADS)

    Santana, Rodolfo

    2015-12-01

    In this thesis, we present three projects on open questions in the Gammaray Burst (GRB) field. In the first project, we used X-ray and optical observations to determine the amount of amplification of the ISM magnetic field needed to explain the GRB afterglow observations. We determined that mild amplification is required, at a level stronger than shock-compression but weaker than predicted by the Weibel mechanism. In the second project, we present a Monte Carlo code we wrote from scratch to perform realistic simulations of the photospheric process, one of the mechanisms considered to explain the GRB gamma-ray emission. We determined that photospheric emission can explain the GRB gamma-ray spectrum above the peak-energy if the photons are taken to have a temperature much smaller than the electron temperature and if the interactions between photons and electrons take place at a large optical depth. In the third project, we used multi-wavelength observations to constrain the X-ray flare radiation mechanism. We determined that synchrotron from a Poynting jet and the Photospheric process are the best candidates to explain the X-ray flare observations.

  1. SWIFT OBSERVATIONS OF GAMMA-RAY BURST PULSE SHAPES: GRB PULSE SPECTRAL EVOLUTION CLARIFIED

    SciTech Connect

    Hakkila, Jon; Lien, Amy; Sakamoto, Takanori; Morris, David; Neff, James E.; Giblin, Timothy W.

    2015-12-20

    Isolated Swift gamma-ray burst (GRB) pulses, like their higher-energy BATSE counterparts, emit the bulk of their pulsed emission as a hard-to-soft component that can be fitted by the Norris et al. empirical pulse model. This signal is overlaid by a fainter, three-peaked signal that can be modeled by the residual fit of Hakkila and Preece: the two fits combine to reproduce GRB pulses with distinctive three-peaked shapes. The precursor peak appears on or before the pulse rise and is often the hardest component, the central peak is the brightest, and the decay peak converts exponentially decaying emission into a long, soft, power-law tail. Accounting for systematic instrumental differences, the general characteristics of the fitted pulses are remarkably similar. Isolated GRB pulses are dominated by hard-to-soft evolution; this is more pronounced for asymmetric pulses than for symmetric ones. Isolated GRB pulses can also exhibit intensity tracking behaviors that, when observed, are tied to the timing of the three peaks: pulses with the largest maximum hardnesses are hardest during the precursor, those with smaller maximum hardnesses are hardest during the central peak, and all pulses can re-harden during the central peak and/or during the decay peak. Since these behaviors are essentially seen in all isolated pulses, the distinction between “hard-to-soft and “intensity-tracking” pulses really no longer applies. Additionally, the triple-peaked nature of isolated GRB pulses seems to indicate that energy is injected on three separate occasions during the pulse duration: theoretical pulse models need to account for this.

  2. Swift Observations of Gamma-Ray Burst Pulse Shapes: GRB Pulse Spectral Evolution Clarified

    NASA Astrophysics Data System (ADS)

    Hakkila, Jon; Lien, Amy; Sakamoto, Takanori; Morris, David; Neff, James E.; Giblin, Timothy W.

    2015-12-01

    Isolated Swift gamma-ray burst (GRB) pulses, like their higher-energy BATSE counterparts, emit the bulk of their pulsed emission as a hard-to-soft component that can be fitted by the Norris et al. empirical pulse model. This signal is overlaid by a fainter, three-peaked signal that can be modeled by the residual fit of Hakkila & Preece: the two fits combine to reproduce GRB pulses with distinctive three-peaked shapes. The precursor peak appears on or before the pulse rise and is often the hardest component, the central peak is the brightest, and the decay peak converts exponentially decaying emission into a long, soft, power-law tail. Accounting for systematic instrumental differences, the general characteristics of the fitted pulses are remarkably similar. Isolated GRB pulses are dominated by hard-to-soft evolution; this is more pronounced for asymmetric pulses than for symmetric ones. Isolated GRB pulses can also exhibit intensity tracking behaviors that, when observed, are tied to the timing of the three peaks: pulses with the largest maximum hardnesses are hardest during the precursor, those with smaller maximum hardnesses are hardest during the central peak, and all pulses can re-harden during the central peak and/or during the decay peak. Since these behaviors are essentially seen in all isolated pulses, the distinction between “hard-to-soft and “intensity-tracking” pulses really no longer applies. Additionally, the triple-peaked nature of isolated GRB pulses seems to indicate that energy is injected on three separate occasions during the pulse duration: theoretical pulse models need to account for this.

  3. RAPID, MACHINE-LEARNED RESOURCE ALLOCATION: APPLICATION TO HIGH-REDSHIFT GAMMA-RAY BURST FOLLOW-UP

    SciTech Connect

    Morgan, A. N.; Richards, Joseph W.; Butler, Nathaniel R.; Bloom, Joshua S.; Long, James; Broderick, Tamara

    2012-02-20

    As the number of observed gamma-ray bursts (GRBs) continues to grow, follow-up resources need to be used more efficiently in order to maximize science output from limited telescope time. As such, it is becoming increasingly important to rapidly identify bursts of interest as soon as possible after the event, before the afterglows fade beyond detectability. Studying the most distant (highest redshift) events, for instance, remains a primary goal for many in the field. Here, we present our Random Forest Automated Triage Estimator for GRB redshifts (RATE GRB-z ) for rapid identification of high-redshift candidates using early-time metrics from the three telescopes onboard Swift. While the basic RATE methodology is generalizable to a number of resource allocation problems, here we demonstrate its utility for telescope-constrained follow-up efforts with the primary goal to identify and study high-z GRBs. For each new GRB, RATE GRB-z provides a recommendation-based on the available telescope time-of whether the event warrants additional follow-up resources. We train RATE GRB-z using a set consisting of 135 Swift bursts with known redshifts, only 18 of which are z > 4. Cross-validated performance metrics on these training data suggest that {approx}56% of high-z bursts can be captured from following up the top 20% of the ranked candidates, and {approx}84% of high-z bursts are identified after following up the top {approx}40% of candidates. We further use the method to rank 200 + Swift bursts with unknown redshifts according to their likelihood of being high-z.

  4. Evaluating integrated headache care: a one-year follow-up observational study in patients treated at the Essen headache centre

    PubMed Central

    2011-01-01

    Background Outpatient integrated headache care was established in 2005 at the Essen Headache Centre in Germany. This paper reports outcome data for this approach. Methods Patients were seen by a neurologist for headache diagnosis and recommendation for drug treatment. Depending on clinical needs, patients were seen by a psychologist and/or physical therapist. A 5-day headache-specific multidisciplinary treatment programme (MTP) was provided for patients with frequent or chronic migraine, tension type headache (TTH) and medication overuse headache (MOH). Subsequent outpatient treatment was provided by neurologists in private practice. Results Follow-up data on headache frequency and burden of disease were prospectively obtained in 841 patients (mean age 41.5 years) after 3, 6 and 12 months. At baseline mean headache frequency was 18.1 (SD = 1.6) days per month, compared to measurement at 1 year follow-up a mean reduction of 5.8 (SD = 11.9) headache days per month was observed in 486 patients (57.8%) after one year (TTH patients mean: -8.5 days per month; migraine mean: -3.2 days per month, patients with migraine and TTH mean: -5.9 days per month). A reduction in headache days ≥ 50% was observed in 306 patients (36.4%) independent of diagnosis, while headache frequency remains unchanged in 20.9% and increase in 21.3% of the patient. Conclusion Multidisciplinary outpatient headache centres offer an effective way to establish a three-tier treatment offer for difficult headache patients depending on clinical needs. PMID:21985562

  5. Fermi observations of high-energy gamma-ray emission from GRB 080916C.

    PubMed

    Abdo, A A; Ackermann, M; Arimoto, M; Asano, K; Atwood, W B; Axelsson, M; Baldini, L; Ballet, J; Band, D L; Barbiellini, G; Baring, M G; Bastieri, D; Battelino, M; Baughman, B M; Bechtol, K; Bellardi, F; Bellazzini, R; Berenji, B; Bhat, P N; Bissaldi, E; Blandford, R D; Bloom, E D; Bogaert, G; Bogart, J R; Bonamente, E; Bonnell, J; Borgland, A W; Bouvier, A; Bregeon, J; Brez, A; Briggs, M S; Brigida, M; Bruel, P; Burnett, T H; Burrows, D; Busetto, G; Caliandro, G A; Cameron, R A; Caraveo, P A; Casandjian, J M; Ceccanti, M; Cecchi, C; Celotti, A; Charles, E; Chekhtman, A; Cheung, C C; Chiang, J; Ciprini, S; Claus, R; Cohen-Tanugi, J; Cominsky, L R; Connaughton, V; Conrad, J; Costamante, L; Cutini, S; Deklotz, M; Dermer, C D; de Angelis, A; de Palma, F; Digel, S W; Dingus, B L; do Couto E Silva, E; Drell, P S; Dubois, R; Dumora, D; Edmonds, Y; Evans, P A; Fabiani, D; Farnier, C; Favuzzi, C; Finke, J; Fishman, G; Focke, W B; Frailis, M; Fukazawa, Y; Funk, S; Fusco, P; Gargano, F; Gasparrini, D; Gehrels, N; Germani, S; Giebels, B; Giglietto, N; Giommi, P; Giordano, F; Glanzman, T; Godfrey, G; Goldstein, A; Granot, J; Greiner, J; Grenier, I A; Grondin, M-H; Grove, J E; Guillemot, L; Guiriec, S; Haller, G; Hanabata, Y; Harding, A K; Hayashida, M; Hays, E; Hernando Morat, J A; Hoover, A; Hughes, R E; Jóhannesson, G; Johnson, A S; Johnson, R P; Johnson, T J; Johnson, W N; Kamae, T; Katagiri, H; Kataoka, J; Kavelaars, A; Kawai, N; Kelly, H; Kennea, J; Kerr, M; Kippen, R M; Knödlseder, J; Kocevski, D; Kocian, M L; Komin, N; Kouveliotou, C; Kuehn, F; Kuss, M; Lande, J; Landriu, D; Larsson, S; Latronico, L; Lavalley, C; Lee, B; Lee, S-H; Lemoine-Goumard, M; Lichti, G G; Longo, F; Loparco, F; Lott, B; Lovellette, M N; Lubrano, P; Madejski, G M; Makeev, A; Marangelli, B; Mazziotta, M N; McBreen, S; McEnery, J E; McGlynn, S; Meegan, C; Mészáros, P; Meurer, C; Michelson, P F; Minuti, M; Mirizzi, N; Mitthumsiri, W; Mizuno, T; Moiseev, A A; Monte, C; Monzani, M E; Moretti, E; Morselli, A; Moskalenko, I V; Murgia, S; Nakamori, T; Nelson, D; Nolan, P L; Norris, J P; Nuss, E; Ohno, M; Ohsugi, T; Okumura, A; Omodei, N; Orlando, E; Ormes, J F; Ozaki, M; Paciesas, W S; Paneque, D; Panetta, J H; Parent, D; Pelassa, V; Pepe, M; Perri, M; Pesce-Rollins, M; Petrosian, V; Pinchera, M; Piron, F; Porter, T A; Preece, R; Rainò, S; Ramirez-Ruiz, E; Rando, R; Rapposelli, E; Razzano, M; Razzaque, S; Rea, N; Reimer, A; Reimer, O; Reposeur, T; Reyes, L C; Ritz, S; Rochester, L S; Rodriguez, A Y; Roth, M; Ryde, F; Sadrozinski, H F-W; Sanchez, D; Sander, A; Saz Parkinson, P M; Scargle, J D; Schalk, T L; Segal, K N; Sgrò, C; Shimokawabe, T; Siskind, E J; Smith, D A; Smith, P D; Spandre, G; Spinelli, P; Stamatikos, M; Starck, J-L; Stecker, F W; Steinle, H; Stephens, T E; Strickman, M S; Suson, D J; Tagliaferri, G; Tajima, H; Takahashi, H; Takahashi, T; Tanaka, T; Tenze, A; Thayer, J B; Thayer, J G; Thompson, D J; Tibaldo, L; Torres, D F; Tosti, G; Tramacere, A; Turri, M; Tuvi, S; Usher, T L; van der Horst, A J; Vigiani, L; Vilchez, N; Vitale, V; von Kienlin, A; Waite, A P; Williams, D A; Wilson-Hodge, C; Winer, B L; Wood, K S; Wu, X F; Yamazaki, R; Ylinen, T; Ziegler, M

    2009-03-27

    Gamma-ray bursts (GRBs) are highly energetic explosions signaling the death of massive stars in distant galaxies. The Gamma-ray Burst Monitor and Large Area Telescope onboard the Fermi Observatory together record GRBs over a broad energy range spanning about 7 decades of gammaray energy. In September 2008, Fermi observed the exceptionally luminous GRB 080916C, with the largest apparent energy release yet measured. The high-energy gamma rays are observed to start later and persist longer than the lower energy photons. A simple spectral form fits the entire GRB spectrum, providing strong constraints on emission models. The known distance of the burst enables placing lower limits on the bulk Lorentz factor of the outflow and on the quantum gravity mass.

  6. Multiwavelength Observations of GRB 110731A: GeV Emission from Onset to Afterglow

    NASA Astrophysics Data System (ADS)

    Ackermann, M.; Ajello, M.; Asano, K.; Baldini, L.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bellazzini, R.; Blandford, R. D.; Bonamente, E.; Borgland, A. W.; Bottacini, E.; Bregeon, J.; Brigida, M.; Bruel, P.; Buehler, R.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Cecchi, C.; Charles, E.; Chaves, R. C. G.; Chekhtman, A.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Conrad, J.; Cutini, S.; D'Ammando, F.; de Angelis, A.; de Palma, F.; Dermer, C. D.; Silva, E. do Couto e.; Drell, P. S.; Drlica-Wagner, A.; Favuzzi, C.; Fegan, S. J.; Focke, W. B.; Franckowiak, A.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Giglietto, N.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Granot, J.; Greiner, J.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Hanabata, Y.; Hayashida, M.; Hays, E.; Hughes, R. E.; Jackson, M. S.; Jogler, T.; Jóhannesson, G.; Johnson, A. S.; Knödlseder, J.; Kocevski, D.; Kuss, M.; Lande, J.; Larsson, S.; Latronico, L.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Mazziotta, M. N.; McEnery, J. E.; Mehault, J.; Mészáros, P.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Naumann-Godo, M.; Norris, J. P.; Nuss, E.; Nymark, T.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orienti, M.; Orlando, E.; Paneque, D.; Perkins, J. S.; Pesce-Rollins, M.; Piron, F.; Pivato, G.; Racusin, J. L.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Romoli, C.; Roth, M.; Ryde, F.; Sanchez, D. A.; Sgrò, C.; Siskind, E. J.; Sonbas, E.; Spinelli, P.; Stamatikos, M.; Takahashi, H.; Tanaka, T.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Tinivella, M.; Tosti, G.; Troja, E.; Usher, T. L.; Vandenbroucke, J.; Vasileiou, V.; Vianello, G.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Yang, Z.; Gruber, D.; Bhat, P. N.; Bissaldi, E.; Briggs, M. S.; Burgess, J. M.; Connaughton, V.; Foley, S.; Kippen, R. M.; Kouveliotou, C.; McBreen, S.; McGlynn, S.; Paciesas, W. S.; Pelassa, V.; Preece, R.; Rau, A.; van der Horst, A. J.; von Kienlin, A.; Kann, D. A.; Filgas, R.; Klose, S.; Krühler, T.; Fukui, A.; Sako, T.; Tristram, P. J.; Oates, S. R.; Ukwatta, T. N.; Littlejohns, O.

    2013-02-01

    We report on the multiwavelength observations of the bright, long gamma-ray burst GRB 110731A, by the Fermi and Swift observatories, and by the MOA and GROND optical telescopes. The analysis of the prompt phase reveals that GRB 110731A shares many features with bright Large Area Telescope bursts observed by Fermi during the first three years on-orbit: a light curve with short time variability across the whole energy range during the prompt phase, delayed onset of the emission above 100 MeV, extra power-law component and temporally extended high-energy emission. In addition, this is the first GRB for which simultaneous GeV, X-ray, and optical data are available over multiple epochs beginning just after the trigger time and extending for more than 800 s, allowing temporal and spectral analysis in different epochs that favor emission from the forward shock in a wind-type medium. The observed temporally extended GeV emission is most likely part of the high-energy end of the afterglow emission. Both the single-zone pair transparency constraint for the prompt signal and the spectral and temporal analysis of the forward-shock afterglow emission independently lead to an estimate of the bulk Lorentz factor of the jet Γ ~ 500-550.

  7. The GRB luminosity function: prediction of the internal shock model and comparison to observations

    SciTech Connect

    Zitouni, H.; Daigne, F.; Mochkovitch, R.

    2008-05-22

    We compute the expected GRB luminosity function in the internal shock model. We find that if the population of GRB central engines produces all kind of relativistic outflows, from very smooth to highly variable, the luminosity function has to branchs: at low luminosity, the distribution is dominated by low efficiency GRBs and is close to a power law of slope -0.5, whereas at high luminosity, the luminosity function follows the distribution of injected kinetic power. Using Monte Carlo simulations and several observational constrains (BATSE logN-logP diagram, peak energy distribution of bright BATSE bursts, fraction of XRFs in the HETE2 sample), we show that it is currently impossible to distinguish between a single power law or a broken power law luminosity function. However, when the second case is considered, the low-luminosity slope is found to be -0.6{+-}0.2, which is compatible with the prediction of the internal shock model.

  8. VLBI AND ARCHIVAL VLA AND WSRT OBSERVATIONS OF THE GRB 030329 RADIO AFTERGLOW

    SciTech Connect

    Mesler, Robert A.; Pihlstroem, Ylva M.; Taylor, Greg B.; Granot, Johnathan

    2012-11-01

    We present VLBI and archival Karl G. Jansky Very Large Array (VLA) and Westerbork Synthesis Radio Telescope (WSRT) observations of the radio afterglow from the gamma-ray burst (GRB) of 2003 March 29 (GRB 030329) taken between 672 and 2032 days after the burst. The VLA and WSRT data suggest a simple power-law decay in the flux at 5 GHz, with no clear signature of any rebrightening from the counterjet. We report an unresolved source at day 2032 of size 1.18 {+-} 0.13 mas, which we use in conjunction with the expansion rate of the burst to argue for the presence of a uniform, interstellar-medium-like circumburst medium. A limit of <0.067 mas yr{sup -1} is placed on the proper motion, supporting the standard afterglow model for gamma-ray bursts.

  9. Radio and X-ray observations of the Ultra-long GRB 150518A

    NASA Astrophysics Data System (ADS)

    Johnson, Louis; Kamble, Atish; Margutti, Raffaella; Soderberg, Alicia Margarita; Supernova Forensics

    2016-01-01

    Gamma Ray Burst (GRB) 150518A, discovered on 2015 May 18 by the MAXI and KONUS-Wind satellites, lasted for about 1000s, making it an important addition to the recently established class of very long duration GRBs. We report on the JVLA radio observations of the afterglow of GRB 150518A. Additionally, we report the analysis of Xray afterglow observations by Swift-XRT. Multi-band light curves of the radio afterglow display an unusual, conspicuous rise around 10 days after the burst, possibly due to enhanced mass-loss from the progenitor in the final stages of evolution before the GRB. The X-ray afterglow spectrum is significantly soft (photon index Γx > 3) and heavily absorbed (NHx,i > 8 × 10^{21}/cm^2). These properties suggest peculiar behavior that is different from the predictions of the standard fireball model of GRBs. In the light of these properties, we compare different models of progenitors for very long duration GRBs. This work was supported in part by the NSF REU and DoD ASSURE programs under NSF grant no. 1262851 and by the Smithsonian Institution.

  10. GRB 050717: A Long, Short-Lag Burst Observed by Swift and Konus

    SciTech Connect

    Krimm, H. A.; Hurkett, C.; Osborne, J. P.; Pal'shin, V.; Golenetskii, S.; Norris, J. P.; Barthelmy, S. D.; Gehrels, N.; Parsons, A. M.; Zhang, B.; Burrows, D. N.; Perri, M.

    2006-05-19

    The long burst GRB 050717 was observed simultaneously by the Burst Alert Telescope (BAT) on Swift and the Konus instrument on Wind. Significant hard to soft spectral evolution was seen. Early gamma-ray and X-ray emission was detected by both BAT and the X-Ray Telescope (XRT) on Swift. The XRT continued to observe the burst for 7.1 days and detect it for 1.4 days. The X-ray light curve showed a classic decay pattern including evidence of the onset of the external shock emission at {approx} 45 s after the trigger; the afterglow was too faint for a jet break to be detected. No optical, infrared or ultraviolet counterpart was discovered despite deep searches within 14 hours of the burst. The spectral lag for GRB 050717 was determined to be 2.5 {+-} 2.6 ms, consistent with zero and unusually short for a long burst. This lag measurement suggests that this burst has a high intrinsic luminosity and hence is at high redshift (z > 2.7). GRB 050717 provides a good example of classic prompt and afterglow behavior for a gamma-ray burst.

  11. The Sub-Energetic GRB 031203 as a Cosmic Analogue to GRB 980425

    SciTech Connect

    Soderberg, A

    2004-08-27

    Over the six years since the discovery of the {gamma}-ray burst GRB 980425, associated with the nearby (distance {approx}40 Mpc) supernova 1998bw, astronomers have fiercely debated the nature of this event. Relative to bursts located at cosmological distances, (redshift, z {approx} 1), GRB 980425 was under-luminous in {gamma}-rays by three orders of magnitude. Radio calorimetry showed the explosion was sub-energetic by a factor of 10. Here, the authors report observations of the radio and X-ray afterglow of the recent z = 0.105 GRB031203 and demonstrate that it too is sub-energetic. The result, when taken together with the low {gamma}-ray luminosity, suggest that GRB031203 is the first cosmic analogue to GRB980425. They find no evidence that this event was a highly collimated explosion viewed off-axis. Like GRB980425, GRB031203 appears to be an intrinsically sub-energetic {gamma}-burst. Such sub-energetic events have faint afterglows. Intensive follow-up of faint bursts with smooth {gamma}-ray light curves (common to both GRBs 031203 and 980425) may enable the authors to reveal their expected large population.

  12. Swift X-ray follow-up observations of two INTEGRAL sources: IGRJ12470-5407 and IGRJ18532+0416

    NASA Astrophysics Data System (ADS)

    Fiocchi, M.; Landi, R.; Bassani, L.; Bazzano, A.; Bird, A. J.; Gehrels; Kennea, J. A.

    2011-04-01

    We report the results of X-ray follow-up observations performed with Swift/XRT of two unidentified INTEGRAL sources, IGRJ12470-5407 and IGRJ18532+0416, listed in the 4th IBIS Survey Catalogue (Bird et al. 2010, ApJS, 186, 1). IGRJ12470-5407 This source is a very weak IBIS unidentified object with a flux < 0.3 mCrab in the 20-40 keV energy band ( Bird et al. 2010, ApJS, 186, 1). The field of this source was observed with Swift-XRT on 2011-02-17 03:33:01 and 2011-02-19 18:06:01, for a total exposure time of 4312 s. Within the 99% IBIS positional uncertainty we found only one XRT source above 3 sigma c.l., located at R.A.(J2000) = 12h 47m 50.80s and Dec.(J2000) = -54d 06m 30.80s with an uncertainty of 5 arcsec.

  13. Influence of Anti-TNF and Disease Modifying Antirheumatic Drugs Therapy on Pulmonary Forced Vital Capacity Associated to Ankylosing Spondylitis: A 2-Year Follow-Up Observational Study

    PubMed Central

    Rocha-Muñoz, Alberto Daniel; Brambila-Tapia, Aniel Jessica Leticia; Zavala-Cerna, María Guadalupe; Vásquez-Jiménez, José Clemente; De la Cerda-Trujillo, Liliana Faviola; Vázquez-Del Mercado, Mónica; Rodriguez-Jimenez, Norma Alejandra; Díaz-Rizo, Valeria; Díaz-González, Viviana; Cardona-Muñoz, Ernesto German; Dávalos-Rodríguez, Ingrid Patricia; Salazar-Paramo, Mario; Gamez-Nava, Jorge Ivan; Nava-Zavala, Arnulfo Hernan; Gonzalez-Lopez, Laura

    2015-01-01

    Objective. To evaluate the effect of anti-TNF agents plus synthetic disease modifying antirheumatic drugs (DMARDs) versus DMARDs alone for ankylosing spondylitis (AS) with reduced pulmonary function vital capacity (FVC%). Methods. In an observational study, we included AS who had FVC% <80% at baseline. Twenty patients were taking DMARDs and 16 received anti-TNF + DMARDs. Outcome measures: changes in FVC%, BASDAI, BASFI, 6-minute walk test (6MWT), Borg scale after 6MWT, and St. George's Respiratory Questionnaire at 24 months. Results. Both DMARDs and anti-TNF + DMARDs groups had similar baseline values in FVC%. Significant improvement was achieved with anti-TNF + DMARDs in FVC%, at 24 months, when compared to DMARDs alone (P = 0.04). Similarly, patients in anti-TNF + DMARDs group had greater improvement in BASDAI, BASFI, Borg scale, and 6MWT when compared to DMARDs alone. After 2 years of follow-up, 14/16 (87.5%) in the anti-TNF + DMARDs group achieved the primary outcome: FVC% ≥80%, compared with 11/20 (55%) in the DMARDs group (P = 0.04). Conclusions. Patients with anti-TNF + DMARDs had a greater improvement in FVC% and cardiopulmonary scales at 24 months compared with DMARDs. This preliminary study supports the fact that anti-TNF agents may offer additional benefits compared to DMARDs in patients with AS who have reduced FVC%. PMID:26078986

  14. Investigating the Impact of Optical Selection Effects on Observed Rest-frame Prompt GRB Properties

    NASA Astrophysics Data System (ADS)

    Turpin, D.; Heussaff, V.; Dezalay, J.-P.; Atteia, J.-L.; Klotz, A.; Dornic, D.

    2016-11-01

    Measuring gamma-ray burst (GRB) properties in their rest frame is crucial for understanding the physics at work in GRBs. This can only be done for GRBs with known redshifts. Since redshifts are usually measured from the optical spectrum of the afterglow, correlations between prompt and afterglow emissions may introduce biases into the distribution of the rest-frame properties of the prompt emission, especially considering that we measure the redshift of only one-third of Swift GRBs. In this paper, we study the optical flux of GRB afterglows and its connection to various intrinsic properties of GRBs. We also discuss the impact of the optical selection effect on the distribution of rest-frame prompt properties of GRBs. Our analysis is based on a sample of 90 GRBs with good optical follow-up and well-measured prompt emission. Seventy-six of them have a measure of redshift and 14 have no redshift. We compare the rest-frame prompt properties of GRBs with different afterglow optical fluxes in order to check for possible correlations between the promt properties and the optical flux of the afterglow. The optical flux is measured two hours after the trigger, which is a typical time for the measure of the redshift. We find that the optical flux of GRB afterglows in our sample is mainly driven by their optical luminosity and depends only slightly on their redshift. We show that GRBs with low and high afterglow optical fluxes have similar E {}{{pi}}, E {}{{iso}}, and L {}{{iso}}, indicating that the rest-frame distributions computed from GRBs with a redshift are not significantly distorted by optical selection effects. However, we found that the {T}90{rest} distribution is not immune to optical selection effects, which favor the selection of GRBs with longer durations. Finally, we note that GRBs well above the E {}{{pi}}–E {}{{iso}} relation have lower optical fluxes and we show that optical selection effects favor the detection of GRBs with bright optical afterglows

  15. HAT-P-56b: An Inflated Massive Hot Jupiter Transiting a Bright F Star Followed Up with K2 Campaign 0 Observations

    NASA Astrophysics Data System (ADS)

    Huang, C. X.; Hartman, J. D.; Bakos, G. Á.; Penev, K.; Bhatti, W.; Bieryla, A.; de Val-Borro, M.; Latham, D. W.; Buchhave, L. A.; Csubry, Z.; Kovács, G.; Béky, B.; Falco, E.; Berlind, P.; Calkins, M. L.; Esquerdo, G. A.; Lázár, J.; Papp, I.; Sári, P.

    2015-09-01

    We report the discovery of HAT-P-56b by the HATNet survey, an inflated hot Jupiter transiting a bright F-type star in Field 0 of NASA's K2 mission. We combine ground-based discovery and follow-up light curves with high precision photometry from K2, as well as ground-based radial velocities from the Tillinghast Reflector Echelle Spectrograph on the Fred Lawrence Whipple Observatory 1.5 m telescope to determine the physical properties of this system. HAT-P-56b has a mass of 2.18 {M}{{J}}, radius of 1.47 {R}{{J}}, and transits its host star on a near-grazing orbit with a period of 2.7908 day. The radius of HAT-P-56b is among the largest known for a planet with {M}p\\gt 2 {M}{{J}}. The host star has a V-band magnitude of 10.9, mass of 1.30 {M}⊙ , and radius of 1.43 {R}⊙ . The periodogram of the K2 light curve suggests that the star is a γ Dor variable. HAT-P-56b is an example of a ground-based discovery of a transiting planet, where space-based observations greatly improve the confidence in the confirmation of its planetary nature, and also improve the accuracy of the planetary parameters. Based on observations obtained with the Hungarian-made Automated Telescope Network. Based in part on observations obtained with the Tillinghast Reflector 1.5 m telescope and the 1.2 m telescope, both operated by the Smithsonian Astrophysical Observatory at the Fred Lawrence Whipple Observatory in Arizona. Based in part on observations obtained with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. Based in part on observations obtained with the Kepler Space Craft in the K2 Campaign 0 Mission.

  16. X-RAY AND RADIO FOLLOW-UP OBSERVATIONS OF HIGH-REDSHIFT BLAZAR CANDIDATES IN THE FERMI-LAT UNASSOCIATED SOURCE POPULATION

    SciTech Connect

    Takahashi, Y.; Kataoka, J.; Nakamori, T.; Maeda, K.; Niinuma, K.; Honma, M.; Inoue, Y.; Totani, T.; Inoue, S.

    2013-08-10

    We report on the results of X-ray and radio follow-up observations of two GeV gamma-ray sources 2FGL J0923.5+1508 and 2FGL J1502.1+5548, selected as candidates for high-redshift blazars from unassociated sources in the Fermi Large Area Telescope Second Source Catalog. We utilize the Suzaku satellite and the VLBI Exploration of Radio Astrometry (VERA) telescopes for X-ray and radio observations, respectively. For 2FGL J0923.5+1508, a possible radio counterpart NVSS J092357+150518 is found at 1.4 GHz from an existing catalog, but we do not detect any X-ray emission from it and derive a flux upper limit F{sub 2-8{sub keV}} < 1.37 Multiplication-Sign 10{sup -14} erg cm{sup -2} s{sup -1}. Radio observations at 6.7 GHz also result in an upper limit of S{sub 6.7{sub GHz}} < 19 mJy, implying a steep radio spectrum that is not expected for a blazar. On the other hand, we detect X-rays from NVSS J150229+555204, the potential 1.4 GHz radio counterpart of 2FGL J1502.1+5548. The X-ray spectrum can be fitted with an absorbed power-law model with a photon index {gamma} = 1.8{sup +0.3}{sub -0.2} and the unabsorbed flux is F{sub 2-8{sub keV}} = 4.3{sup +1.1}{sub -1.0} Multiplication-Sign 10{sup -14} erg cm{sup -2} s{sup -1}. Moreover, we detect unresolved radio emission at 6.7 GHz with flux S{sub 6.7{sub GHz}} = 30.1 mJy, indicating a compact, flat-spectrum radio source. If NVSS J150229+555204 is indeed associated with 2FGL J1502.1+5548, then we find that its multiwavelength spectrum is consistent with a blazar at redshift z {approx} 3-4.

  17. Effects of arthroscopic-assisted surgery on irreducible developmental dislocation of hip by mid-term follow-up: An observational study.

    PubMed

    Xu, Hui-Fa; Yan, Ya-Bo; Xu, Chao; Li, Tian-Qing; Zhao, Tian-Feng; Liu, Ning; Huang, Lu-Yu; Zhang, Chun-Li; Lei, Wei

    2016-08-01

    The purpose of this study was to investigate the indications, surgical technique, and the clinical effects of arthroscopic-assisted treatment of irreducible developmental dislocation of the hip by mid-term follow-up. Arthroscopic-assisted surgeries were performed on 40 children (52 hips) between January 2005 and December 2009. Anterior and antero-superior greater trochanter portals were used in these treatments. Spica cast and abduction splint were applied for 3 months postoperatively. The follow-up was conducted on every 3 months postoperatively. During 12-month follow-up, a secondary treatment such as acetabuloplasty and/or femoral osteotomy (shortening, varus, and derotation) was applied if the acetabular angle was greater than 25°. The pelvic acetabular angle, Mckay and Severin score were evaluated every 6 months in all children. With 36 to 96 months (average 71 months) follow-up, 35 children (44 hips) were successfully followed up with complete case data while 5 children unsuccessfully. According to Tönnis classification, there were 5 grade 1 hips, 14 grade 2 hips, 14 grade 3 hips, 11 grade 4 hips, in which 3 children (4 hips) were failed in arthroscopic reduction and femoral head avascular necrosis occurred in 2 children (4 hips). According to Mckay standard, the good rate is 100%. According to Severin standard, the good rate is 84.1%. Arthroscopic assisted treatment is an effective way of reduction of the irreducible hip. Compared with the open reduction, arthroscopic treatment combined with acetabuloplasty and/or femoral osteotomy has advantages of less trauma and better function preservation. PMID:27537595

  18. PANCHROMATIC OBSERVATIONS OF THE TEXTBOOK GRB 110205A: CONSTRAINING PHYSICAL MECHANISMS OF PROMPT EMISSION AND AFTERGLOW

    SciTech Connect

    Zheng, W.; Shen, R. F.; Sakamoto, T.; Beardmore, A. P.; De Pasquale, M.; Wu, X. F.; Zhang, B.; Gorosabel, J.; Urata, Y.; Sugita, S.; Pozanenko, A.; Sahu, D. K.; Im, M.; Ukwatta, T. N.; Andreev, M.; Klunko, E. E-mail: rfshen@astro.utoronto.ca; and others

    2012-06-01

    We present a comprehensive analysis of a bright, long-duration (T{sub 90} {approx} 257 s) GRB 110205A at redshift z = 2.22. The optical prompt emission was detected by Swift/UVOT, ROTSE-IIIb, and BOOTES telescopes when the gamma-ray burst (GRB) was still radiating in the {gamma}-ray band, with optical light curve showing correlation with {gamma}-ray data. Nearly 200 s of observations were obtained simultaneously from optical, X-ray, to {gamma}-ray (1 eV to 5 MeV), which makes it one of the exceptional cases to study the broadband spectral energy distribution during the prompt emission phase. In particular, we clearly identify, for the first time, an interesting two-break energy spectrum, roughly consistent with the standard synchrotron emission model in the fast cooling regime. Shortly after prompt emission ({approx}1100 s), a bright (R = 14.0) optical emission hump with very steep rise ({alpha} {approx} 5.5) was observed, which we interpret as the reverse shock (RS) emission. It is the first time that the rising phase of an RS component has been closely observed. The full optical and X-ray afterglow light curves can be interpreted within the standard reverse shock (RS) + forward shock (FS) model. In general, the high-quality prompt and afterglow data allow us to apply the standard fireball model to extract valuable information, including the radiation mechanism (synchrotron), radius of prompt emission (R{sub GRB} {approx} 3 Multiplication-Sign 10{sup 13} cm), initial Lorentz factor of the outflow ({Gamma}{sub 0} {approx} 250), the composition of the ejecta (mildly magnetized), the collimation angle, and the total energy budget.

  19. Panchromatic Observations of the Textbook GRB 110205A: Constraining Physical Mechanisms of Prompt Emission and Afterglow

    NASA Technical Reports Server (NTRS)

    Zheng, W.; Shen, R. F.; Sakamoto, T.; Beardmore, A. P.; De Pasquale, M.; Wu, X. F.; Gorosabel, J.; Urata, Y.; Sugita, S.; Zhang, B.; Pozanenko, A.; Nissinen, M.; Sahu, D. K.; Im, M.; Ukwatta, T. N.; Andreev, M.; Klunko, E.; Volnova, A.; Akerlof, C. W.; Anto, P.; Barthelmy, S. D.; Breeveld, A.; Carsenty, U.; Gehrels, N.; Sonbas, E.

    2011-01-01

    We present a comprehensive analysis of a bright, long duration (T(sub 90) approx. 257 s) GRB 110205A at redshift z = 2.22. The optical prompt emission was detected by Swift/UVOT, ROTSE-IIIb and BOOTES telescopes when the GRB was still radiating in the gamma-ray band. Thanks to its long duration, nearly 200 s of observations were obtained simultaneously from optical, X-ray to gamma-ray (1 eV - 5 MeV), which makes it one of the exceptional cases to study the broadband spectral energy distribution across 6 orders of magnitude in energy during the prompt emission phase. In particular, by fitting the time resolved prompt spectra, we clearly identify, for the first time, an interesting two-break energy spectrum, roughly consistent with the standard GRB synchrotron emission model in the fast cooling regime. Although the prompt optical emission is brighter than the extrapolation of the best fit X/ -ray spectra, it traces the -ray light curve shape, suggesting a relation to the prompt high energy emission. The synchrotron + synchrotron self-Compton (SSC) scenario is disfavored by the data, but the models invoking a pair of internal shocks or having two emission regions can interpret the data well. Shortly after prompt emission (approx. 1100 s), a bright (R = 14.0) optical emission hump with very steep rise ( alpha approx. 5.5) was observed which we interpret as the emission from the reverse shock. It is the first time that the rising phase of a reverse shock component has been closely observed.

  20. Effect of deletion polymorphism of angiotensin converting enzyme gene on progression of diabetic nephropathy during inhibition of angiotensin converting enzyme: observational follow up study.

    PubMed Central

    Parving, H. H.; Jacobsen, P.; Tarnow, L.; Rossing, P.; Lecerf, L.; Poirier, O.; Cambien, F.

    1996-01-01

    OBJECTIVE: To evaluate the concept that an insertion/deletion polymorphism of the angiotensin converting enzyme gene predicts the therapeutic efficacy of inhibition of angiotensin converting enzyme on progression of diabetic nephropathy. DESIGN: Observational follow up study of patients with insulin dependent diabetes and nephropathy who had been treated with captopril for a median of 7 years (range 3-9 years). SETTING: Outpatient diabetic clinic in a tertiary referral centre. PATIENTS: 35 patients with insulin dependent diabetes and nephropathy were investigated during captopril treatment (median 75 mg/day (range 12.5 to 150 mg/day)) that was in many cases combined with a loop diuretic, 11 patients were homozygous for the deletion allele and 24 were heterozygous or homozygous for the insertion allele of the angiotensin converting enzyme gene. MAIN OUTCOME MEASURES: Albuminuria, arterial blood pressure, and glomerular filtration rate according to insertion/deletion polymorphism. RESULTS: The two groups had comparable glomerular filtration rate, albuminuria, blood pressure, and haemoglobin A1c concentration at baseline. Captopril induced nearly the same reduction in mean blood pressure in the two groups-to 103 (SD 5) mm Hg in the group with the deletion and 102 (8) mm Hg in the group with the insertion-and in geometric mean albumin excretion-573 (antilog SE 1.3) micrograms/min and 470 (1.2) micrograms/min, respectively. The rate of decline in glomerular filtration rate (linear regression of all glomerular filtration rate measurements during antihypertensive treatment) was significantly steeper in the group homozygous for the double deletion allele than in the other group (mean 5.7 (3.7) ml/min/year and 2.6 (2.8) ml/min/year, respectively; P = 0.01). Multiple linear regression analysis showed that haemoglobin A1c concentration, albuminuria, and the double deletion genotype independently influenced the sustained rate of decline in glomerular filtration rate (R1

  1. XMM-Newton and Optical Follow-up Observations of SDSS J093249.57+472523.0 and SDSS J102347.67+003841.2

    NASA Astrophysics Data System (ADS)

    Homer, Lee; Szkody, Paula; Chen, Bing; Henden, Arne; Schmidt, Gary; Anderson, Scott F.; Silvestri, Nicole M.; Brinkmann, J.

    2006-01-01

    We report follow-up XMM-Newton and ground-based optical observations of the unusual X-ray binary SDSS J102347.67+003841.2 (=FIRST J102347.6+003841) and a new candidate intermediate polar (IP) found in the Sloan Digital Sky Survey: SDSS J093249.57+472523.0. SDSS J1023 was observed in its low state, with similar magnitude/color (V=17.4 and B=17.9) and smooth orbital modulation as seen in most previous observations. We further refine the ephemeris (for photometric minimum) to HJD(TT)min=2,453,081.8546(3)+E0.198094(1) days. It is easily detected in X-rays at an unabsorbed flux (0.01-10.0 keV) of 5×10-13 ergs cm-2 s-1. Fitting a variety of models we find that (1) either a hot (kT>~15 keV) optically thin plasma emission model (bremsstrahlung or MEKAL) or a simple power law can provide adequate fits to the data; (2) these models prefer a low column density ~1019 cm-2 (3) a neutron star atmosphere plus power-law model (as found for quiescent low-mass X-ray binaries) can also produce a good fit (for plausible distances), although only for a much higher column ~4×1020 cm-2 and a very cool atmosphere (kT<~50 eV). These results support the case that SDSS J1023 is a transient LMXB and indeed place it in the subclass of such systems whose quiescent X-ray emission is dominated by a hard power-law component. Our optical photometry of SDSS J0932 reveals that it is a high-inclination eclipsing system. From our two epochs of data and seven eclipse times, we are able to derive a best-fit ephemeris for minimum light: HJD(TT)min=2,453,122.2324(1)+E0.0661618(4) days, although aliases, with one cycle count different between epochs, are acceptable. The X-ray spectrum is well fit by either a hard bremsstrahlung or power law, with a partial covering absorption model, with a high covering fraction ~0.9 and column ~1023 cm-2. Combined with its optical characteristics-high excitation emission lines and its brightness, yielding a large FX/Fopt ratio-this highly absorbed X-ray spectrum argues

  2. Effect of bivalent human papillomavirus vaccination on pregnancy outcomes: long term observational follow-up in the Costa Rica HPV Vaccine Trial

    PubMed Central

    Befano, Brian L; Gonzalez, Paula; Rodríguez, Ana Cecilia; Herrero, Rolando; Schiller, John T; Kreimer, Aimée R; Schiffman, Mark; Hildesheim, Allan; Wilcox, Allen J

    2015-01-01

    Objective To examine the effect of the bivalent human papillomavirus (HPV) vaccine on miscarriage. Design Observational long term follow-up of a randomized, double blinded trial combined with an independent unvaccinated population based cohort. Setting Single center study in Costa Rica. Participants 7466 women in the trial and 2836 women in the unvaccinated cohort enrolled at the end of the randomized trial and in parallel with the observational trial component. Intervention Women in the trial were assigned to receive three doses of bivalent HPV vaccine (n=3727) or the control hepatitis A vaccine (n=3739). Crossover bivalent HPV vaccination occurred in the hepatitis A vaccine arm at the end of the trial. Women in the unvaccinated cohort received (n=2836) no vaccination. Main outcome measure Risk of miscarriage, defined by the US Centers for Disease Control and Prevention as fetal loss within 20 weeks of gestation, in pregnancies exposed to bivalent HPV vaccination in less than 90 days and any time from vaccination compared with pregnancies exposed to hepatitis A vaccine and pregnancies in the unvaccinated cohort. Results Of 3394 pregnancies conceived at any time since bivalent HPV vaccination, 381 pregnancies were conceived less than 90 days from vaccination. Unexposed pregnancies comprised 2507 pregnancies conceived after hepatitis A vaccination and 720 conceived in the unvaccinated cohort. Miscarriages occurred in 451 (13.3%) of all exposed pregnancies, in 50 (13.1%) of the pregnancies conceived less than 90 days from bivalent HPV vaccination, and in 414 (12.8%) of the unexposed pregnancies, of which 316 (12.6%) were in the hepatitis A vaccine group and 98 (13.6%) in the unvaccinated cohort. The relative risk of miscarriage for pregnancies conceived less than 90 days from vaccination compared with all unexposed pregnancies was 1.02 (95% confidence interval 0.78 to 1.34, one sided P=0.436) in unadjusted analyses. Results were similar after adjusting for age at

  3. Stirring the Embers: High-Sensitivity VLBI Observations of GRB 030329

    SciTech Connect

    Pihlstrom, Y.M.; Taylor, G.B.; Granot, J.; Doeleman, S.; /MIT, Haystack Observ.

    2007-09-24

    We present high-sensitivity Very Long Baseline Interferometry (VLBI) observations 806 days after the {gamma}-ray burst of 2003 March 29 (GRB 030329). The angular diameter of the radio afterglow is measured to be 0:347 {+-} 0:09 mas, corresponding to 0:99 {+-} 0:26 pc at the redshift of GRB 030329 (z = 0:1685). The evolution of the image size favors a uniform external density over an R{sup -2} windlike density profile (at distances of R {approx}> 10{sup 18} cm from the source), although the latter cannot be ruled out yet. The current apparent expansion velocity of the image size is only mildly relativistic, suggesting a nonrelativistic transition time of tNR {approx} 1 yr. A rebrightening, or at least a significant flattening in the flux decay, is expected within the next several years as the counterjet becomes visible (this has not yet been observed). An upper limit of <1.9c is set on the proper motion of the flux centroid.

  4. GRB 050717: A Long, Short-Lag Burst Observed by Swift and Konus

    NASA Technical Reports Server (NTRS)

    Krimm, H. A.; Hurkett, C.; Pal'shin, V.; Norris, J. P.; Zhang, B.; Barthelmy, S. D.; Burrows, D. N.; Gehrels, N.; Golenetskii, S.; Osborne, J. P.; Parsons, A. M.; Perri, M.; Willingale, R.

    2005-01-01

    The long burst GRB 050717 was observed simultaneously by the Burst Alert Telescope (BAT) on Swift and the Konus instrument on Wind. Significant hard to soft spectral evolution was seen. Early gamma-ray and X-ray emission was detected by both BAT and the X-Ray Telescope (XRT) on Swift. The XRT continued to observe the burst for 7.1 days and detect it for 1.4 days. The X-ray light curve showed a classic decay pattern including evidence of the onset of the external shock emission at approx. 50 s after the trigger; the afterglow was too faint for a jet break to be detected. No optical, infrared or ultraviolet counterpart was discovered despite deep searches within 14 hours of the burst. The spectral lag for GRB 050717 was determined to be 2.5 +/- 2.6 ms, consistent, with zero and unusually short for a long burst. This lag measurement suggests that this burst has a high intrinsic luminosity and hence is at high redshift (z > 2.7). 050717 provides a good example of classic prompt and afterglow behavior for a gamma-ray burst.

  5. MASTERS-D Study: A Prospective, Multicenter, Pragmatic, Observational, Data-Monitored Trial of Minimally Invasive Fusion to Treat Degenerative Lumbar Disorders, One-Year Follow-Up

    PubMed Central

    Manson, Neil; Buzek, David; Kosmala, Arkadiusz; Hubbe, Ulrich; Rosenberg, Wout; Pereira, Paulo; Assietti, Roberto; Martens, Frederic; Lam, Khai; Barbanti Brodano, Giovanni; Durny, Peter; Lidar, Zvi; Scheufler, Kai; Senker, Wolfgang

    2016-01-01

    The objective of the study is to assess effectiveness and safety of minimally invasive lumbar interbody fusion (MILIF) for degenerative lumbar disorders (DLD) in daily surgical practice and follow up with patients for one year after surgery. A prospective, multicenter, pragmatic, monitored, international outcome study in patients with DLD causing back/leg pain was conducted (19 centers). Two hundred fifty-two patients received standard of care available in the centers. Patients were included if they were aged >18 years, required one- or two-level lumbar fusion for DLD, and met the criteria for approved device indications. Primary endpoints: time to first ambulation (TFA) and time to surgery recovery (TSR). Secondary endpoints: patient-reported outcomes (PROs)--back and leg pain (visual analog scale), disability (Oswestry Disability Index (ODI)), health status (EQ-5D), fusion rates, reoperation rates, change in pain medication, rehabilitation, return to work, patient satisfaction, and adverse events (AEs). Experienced surgeons (≥30 surgeries pre-study) treated patients with DLD by one- or two-level MILIF and patients were evaluated for one year (NCT01143324). At one year, 92% (233/252) of patients remained in the study. Primary outcomes: TFA, 1.3 ±0.5 days and TSR, 3.2 ±2.0 days. Secondary outcomes: Most patients (83.3%) received one level MILIF; one (two-level) MILIF mean surgery duration, 128 (182) min; fluoroscopy time, 115 (154) sec; blood loss, 164 (233) mL; at one year statistically significant (P<.0001) and clinically meaningful changes from baseline were reported in all PROs--reduced back pain (2.9 ±2.5 vs. 6.2 ±2.3 at intake), reduced leg pain (2.2 ±2.6 vs. 5.9 ±2.8), and ODI (22.4% ± 18.6 vs. 45.3% ± 15.3), as well as health-related quality of life (EQ-5D index: 0.71 ±0.28 vs. 0.34 ±0.32). More of the professional workers were working at one year than those prior to surgery (70.3% vs. 55.2%). Three AEs and one serious AE were considered

  6. Broadband observations of the naked-eye gamma-ray burst GRB 080319B.

    PubMed

    Racusin, J L; Karpov, S V; Sokolowski, M; Granot, J; Wu, X F; Pal'shin, V; Covino, S; van der Horst, A J; Oates, S R; Schady, P; Smith, R J; Cummings, J; Starling, R L C; Piotrowski, L W; Zhang, B; Evans, P A; Holland, S T; Malek, K; Page, M T; Vetere, L; Margutti, R; Guidorzi, C; Kamble, A P; Curran, P A; Beardmore, A; Kouveliotou, C; Mankiewicz, L; Melandri, A; O'Brien, P T; Page, K L; Piran, T; Tanvir, N R; Wrochna, G; Aptekar, R L; Barthelmy, S; Bartolini, C; Beskin, G M; Bondar, S; Bremer, M; Campana, S; Castro-Tirado, A; Cucchiara, A; Cwiok, M; D'Avanzo, P; D'Elia, V; Valle, M Della; de Ugarte Postigo, A; Dominik, W; Falcone, A; Fiore, F; Fox, D B; Frederiks, D D; Fruchter, A S; Fugazza, D; Garrett, M A; Gehrels, N; Golenetskii, S; Gomboc, A; Gorosabel, J; Greco, G; Guarnieri, A; Immler, S; Jelinek, M; Kasprowicz, G; La Parola, V; Levan, A J; Mangano, V; Mazets, E P; Molinari, E; Moretti, A; Nawrocki, K; Oleynik, P P; Osborne, J P; Pagani, C; Pandey, S B; Paragi, Z; Perri, M; Piccioni, A; Ramirez-Ruiz, E; Roming, P W A; Steele, I A; Strom, R G; Testa, V; Tosti, G; Ulanov, M V; Wiersema, K; Wijers, R A M J; Winters, J M; Zarnecki, A F; Zerbi, F; Mészáros, P; Chincarini, G; Burrows, D N

    2008-09-11

    Long-duration gamma-ray bursts (GRBs) release copious amounts of energy across the entire electromagnetic spectrum, and so provide a window into the process of black hole formation from the collapse of massive stars. Previous early optical observations of even the most exceptional GRBs (990123 and 030329) lacked both the temporal resolution to probe the optical flash in detail and the accuracy needed to trace the transition from the prompt emission within the outflow to external shocks caused by interaction with the progenitor environment. Here we report observations of the extraordinarily bright prompt optical and gamma-ray emission of GRB 080319B that provide diagnostics within seconds of its formation, followed by broadband observations of the afterglow decay that continued for weeks. We show that the prompt emission stems from a single physical region, implying an extremely relativistic outflow that propagates within the narrow inner core of a two-component jet.

  7. Soft X-ray observation of the prompt emission of GRB 100418A

    NASA Astrophysics Data System (ADS)

    Imatani, Ritsuko; Tomida, Hiroshi; Nakahira, Satoshi; Kimura, Masashi; Sakamoto, Takanori; Arimoto, Makoto; Morooka, Yoshitaka; Yonetoku, Daisuke; Kawai, Nobuyuki; Tsunemi, Hiroshi

    2016-06-01

    We have observed the prompt emission of GRB 100418A from its beginning captured by the MAXI SSC (0.7-7 keV) on board the International Space Station followed by the Swift XRT (0.3-10 keV) observation. The light curve can be fitted by a combination of a power-law component and an exponential component (the decay constant is 31.6 ± 1.6 s). The X-ray spectrum is well expressed by the Band function with Ep ≤ 8.3 keV. This is the brightest gamma-ray burst showing a very low value of Ep. It satisfies the Yonetoku relation (Ep-Lp). It is also consistent with the Amati relation (Ep-Eiso) within a 2.5σ level.

  8. Multi-wavelength Observations of GRB 111228A and Implications for the Fireball and its Environment

    NASA Astrophysics Data System (ADS)

    Xin, Li-Ping; Wang, Yuan-Zhu; Lin, Ting-Ting; Liang, En-Wei; Lü, Hou-Jun; Zhong, Shu-Qing; Urata, Yuji; Zhao, Xiao-Hong; Wu, Chao; Wei, Jian-Yan; Huang, Kui-Yun; Qiu, Yu-Lei; Deng, Jin-Song

    2016-02-01

    Observations of very early multi-wavelength afterglows are critical to reveal the properties of the radiating fireball and its environment as well as the central engine of gamma-ray bursts (GRBs). We report our optical observations of GRB 111228A from 95 s to about 50 hr after the burst trigger and investigate its properties of the prompt gamma-rays and the ambient medium using our data and the data from the Swift and Fermi missions. Our joint optical and X-ray spectral fits to the afterglow data show that the ambient medium features a low dust-to-gas ratio. Incorporating the energy injection effect, our best fit to the afterglow light curves with the standard afterglow model via the Markov Chain Monte Carlo technique shows that {ɛ }e=(6.9+/- 0.3)× {10}-2, {ɛ }B=(7.73+/- 0.62)× {10}-6,{E}K=(6.32+/- 0.86)× {10}53 {erg}, n=0.100+/- 0.014 cm-3. The low medium density likely implies that the afterglow jet may be in a halo or in a hot ISM. A chromatic shallow decay segment observed in the optical and X-ray bands is well explained with the long-lasting energy injection from the central engine, which would be a magnetar with a period of about 1.92 ms inferred from the data. The Ep of its time-integrated prompt gamma-ray spectrum is ˜26 KeV. Using the initial Lorentz factor ({{{Γ }}}0={476}-237+225) derived from our afterglow model fit, it is found that GRB 111228A satisfies the {L}{{iso}}-{E}p,z-{{{Γ }}}0 relation and bridges the typical GRBs and low luminosity GRBs in this relation.

  9. OBSERVATIONAL SEARCH FOR PeV-EeV TAU NEUTRINO FROM GRB081203A

    SciTech Connect

    Aita, Y.; Aoki, T.; Asaoka, Y.; Chonan, T.; Jobashi, M.; Masuda, M.; Morimoto, Y.; Noda, K.; Sasaki, M.; Asoh, J.; Ishikawa, N.; Ogawa, S.; Learned, J. G.; Matsuno, S.; Olsen, S.; Binder, P.-M.; Hamilton, J.; Sugiyama, N.; Watanabe, Y. E-mail: sasakim@icrr.u-tokyo.ac.jp

    2011-07-20

    We report the first observational search for tau neutrinos ({nu}{sub {tau}}) from gamma-ray bursts (GRBs) using one of the Ashra light collectors. The Earth-skimming {nu}{sub {tau}} technique of imaging Cherenkov {tau} showers was applied as a detection method. We set stringent upper limits on the {nu}{sub {tau}} fluence in PeV-EeV region for 3780 s (between 2.83 and 1.78 hr before) and another 3780 s (between 21.2 and 22.2 hr after) surrounding GRB081203A triggered by the Swift satellite. This first search for PeV-EeV {nu}{sub {tau}} complements other experiments in energy range and methodology, and suggests the prologue of 'multi-particle astronomy' with a precise determination of time and location.

  10. Upper limb evaluation and one-year follow up of non-ambulant patients with spinal muscular atrophy: an observational multicenter trial.

    PubMed

    Seferian, Andreea Mihaela; Moraux, Amélie; Canal, Aurélie; Decostre, Valérie; Diebate, Oumar; Le Moing, Anne Gaëlle; Gidaro, Teresa; Deconinck, Nicolas; Van Parys, Frauke; Vereecke, Wendy; Wittevrongel, Sylvia; Annoussamy, Mélanie; Mayer, Michèle; Maincent, Kim; Cuisset, Jean-Marie; Tiffreau, Vincent; Denis, Severine; Jousten, Virginie; Quijano-Roy, Susana; Voit, Thomas; Hogrel, Jean-Yves; Servais, Laurent

    2015-01-01

    Assessment of the upper limb strength in non-ambulant neuromuscular patients remains challenging. Although potential outcome measures have been reported, longitudinal data demonstrating sensitivity to clinical evolution in spinal muscular atrophy patients are critically lacking. Our study recruited 23 non-ambulant patients, 16 patients (males/females = 6/10; median age 15.4 years with a range from 10.7 to 31.1 years) with spinal muscular atrophy type II and 7 patients (males/females = 2/5; median age 19.9 years with a range from 8.3 to 29.9 years) with type III. The Brooke functional score was on median 3 with a range from 2 to 6. The average total vital capacity was 46%, and seven patients required non-invasive ventilation at night. Patients were assessed at baseline, 6 months, and 1 year using the Motor Function Measure and innovative devices MyoGrip, MyoPinch, and MoviPlate, which assess handgrip strength, key pinch strength, and hand/finger extension-flexion function, respectively. The study demonstrated the feasibility and reliability of these measures for all patients, and sensitivity to negative changes after the age of 14 years. The younger patients showed an increase of the distal force in the follow-up period. The distal force measurements and function were correlated to different functional scales. These data represent an important step in the process of validating these devices as potential outcome measures for future clinical trials.

  11. Upper Limb Evaluation and One-Year Follow Up of Non-Ambulant Patients with Spinal Muscular Atrophy: An Observational Multicenter Trial

    PubMed Central

    Canal, Aurélie; Decostre, Valérie; Diebate, Oumar; Le Moing, Anne Gaëlle; Gidaro, Teresa; Deconinck, Nicolas; Van Parys, Frauke; Vereecke, Wendy; Wittevrongel, Sylvia; Annoussamy, Mélanie; Mayer, Michèle; Maincent, Kim; Cuisset, Jean-Marie; Tiffreau, Vincent; Denis, Severine; Jousten, Virginie; Quijano-Roy, Susana; Voit, Thomas; Hogrel, Jean-Yves; Servais, Laurent

    2015-01-01

    Assessment of the upper limb strength in non-ambulant neuromuscular patients remains challenging. Although potential outcome measures have been reported, longitudinal data demonstrating sensitivity to clinical evolution in spinal muscular atrophy patients are critically lacking. Our study recruited 23 non-ambulant patients, 16 patients (males/females = 6/10; median age 15.4 years with a range from 10.7 to 31.1 years) with spinal muscular atrophy type II and 7 patients (males/females = 2/5; median age 19.9 years with a range from 8.3 to 29.9 years) with type III. The Brooke functional score was on median 3 with a range from 2 to 6. The average total vital capacity was 46%, and seven patients required non-invasive ventilation at night. Patients were assessed at baseline, 6 months, and 1 year using the Motor Function Measure and innovative devices MyoGrip, MyoPinch, and MoviPlate, which assess handgrip strength, key pinch strength, and hand/finger extension-flexion function, respectively. The study demonstrated the feasibility and reliability of these measures for all patients, and sensitivity to negative changes after the age of 14 years. The younger patients showed an increase of the distal force in the follow-up period. The distal force measurements and function were correlated to different functional scales. These data represent an important step in the process of validating these devices as potential outcome measures for future clinical trials. Trial Registration ClinicalTrials.gov NCT00993161 PMID:25861036

  12. Hubble space telescope observations of the afterglow, supernova, and host galaxy associated with the extremely bright GRB 130427A

    SciTech Connect

    Levan, A. J.; Tanvir, N. R.; Wiersema, K.; Fruchter, A. S.; Hounsell, R. A.; Graham, J.; Hjorth, J.; Fynbo, J. P. U.; Pian, E.; Mazzali, P.; Perley, D. A.; Cano, Z.; Cenko, S. B.; Kouveliotou, C.; Misra, K.

    2014-09-10

    We present Hubble Space Telescope (HST) observations of the exceptionally bright and luminous Swift gamma-ray burst (GRB), GRB 130427A. At z = 0.34, this burst affords an excellent opportunity to study the supernova (SN) and host galaxy associated with an intrinsically extremely luminous burst (E {sub iso} > 10{sup 54} erg): more luminous than any previous GRB with a spectroscopically associated SN. We use the combination of the image quality, UV capability, and invariant point-spread function of HST to provide the best possible separation of the afterglow, host, and SN contributions to the observed light ∼17 rest-frame days after the burst, utilizing a host subtraction spectrum obtained one year later. Advanced Camera for Surveys grism observations show that the associated SN, SN 2013cq, has an overall spectral shape and luminosity similar to SN 1998bw (with a photospheric velocity, v {sub ph} ∼ 15, 000 km s{sup –1}). The positions of the bluer features are better matched by the higher velocity SN 2010bh (v {sub ph} ∼ 30, 000 km s{sup –1}), but this SN is significantly fainter and fails to reproduce the overall spectral shape, perhaps indicative of velocity structure in the ejecta. We find that the burst originated ∼4 kpc from the nucleus of a moderately star forming (1 M {sub ☉} yr{sup –1}), possibly interacting disk galaxy. The absolute magnitude, physical size, and morphology of this galaxy, as well as the location of the GRB within it, are also strikingly similar to those of GRB 980425/SN 1998bw. The similarity of the SNe and environment from both the most luminous and least luminous GRBs suggests that broadly similar progenitor stars can create GRBs across six orders of magnitude in isotropic energy.

  13. Hubble Space Telescope Observations of the Afterglow, Supernova, and Host Galaxy Associated with the Extremely Bright GRB 130427A

    NASA Astrophysics Data System (ADS)

    Levan, A. J.; Tanvir, N. R.; Fruchter, A. S.; Hjorth, J.; Pian, E.; Mazzali, P.; Hounsell, R. A.; Perley, D. A.; Cano, Z.; Graham, J.; Cenko, S. B.; Fynbo, J. P. U.; Kouveliotou, C.; Pe'er, A.; Misra, K.; Wiersema, K.

    2014-09-01

    We present Hubble Space Telescope (HST) observations of the exceptionally bright and luminous Swift gamma-ray burst (GRB), GRB 130427A. At z = 0.34, this burst affords an excellent opportunity to study the supernova (SN) and host galaxy associated with an intrinsically extremely luminous burst (E iso > 1054 erg): more luminous than any previous GRB with a spectroscopically associated SN. We use the combination of the image quality, UV capability, and invariant point-spread function of HST to provide the best possible separation of the afterglow, host, and SN contributions to the observed light ~17 rest-frame days after the burst, utilizing a host subtraction spectrum obtained one year later. Advanced Camera for Surveys grism observations show that the associated SN, SN 2013cq, has an overall spectral shape and luminosity similar to SN 1998bw (with a photospheric velocity, v ph ~ 15, 000 km s-1). The positions of the bluer features are better matched by the higher velocity SN 2010bh (v ph ~ 30, 000 km s-1), but this SN is significantly fainter and fails to reproduce the overall spectral shape, perhaps indicative of velocity structure in the ejecta. We find that the burst originated ~4 kpc from the nucleus of a moderately star forming (1 M ⊙ yr-1), possibly interacting disk galaxy. The absolute magnitude, physical size, and morphology of this galaxy, as well as the location of the GRB within it, are also strikingly similar to those of GRB 980425/SN 1998bw. The similarity of the SNe and environment from both the most luminous and least luminous GRBs suggests that broadly similar progenitor stars can create GRBs across six orders of magnitude in isotropic energy.

  14. Constraints on Very High Energy Emission from GRB 130427A

    NASA Astrophysics Data System (ADS)

    Aliu, E.; Aune, T.; Barnacka, A.; Beilicke, M.; Benbow, W.; Berger, K.; Biteau, J.; Buckley, J. H.; Bugaev, V.; Byrum, K.; Cardenzana, J. V.; Cerruti, M.; Chen, X.; Ciupik, L.; Connaughton, V.; Cui, W.; Dickinson, H. J.; Eisch, J. D.; Errando, M.; Falcone, A.; Federici, S.; Feng, Q.; Finley, J. P.; Fleischhack, H.; Fortin, P.; Fortson, L.; Furniss, A.; Galante, N.; Gillanders, G. H.; Griffin, S.; Griffiths, S. T.; Grube, J.; Gyuk, G.; Håkansson, N.; Hanna, D.; Holder, J.; Hughes, G.; Humensky, T. B.; Johnson, C. A.; Kaaret, P.; Kar, P.; Kertzman, M.; Khassen, Y.; Kieda, D.; Krawczynski, H.; Krennrich, F.; Lang, M. J.; Madhavan, A. S.; Maier, G.; McArthur, S.; McCann, A.; Meagher, K.; Millis, J.; Moriarty, P.; Mukherjee, R.; Nieto, D.; O'Faoláin de Bhróithe, A.; Ong, R. A.; Otte, A. N.; Park, N.; Pohl, M.; Popkow, A.; Prokoph, H.; Pueschel, E.; Quinn, J.; Ragan, K.; Rajotte, J.; Reyes, L. C.; Reynolds, P. T.; Richards, G. T.; Roache, E.; Sembroski, G. H.; Shahinyan, K.; Smith, A. W.; Staszak, D.; Telezhinsky, I.; Tucci, J. V.; Tyler, J.; Varlotta, A.; Vassiliev, V. V.; Vincent, S.; Wakely, S. P.; Weiner, O. M.; Weinstein, A.; Welsing, R.; Wilhelm, A.; Williams, D. A.; Zitzer, B.; McEnery, J. E.; Perkins, J. S.; Veres, P.; Zhu, S.

    2014-11-01

    Prompt emission from the very fluent and nearby (z = 0.34) gamma-ray burst GRB 130427A was detected by several orbiting telescopes and by ground-based, wide-field-of-view optical transient monitors. Apart from the intensity and proximity of this GRB, it is exceptional due to the extremely long-lived high-energy (100 MeV to 100 GeV) gamma-ray emission, which was detected by the Large Area Telescope on the Fermi Gamma-Ray Space Telescope for ~70 ks after the initial burst. The persistent, hard-spectrum, high-energy emission suggests that the highest-energy gamma rays may have been produced via synchrotron self-Compton processes though there is also evidence that the high-energy emission may instead be an extension of the synchrotron spectrum. VERITAS, a ground-based imaging atmospheric Cherenkov telescope array, began follow-up observations of GRB 130427A ~71 ks (~20 hr) after the onset of the burst. The GRB was not detected with VERITAS; however, the high elevation of the observations, coupled with the low redshift of the GRB, make VERITAS a very sensitive probe of the emission from GRB 130427A for E > 100 GeV. The non-detection and consequent upper limit derived place constraints on the synchrotron self-Compton model of high-energy gamma-ray emission from this burst.

  15. CONSTRAINTS ON VERY HIGH ENERGY EMISSION FROM GRB 130427A

    SciTech Connect

    Aliu, E.; Errando, M.; Aune, T.; Barnacka, A.; Beilicke, M.; Buckley, J. H.; Bugaev, V.; Benbow, W.; Cerruti, M.; Berger, K.; Biteau, J.; Byrum, K.; Cardenzana, J. V; Dickinson, H. J.; Eisch, J. D.; Chen, X.; Ciupik, L.; Connaughton, V.; Cui, W.; Falcone, A. E-mail: sjzhu@umd.edu; and others

    2014-11-01

    Prompt emission from the very fluent and nearby (z = 0.34) gamma-ray burst GRB 130427A was detected by several orbiting telescopes and by ground-based, wide-field-of-view optical transient monitors. Apart from the intensity and proximity of this GRB, it is exceptional due to the extremely long-lived high-energy (100 MeV to 100 GeV) gamma-ray emission, which was detected by the Large Area Telescope on the Fermi Gamma-Ray Space Telescope for ∼70 ks after the initial burst. The persistent, hard-spectrum, high-energy emission suggests that the highest-energy gamma rays may have been produced via synchrotron self-Compton processes though there is also evidence that the high-energy emission may instead be an extension of the synchrotron spectrum. VERITAS, a ground-based imaging atmospheric Cherenkov telescope array, began follow-up observations of GRB 130427A ∼71 ks (∼20 hr) after the onset of the burst. The GRB was not detected with VERITAS; however, the high elevation of the observations, coupled with the low redshift of the GRB, make VERITAS a very sensitive probe of the emission from GRB 130427A for E > 100 GeV. The non-detection and consequent upper limit derived place constraints on the synchrotron self-Compton model of high-energy gamma-ray emission from this burst.

  16. Constraining properties of GRB magnetar central engines using the observed plateau luminosity and duration correlation

    NASA Astrophysics Data System (ADS)

    Rowlinson, A.; Gompertz, B. P.; Dainotti, M.; O'Brien, P. T.; Wijers, R. A. M. J.; van der Horst, A. J.

    2014-09-01

    An intrinsic correlation has been identified between the luminosity and duration of plateaus in the X-ray afterglows of gamma-ray bursts (GRBs; Dainotti et al. 2008), suggesting a central engine origin. The magnetar central engine model predicts an observable plateau phase, with plateau durations and luminosities being determined by the magnetic fields and spin periods of the newly formed magnetar. This paper analytically shows that the magnetar central engine model can explain, within the 1σ uncertainties, the correlation between plateau luminosity and duration. The observed scatter in the correlation most likely originates in the spread of initial spin periods of the newly formed magnetar and provides an estimate of the maximum spin period of ˜35 ms (assuming a constant mass, efficiency and beaming across the GRB sample). Additionally, by combining the observed data and simulations, we show that the magnetar emission is most likely narrowly beamed and has ≲20 per cent efficiency in conversion of rotational energy from the magnetar into the observed plateau luminosity. The beaming angles and efficiencies obtained by this method are fully consistent with both predicted and observed values. We find that short GRBs and short GRBs with extended emission lie on the same correlation but are statistically inconsistent with being drawn from the same distribution as long GRBs, this is consistent with them having a wider beaming angle than long GRBs.

  17. Hyper Cold Systems follow up

    NASA Astrophysics Data System (ADS)

    Berges, Jean Claude; Beltrando, Gerard; Cacault, Philippe

    2016-04-01

    The follow up of intense precipitation system is a key information for climate studies. Whereas some rainfall measurement series cover more than one century they cannot retrieve these phenomena in their spatial and temporal continuity. The geostationary satellite data offer a good trade-off between the length of data series and the retrieval accuracy. However a difficulty arise from ambiguous interpretation of the lone infrared signal in nephanalysis. Hence the tropopause temperature is used as a proxy to characterize extreme precipitation event. That does not mean that the more intense rain-rate will be always collocated with the coldest temperature but that most of these intense events is produced by systems whose a part is colder than tropopause. Computations have been carried out on 38 months of MSG and Meteosat/IODC. System follow up is achieved by a simple 3D connexity algorithm, the time being considered as the third dimension. This algorithm produce three dimension clusters from where the main system parameters can be easily extracted. Thus the systems can be classified trajectory characteristic (duration, speed ans size variation). A drawback of this simple threshold method relies is some over-segmentation. In most of case the bias is minor as unconnected clusters are small and short-lived. However an aggregating algorithm have been developed to retrieve the most complex system trajectories. To assess the efficiency of this method three regional studies are displayed: the North African Maghreb, the West African Sahel and the Indian Ocean. On Maghreb, the location of system initialization shows a dramatic difference between the eastern and western parts. Whereas in Tunisia a significant part of these systems are generated on sea and most have no clear relation with relief, the Morocco is mainly characterized with land initiated system with a strong orographic effect on system triggering. Another difference relies on the low level wind shear impact which

  18. The Optically Unbiased GRB Host (TOUGH) Survey. VI. Radio Observations at z <~ 1 and Consistency with Typical Star-forming Galaxies

    NASA Astrophysics Data System (ADS)

    Michałowski, M. J.; Kamble, A.; Hjorth, J.; Malesani, D.; Reinfrank, R. F.; Bonavera, L.; Castro Cerón, J. M.; Ibar, E.; Dunlop, J. S.; Fynbo, J. P. U.; Garrett, M. A.; Jakobsson, P.; Kaplan, D. L.; Krühler, T.; Levan, A. J.; Massardi, M.; Pal, S.; Sollerman, J.; Tanvir, N. R.; van der Horst, A. J.; Watson, D.; Wiersema, K.

    2012-08-01

    The objective of this paper is to determine the level of obscured star formation activity and dust attenuation in a sample of gamma-ray burst (GRB) hosts, and to test the hypothesis that GRB hosts have properties consistent with those of the general star-forming galaxy populations. We present a radio continuum survey of all z < 1 GRB hosts in The Optically Unbiased GRB Host (TOUGH) sample supplemented with radio data for all (mostly pre-Swift) GRB-SN hosts discovered before 2006 October. We present new radio data for 22 objects and have obtained a detection for three of them (GRB 980425, 021211, 031203; none in the TOUGH sample), increasing the number of radio-detected GRB hosts from two to five. The star formation rate (SFR) for the GRB 021211 host of ~825 M ⊙ yr-1, the highest ever reported for a GRB host, places it in the category of ultraluminous infrared galaxies. We found that at least ~63% of GRB hosts have SFR < 100 M ⊙ yr-1 and at most ~8% can have SFR > 500 M ⊙ yr-1. For the undetected hosts the mean radio flux (<35 μJy 3σ) corresponds to an average SFR < 15 M ⊙ yr-1. Moreover, >~ 88% of the z <~ 1 GRB hosts have ultraviolet dust attenuation A UV < 6.7 mag (visual attenuation AV < 3 mag). Hence, we did not find evidence for large dust obscuration in a majority of GRB hosts. Finally, we found that the distributions of SFRs and A UV of GRB hosts are consistent with those of Lyman break galaxies, Hα emitters at similar redshifts, and of galaxies from cosmological simulations. The similarity of the GRB population with other star-forming galaxies is consistent with the hypothesis that GRBs, a least at z <~ 1, trace a large fraction of all star formation, and are therefore less biased indicators than once thought. Based on observations collected at the European Southern Observatory, Paranal, Chile (ESO Large Programme 177.A-0591), the Australian Telescope Compact Array, the Giant Metrewave Radio Telescope, the Very Large Array, and the Westerbork

  19. GRB 011121: A Collimated Outflow into Wind-Blown Surroundings

    NASA Technical Reports Server (NTRS)

    Greiner, J.; Klose, S.; Salvato, M.; Zeh, A.; Schwarz, R.; Hartmann, D. H.; Masetti, N.; Stecklum, B.; Lamer, G.; Lodieu, N.; Burud, I.; Rhoads, J.; Fruchter, A.

    2003-01-01

    We report optical and near-infrared follow-up observations of GRB 011121 collected predominantly at ESO telescopes in Chile. We discover a break in the afterglow light curve after 1.3 days, which implies an initial jet opening angle of about 9 deg. The jet origin of this break is supported by the fact that the spectral energy distribution is achromatic during the first four days. During later phases, GRB 011121 shows significant excess emission above the flux predicted by a power law, which we interpret as additional light from an underlying supernova. In particular, the spectral energy distribution of the optical transient approximately 2 weeks after the burst is clearly not of power-law type, but can be presented by a black body with a temperature of approx. 6000 K. The deduced parameters for the decay slope as well as the spectral index favor a wind scenario, i.e. an outflow into a circum-burst environment shaped by the stellar wind of a massive GRB progenitor. Due to its low redshift of z=0.36, GRB 011121 has been the best example for the GRB-supernova connection until GRB 030329, and provides compelling evidence for a circum-burster wind region expected to exist if the progenitor was a massive star.

  20. Observed Communication in Couples Two Years after Integrative and Traditional Behavioral Couple Therapy: Outcome and Link with Five-Year Follow-up

    ERIC Educational Resources Information Center

    Baucom, Katherine J. W.; Sevier, Mia; Eldridge, Kathleen A.; Doss, Brian D.; Christensen, Andrew

    2011-01-01

    Objective: To examine changes in observed communication after therapy termination in distressed couples from a randomized clinical trial. Method: A total of 134 distressed couples were randomly assigned to either traditional behavioral couple therapy (TBCT; Jacobson & Margolin, 1979) or integrative behavioral couple therapy (IBCT; Jacobson &…

  1. GRB110715A: Multifrequency study of the first gamma-ray burst observed with ALMA

    NASA Astrophysics Data System (ADS)

    Sánchez-Ramírez, R.; de Ugarte Postigo, A.; Gorosabel, J.; Hankcock, P.; Murphy, T.; Lundgren, A.; Kann, D. A.; de Gregorio Monsalvo, I.; Fynbo, J. P. U.; Garcia-Appadoo, D.; Martín, S.; Kamble, A.; Kuin, M. P. M.; Oates, S. R.; Castro-Tirado, A. J.; Greiner, J.

    2013-05-01

    GRB 110715A had a bright afterglow that was obscured by a high Galactic extinction. We discovered the submillimetre counterpart with APEX and followed it in radio with ATCA for over 2 months. Additional submillimetre observations were performed with ALMA as a test of the ToO procedures during commissioning. UV, optical and NIR observations were performed with UVOT/Swift and GROND at the 2.2 m telescope in La Silla and X-ray data was obtained by XRT/Swift. The dataset is complemented with spectroscopic data from the X-shooter spectrograph at the VLT. From a broadband model we derive a peculiar density profile in the environment of the progenitor, with a discontinuity that produces a break in the light curve at ˜1 day after the burst onset. The absorption features present in the intermediate resolution optical/nIR spectra reveal a redshift of 0.8224 and a host galaxy environment with low ionisation and no velocity components beyond 30 km s^{-1}. These preliminary results will be published elsewhere Sanchez-Ramirez et al. (in preparation).

  2. The LCOGT NEO Follow-up Network

    NASA Astrophysics Data System (ADS)

    Lister, Tim; Greenstreet, Sarah; Gomez, Edward; Christensen, Eric J.; Larson, Stephen M.

    2016-10-01

    The LCOGT NEO Follow-up Network is using the telescopes of the Las Cumbres Observatory Global Telescope Network (LCOGT) and a web-based target selection, scheduling and data reduction system to confirm NEO candidates and characterize radar-targeted known NEOs. Starting in July 2014, the LCOGT NEO Follow-up Network has observed over 3,500 targets and reported more than 16,000 astrometric and photometric measurements to the Minor Planet Center (MPC).The LCOGT NEO Follow-up Network's main aims are to perform confirming follow-up of the large number of NEO candidates and to perform characterization measurements of radar targets to obtain light curves and rotation rates. The NEO candidates come from the NEO surveys such as Catalina, PanSTARRS, ATLAS, NEOWISE and others. In particular, we are targeting objects in the Southern Hemisphere, where the LCOGT NEO Follow-up Network is the largest resource for NEO observations.LCOGT has completed the first phase of the deployment with the installation and commissioning of the nine 1-meter telescopes at McDonald Observatory (Texas), Cerro Tololo (Chile), SAAO (South Africa) and Siding Spring Observatory (Australia). The telescope network has been fully operational since 2014 May, and observations are being executed remotely and robotically. Future expansion to a site at Ali Observatory, Tibet is planned for 2017-2018.We have developed web-based software called NEOexchange which automatically downloads and aggregates NEO candidates from the Minor Planet Center's NEO Confirmation Page, the Arecibo and Goldstone radar target lists and the NASA ARM list. NEOexchange allows the planning and scheduling of observations on the LCOGT Telescope Network and the tracking of the resulting blocks and generated data. We have recently extended the NEOexchange software to include automated data reduction to re-compute the astrometric solution, determine the photometric zeropoint and find moving objects and present these results to the user via

  3. The University of Arizona Astronomy Club Follow-up Observations of Transiting Extra-solar Planet HAT-P-36b

    NASA Astrophysics Data System (ADS)

    Thompson, Robert; Turner, J.; Jones, C.; Pearson, K.; Biddle, L. I.; Berube, M.

    2013-06-01

    We observed 5 primary transits of exoplanet HAT-P-36b with the Steward Observatory 1.55 meter Kuiper Telescope in the U and R photometric bands. With our results, we have been able to produce a more complete light curve and refine previously published values for the planet’s mass, radius, density, surface gravity, Safronov number, equilibrium temperature, orbital distance, orbital inclination. We developed a modeling package that uses the Levenberg-Marquardt minimization algorithm to find the least-squares best fit to the light curve. The errors were generated using a bootstrap Monte Carlo method. The red noise of the transit was determined by using the permutation “rosary bead” method, which constrains the red noise in our transits better than the publicly available modeling package, TAP.

  4. Observations related to the Salmonella EU layer baseline survey in the United Kingdom: follow-up of positive flocks and sensitivity issues

    PubMed Central

    CARRIQUE-MAS, J. J.; BRESLIN, M.; SNOW, L.; ARNOLD, M. E.; WALES, A.; McLAREN, I.; DAVIES, R. H.

    2008-01-01

    SUMMARY A follow-on study was carried out on 23 holdings identified as Salmonella positive in the 2004/2005 European Union (EU) baseline survey of Salmonella in laying hens. Eleven of 13 cage and 4/7 floor houses remained positive for Salmonella when the new flock was tested, and from 10/13 cage and 3/7 floor houses a Salmonella of the same serovar/phage type as found in the EU survey was isolated. There was a high correlation between the level of contamination in the houses at the time of the EU survey and in the follow-on flock. On seven occasions the house identified as positive in the EU survey was sampled after cleaning and disinfection but before a new flock was placed, and in all of them Salmonella could be isolated from the houses. The observed number of infected houses in infected holdings suggests that the holding-level prevalence in the United Kingdom would be about 21% higher than the results obtained in the EU survey. PMID:18177519

  5. [A follow-up study on pulmonary functions of workers exposed to various forms of dust. Observation on the workers of pneumoconiosis in Kitakyushu].

    PubMed

    Baba, Y; Iwao, S; Kodama, Y

    1983-09-01

    Serial spirograms of 121 dust workers whose chest X-rays were found to be "class 1" of the diagnostic criteria for pneumoconiosis were obtained during 1978-80. Yearly changes of pulmonary function variables (%VC, FEV1, FEV1/FVC%,V25/H, and V50/V25) by age, smoking habit, total years of exposure to dust, and work history were evaluated. The average age of the dust workers was 48.0 +/- 5.5 years, and the average years of exposure to dust was 21.6 +/- 6.8 years in 1978. Eighty-two dust workers smoked with the mean smoking history of 24.7 pack-years. No significant differences of spirograms were found between the smoking and non-smoking groups. Among the smokers, however, linear regression of FEV1/FVC% by age gradually decreased during 1978-80. All the pulmonary function variables showed no correlation with smoking history as well as total years of dust exposure. All the dust workers were classified into eight types of work by their histories; crushing and quarrying operators, brick mason, foundry and grinding operators, asbestos workers, underground miners, refractory material workers, pyrites roasters, and welders. The underground miners showed lower FEV1/FVC% and V25 than the average. However, the difference of such pulmonary function variables by eight types of work was not significant by analysis of variance. Since aging is the most dominant factor for pulmonary dysfunction, a longer observation on this group will be needed.

  6. [A follow-up study on pulmonary functions of workers exposed to various forms of dust. Observation on the workers of pneumoconiosis in Kitakyushu].

    PubMed

    Baba, Y; Iwao, S; Kodama, Y

    1983-09-01

    Serial spirograms of 121 dust workers whose chest X-rays were found to be "class 1" of the diagnostic criteria for pneumoconiosis were obtained during 1978-80. Yearly changes of pulmonary function variables (%VC, FEV1, FEV1/FVC%,V25/H, and V50/V25) by age, smoking habit, total years of exposure to dust, and work history were evaluated. The average age of the dust workers was 48.0 +/- 5.5 years, and the average years of exposure to dust was 21.6 +/- 6.8 years in 1978. Eighty-two dust workers smoked with the mean smoking history of 24.7 pack-years. No significant differences of spirograms were found between the smoking and non-smoking groups. Among the smokers, however, linear regression of FEV1/FVC% by age gradually decreased during 1978-80. All the pulmonary function variables showed no correlation with smoking history as well as total years of dust exposure. All the dust workers were classified into eight types of work by their histories; crushing and quarrying operators, brick mason, foundry and grinding operators, asbestos workers, underground miners, refractory material workers, pyrites roasters, and welders. The underground miners showed lower FEV1/FVC% and V25 than the average. However, the difference of such pulmonary function variables by eight types of work was not significant by analysis of variance. Since aging is the most dominant factor for pulmonary dysfunction, a longer observation on this group will be needed. PMID:6679643

  7. Upper Limb Strength and Function Changes during a One-Year Follow-Up in Non-Ambulant Patients with Duchenne Muscular Dystrophy: An Observational Multicenter Trial

    PubMed Central

    Seferian, Andreea Mihaela; Moraux, Amélie; Annoussamy, Mélanie; Canal, Aurélie; Decostre, Valérie; Diebate, Oumar; Le Moing, Anne-Gaëlle; Gidaro, Teresa; Deconinck, Nicolas; Van Parys, Frauke; Vereecke, Wendy; Wittevrongel, Sylvia; Mayer, Michèle; Maincent, Kim; Desguerre, Isabelle; Thémar-Noël, Christine; Cuisset, Jean-Marie; Tiffreau, Vincent; Denis, Severine; Jousten, Virginie; Quijano-Roy, Susana; Voit, Thomas; Hogrel, Jean-Yves; Servais, Laurent

    2015-01-01

    Introduction Upper limb evaluation of patients with Duchenne Muscular Dystrophy is crucially important to evaluations of efficacy of new treatments in non-ambulant patients. In patients who have lost ambulation, there are few validated and informative outcome measures. In addition, longitudinal data demonstrating sensitivity to clinical evolution of outcome measures over short-term periods are lacking. Patients and Methods We report here the results of a one-year multicenter study using specifically designed tools to assess grip, pinch strength, and hand function in wheelchair-bound patients. Our study assessed 53 non-ambulant patients with Duchenne muscular dystrophy aged 17.1 ± 4.8 years (range: 9 – 28.1 years). The average Brooke functional score of these patients was 4.6 ± 1.1. The average forced vital capacity was 44.5% predicted and 19 patients used non-invasive ventilation. Patients were assessed at baseline, 6 months, and one year using the Motor Function Measure and innovative devices (namely the MyoSet composed of MyoGrip, MyoPinch, and MoviPlate). Results Our study confirmed preliminary data previously reported regarding feasibility of use and of reliability of the MyoSet and the correlation at baseline between distal strength and clinical outcomes such as FVC, Brooke score, age, and duration since loss of ambulation. A significant correlation was observed between the distal upper limb strength and clinical variables. The sensitive dynamometers (MyoGrip and MyoPinch) and MoviPlate captured a 12-month change in non-ambulant Duchenne muscular dystrophy patients of all ages. Trial Registration ClinicalTrials.gov NCT00993161 NCT00993161 PMID:25643053

  8. Robotic Follow-up of Microlensing Events

    NASA Astrophysics Data System (ADS)

    Street, Rachel; Microlensing Project, RoboNet

    2009-05-01

    Several hundred galactic microlensing events are now routinely discovered every year, of which a few exhibit anomalous behavior due to the presence of an exoplanet orbiting the lensing body. Ground based follow-up of these events requires a co-ordinated observing program using network of telescopes observing around the clock. The RoboNet microlensing project is taking advantage of the robotic scheduling capabilities of LCOGT and the Liverpool Telescope to provide responsive photometric follow-up of carefully selected events. Currently LCOGT has two, 2m telescopes available via our network and are in the process of building and deploying networks of 1m and 0.4m telescopes. Once online, these facilities will provide 24hr coverage of microlensing events. Here we highlight results from the RoboNet Project to date and describe the software we have developed to optimize our response to planetary events.

  9. X-Ray Spectral Components Observed in the Afterglow of GRB 130925A

    NASA Technical Reports Server (NTRS)

    Bellm, Eric C.; Barriere, Nicolas M.; Bhalerao, Varun; Boggs, Steven E.; Cenko, S. Bradley; Christensen, Finn E.; Craig, William W.; Forster, Karl; Fryer, Chris L.; Hailey, Charles J.; Harrison, Fiona A.; Horesh, Assaf; Kouveliotou, Chryssa; Madsen, Kristin K.; Miller, Jon M.; Ofek, Eran O.; Perley, Daniel A.; Rana, Vikram R.; Miller, Jon M.; Stern, Daniel; Tomsick, John A.; Zhang, William W.

    2014-01-01

    We have identified spectral features in the late-time X-ray afterglow of the unusually long, slow-decaying GRB 130925A using NuSTAR, Swift/X-Ray Telescope, and Chandra. A spectral component in addition to an absorbed power law is required at greater than 4 less than 1 significance, and its spectral shape varies between two observation epochs at 2 x 10 (sup 5) and 10 (sup 6) seconds after the burst. Several models can fit this additional component, each with very different physical implications. A broad, resolved Gaussian absorption feature of several kiloelectronvolts width improves the fit, but it is poorly constrained in the second epoch. An additive blackbody or second power-law component provide better fits. Both are challenging to interpret: the blackbody radius is near the scale of a compact remnant (10 (sup 8) centimeters), while the second power-law component requires an unobserved high-energy cutoff in order to be consistent with the non-detection by Fermi/Large Area Telescope.

  10. X-ray follow-up observations of the two γ-ray pulsars PSR J1459-6053 and PSR J1614-2230

    NASA Astrophysics Data System (ADS)

    Pancrazi, B.; Webb, N. A.; Becker, W.; Cognard, I.; Guillemot, L.; Hill, A. B.; Jackson, M.; Mignani, R. P.; Rea, N.

    2012-08-01

    Aims: We have observed two newly detected γ-ray pulsars, PSR J1459-6053 and PSR J1614-2230, in the X-ray domain with XMM-Newton to try to enlarge the sample of pulsars for which multi-wavelength data exist. We use these data with the aim of understanding the pulsar emission mechanisms of these pulsars. Methods: We analysed the X-ray spectra to determine whether the emission emanates from the neutron star surface (thermal emission) or from the magnetosphere (non-thermal emission) and compared this to the region in the magnetosphere in which the γ-ray emission is generated. Furthermore, we compared the phase-folded X-ray lightcurves with those in the γ-ray and, where possible, radio domains, to elicit additional information on the emission sites. Results: J1459-6053 shows X-ray spectra that are best fitted with a power law model with a photon index Γ=2.10+1.24-0.85. The γ-ray data suggest that either the slot gap or the outer gap model may be best to describe the emission from this pulsar. Analysis of the X-ray lightcurve folded on the γ-ray ephemeris shows modulation at the 3.7σ level in the 1.0-4.5 keV domain. Possible alignment of the main γ-ray and X-ray peaks also supports the interpretation that the emission in the two energy domains emanates from similar regions. The millisecond pulsar J1614-2230 exhibits an X-ray spectrum with a substantial thermal component, where the best-fitting spectral model is either two blackbodies, with kT=0.15+0.04-0.04 and 0.88+2.54-0.54 keV or a blackbody with similar temperature to the previous cooler component, kT=0.13+0.04-0.02 keV and a power law component with a photon index Γ=1.25+2.30-1.75. The cooler blackbody component is likely to originate from the hot surface at the polar cap. Analysis of the X-ray lightcurve folded on the radio ephemeris shows modulation at the 4.0σ level in the 0.4-3.0 keV domain.

  11. Hubble Space Telescope Observations of the Afterglow, Supernova and Host Galaxy Associated with the Extremely Bright GRB 130427A

    NASA Technical Reports Server (NTRS)

    Levan, A.J.; Tanvir, N. R.; Fruchter, A. S.; Hjorth, J.; Pian, E.; Mazzali, P.; Hounsell, R. A.; Perley, D. A.; Cano, Z.; Graham, J.; Cenko, S. B.; Fynbo, J. P. U.; Kouveliotou, C.; Pe'er, A.; Misra, K.; Wiersema, K.

    2014-01-01

    We present Hubble Space Telescope (HST) observations of the exceptionally bright and luminous Swift gamma-ray burst, GRB 130427A. At z=0.34 this burst affords an excellent opportunity to study the supernova and host galaxy associated with an intrinsically extremely luminous burst (E(sub iso) greater than 10(exp 54) erg): more luminous than any previous GRB with a spectroscopically associated supernova. We use the combination of the image quality, UV capability and and invariant PSF of HST to provide the best possible separation of the afterglow, host and supernova contributions to the observed light approximately 17 rest-frame days after the burst utilising a host subtraction spectrum obtained 1 year later. Advanced Camera for Surveys (ACS) grism observations show that the associated supernova, SN 2013cq, has an overall spectral shape and luminosity similar to SN 1998bw (with a photospheric velocity, vph approximately 15,000 kilometers per second). The positions of the bluer features are better matched by the higher velocity SN 2010bh (vph approximately 30,000 kilometers per second), but SN 2010bh (vph approximately 30,000 kilometers per second but this SN is significantly fainter, and fails to reproduce the overall spectral shape, perhaps indicative of velocity structure in the ejecta. We find that the burst originated approximately 4 kpc from the nucleus of a moderately star forming (1 Solar Mass yr(exp-1)), possibly interacting disc galaxy. The absolute magnitude, physical size and morphology of this galaxy, as well as the location of the GRB within it are also strikingly similar to those of GRB980425SN 1998bw. The similarity of supernovae and environment from both the most luminous and least luminous GRBs suggests broadly similar progenitor stars can create GRBs across six orders of magnitude in isotropic energy.

  12. Fermi/GBM observations of the ultra-long GRB 091024. A burst with an optical flash

    NASA Astrophysics Data System (ADS)

    Gruber, D.; Krühler, T.; Foley, S.; Nardini, M.; Burlon, D.; Rau, A.; Bissaldi, E.; von Kienlin, A.; McBreen, S.; Greiner, J.; Bhat, P. N.; Briggs, M. S.; Burgess, J. M.; Chaplin, V. L.; Connaughton, V.; Diehl, R.; Fishman, G. J.; Gibby, M. H.; Giles, M. M.; Goldstein, A.; Guiriec, S.; van der Horst, A. J.; Kippen, R. M.; Kouveliotou, C.; Lin, L.; Meegan, C. A.; Paciesas, W. S.; Preece, R. D.; Tierney, D.; Wilson-Hodge, C.

    2011-04-01

    Aims: In this paper we examine gamma-ray and optical data of GRB 091024, a gamma-ray burst (GRB) with an extremely long duration of T90 ≈ 1020 s, as observed with the Fermi Gamma-ray Burst Monitor (GBM). Methods: We present spectral analysis of all three distinct emission episodes using data from Fermi/GBM. Because of the long nature of this event, many ground-based optical telescopes slewed to its location within a few minutes and thus were able to observe the GRB during its active period. We compare the optical and gamma-ray light curves. Furthermore, we estimate a lower limit on the bulk Lorentz factor from the variability and spectrum of the GBM light curve and compare it with that obtained from the peak time of the forward shock of the optical afterglow. Results: From the spectral analysis we note that, despite its unusually long duration, this burst is similar to other long GRBs, i.e. there is spectral evolution (both the peak energy and the spectral index vary with time) and spectral lags are measured. We find that the optical light curve is highly anti-correlated to the prompt gamma-ray emission, with the optical emission reaching the maximum during an epoch of quiescence in the prompt emission. We interpret this behavior as the reverse shock (optical flash), expected in the internal-external shock model of GRB emission but observed only in a handful of GRBs so far. The lower limit on the initial Lorentz factor deduced from the variability time scale (Γmin = 195_{-110+90}) is consistent within the error to the one obtained using the peak time of the forward shock (Γ0 = 120) and is also consistent with Lorentz factors of other long GRBs.

  13. Constraints on an Optical Afterglow and on Supernova Light Following the Short Burst GRB 050813

    NASA Technical Reports Server (NTRS)

    Ferrero, P.; Sanchez, S. F.; Kann, D. A.; Klose, S.; Greiner, J.; Gorosabel, J.; Hartmann, D. H.; Henden, A. A.; Moller, P.; Palazzi, E.; Rau, A.; Stecklum, B.; Castro-Tirado, A. J.; Fynbok J. P. U.; Hjorth, J.; Jakobsson, P.; Kouveliotou, C.; Masetti, N.; Pian, E.; Tanvir, N. R.; Wijers, R. A. M. J.

    2006-01-01

    We report early follow-up observations of the error box of the short burst 050813 using the telescopes at Calar Alto and at Observatorio Sierra Nevada (OSN), followed by deep VLT/FORS2 I-band observations obtained under very good seeing conditions 5.7 and 11.7 days after the event. No evidence for a GRB afterglow was found in our Calar Alto and OSN data, no rising supernova component was detected in our FORS2 images. A potential host galaxy can be identified in our FORS2 images, even though we cannot state with certainty its association with GRB 050813. IN any case, the optical afterglow of GRB 050813 was very faint, well in agreement with what is known so far about the optical properties of afterglows of short bursts. We conclude that all optical data are not in conflict with the interpretation that GRB 050813 was a short burst.

  14. DESAlert: Enabling real-time transient follow-up with Dark Energy Survey data

    SciTech Connect

    Poci, A.

    2015-04-12

    The Dark Energy Survey (DES) is currently undertaking an observational program imaging 1/4 of the southern hemisphere sky with unprecedented photometric accuracy. In the process of observing millions of faint stars and galaxies to constrain the parameters of the dark energy equation of state, the DES will obtain pre-discovery images of the regions surrounding an estimated 100 gamma-ray bursts (GRBs) over five years. Once GRBs are detected by, e.g., the Swift satellite, the DES data will be extremely useful for follow-up observations by the transient astronomy community. We describe a recently-commissioned suite of software that listens continuously for automated notices of GRB activity, collates useful information from archival DES data, and promulgates relevant data products back to the community in near-real-time. Of particular importance are the opportunities that DES data provide for relative photometry of GRBs or their afterglows, as well as for identifying key characteristics (e.g., photometric redshifts) of potential GRB host galaxies. We provide the functional details of the DESAlert software as it presently operates, as well as the data products that it produces, and we show sample results from the application of DESAlert to several previously-detected GRBs.

  15. The LCOGT NEO Follow-up Network

    NASA Astrophysics Data System (ADS)

    Lister, Tim A.; Greenstreet, S.; Gomez, E.; Christensen, E.; Larson, S.

    2016-01-01

    Las Cumbres Observatory Global Telescope Network (LCOGT) has deployed a homogeneous telescope network of nine 1-meter telescopes to four locations in the northern and southern hemispheres, with a planned network size of twelve 1-meter telescopes at 6 locations. This network is very versatile and is designed to respond rapidly to target of opportunity events and also to perform long term monitoring of slowly changing astronomical phenomena. The global coverage of the network and the apertures of telescope available make LCOGT ideal for follow-up and characterization of Solar System objects (e.g. asteroids, Kuiper Belt Objects, comets, Near-Earth Objects (NEOs)) and additionally for the discovery of new objects. We are using the LCOGT network to confirm newly detected NEO candidates produced by the major sky surveys such as Catalina Sky Survey (CSS) and PanSTARRS (PS1&2) and several hundred targets are now being followed per year. An increasing amount of time is being spent to obtain follow-up astrometry and photometry for radar-targeted objects and those on the Near-Earth Object Human Space Flight Accessible Targets Study (NHATS) or Asteroid Retrieval Mission (ARM) lists in order to improve the orbits, determine the light curves and rotation periods and improve the characterization. This will be extended to obtain more light curves of other NEOs which could be targets. Recent results have included the first period determinations for several of the Goldstone-targeted NEOs. We are in the process of building a NEO follow-up portal which will allow professionals, amateurs and Citizen Scientists to plan, schedule and analyze NEO imaging and spectroscopy observations and data using the LCOGT Network and to act as a co-ordination hub for the NEO follow-up efforts.

  16. A Reverse Shock in GRB 160509A

    NASA Astrophysics Data System (ADS)

    Laskar, T.; Alexander, K. D.; Berger, E.

    2016-10-01

    Through detailed multi-wavelength observations and modeling, we present the discovery and characterization a reverse shock in GRB 160509A. This result highlights the unique power of radio observations in the study of GRB reverse shocks.

  17. Optical and X-Ray Observations of GRB 060526: A Complex Afterglow Consistent with an Achromatic Jet Break

    NASA Technical Reports Server (NTRS)

    Dai, X.; Halpern, J. P.; Morgan, N. D.; Armstrong, E.; Mirabal, N.; Haislip. J. B.; Reichart, D. E.; Stanek, K. Z.

    2007-01-01

    We obtained 98 R-band and 18 B, r', i' images of the optical afterglow of GRB 060526 (z = 3.21) with the MDM 1.3 m, 2.4 m, and the PROMPT telescopes at CTIO over the five nights following the burst trigger. Combining these data with other optical observations reported in GCN and the Swift XRT observations, we compare the optical and X-ray afterglow light curves of GRB 060526. Both the optical and X-ray afterglow light curves show rich features, such as flares and breaks. The densely sampled optical observations provide very good coverage at T > 10(exp 4) s. We observed a break at 2.4 x 10(exp 5) sin the optical afterglow light curve. Compared with the X-ray afterglow light curve, the break is consistent with an achromatic break supporting the beaming models of GRBs. However, the prebreak and postbreak temporal decay slopes are difficult to explain in simple afterglow models. We estimated a jet angle of theta(sub j) approx. 7deg and a prompt emission size of R(sub prompt) approx. 2 x 10(exp 14) cm. In addition, we detected several optical flares with amplitudes of (Delta)m approx. 0.2,0.6, and 0.2 mag. The X-ray afterglows detected by Swift have shown complicated decay patterns. Recently, many well-sampled optical afterglows also show decays with flares and multiple breaks. GRB 060526 provides an additional case of such a complex, well-observed optical afterglow. The accumulated well-sampled afterglows indicate that most of the optical afterglows are complex.

  18. Outcomes observed during a 1-year clinical and radiographic follow-up of patients treated for 1- or 2-level cervical degenerative disease using a biodegradable anterior cervical plate.

    PubMed

    Chen, Mengcun; Yang, Shuhua; Yang, Cao; Xu, Weihua; Ye, Shunan; Wang, Jing; Feng, Yong; Yang, Wen; Liu, Xianzhe

    2016-08-01

    OBJECTIVE The purpose of this study was to present an initial surgical experience in the management of 1- or 2-level degenerative disc disease of the cervical spine using biodegradable anterior cervical plates (bACPs) in anterior cervical discectomy and fusion (ACDF). The authors also aimed to provide insight into this critical and controversial clinical issue by clarifying outcomes for patients receiving bACPs and by comparing their outcomes with those achieved using a traditional metallic anterior cervical plate (mACP) implant. METHODS A retrospective review was conducted for 2 series of patients who had undergone ACDF using either bACP (31 patients, 38 segments) or mACP (47 patients, 57 segments) instrumentation. The patients were followed up for a mean 13.5 ± 0.9 months (range 12-18 months) in the bACP group and 14.8 ± 1.5 months (range 14-22 months) in the mACP group. Clinical outcomes were determined according to scores on the visual analog scale (VAS), the modified Japanese Orthopaedic Association (mJOA) scoring system, and Odom's criteria. Radiological images were used to assess fusion rates, intervertebral height, Cobb's angle, and the width of prevertebral soft tissue. RESULTS Both VAS and mJOA scores were significantly improved at each follow-up in both groups. Excellent or good results according to Odom's criteria were achieved in 93.5% (29/31) of patients in the bACP group and 93.6% (44/47) of patients in the mACP group. At 6 months postoperatively, the fusion rate was 94.7% (36/38) in the bACP group and 96.5% (55/57) in the mACP group, but subsidence of the intervertebral space at the surgical level was more evident in the bACP group. Angulation, as measured by Cobb's angle, demonstrated obvious healing in both groups, while better maintenance was observed in the mACP group. The local inflammatory reaction was uneventful during follow-up. Dysphonia and dysphagia were observed in both groups during the follow-up. CONCLUSIONS The relatively comparable

  19. Outcomes observed during a 1-year clinical and radiographic follow-up of patients treated for 1- or 2-level cervical degenerative disease using a biodegradable anterior cervical plate.

    PubMed

    Chen, Mengcun; Yang, Shuhua; Yang, Cao; Xu, Weihua; Ye, Shunan; Wang, Jing; Feng, Yong; Yang, Wen; Liu, Xianzhe

    2016-08-01

    OBJECTIVE The purpose of this study was to present an initial surgical experience in the management of 1- or 2-level degenerative disc disease of the cervical spine using biodegradable anterior cervical plates (bACPs) in anterior cervical discectomy and fusion (ACDF). The authors also aimed to provide insight into this critical and controversial clinical issue by clarifying outcomes for patients receiving bACPs and by comparing their outcomes with those achieved using a traditional metallic anterior cervical plate (mACP) implant. METHODS A retrospective review was conducted for 2 series of patients who had undergone ACDF using either bACP (31 patients, 38 segments) or mACP (47 patients, 57 segments) instrumentation. The patients were followed up for a mean 13.5 ± 0.9 months (range 12-18 months) in the bACP group and 14.8 ± 1.5 months (range 14-22 months) in the mACP group. Clinical outcomes were determined according to scores on the visual analog scale (VAS), the modified Japanese Orthopaedic Association (mJOA) scoring system, and Odom's criteria. Radiological images were used to assess fusion rates, intervertebral height, Cobb's angle, and the width of prevertebral soft tissue. RESULTS Both VAS and mJOA scores were significantly improved at each follow-up in both groups. Excellent or good results according to Odom's criteria were achieved in 93.5% (29/31) of patients in the bACP group and 93.6% (44/47) of patients in the mACP group. At 6 months postoperatively, the fusion rate was 94.7% (36/38) in the bACP group and 96.5% (55/57) in the mACP group, but subsidence of the intervertebral space at the surgical level was more evident in the bACP group. Angulation, as measured by Cobb's angle, demonstrated obvious healing in both groups, while better maintenance was observed in the mACP group. The local inflammatory reaction was uneventful during follow-up. Dysphonia and dysphagia were observed in both groups during the follow-up. CONCLUSIONS The relatively comparable

  20. The LCOGT NEO Follow-up Network

    NASA Astrophysics Data System (ADS)

    Lister, Tim; Gomez, Edward; Greenstreet, Sarah

    2015-08-01

    Las Cumbres Observatory Global Telescope Network (LCOGT) has deployed a homogeneous telescope network of nine 1-meter telescopes to four locations in the northern and southern hemispheres, with a planned network of twelve 1-meter telescopes at 6 locations. This network is very versatile and is designed to respond rapidly to target of opportunity events and also to perform long term monitoring of slowly changing astronomical phenomena. The global coverage of the network and the apertures of telescope available make LCOGT ideal for follow-up and characterization of Solar System objects (e.g. asteroids, Kuiper Belt Objects, comets, Near-Earth Objects (NEOs)) and ultimately for the discovery of new objects.LCOGT has completed the first phase of the deployment with the installation and commissioning of the nine 1-meter telescopes at McDonald Observatory (Texas), Cerro Tololo (Chile), SAAO (South Africa) and Siding Spring Observatory (Australia). The telescope network has been fully operational since 2014 May, and observations are being executed remotely and robotically. Future expansion to sites in the Canary Islands and Tibet is planned for 2016.I am using the LCOGT network to confirm newly detected NEO candidates produced by the major sky surveys such as Catalina Sky Survey (CSS) and PanSTARRS (PS1) and several hundred targets are now being followed-up per year. An increasing amount of time is being spent to obtain follow-up astrometry and photometry for radar-targeted objects and those on the Near-Earth Object Human Space Flight Accessible Targets Study (NHATS) or Asteroid Retrieval Mission (ARM) lists in order to improve the orbits, determine the light curves and rotation periods and improve the characterization. This will be extended to obtain more light curves of other NEOs which could be targets. Recent results have included the first period determinations for several of the Goldstone-targeted NEOs. We are in the process of building a NEO Portal which will allow

  1. CONSTRAINTS ON THE SYNCHROTRON SHOCK MODEL FOR THE FERMI GRB 090820A OBSERVED BY GAMMA-RAY BURST MONITOR

    SciTech Connect

    Burgess, J. Michael; Preece, Robert D.; Briggs, Michael S.; Connaughton, Valerie; Guiriec, Sylvain; Paciesas, William S.; Bhat, P. N.; Chaplin, Vandiver; Goldstein, Adam; Baring, Matthew G.; Meegan, Charles A.; Bissaldi, Elisabetta; Diehl, Roland; Greiner, Jochen; Gruber, David; Fishman, Gerald J.; Gibby, Melissa; Giles, Misty E-mail: baring@rice.edu

    2011-11-01

    Discerning the radiative dissipation mechanism for prompt emission in gamma-ray bursts (GRBs) requires detailed spectroscopic modeling that straddles the {nu}F{sub {nu}} peak in the 100 keV-1 MeV range. Historically, empirical fits such as the popular Band function have been employed with considerable success in interpreting the observations. While extrapolations of the Band parameters can provide some physical insight into the emission mechanisms responsible for GRBs, these inferences do not provide a unique way of discerning between models. By fitting physical models directly, this degeneracy can be broken, eliminating the need for empirical functions; our analysis here offers a first step in this direction. One of the oldest, and leading, theoretical ideas for the production of the prompt signal is the synchrotron shock model. Here we explore the applicability of this model to a bright Fermi gamma-ray burst monitor (GBM) burst with a simple temporal structure, GRB 090820A. Our investigation implements, for the first time, thermal and non-thermal synchrotron emissivities in the RMFIT forward-folding spectral analysis software often used in GBM burst studies. We find that these synchrotron emissivities, together with a blackbody shape, provide at least as good a match to the data as the Band GRB spectral fitting function. This success is achieved in both time-integrated and time-resolved spectral fits.

  2. Constraints on the Synchrotron Shock Model for the Fermi GRB 090820A Observed by Gamma-Ray Burst Monitor

    NASA Astrophysics Data System (ADS)

    Burgess, J. Michael; Preece, Robert D.; Baring, Matthew G.; Briggs, Michael S.; Connaughton, Valerie; Guiriec, Sylvain; Paciesas, William S.; Meegan, Charles A.; Bhat, P. N.; Bissaldi, Elisabetta; Chaplin, Vandiver; Diehl, Roland; Fishman, Gerald J.; Fitzpatrick, Gerard; Foley, Suzanne; Gibby, Melissa; Giles, Misty; Goldstein, Adam; Greiner, Jochen; Gruber, David; van der Horst, Alexander J.; von Kienlin, Andreas; Kippen, Marc; Kouveliotou, Chryssa; McBreen, Sheila; Rau, Arne; Tierney, Dave; Wilson-Hodge, Colleen

    2011-11-01

    Discerning the radiative dissipation mechanism for prompt emission in gamma-ray bursts (GRBs) requires detailed spectroscopic modeling that straddles the νF ν peak in the 100 keV-1 MeV range. Historically, empirical fits such as the popular Band function have been employed with considerable success in interpreting the observations. While extrapolations of the Band parameters can provide some physical insight into the emission mechanisms responsible for GRBs, these inferences do not provide a unique way of discerning between models. By fitting physical models directly, this degeneracy can be broken, eliminating the need for empirical functions; our analysis here offers a first step in this direction. One of the oldest, and leading, theoretical ideas for the production of the prompt signal is the synchrotron shock model. Here we explore the applicability of this model to a bright Fermi gamma-ray burst monitor (GBM) burst with a simple temporal structure, GRB 090820A. Our investigation implements, for the first time, thermal and non-thermal synchrotron emissivities in the RMFIT forward-folding spectral analysis software often used in GBM burst studies. We find that these synchrotron emissivities, together with a blackbody shape, provide at least as good a match to the data as the Band GRB spectral fitting function. This success is achieved in both time-integrated and time-resolved spectral fits.

  3. SYNCHROTRON SELF-COMPTON EMISSION AS THE ORIGIN OF THE GAMMA-RAY AFTERGLOW OBSERVED IN GRB 980923

    SciTech Connect

    Fraija, N.; Gonzalez, M. M.; Lee, W. H. E-mail: magda@astro.unam.mx

    2012-05-20

    GRB 980923 was one of the brightest bursts observed by the Burst and Transient Source Experiment. Previous studies have detected two distinct components in addition to the main prompt episode, which is well described by a Band function. The first of these is a tail with a duration of {approx_equal} 400 s, while the second is a high-energy component lasting {approx_equal} 2 s. We summarize the observations and argue for a unified model in which the tail can be understood as the early {gamma}-ray afterglow from forward shock synchrotron emission, while the high-energy component arises from synchrotron self-Compton from the reverse shock. Consistency between the main assumption of thick shell emission and agreement between the observed and computed values for fluxes, break energies, starting times, and spectral indices leads to a requirement that the ejecta must be highly magnetized.

  4. Francoise, a Fifteen-Year Follow Up.

    ERIC Educational Resources Information Center

    Rondal, J. A.; Elbouz, M.; Ylieff, M.; Docquier, L.

    2003-01-01

    This paper reports on a 15-year follow-up of the linguistic and cognitive profile of a woman with standard trisomy 21 (Down syndrome). The follow-up found recent rapid deterioration in receptive and productive language skills. However, basic phonological and morphosyntactic skills are preserved. Her changing profile mirrors that found in aging…

  5. Towards sustainability assessment follow-up

    SciTech Connect

    Morrison-Saunders, Angus; Pope, Jenny; Bond, Alan; Retief, Francois

    2014-02-15

    This paper conceptualises what sustainability assessment follow-up might entail for three models of sustainability assessment: EIA-driven integrated assessment, objectives-led integrated assessment and the contribution to sustainability model. The first two are characterised by proponent monitoring and evaluation of individual impacts and indicators while the latter takes a holistic view based around focused sustainability criteria relevant to the context. The implications of three sustainability challenges on follow-up are also examined: contested time horizons and value changes, trade-offs, and interdisciplinarity. We conclude that in order to meet these challenges some form of adaptive follow-up is necessary and that the contribution to sustainability approach is the best approach. -- Highlights: • We explore sustainability follow-up for three different sustainability models. • Long-time frames require adaptive follow-up and are a key follow-up challenge. • Other key challenges include interdisciplinarity, and trade-offs. • Sustainability follow-up should be a direction of travel and not an outcome. • Only the follow-up for contribution to sustainability model addresses sustainability challenges sufficiently.

  6. The dangers of "follow-up" feeds.

    PubMed

    Greiner, T

    1991-09-01

    Artificial feeds constituted with contaminated water and unclean bottles are the leading cause of diarrhea in infants. Companies market artificial feeds globally as infant formula (a substitute for breast milk) and follow-up formula (a complement to breast milk). Breast milk is best for all 0-12 month old infants. Breast-fed infants do not need any formula even follow-up formula. Indeed 6-month old infants require solid healthful foods and breast milk. Like infant formulas, follow-up formula made with contaminated water or bottles can cause the infant to become ill with an infection, and offering follow-up formulas to infants impedes weaning and is costly. Follow-up formulas do not complement breast milk, but instead tend to replace it. The 1986 WHO World Health Assembly has even declared that, in some countries, provision of follow-up formula is not necessary. WHO fears mothers could use follow-up formula instead of infant formula because it has a higher protein and mineral content thus increasing the risk of dehydration during diarrhea. Follow-up formula can result in an unbalanced diet. Since the International Code of Marketing of Breastmilk Substitutes does not address formulas marketed as a complement to breast milk, formula companies market follow-up formulas in both developed and developing countries. Most mothers do not know the risks of using follow-up formulas, however. Governments have several alternatives to stop the marketing of these formulas. They can design and implement a code that defines breast-milk substitutes as any formula perceived and used as a breast milk option even if promoted as a breast-milk complement. They can also amend an existing code. WHO offers technical assistance to any member government who wishes to design, implement, and monitor such a code.

  7. Robotic Follow-Up for Human Exploration

    NASA Technical Reports Server (NTRS)

    Fong, Terrence; Bualat, Maria; Deans, Matthew C.; Adams, Byron; Allan, Mark; Altobelli, Martha; Bouyssounouse, Xavier; Cohen, Tamar; Flueckiger, Lorenzo; Garber, Joshua; Palmer, Elizabeth; Heggy, Essam; Jurgens, Frank; Kennedy, Tim; Kobayashi, Linda; Lee, Pascal; Lee, Susan Y.; Lees, David; Lundy, Mike; Park, Eric; Pedersen, Liam; Smith, Trey; To, Vinh; Utz, Hans; Wheeler, Dawn

    2010-01-01

    We are studying how "robotic follow-up" can improve future planetary exploration. Robotic follow-up, which we define as augmenting human field work with subsequent robot activity, is a field exploration technique designed to increase human productivity and science return. To better understand the benefits, requirements, limitations and risks associated with this technique, we are conducting analog field tests with human and robot teams at the Haughton Crater impact structure on Devon Island, Canada. In this paper, we discuss the motivation for robotic follow-up, describe the scientific context and system design for our work, and present results and lessons learned from field testing.

  8. Follow-up of natural products isolation.

    PubMed

    Cannell, Richard J P; Sarker, Satyajit D; Nahar, Lutfun

    2012-01-01

    Follow-up of natural products isolation refers to re-isolation of compound(s) of interest in larger amounts for further pharmacological testing, conclusive structure elucidation, structure modifications to synthesize analogs for structure-activity relationships (SAR) studies, preformulation and formulation studies or clinical trials. In addition to conventional synthetic chemistry approaches, several other methodologies can be applied for following-up natural products isolation. This chapter outlines, with specific examples, various strategies and methods involved in follow-up of natural products isolation. PMID:22367909

  9. CALORIMETRY OF GRB 030329: SIMULTANEOUS MODEL FITTING TO THE BROADBAND RADIO AFTERGLOW AND THE OBSERVED IMAGE EXPANSION RATE

    SciTech Connect

    Mesler, Robert A.; Pihlstroem, Ylva M.

    2013-09-01

    We perform calorimetry on the bright gamma-ray burst GRB 030329 by fitting simultaneously the broadband radio afterglow and the observed afterglow image size to a semi-analytic MHD and afterglow emission model. Our semi-analytic method is valid in both the relativistic and non-relativistic regimes, and incorporates a model of the interstellar scintillation that substantially effects the broadband afterglow below 10 GHz. The model is fitted to archival measurements of the afterglow flux from 1 day to 8.3 yr after the burst. Values for the initial burst parameters are determined and the nature of the circumburst medium is explored. Additionally, direct measurements of the lateral expansion rate of the radio afterglow image size allow us to estimate the initial Lorentz factor of the jet.

  10. Failure to follow up CT reports.

    PubMed

    Bird, Sara

    2007-11-01

    Case histories are based on actual medical negligence claims or medicolegal referrals, however certain facts have been omitted or changed by the author to ensure the anonymity of the parties involved. A failure to follow up test results is a common underlying cause of medical negligence claims and complaints involving general practitioners. This article examines a case in which an incidental finding of an aneurysm on cerebral computerised tomography scan was not followed up with disastrous consequences for the patient. PMID:18043783

  11. Progress with the real-time GRB coordinates distribution network (BACODINE)

    SciTech Connect

    Barthelmy, S. D.; Butterworth, P. S.; Cline, T. L.; Gehrels, N.; Fishman, G. J.; Kouveliotou, C.; Meegan, C.; Hurley, K.

    1996-08-01

    The RA, Dec coordinates of gamma-ray burst (GRB) sources observed with BATSE on GRO are automatically determined and distributed in real time to members of the global scientific community. These data are now being used by 27 operations to enable searches for associated transients in a variety of other wavelength or energy regimes to identify the burst source objects. The minimum total delay time from the onset of a GRB to the receipt of its coordinates by distant experimenters can be under 4 sec, less than the duration of a typical GRB, and the maximum total delay is 7 sec, or longer, depending on the distribution method. Recent improvements to the BACODINE system and some future improvements are discussed. A summary of the follow-up observations made by the BACODINE sites is given.

  12. The transitioning from trials to extended follow-up studies

    PubMed Central

    Drye, Lea T.; Casper, Anne S.; Sternberg, Alice L.; Holbrook, Janet T.; Jenkins, Gabrielle; Meinert, Curtis L.

    2014-01-01

    Background Investigators may elect to extend follow-up of participants enrolled in a randomized clinical trial after the trial comes to its planned end. The additional follow-up may be initiated to learn about longer term effects of treatments including adverse events, costs related to treatment, or for reasons unrelated to treatment such as to observe the natural course of the disease using the established cohort from the trial. Purpose We examine transitioning from trials to extended follow-up studies when the goal of additional follow-up is to observe longer term treatment effects. Methods We conducted a literature search in selected journals from 2000–2012 to identify trials that extended follow-up for the purpose of studying longer term treatment effects and extracted information on the operational and logistical issues in the transition. We also draw experience from three trials coordinated by the Johns Hopkins Coordinating Centers that made transitions to extended followup: the Alzheimer’s Disease Anti-inflammatory Prevention Trial (ADAPT); Multicenter Uveitis Steroid Treatment (MUST) trial; and Childhood Asthma Management Program (CAMP). Results Transitions are not uncommon in multicenter clinical trials, even in trials that continued to the planned end of the trial. Transitioning usually necessitates new participant consents. If study infrastructure is not maintained during the transition, participants will be lost and re-establishing the staff and facilities will be costly. Merging data from the trial and follow-up study can be complicated by changes in data collection measures and schedules. Limitations Our discussion and recommendations are limited to issues that we have experienced in transitions from trials to follow-up studies. Discussion We discuss issues such as maintaining funding, IRB and consent requirements, contacting participants, and combining data from the trial and follow-up phases. We conclude with a list of recommendations to

  13. Multiwavelength observations of the energetic GRB 080810: detailed mapping of the broad-band spectral evolution

    NASA Astrophysics Data System (ADS)

    Page, K. L.; Willingale, R.; Bissaldi, E.; Postigo, A. De Ugarte; Holland, S. T.; McBreen, S.; O'Brien, P. T.; Osborne, J. P.; Prochaska, J. X.; Rol, E.; Rykoff, E. S.; Starling, R. L. C.; Tanvir, N. R.; van der Horst, A. J.; Wiersema, K.; Zhang, B.; Aceituno, F. J.; Akerlof, C.; Beardmore, A. P.; Briggs, M. S.; Burrows, D. N.; Castro-Tirado, A. J.; Connaughton, V.; Evans, P. A.; Fynbo, J. P. U.; Gehrels, N.; Guidorzi, C.; Howard, A. W.; Kennea, J. A.; Kouveliotou, C.; Pagani, C.; Preece, R.; Perley, D.; Steele, I. A.; Yuan, F.

    2009-11-01

    GRB 080810 was one of the first bursts to trigger both Swift and the Fermi Gamma-ray Space Telescope. It was subsequently monitored over the X-ray and UV/optical bands by Swift, in the optical by Robotic Optical Transient Search Experiment (ROTSE) and a host of other telescopes, and was detected in the radio by the Very Large Array. The redshift of z = 3.355 +/- 0.005 was determined by Keck/High Resolution Echelle Spectrometer (HIRES) and confirmed by RTT150 and NOT. The prompt gamma/X-ray emission, detected over 0.3-103 keV, systematically softens over time, with Epeak moving from ~600 keV at the start to ~40 keV around 100s after the trigger; alternatively, this spectral evolution could be identified with the blackbody temperature of a quasi-thermal model shifting from ~60 to ~3keV over the same time interval. The first optical detection was made at 38s, but the smooth, featureless profile of the full optical coverage implies that this is originated from the afterglow component, not from the pulsed/flaring prompt emission. Broad-band optical and X-ray coverage of the afterglow at the start of the final X-ray decay (~8ks) reveals a spectral break between the optical and X-ray bands in the range of 1015-2 × 1016Hz. The decay profiles of the X-ray and optical bands show that this break initially migrates blueward to this frequency and then subsequently drifts redward to below the optical band by ~3 × 105s. GRB 080810 was very energetic, with an isotropic energy output for the prompt component of 3 × 1053 and 1.6 × 1052 erg for the afterglow; there is no evidence for a jet break in the afterglow up to 6d following the burst. This paper is dedicated to the memory of Professor Martin Turner, who sadly passed away during its writing. Martin was an influential figure in X-ray Astronomy and an excellent PhD supervisor. He will be greatly missed. E-mail: kpa@star.le.ac.uk ‡ NASA postdoctoral program fellow.

  14. TEX-SIS FOLLOW-UP: Student Follow-up Management Information System. Data Processing Manual.

    ERIC Educational Resources Information Center

    Tarrant County Junior Coll. District, Ft. Worth, TX.

    Project FOLLOW-UP was conducted to develop, test, and validate a statewide management information system for follow-up of Texas public junior and community college students. The result of this project was a student information system (TEX-SIS) consisting of seven subsystems: (1) Student's Educational Intent, (2) Nonreturning Student Follow-up, (3)…

  15. Clinical evaluation of 860 anterior and posterior lithium disilicate restorations: retrospective study with a mean follow-up of 3 years and a maximum observational period of 6 years.

    PubMed

    Fabbri, Giacomo; Zarone, Fernando; Dellificorelli, Gianluca; Cannistraro, Giorgio; De Lorenzi, Marco; Mosca, Alberto; Sorrentino, Roberto

    2014-01-01

    This study aimed to assess the clinical performance of lithium disilicate restorations supported by natural teeth or implants. Eight hundred sixty lithium disilicate adhesive restorations, including crowns on natural teeth and implant abutments, veneers, and onlays, were made in 312 patients. Parafunctional patients were included, but subjects with uncontrolled periodontitis and gingival inflammation were excluded. Veneers up to 0.5 mm thick were luted with flowable composite resin or light curing cements, while dual-curing composite systems were used with veneers up to 0.8 mm thick. Onlays up to 2 mm in thickness were luted with flowable composite resins or dual-curing composite cements. Crowns up to 1 mm in thickness were cemented with self-adhesive or dual-curing resin cements. The observational period ranged from 12 to 72 months, with a mean follow-up of 3 years. The mechanical and esthetic outcomes of the restorations were evaluated according to the modified California Dental Association (CDA) criteria. Data were analyzed with descriptive statistics. Twenty-six mechanical complications were observed: 17 porcelain chippings, 5 fractures, and 4 losses of retention. Structural drawbacks occurred mainly in posterior segments, and monolithic restorations showed the lowest number of mechanical complications. The clinical ratings of the successful restorations, both monolithic and layered, were satisfactory according to the modified CDA criteria for color match, porcelain surface, and marginal integrity. The cumulative survival rates of lithium disilicate restorations ranged from 95.46% to 100%, while cumulative success rates ranged from 95.39% to 100%. All restorations recorded very high survival and success rates. The use of lithium disilicate restorations in fixed prosthodontics proved to be effective and reliable in the short- and medium-term.

  16. The Community Follow-up Project (CFUP).

    PubMed

    Sherina, M S; Azhar, M Z; Mohd Yunus, A; Azlan Hamzah, S A

    2005-08-01

    The Community Follow-up Project (CFUP) is a project where medical students choose a hospital in-ward patient during their clinical ward-based attachments and follow-up this patient's progress after discharge from the hospital. The students do a series of home visits and also accompany their patients for some of their follow-ups at the hospital, government clinics, general practitioners' clinics and even to the palliative care or social welfare centres. The students assess the physical, psychological and social impact of the illness on the patient, family and community. By following their patients from the time their patients were in the hospital and back to their homes and community, the students are able to understand in depth the problems faced by patients, the importance of communication skills in educating patients on their illness and the importance of good communication between primary, secondary and tertiary care.

  17. Follow-up of erlotinib related uveitis

    PubMed Central

    Kumar, Indu; Ali, Kashif; Usman-Saeed, Muniba; Saeed, Muhammad Usman

    2012-01-01

    The authors report the follow-up of a 68-year-old lady with bilateral anterior uveitis secondary to erlotinib. Erlotinib was started and stopped after symptoms and signs suggestive of severe bilateral anterior uveitis were noted. The patient developed signs of a non-ST elevation myocardial infarction, 12 days after stopping the erlotinib, and recovered without major problems. The patient also reported intermittent low-grade fever since starting erlotinib which resolved after stopping this drug. No further symptoms of uveitis were noted up to 6 month follow-up. The patient reported improved well being, resolution of ocular symptoms and intermittent low-grade fever at last follow-up (6 months after stopping erlotinib). PMID:22892235

  18. RAPTOR: Closed-Loop monitoring of the night sky and the earliest optical detection of GRB 021211

    NASA Astrophysics Data System (ADS)

    Vestrand, W. T.; Borozdin, K.; Casperson, D. J.; Fenimore, E.; Galassi, M.; McGowan, K.; Starr, D.; White, R. R.; Wozniak, P.; Wren, J.

    2004-10-01

    We discuss the RAPTOR (Rapid Telescopes for Optical Response) sky monitoring system at Los Alamos National Laboratory. RAPTOR is a fully autonomous robotic system that is designed to identify and make follow-up observations of optical transients with durations as short as one minute. The RAPTOR design is based on Biomimicry of Human Vision. The sky monitor is composed of two identical arrays of telescopes, separated by 38 kilometers, which stereoscopically monitor a field of about 1300 square-degrees for transients. Both monitoring arrays are carried on rapidly slewing mounts and are composed of an ensemble of wide-field telescopes clustered around a more powerful narrow-field telescope called the ``fovea'' telescope. All telescopes are coupled to real-time analysis pipelines that identify candidate transients and relay the information to a central decision unit that filters the candidates to find real celestial transients and command a response. When a celestial transient is found, the system can point the fovea telescopes to any position on the sky within five seconds and begin follow-up observations. RAPTOR also responds to Gamma Ray Burst (GRB) alerts generated by GRB monitoring spacecraft. Here we present RAPTOR observations of GRB 021211 that constitute the earliest detection of optical emission from that event and are the second fastest achieved for any GRB. The detection of bright optical emission from GRB021211, a burst with modest gamma-ray fluence, indicates that prompt optical emission, detectable with small robotic telescopes, is more common than previously thought. Further, the very fast decline of the optical afterglow from GRB 021211 suggests that some so-called ``optically dark'' GRBs were not detected only because of the slow response of the follow-up telescopes.

  19. Follow-up of differentiated thyroid carcinoma.

    PubMed

    Bournaud, C; Raverot, V

    2015-02-01

    The aim of follow-up of differentiated thyroid carcinoma (CTD) is the assessment of remission, and, in further steps, the early recognition of patients who develop a recurrence. Tools for the follow-up of CTD include the assessment of thyroglobulin and imaging procedures. Thyroglobulin (Tg) is a strong marker of persistent or recurrent disease, but it must be known that Tg antibodies may give falsely low Tg concentration. TSH stimulation, mainly by the mean of recombinant human TSH, improves the sensitivity of Tg determination. New highly sensitive assays may preclude the need for TSH stimulation, at least in some situations. In the last decades, (131)iodine whole body scan gave place to neck ultrasonography (US) as the most performing imaging procedure in the follow-up of CTD. Criteria to identify cervical lymph node suspect of metastasis have been described, and standardized procedures proposed. Finally, the proof of tumoral invasion is brought by cytological analysis of fine needle biopsies of suspicious lymph nodes. (18)FDG PET is a valuable tool for diagnosis and prognosis in metastatic patients, especially with negative (131)I WBS. Initial response to therapy, assessed by Tg determination and neck US, allows re-stratification of the risk of relapse. According to this "reassessed risk", adapted rhythms and modalities of follow-up have been recently proposed. PMID:26826480

  20. Follow-Up Research on Agoraphobics.

    ERIC Educational Resources Information Center

    Chambless, Dianne L.

    In vivo exposure is the most commonly used and generally the most effective behavioral treatment for agoraphobia. Follow-up studies are difficult to interpret because additional treatment does not necessarily indicate relapse and non-treatment does not necessarily indicate non-relapse. Relapse rates are difficult to estimate because of lack of…

  1. WCTC Graduate Follow-Up Report, 2002.

    ERIC Educational Resources Information Center

    Waukesha County Technical Coll., Pewaukee, WI.

    This paper reports on a survey of 2001-02 graduates of Waukesha County Technical College (WCTC), Wisconsin. The report indicates 1,257 students were awarded Associate's Degrees, technical diplomas, and apprenticeship certificates by WCTC in 2001-02. Of those graduates, 702 (56%) responded to the Graduate Follow-up Survey. Also, 84% of all…

  2. Following Up Performance: Lessons from the Field.

    ERIC Educational Resources Information Center

    Newman, Constance

    2002-01-01

    Presents practices from post-training performance evaluation for continuous quality improvement in developing countries. Highlights include performance specification and analysis of performance factors; guidelines for planning follow-up performance evaluations; human performance models and cross-cultural portability; and an example from Togo, West…

  3. GRB off-axis afterglows and the emission from the accompanying supernovae

    NASA Astrophysics Data System (ADS)

    Kathirgamaraju, Adithan; Barniol Duran, Rodolfo; Giannios, Dimitrios

    2016-09-01

    Gamma-ray burst (GRB) afterglows are likely produced in the shock that is driven as the GRB jet interacts with the external medium. Long-duration GRBs are also associated with powerful supernovae (SNe). We consider the optical and radio afterglows of long GRBs for both blasts viewed along the jet axis (`on-axis' afterglows) and misaligned observes (`off-axis' afterglows). Comparing the optical emission from the afterglow with that of the accompanying SN, using SN 1998bw as an archetype, we find that only a few per cent of afterglows viewed off-axis are brighter than the SN. For observable optical off-axis afterglows, the viewing angle is at most twice the half-opening angle of the GRB jet. Radio off-axis afterglows should be detected with upcoming radio surveys within a few hundred Mpc. We propose that these surveys will act as `radio triggers', and that dedicated radio facilities should follow-up these sources. Follow-ups can unveil the presence of the radio SN remnant, if present. In addition, they can probe the presence of a mildly relativistic component, either associated with the GRB jet or the SN ejecta, expected in these sources.

  4. Understanding Grb Physics With Multi-Wavelength Data

    NASA Astrophysics Data System (ADS)

    Zhang, Bing

    The study of Gamma-ray bursts (GRBs) has entered a full multi-wavelength era. A rich trove of data from NASA GRB missions and ground-based follow up observations have been collected. Careful data mining with well-defined scientific objectives holds the key to address open questions in GRB physics, such as jet composition, radiation mechanism, progenitor and central engine physics. We propose to perform data analyses in the following three directions. 1. The time resolved GRB spectra have a dominant component that can be fit with a phenomenological ``Band'' function. The physical meaning of this function remains unclear. Recently we made a breakthrough in theoretical modeling, and showed that fast-cooling synchrotron radiation of electrons in a decreasing magnetic field can mimic the Band function in detector's bandpass, but differs from Band function slightly. We propose to apply this physically-motivated model to systematically fit the GRB prompt emission data collected by Fermi GBM and LAT, and test whether the dominant GRB emission mechanism is fast cooling synchrotron radiation. We will also fit time-dependent spectra with a time-dependent model to investigate whether a quasi- thermal "photosphere'' emission component is indeed needed to fit the observed spectra. This would shed light onto the unknown composition of GRB jets. By fitting the time resolved spectra, we will also constrain important physical parameters of GRB prompt emission, such as the emission site of GRBs, the strength of magnetic fields, as well as their evolution with radius. 2. Recent GRB multi-wavelength observations suggest that it is not straightforward to define the physical category of a GRB based on the traditional classification in the "duration''-"hardness'' domain. Some long-duration GRBs may not have a massive star origin, while some short-duration GRBs may instead have a massive star origin. We propose to systematically study the gamma-ray Swift/BAT, Fermi/GBM- LAT), X-ray (Swift

  5. Follow-up of colorectal cancer patients: quality of life and attitudes towards follow-up.

    PubMed Central

    Stiggelbout, A. M.; de Haes, J. C.; Vree, R.; van de Velde, C. J.; Bruijninckx, C. M.; van Groningen, K.; Kievit, J.

    1997-01-01

    The aims of our study were to assess the effect of follow-up on the quality of life of colorectal cancer patients and to assess the attitudes of patients towards follow-up as a function of patient characteristics. Patients who had been treated with curative intent were selected from four types of hospitals. Eighty-two patients were interviewed using a structured questionnaire, whereas 130 patients received the questionnaire by mail. To assess the effect of follow-up on the quality of life, the interviewed patients were randomly allocated to three groups and interviewed at different times in relation to the follow-up visit. Analysis did not show an effect of the follow-up visit on quality of life. Patients reported a positive attitude towards follow-up: it reassured them, they judged the communication with the physician to be positive, and they experienced only slight nervous anticipation and few other disadvantages. Patients reported a strong preference for follow-up, and a large majority would prefer follow-up even if it would not lead to earlier detection of a recurrence. Apart from living situation, no patient characteristics were clearly associated with the attitude towards follow-up. Implications for clinical practice are discussed. PMID:9062416

  6. Follow-up of eROSITA and Euclid Clusters

    NASA Astrophysics Data System (ADS)

    Reiprich, T.

    2016-06-01

    In the near future, eROSITA and Euclid will elevate galaxy cluster and cosmology studies to an unprecedented level. Through large area surveys, they will generate huge galaxy cluster samples. Rich science will be enabled through detailed follow-up observations of systematically selected subsamples. In particular, X-ray follow-up will be crucial and XMM-Newton could play the leading role. In this talk, examples for the science enabled and possible strategies for such XMM-Newton observations will be outlined.

  7. GRB 100614A and GRB 100615A: two extremely dark gamma-ray bursts

    NASA Astrophysics Data System (ADS)

    D'Elia, V.; Stratta, G.

    2011-08-01

    Context. Dark gamma-ray bursts (GRBs) are sources with no or faint optical/near infrared (NIR) afterglow with respect to the X-ray one. Three possible explanations of this optical darkness have been proposed, namely: i) the GRB might be at high redshift, such that the Lyman α absorption prevents optical identifications; ii) dust in the GRB host galaxy may absorb the optical/NIR wavelengths; and iii) the optical faintness might have an intrinsic origin. Aims: We study two dark GRBs discovered by Swift, namely, GRB 100614A and GRB 100615A. These sources are bright in the X-rays, but no optical/NIR afterglow has been detected for either source, despite the efforts of several follow-up campaigns that have been performed since soon after the GRB explosion. Methods: We analyze the X-ray data and collect all the optical/NIR upper limits in literature for these bursts. We then build optical-to-X-ray spectral energy distributions (SEDs) at the times at which the reddest upper limits are available, and we model our SEDs with the attenuation curves of the Milky Way (MW), Small Magellanic Cloud (SMC), and one obtained for a sample of starburst galaxies. Results: We find that to explain the deepest NIR upper limits assuming either a MW or SMC extinction law, the visual extinction towards GRB 100614A is AV > 47 mag, while for GRB 100615A we obtain AV > 58 mag using data taken within one day after the burst and AV > 22 mag even 9.2 days after the trigger. Conclusions: If these bursts were strongly extincted by dust, these results imply that a MW or SMC-like dust obscuration is unlikely to be able to explain their optical darkness. Since both GRBs are bright in X-rays, explanation iii) also cannot explain their dark classification, unless optical radiation and X-rays are not part of the same synchrotron spectrum. In particular, the X-ray emission during the first 100 - 10 000 s after the burst, shows in ~70% of the cases a "shallow phase" unexpected by the fireball model

  8. Follow-up imaging after pediatric pyeloplasty

    PubMed Central

    Kumar, Manoj; Singh, Sanjeet Kumar; Arora, Sohrab; Mittal, Varun; Patidar, Nitesh; Sureka, Sanjoy Kumar; Ansari, M. S.

    2016-01-01

    Introduction: The duration, methods and frequency of radiographic follow-up after pediatric pyeloplasty is not well-defined. We prospectively evaluated a cohort of children undergoing pyeloplasty to determine the method for follow-up. Methods: Between 2000 and 2008, children undergoing pyeloplasty for unilateral ureteropelvic junction obstruction were evaluated for this study. All patients were evaluated preoperatively with protocol ultrasound (USG) and diuretic renal scan (RS). On the basis of preoperative split renal function (SRF), these patients were divided into four groups – Group I: SRF > 40%, Group II: SRF 30–39%, Group III: SRF 20–29%, and Group IV: SRF 10–19%. In follow-up, USG and RS were done at 3 months and repeated at 6 months, 1 year, and then yearly after surgery for a minimum period of 5 years. Improvement, stability, or worsening of hydronephrosis was based on the changes in anteroposterior (AP) diameter of pelvis and caliectasis on USG. Absolute increase in split renal function (SRF) >5% was considered significant. Failure was defined as increase in AP diameter of pelvis and decrease in cortical thickness on 3 consecutive USG, t½ >20 min with obstructive drainage on RS and/or symptomatic patient. Results: 145 children were included in the study. Their mean age was 3.26 years and mean follow-up was 7.5 years. Pre- and post-operative SRF remain unchanged within 5% range in 35 of 41 patients (85%) in Group I. While 9 of 20 patients (45%) in Group II, 23 of 50 patients (46%) in Group III, and 14 of 34 patients (41%) in Group IV exhibited changes >5% after surgery. 5 patients failed, 2 in Group III, and 3 in Group IV. None of the patients deteriorated in Group I and II. Conclusion: After pyeloplasty in children with a baseline split GFR >30%, if a diuretic renogram and USG performed 3 months postoperatively shows nonobstructive drainage with t½ <20 min and decreased hydronephrosis, no further follow-up is required. PMID:27555681

  9. [Diagnosis and follow-up of endometriosis during consultation: changes].

    PubMed

    Salvat, J

    2001-09-01

    In a literature review, news in symptomatology and follow-up of endometriosis were analyzed (infertility, pain, hemorrhage, adnexal tumors). Survey and examination can be made with improved quality (pain scale, menorragha scheme of Higham). Diagnosis and follow-up of endometriosis are more perfect by ultrasonographical examination by the gynecologist in his office. Ultrasonography is better for endometrioma and adenomyosis than other localisation (complementary explorations-magnetic resonance imaging, outside of consultation, are useful for deeper and superficial lesions). In follow-up, clinical research and ultrasonic exploration show the true relapses. Treatment's observance and success will be improved by ultrasonic analysis. Intolerances, add-back therapy, contraception, substitutive hormonal treatment of menopauses and cancer risk, are different problem and solution will be offer.

  10. Follow-up photometry of iPTF16geu

    NASA Astrophysics Data System (ADS)

    Lee, C.-H.

    2016-10-01

    We report follow-up photometry of the strongly lensed SNIa iPTF16geu (ATel #9603, #9626). We observed iPTF16geu on 2016/10/17 with the 2.5-m Isaac Newton Telescope (INT) + WFC at La Palma, under ~0.9" seeing condition.

  11. GRBS Followed-up by the bootes network

    NASA Astrophysics Data System (ADS)

    Guziy, S.; Castro-Tirado, A.; Jelínek, M.; Gorosabel, J.; Kubánek, P.; Cunniffe, R.; Lara-Gil, O.; Rabaza-Castillo, O.; de Ugarte Postigo, A.; Sánchez-Ramírez, R.; Tello, J.; Pérez del Pulgar, C.; Castillo-Carrión, S.; Castro Cerón, J.; Mateo Sanguino, T. de J.; Hudec, R.; Vitek, S.; de la Morena Carretero, B.; Díaz Andreu, J.; Fernández-Muñoz, R.; Pérez-Ramírez, D.; Yock, P.; Allen, W.; Bond, I.; Kheyfets, I.; Christie, G.; Sabau-Graziati, L.; Cui, C.; Fan, Y.; Park, I. H.

    2013-07-01

    The Burst Observer and Optical Transient Exploring System (BOOTES), is a global robotic observatory network, which started in 1998 with Spanish leadership devoted to study optical emissions from gamma ray bursts (GRBs) that occur in the Universe. We present shot history and current status of BOOTES network. The Network philosophy, science and some details of 117 GRBs followed-up are discussed.

  12. Gamma Ray Burst Follow-Ups with Bootes-4

    NASA Astrophysics Data System (ADS)

    Guziy, Sergey; Castro-Tirado, Guziy, Alberto J.; Jelinek, Martin; Gorosabel, Javier; Kubanek, Petr; Cunniffe, Ronan; Lara-Gil, Oscar; Tello, Juan C.; Jeong, Soomin; Oates, Samantha R.; Xu, Youdong; Perez-Ramirez, Dolores; Cui, Chenzou; Fan, Yufeng; Wan, Chuanjun; Bai, Jinming; Kheyfets, I.

    The Burst Observer and Optical Transient Exploring System (BOOTES), is a global robotic observatory network, which started in 1998 with Spanish leadership devoted to study optical emissions from gamma ray bursts (GRBs) that occur in the Universe. We present shot history and current status of BOOTES-4 telescope. Some details of 38 GRBs followed-up with BOOTES-4 are discussed.

  13. Urodynamic profile in myelopathies: A follow-up study

    PubMed Central

    Gupta, Anupam; Taly, Arun B.; Srivastava, Abhishek; Thyloth, Murali

    2009-01-01

    Aims: To study the significance of filling cystometry in assessment and management of neurogenic bladder in myelopathies and correlate neurological recovery and bladder management in the follow up. Study Design: Retrospective analysis of reports of filling cystometry in patients with traumatic and non-traumatic myelopathy. Setting: Neuro-rehabilitation unit of a tertiary care university hospital. Methods: The study was carried out between September 2005 and June 2006 and included all subjects with myelopathy who underwent filling cystometry. ASIA impairment scale was used to assess neurological status during admission as well as in the follow up. Bladder management was advised based on the cystometric findings. Neurological recovery and mode of bladder management were correlated during the follow up after a minimum of 6 months. Results: Fifty-two subjects (38 males, 14 females), mean age 33.26 ± 14.66 years (10–80) underwent filling cystometry. Twenty patients had cervical, 24 had thoracic and 8 had lumbar myelopathy. Cystometric findings were overactive detrusor observed in 43 patients, (21 had detrusor sphincter dyssynergia (DSD), 22 without DSD) and areflexic/underactive detrusor in 9. Post-void residual (>15% of voided urine) was significant in 27 patients. Twenty-three patients (44%) reported for follow up (16 males, 7 females) after a mean duration of 9.04 ± 2.44 months (6–15 months). Neurological recovery was seen in 61% cases, while 1 patient showed deterioration. Only 26% patients reported change in bladder management during follow up. Correlation between neurological recovery and bladder management was found to be insignificant (P > 0.05) using spearman correlation co-efficient. Conclusions: Filling cystometry is valuable for assessment and management of neurogenic bladder after myelopathy. No significant relationship was observed between neurological recovery and neurogenic bladder management in the follow up in the present study. PMID:20151007

  14. NASA Audit Follow-up Handbook

    NASA Technical Reports Server (NTRS)

    1990-01-01

    This NASA Audit Follow-up Handbook is issued pursuant to the requirements of the Office of Management and Budget (OMB) Circular A-50, Audit Follow-up, dated September 29, 1982. It sets forth policy, uniform performance standards, and procedural guidance to NASA personnel for use when considering reports issued by the Office of Inspector General (OIG), other executive branch audit organizations, the Defense Contract Audit Agency (DCAA), and the General Accounting Office (GAO). It is intended to: specify principal roles; strengthen the procedures for management decisions (resolution) on audit findings and corrective action on audit report recommendations; emphasize the importance of monitoring agreed upon corrective actions to assure actual accomplishment; and foster the use of audit reports as effective tools of management. A flow chart depicting the NASA audit and management decision process is in Appendix A. This handbook is a controlled handbook issued in loose-leaf form and will be revised by page changes. Additional copies for internal use may be obtained through normal distribution channels.

  15. GRB Simulations in GLAST

    SciTech Connect

    Omodei, Nicola; Battelino, Milan; Komin, Nukri; Longo, Francesco; McEnery, Julie; Ryde, Felix; /Denver U.

    2007-10-22

    The Gamma-ray Large Area Space Telescope (GLAST), scheduled to be launched in fall of 2007, is the next generation satellite for high-energy gamma-ray astronomy. The Large Area Telescope (LAT) is a pair conversion telescope built with a high precision silicon tracker, a segmented CsI electromagnetic calorimeter and a plastic anticoincidence shield. The LAT will survey the sky in the energy range between 20 MeV to more than 300 GeV, shedding light on many issues left open by its highly successful predecessor EGRET. LAT will observe Gamma-Ray Bursts (GRB) in an energy range never explored before; to tie these frontier observations to the better-known properties at lower energies, a second instrument, the GLAST Burst Monitor (GBM) will provide important spectra and timing in the 10 keV to 30 MeV range. We briefly present the instruments onboard the GLAST satellite, their synergy in the GRB observations and the work done so far by the collaboration in simulation, analysis, and GRB sensitivity estimation.

  16. Super-solar metallicity at the position of the ultra-long GRB 130925A

    NASA Astrophysics Data System (ADS)

    Schady, P.; Krühler, T.; Greiner, J.; Graham, J. F.; Kann, D. A.; Bolmer, J.; Delvaux, C.; Elliott, J.; Klose, S.; Knust, F.; Nicuesa Guelbenzu, A.; Rau, A.; Rossi, A.; Savaglio, S.; Schmidl, S.; Schweyer, T.; Sudilovsky, V.; Tanga, M.; Tanvir, N. R.; Varela, K.; Wiseman, P.

    2015-07-01

    Over the last decade there has been immense progress in the follow-up of short and long gamma-ray bursts (GRBs), resulting in a significant rise in the detection rate of X-ray and optical afterglows, in the determination of GRB redshifts, and of the identification of the underlying host galaxies. Nevertheless, our theoretical understanding of the progenitors and central engines powering these vast explosions is lagging behind, and a newly identified class of ultra-long GRBs has fuelled speculation on the existence of a new channel of GRB formation. In this paper we present high signal-to-noise X-Shooter observations of the host galaxy of GRB 130925A, which is the fourth unambiguously identified ultra-long GRB, with prompt γ-ray emission detected for ~20 ks. The GRB line of sight was close to the host galaxy nucleus, and our spectroscopic observations cover this region along the bulge/disk of the galaxy and a bright star-forming region within the outskirts of the galaxy. From our broad wavelength coverage, we obtain accurate metallicity and dust-extinction measurements at the galaxy nucleus and at an outer star-forming region, and measure a super-solar metallicity at both locations, placing this galaxy within the 10-20% most metal-rich GRB host galaxies. Such a high metal enrichment has significant implications on the progenitor models of both long and ultra-long GRBs, although the edge-on orientation of the host galaxy does not allow us to rule out a large metallicity variation along our line of sight. The spatially resolved spectroscopic observations presented in this paper offer important insight into variations in the metal and dust abundance within GRB host galaxies. However, they also illustrate the need for integral field unit observations on a larger sample of GRB host galaxies of a variety of metallicities to provide a more quantitative view on the relation between the GRB circumburst environment and the galaxy-whole properties. Based on observations taken

  17. GRB 150101B/Swift J123205.1-105602: continued WSRT radio and VLT optical observations

    NASA Astrophysics Data System (ADS)

    Van der Horst, A. J.; Levan, A. J.; Wiersema, K.; Tanvir, N. R.; Hjorth, J.

    2015-01-01

    We reobserved the field of GRB 150101B/Swift J123205.1-105602 at 4.9 GHz with the Westerbork Synthesis Radio Telescope (WSRT) at January 9 00.25 to 09.00 UT, and January 17 23.75 to January 18 08.50 UT.

  18. Assessing Risk in Patients with Stable Coronary Disease: When Should We Intensify Care and Follow-Up? Results from a Meta-Analysis of Observational Studies of the COURAGE and FAME Era

    PubMed Central

    Barbero, Umberto; D'Ascenzo, Fabrizio; Nijhoff, Freek; Moretti, Claudio; Biondi-Zoccai, Giuseppe; Mennuni, Marco; Capodanno, Davide; Lococo, Marco; Lipinski, Michael J.; Gaita, Fiorenzo

    2016-01-01

    Background. A large number of clinical and laboratory markers have been appraised to predict prognosis in patients with stable angina, but uncertainty remains regarding which variables are the best predictors of prognosis. Therefore, we performed a meta-analysis of studies in patients with stable angina to assess which variables predict prognosis. Methods. MEDLINE and PubMed were searched for eligible studies published up to 2015, reporting multivariate predictors of major adverse cardiac events (MACE, a composite endpoint of death, myocardial infarction, and revascularization) in patients with stable angina. Study features, patient characteristics, and prevalence and predictors of such events were abstracted and pooled with random-effect methods (95% CIs). Major adverse cardiovascular event (MACE) was the primary endpoint. Results. 42 studies (104,559 patients) were included. After a median follow-up of 57 months, cardiovascular events occurred in 7.8% of patients with MI in 6.2% of patients and need for repeat revascularization (both surgical and percutaneous) in 19.5% of patients. Male sex, reduced EF, diabetes, prior MI, and high C-reactive protein were the most powerful predictors of cardiovascular events. Conclusions. We show that simple and low-cost clinical features may help clinicians in identifying the most appropriate diagnostic and therapeutic approaches within the broad range of outpatients presenting with stable coronary artery disease. PMID:27239372

  19. Constraints on binary neutron star merger product from short GRB observations

    NASA Astrophysics Data System (ADS)

    Gao, He; Zhang, Bing; Lü, Hou-Jun

    2016-02-01

    Binary neutron star (NS) mergers are strong gravitational-wave (GW) sources and the leading candidates to interpret short-duration gamma-ray bursts (SGRBs). Under the assumptions that SGRBs are produced by double neutron star mergers and that the x-ray plateau followed by a steep decay as observed in SGRB x-ray light curves marks the collapse of a supramassive neutron star to a black hole (BH), we use the statistical observational properties of Swift SGRBs and the mass distribution of Galactic double neutron star systems to place constraints on the neutron star equation of state (EoS) and the properties of the post-merger product. We show that current observations already impose the following interesting constraints. (1) A neutron star EoS with a maximum mass close to a parametrization of Mmax=2.37 M⊙(1 +1.58 ×10-10P-2.84) is favored. (2) The fractions for the several outcomes of NS-NS mergers are as follows: ˜40 % prompt BHs, ˜30 % supramassive NSs that collapse to BHs in a range of delay time scales, and ˜30 % stable NSs that never collapse. (3) The initial spin of the newly born supramassive NSs should be near the breakup limit (Pi˜1 ms ), which is consistent with the merger scenario. (4) The surface magnetic field of the merger products is typically ˜1015 G . (5) The ellipticity of the supramassive NSs is ɛ ˜(0.004 -0.007 ), so that strong GW radiation is released after the merger. (6) Even though the initial spin energy of the merger product is similar, the final energy output of the merger product that goes into the electromagnetic channel varies in a wide range from several 1049 to several 1052 erg , since a good fraction of the spin energy is either released in the form of GWs or falls into the black hole as the supramassive NS collapses.

  20. Improving Lunar Exploration with Robotic Follow-up

    NASA Technical Reports Server (NTRS)

    Fong, T.; Bualat, M.; Deans, M.; Heggy E.; Helper, M.; Hodges, K.; Lee, P.

    2011-01-01

    We are investigating how augmenting human field work with subsequent robot activity can improve lunar exploration. Robotic "follow-up" might involve: completing geology observations; making tedious or long-duration measurements of a target site or feature; curating samples in-situ; and performing unskilled, labor-intensive work. To study this technique, we have begun conducting a series of lunar analog field tests at Haughton Crater (Canada). Motivation: In most field geology studies on Earth, explorers often find themselves left with a set of observations they would have liked to make, or samples they would have liked to take, if only they had been able to stay longer in the field. For planetary field geology, we can imagine mobile robots - perhaps teleoperated vehicles previously used for manned exploration or dedicated planetary rovers - being deployed to perform such follow-up activities [1].

  1. ALMA observations of the host galaxy of GRB 090423 at z = 8.23: deep limits on obscured star formation 630 million years after the big bang

    SciTech Connect

    Berger, E.; Zauderer, B. A.; Chary, R.-R.; Laskar, T.; Chornock, R.; Davies, J. E.; Tanvir, N. R.; Stanway, E. R.; Levan, A. J.; Levesque, E. M.

    2014-12-01

    We present rest-frame far-infrared (FIR) and optical observations of the host galaxy of GRB 090423 at z = 8.23 from the Atacama Large Millimeter Array (ALMA) and the Spitzer Space Telescope, respectively. The host remains undetected to 3σ limits of F {sub ν}(222 GHz) ≲ 33 μJy and F {sub ν}(3.6 μm) ≲ 81 nJy. The FIR limit is about 20 times fainter than the luminosity of the local ULIRG Arp 220 and comparable to the local starburst M 82. Comparing this with model spectral energy distributions, we place a limit on the infrared (IR) luminosity of L {sub IR}(8-1000 μm) ≲ 3 × 10{sup 10} L {sub ☉}, corresponding to a limit on the obscured star formation rate of SFR{sub IR}≲5 M {sub ☉} yr{sup –1}. For comparison, the limit on the unobscured star formation rate from Hubble Space Telescope rest-frame ultraviolet (UV) observations is SFR{sub UV} ≲ 1 M {sub ☉} yr{sup –1}. We also place a limit on the host galaxy stellar mass of M {sub *} ≲ 5 × 10{sup 7} M {sub ☉} (for a stellar population age of 100 Myr and constant star formation rate). Finally, we compare our millimeter observations to those of field galaxies at z ≳ 4 (Lyman break galaxies, Lyα emitters, and submillimeter galaxies) and find that our limit on the FIR luminosity is the most constraining to date, although the field galaxies have much larger rest-frame UV/optical luminosities than the host of GRB 090423 by virtue of their selection techniques. We conclude that GRB host galaxies at z ≳ 4, especially those with measured interstellar medium metallicities from afterglow spectroscopy, are an attractive sample for future ALMA studies of high redshift obscured star formation.

  2. Searching for GRB Remnants in Nearby Galaxies

    NASA Astrophysics Data System (ADS)

    Bhargavi, S. G.; Rhoads, J.; Perna, R.; Feldmeier, J.; Greiner, J.

    2004-09-01

    Gamma Ray Bursts (GRBs) are expected to leave behind GRB remnants, similar to how ``standard'' supernovae (SN) leave behind SN remnants. The identification of these remnants in our own and in nearby galaxies would allow a much closer look at GRB birth sites, and possibly lead to the discovery of the compact object left behind. It would also provide independent constraints on GRB rates and energetics. We have initiated an observational program (2002) to search for GRB remnants in nearby galaxies. The identification is based on specific line ratios, such as OIII/Hβ and HeII/Hβ. which are expected to be unusually high in case of GRB remnants according to the theoretical predictions of Perna et al. (2000). The observing strategies and preliminary studies from a test run at 2.34 m VBT as well as archival data from planetary nebulae surveys of spiral galaxies are discussed.

  3. The SEDs and Host Galaxies of the Dustiest GRB Afterglows

    NASA Technical Reports Server (NTRS)

    Kruhler, T.; Greiner, J.; Schady, P.; Savaglio, S.; Afonso, P. M. J.; Clemens, C.; Elliott, J.; Filgas, R.; Gruber, D.; Kann, D. A.; Klose, S.; Kupcu-Yoldas, A.; McBreen, S.; Olivares, E.; Pierini, D.; Rau, A.; Rossi, A.; Nardini, M.; Nicuesa Guelbenzu, A.; Sudilovsky, V.; Updike, A. C.

    2011-01-01

    The afterglows and host galaxies of long gamma-ray bursts (GRBs) offer unique opportunities to study star-forming galaxies in the high-z Universe, Until recently, however. the information inferred from GRB follow-up observations was mostly limited to optically bright afterglows. biasing all demographic studies against sight-lines that contain large amounts of dust. Aims. Here we present afterglow and host observations for a sample of bursts that are exemplary of previously missed ones because of high visual extinction (A(sub v) (Sup GRB) approx > 1 mag) along the sight-line. This facilitates an investigation of the properties, geometry and location of the absorbing dust of these poorly-explored host galaxies. and a comparison to hosts from optically-selected samples. Methods. This work is based on GROND optical/NIR and Swift/XRT X-ray observations of the afterglows, and multi-color imaging for eight GRB hosts. The afterglow and galaxy spectral energy distributions yield detailed insight into physical properties such as the dust and metal content along the GRB sight-line as well as galaxy-integrated characteristics like the host's stellar mass, luminosity. color-excess and star-formation rate. Results. For the eight afterglows considered in this study we report for the first time the redshift of GRBs 081109 (z = 0.97S7 +/- 0.0005). and the visual extinction towards GRBs 0801109 (A(sub v) (Sup GRB) = 3.4(sup +0.4) (sub -0.3) mag) and l00621A (A(sub v) (Sup GRB) = 3.8 +/- 0.2 mag), which are among the largest ever derived for GRB afterglows. Combined with non-extinguished GRBs. there is a strong anti-correlation between the afterglow's metals-to-dust ratio and visual extinction. The hosts of the dustiest afterglows are diverse in their properties, but on average redder(((R - K)(sub AB)) approximates 1.6 mag), more luminous ( approximates 0.9 L (sup *)) and massive ((log M(sup *) [M(solar]) approximates 9.8) than the hosts of optically-bright events. We hence probe

  4. PROMPT GeV EMISSION FROM RESIDUAL COLLISIONS IN GAMMA-RAY BURST OUTFLOWS: EVIDENCE FROM FERMI OBSERVATIONS OF GRB 080916c

    SciTech Connect

    Li Zhuo

    2010-01-20

    The gamma-rays from gamma-ray bursts (GRBs) are believed to be produced by internal shocks driven by small timescale, approx1 ms, variation in the GRB outflows, and a pair-production spectral cutoff is generally expected around the GeV range. However, the observed optical flashes accompanying GRBs suggest that the delayed residual collisions due to large timescale variation continue to accelerate electrons. We show here that the inverse-Compton (IC) scattering of the prompt gamma-rays by these residual internal shock electrons leads to a high-energy emission beyond the previously thought spectral cutoff, in agreement with the previous detections of GeV photons by EGRET in several GRBs in conjunction with MeV emission. We expect a spectral break due to the transition from the primary to residual internal shock emission at the previously thought spectral cutoff and expect systematic time delays of high-energy photons relative to MeV emission, the discovery of which would provide stringent constraint on the outflow properties, but requires large enough collection of high-energy photons by, e.g., Fermi and AGILE satellites. The recent Fermi-detected bright GRB 080916c unambiguously shows the shifting of the prompt emission toward later times as the photon energy increases. The second-scale shifting at >100 MeV is much longer than the MeV variability time, as predicted in the residual collision model. The observations imply that there should be emission above 70 GeV in the source frame, which may not be produced by primary internal shocks but by IC emission in residual collisions. With the method involving time delays of high-energy emission, the bulk Lorentz factor of GRB 080916c is determined to be GAMMA approx 300.

  5. 29 CFR 99.315 - Audit findings follow-up.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 29 Labor 1 2013-07-01 2013-07-01 false Audit findings follow-up. 99.315 Section 99.315 Labor... Auditees § 99.315 Audit findings follow-up. (a) General. The auditee is responsible for follow-up and... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  6. 38 CFR 41.315 - Audit findings follow-up.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 38 Pensions, Bonuses, and Veterans' Relief 2 2013-07-01 2013-07-01 false Audit findings follow-up... findings follow-up. (a) General. The auditee is responsible for follow-up and corrective action on all... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  7. 29 CFR 99.315 - Audit findings follow-up.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 29 Labor 1 2012-07-01 2012-07-01 false Audit findings follow-up. 99.315 Section 99.315 Labor... Auditees § 99.315 Audit findings follow-up. (a) General. The auditee is responsible for follow-up and... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  8. 7 CFR 3052.315 - Audit findings follow-up.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... 7 Agriculture 15 2012-01-01 2012-01-01 false Audit findings follow-up. 3052.315 Section 3052.315....315 Audit findings follow-up. (a) General. The auditee is responsible for follow-up and corrective... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  9. 29 CFR 99.315 - Audit findings follow-up.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 29 Labor 1 2011-07-01 2011-07-01 false Audit findings follow-up. 99.315 Section 99.315 Labor... Auditees § 99.315 Audit findings follow-up. (a) General. The auditee is responsible for follow-up and... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  10. 38 CFR 41.315 - Audit findings follow-up.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 38 Pensions, Bonuses, and Veterans' Relief 2 2011-07-01 2011-07-01 false Audit findings follow-up... findings follow-up. (a) General. The auditee is responsible for follow-up and corrective action on all... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  11. 7 CFR 3052.315 - Audit findings follow-up.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 7 Agriculture 15 2014-01-01 2014-01-01 false Audit findings follow-up. 3052.315 Section 3052.315....315 Audit findings follow-up. (a) General. The auditee is responsible for follow-up and corrective... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  12. 29 CFR 99.315 - Audit findings follow-up.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 29 Labor 1 2014-07-01 2013-07-01 true Audit findings follow-up. 99.315 Section 99.315 Labor Office... § 99.315 Audit findings follow-up. (a) General. The auditee is responsible for follow-up and corrective... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  13. 7 CFR 3052.315 - Audit findings follow-up.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... 7 Agriculture 15 2013-01-01 2013-01-01 false Audit findings follow-up. 3052.315 Section 3052.315....315 Audit findings follow-up. (a) General. The auditee is responsible for follow-up and corrective... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  14. 7 CFR 3052.315 - Audit findings follow-up.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... 7 Agriculture 15 2010-01-01 2010-01-01 false Audit findings follow-up. 3052.315 Section 3052.315....315 Audit findings follow-up. (a) General. The auditee is responsible for follow-up and corrective... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  15. 38 CFR 41.315 - Audit findings follow-up.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 38 Pensions, Bonuses, and Veterans' Relief 2 2014-07-01 2014-07-01 false Audit findings follow-up... findings follow-up. (a) General. The auditee is responsible for follow-up and corrective action on all... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  16. 38 CFR 41.315 - Audit findings follow-up.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 38 Pensions, Bonuses, and Veterans' Relief 2 2012-07-01 2012-07-01 false Audit findings follow-up... findings follow-up. (a) General. The auditee is responsible for follow-up and corrective action on all... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  17. 7 CFR 3052.315 - Audit findings follow-up.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... 7 Agriculture 15 2011-01-01 2011-01-01 false Audit findings follow-up. 3052.315 Section 3052.315....315 Audit findings follow-up. (a) General. The auditee is responsible for follow-up and corrective... currently following up with the auditee on the audit finding; and (iii) A management decision was not...

  18. GRB Discoveries with Swift

    NASA Technical Reports Server (NTRS)

    Gehrels, Neil

    2008-01-01

    This brief presentation presents Swift Observatory recordings of gamma ray burst (GRB) activity. Long and short GRBs and afterglows are highlighted. Recordings of GRB emission, afterglow, optical/IR brightness, and flux density are presented. The time structure and current status of short GRB structures is also included.

  19. Discovery and follow up of asteroids

    NASA Technical Reports Server (NTRS)

    Bowell, E.; Chernykh, N. S.; Marsden, B. G.

    1989-01-01

    After a summary of the increasing activity in steroid discovery during the past few years, the importance of carefully thought out observing strategy is discussed, in particular with regard to target selection, observing frequency, and the time distribution of observations. Problems of cataloging and orbit linkage are outlined, inasmuch as they affect individual observers and orbit computers, as well as the work of the Minor Planet Center. There is some discussion of appropriate two-way communication between observers and the Minor Planet Center.

  20. Concluding Remarks: The Current Status and Future Prospects for GRB Astronomy

    NASA Technical Reports Server (NTRS)

    Gehrels, Neil

    2009-01-01

    We are in a remarkable period of discovery in GRB astronomy. The current satellites including Swift, Fermi. AGILE and INTEGRAL are detecting and observing bursts of all varieties. Increasing capabilities for follow-up observations on the ground and in space are leading to rapid and deep coverage across the electromagnetic spectrum, The future will see continued operation of the current experiments and with future missions like SVOM plus possible rni_Ssions like JANUS and EXIST. An exciting expansion of capabilities is occurring in areas of gravitational waves and neutrinos that could open new windows on the GRB phenomenon. Increased IR capabilities on the ground and with missions like JWST will enable further exploration of high redshift bursts. The future is bright.

  1. Following up the follow up--long-term complications in paediatric burns.

    PubMed

    Kidd, L R; Nguyen, D Q; Lyons, S C; Dickson, W A

    2013-02-01

    Paediatric burn follow-up optimally follows a balance between complication detection and avoiding unnecessary hospital visits. In a long-term review, we assessed complication patterns in children with burns requiring surgery. Using the Welsh Burns Centre database, a retrospective note review of paediatric burns over 3 years from 1995 was performed, identifying all children undergoing surgery for their burns. 94 patients were identified with a median follow-up since injury of 13.6 years. Mean age was 5.27 (SD=4.9) years. TBSA ranged from <1 to 70%. 94% underwent split-skin grafting. 18% (n=17) developed contractures and 33% (n=31) developed hypertrophic scarring. Those developing contractures were younger, and suffered significantly greater TBSA burns (p<0.05) than those developing hypertrophic scarring or those without complications. All contractures developed within 1-13 months, and hypertrophic scarring within 1-17 months. All patients sustaining axillary burns developed contractures, whilst 75% of contractures developed around the upper limb. In conclusion, younger patients with larger TBSA burns in the upper limb were at higher risk for contractures and hypertrophic scarring, which all presented within 18 months. Therefore any patients that are complication-free 18 months after-injury can be safely discharged, allowing streamlining of follow-up for the benefit of patients, parents and hospital resources.

  2. Extremely dark GRBs: the case of GRB 100614A and GRB 100615A.

    NASA Astrophysics Data System (ADS)

    D'Elia, V.; Stratta, G.

    Dark gamma-ray bursts (GRBs) are sources with a low optical-to-X-ray flux ratio. Proposed explanations for this darkness are: i) the GRB is at high redshift ii) dust in the GRB host galaxy absorbs the optical/NIR flux iii) GRBs have an intrinsically faint afterglow emission. Within this framework, GRB 100614A and GRB 100615A are extreme. In fact, they are bright in the X-rays, but no optical/NIR afterglow has been detected for either source, despite several follow-up campaigns began early after the triggers. We analyze the X-ray data and collect all the optical/NIR upper limits in literature for these bursts. We then build optical-to-X-ray spectral energy distributions (SEDs) at the times at which the reddest upper limits are available, and we model our SEDs with the extinction curves of the Milky Way (MW), Small Magellanic Cloud (SMC), and the attenuation curve obtained for a sample of starburst galaxies. We find that to explain the deepest NIR upper limits assuming either a MW or SMC extinction law, a visual extinction of A_V > 50 is required, which is extremely unlikely. Since both GRBs are bright in X-rays, explanation iii) also cannot explain their dark classification, unless optical radiation and X-rays are not part of the same synchrotron spectrum. An alternative, or complementary explanation of the previous possibility, involves greyer extinction laws. A starburst attenuation curve gives A_V>10, which is less extreme, despite still very high. Assuming high redshift in addition to extinction, implies an A_V>10 at z=2 and A_V>4-5 at z=5, regardless of the adopted extinction recipe. A different, exotic possibility would be an extremely high redshift origin (z>17 given the missing K detections). Population III stars are expected to emerge at z ˜ 20 and can produce GRBs with energies well above those inferred for our GRBs at these redshifts. Mid- and far-IR observations of these extreme class of GRBs can help us to differentiate between the proposed scenarios.

  3. Timeliness of Follow-up after Abnormal Screening Mammogram: Variability of Facilities

    PubMed Central

    Haneuse, Sebastien J. P. A.; Geller, Berta M.; Buist, Diana S. M.; Miglioretti, Diana L.; Brenner, R. James; Smith-Bindman, Rebecca; Taplin, Stephen H.

    2011-01-01

    Purpose: To describe the timeliness of follow-up care in community-based settings among women who receive a recommendation for immediate follow-up during the screening mammography process and how follow-up timeliness varies according to facility and facility-level characteristics. Materials and Methods: This was an institutional review board–approved and HIPAA-compliant study. Screening mammograms obtained from 1996 to 2007 in women 40–80 years old in the Breast Cancer Surveillance Consortium were examined. Inclusion criteria were a recommendation for immediate follow-up at screening, or subsequent imaging, and observed follow-up within 180 days of the recommendation. Recommendations for additional imaging (AI) and biopsy or surgical consultation (BSC) were analyzed separately. The distribution of time to follow-up care was estimated by using the Kaplan-Meier estimator. Results: Data were available on 214 897 AI recommendations from 118 facilities and 35 622 BSC recommendations from 101 facilities. The median time to subsequent follow-up care after recommendation was 14 days for AI and 16 days for BSC. Approximately 90% of AI follow-up and 81% of BSC follow-up occurred within 30 days. Facilities with higher recall rates tended to have longer AI follow-up times (P < .001). Over the study period, BSC follow-up rates at 15 and 30 days improved (P < .001). Follow-up times varied substantially across facilities. Timely follow-up was associated with larger volumes of the recommended procedures but not notably associated with facility type nor observed facility-level characteristics. Conclusion: Most patients with follow-up returned within 3 weeks of the recommendation. © RSNA, 2011 PMID:21900620

  4. Electromagnetic follow-up of gravitational wave candidates

    NASA Astrophysics Data System (ADS)

    Nuttall, L. K.

    Observations of astrophysical systems in different wavelengths can reveal insights in to systems which are not available from a single wavelength. The same can be expected from multi-channel observations of systems which also produce gravitational waves (GWs). The most likely source of strong, detectable GWs, which will also produce an electromagnetic (EM) signature, is the merger of compact objects containing neutron stars (NS) and black holes (BH), namely NS-NS and NS-BH systems. The focus of this thesis is to summarise current and past efforts to detect an EM counterpart of a GW event, with emphasis on compact merger sources. To begin, the formulation of GWs in general relativity is brie y discussed, as well as the main classes of GW sources. The global networks of GW interferometers in the recent past and near future are described, together with brief explanations of operational principles and the main challenges GW detectors face to make a confident detection. Current literature is reviewed to give a brief summary of the most promising sources which produce both GW and EM signals. Emphasis is given to gamma-ray bursts (GRBs), their afterglows, and kilonovae. In addition a brief description of GW searches triggered by an external source (such as a GRB) is given. A new form of search is then discussed in which GW events are used to point conventional EM telescopes, with emphasis on rapidly slewing, wide field of view optical telescopes. The main challenge in this form of search is that timing information from a network of GW interferometers yields large error regions for the source sky direction making it diffcult to locate an EM transient. Therefore a new statistic is presented in which galaxies (taken from a galaxy catalogue) within this search region are ranked. The probability of identifying the host galaxy of a GW signal from NS-NS and NS-BH systems is investigated and results presented for past and future GW detector configurations. The ROTSE-III telescope

  5. The Very Bright and Nearby GRB130427A: the Extra Hard Spectral Component and Implications for Very High-Energy Gamma-Ray Observations of Gamma-Ray Bursts

    NASA Astrophysics Data System (ADS)

    Tam, Pak-Hin Thomas

    2014-03-01

    The extended high-energy gamma-ray (>100 MeV) emission occurring after the prompt gamma-ray bursts (GRBs) is usually characterized by a single power-law spectrum, which has been explained as the afterglow synchrotron radiation. We report on the Fermi Large Area Telescope (LAT) observations of the >100 MeV emission from the very bright and nearby GRB 130427A, up to 100 GeV. By performing time-resolved spectral fits of GRB 130427A, we found a strong evidence of an extra hard spectral component above a few GeV that exists in the extended high-energy emission of this GRB. This extra spectral component may represent the first clear evidence of the long sought-after afterglow inverse Compton emission. Prospects for observations at the very high-energy gamma-rays, i.e., above 100 GeV, are described.

  6. Rapid searches for counterparts of GRB 930131

    NASA Technical Reports Server (NTRS)

    Schaefer, Bradley E.; Barthelmy, Scott D.; Palmer, David M.; Cline, Thomas L.; Hurley, Kevin C.; Sommer, Michael; Boer, Michel; Niel, Michel; Fishman, Gerald J.; Kouveliotou, Chryssa

    1994-01-01

    A fading counterpart to a gamma-ray burst (GRB) would appear as a point source inside a GRB error region soon after the burst which dims on a timescale from minutes to days. The favorable circumstances of the burst GRB 930131 allowed for an international campaign to search for fading counterparts starting 6.8 hr after the burst. We report observations from many optical sites, two radio telescopes, and archival ROSAT data, including deep Schmidt exposures 35, 44, and 64 hr after the burst. No fading counterparts were detected with our observations.

  7. Follow-up study of alcoholic hallucinosis

    PubMed Central

    Perme, Bojir; Vijaysagar, Kommu John; Chandrasekharan, R.

    2003-01-01

    Alcoholic hallucinosis is a pathological mental state characterized by an acute onset of predominant auditory hallucinations that occur either during or after a period of heavy alcohol consumption. In this study, 52 patients with a diagnosis of Psychotic disorder predominantly hallucinatory associated with alcohol use (F 10.52) were evaluated after a period of three years. Past history of withdrawal hallucinations was associated with alcoholic hallucinosis The study has found a wide spectrum of outcome confirming the earlier observations that alcoholic hallucinosis is a heterogeneous disorder. PMID:21206866

  8. Autism and epilepsy: a retrospective follow-up study.

    PubMed

    Hara, Hitoshi

    2007-09-01

    So-called "idiopathic" autism, which exhibited no major complications before diagnosis is well-known as one of the risk factors for epilepsy. This retrospective follow-up study aimed to clarify the characteristics of epilepsy in the autism; onset of seizure, seizure types, EEG findings and epilepsy outcome and the differences as a group between the autism with epilepsy and those without epilepsy. One hundred thirty individuals with autistic disorder or atypical autism diagnosed in childhood were followed up over 10 years and were evaluated almost every year up to 18-35 years of age. Their medical records related to perinatal conditions, IQ, social maturity scores and several factors of epilepsy were reviewed in October 2005. Thirty-three of the follow-up group (25%) exhibited epileptic seizures. The onset of epilepsy was distributed from 8 to 26 years of age. Two types of seizure were observed; partial seizure with secondarily generalized seizure and generalized seizure. Twenty of the epileptics (61%) showed the partial seizure. Although 18% of the non-epileptic group exhibited epileptic discharges on EEG, 68% of the epileptic group revealed epileptiform EEG findings before the onset of epilepsy. No differences were observed concerning the sex ratio, autistic disorder/atypical autism and past history of febrile seizures between the epileptic and non-epileptic groups. Lower IQ, lower social maturity score and higher frequency of prescribed psychotropics were observed in the epileptic group compared to the non-epileptics. Idiopathic autism was confirmed as the high risk factor for epilepsy. Epileptiform EEG findings predict subsequent onset of epileptic seizures in adolescence. Epilepsy is one of negative factors on cognitive, adaptive and behavioral/emotional outcomes for individuals with autism. PMID:17321709

  9. Klenot Project - Near Earth Objects Follow-Up Program

    NASA Astrophysics Data System (ADS)

    Tichý, Miloš; Tichá, Jana; Kočer, Michal

    2016-01-01

    NEO research is a great challenge just now - for science, for exploration and for planetary defence. Therefore NEO discoveries, astrometric follow-up, orbit computations as well as physical studies are of high interest both to science community and humankind. The KLENOT Project of the Klet Observatory, South Bohemia, Czech Republic pursued the confirmation, early follow-up, long-arc follow-up and recovery of Near Earth Objects since 2002. Tens of thousands astrometric measurements helped to make inventory of NEOs as well as to understand the NEO population. It ranked among the world most prolific professional NEO follow-up programmes during its first phase from 2002 to 2008. The fundamental improvement of the 1.06-m KLENOT Telescope was started in autumn 2008. The new computer controlled paralactic mount was built to substantially increase telescope-time efficiency, the number of observations, their accuracy and limiting magnitude. The testing observations of the KLENOT Telescope Next Generation (NG) were started in October 2011. The new more efficient CCD camera FLI ProLine 230 was installed in summer 2013. The original Klet Software Package has been continually upgraded over the past two decades of operation. Along with huge hardware changes we have decided for essential changes in software and the whole KLENOT work-flow. Using the current higher computing power available, enhancing and updating our databases and astrometry program, the core of our software package, will prove highly beneficial. Moreover, the UCAC4 as the more precise astrometric star catalog was implemented. The modernized KLENOT System was put into full operation in September 2013. This step opens new possibilities for the KLENOT Project, the long-term European Contribution to Monitoring and Cataloging Near Earth Objects. KLENOT Project Goals are confirmatory observations of newly discovered fainter NEO candidates, early follow-up of newly discovered NEOs, long-arc follow-up astrometry of NEOs

  10. Klenot Project - Near Earth Objects Follow-Up Program

    NASA Astrophysics Data System (ADS)

    Tichý, Miloš; Tichá, Jana; Kočer, Michal

    2016-01-01

    NEO research is a great challenge just now - for science, for exploration and for planetary defence. Therefore NEO discoveries, astrometric follow-up, orbit computations as well as physical studies are of high interest both to science community and humankind. The KLENOT Project of the Klet Observatory, South Bohemia, Czech Republic pursued the confirmation, early follow-up, long-arc follow-up and recovery of Near Earth Objects since 2002. Tens of thousands astrometric measurements helped to make inventory of NEOs as well as to understand the NEO population. It ranked among the world most prolific professional NEO follow-up programmes during its first phase from 2002 to 2008. The fundamental improvement of the 1.06-m KLENOT Telescope was started in autumn 2008. The new computer controlled paralactic mount was built to substantially increase telescope-time efficiency, the number of observations, their accuracy and limiting magnitude. The testing observations of the KLENOT Telescope Next Generation (NG) were started in October 2011. The new more efficient CCD camera FLI ProLine 230 was installed in summer 2013. The original Klet Software Package has been continually upgraded over the past two decades of operation. Along with huge hardware changes we have decided for essential changes in software and the whole KLENOT work-flow. Using the current higher computing power available, enhancing and updating our databases and astrometry program, the core of our software package, will prove highly beneficial. Moreover, the UCAC4 as the more precise astrometric star catalog was implemented. The modernized KLENOT System was put into full operation in September 2013. This step opens new possibilities for the KLENOT Project, the long-term European Contribution to Monitoring and Cataloging Near Earth Objects. KLENOT Project Goals are confirmatory observations of newly discovered fainter NEO candidates, early follow-up of newly discovered NEOs, long-arc follow-up astrometry of NEOs

  11. 33 CFR 179.15 - Follow-up report.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... discovered as of the date of the follow-up report; (3) The number of units in which corrective action has been completed as of the date of the follow-up report; (4) The number of first purchasers not notified... 33 Navigation and Navigable Waters 2 2010-07-01 2010-07-01 false Follow-up report. 179.15...

  12. 29 CFR 99.315 - Audit findings follow-up.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 29 Labor 1 2010-07-01 2010-07-01 true Audit findings follow-up. 99.315 Section 99.315 Labor Office of the Secretary of Labor AUDITS OF STATES, LOCAL GOVERNMENTS, AND NON-PROFIT ORGANIZATIONS Auditees § 99.315 Audit findings follow-up. (a) General. The auditee is responsible for follow-up and...

  13. 49 CFR 382.311 - Follow-up testing.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... ALCOHOL USE AND TESTING Tests Required § 382.311 Follow-up testing. The requirements for follow-up testing must be performed in accordance with 49 CFR part 40, subpart O. ... 49 Transportation 5 2010-10-01 2010-10-01 false Follow-up testing. 382.311 Section...

  14. 2 CFR 200.511 - Audit findings follow-up.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... 2 Grants and Agreements 1 2014-01-01 2014-01-01 false Audit findings follow-up. 200.511 Section...-up. (a) General. The auditee is responsible for follow-up and corrective action on all audit findings... submitted to the FAC; (ii) The Federal agency or pass-through entity is not currently following up with...

  15. 49 CFR 577.10 - Follow-up notification.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... 49 Transportation 7 2010-10-01 2010-10-01 false Follow-up notification. 577.10 Section 577.10... ADMINISTRATION, DEPARTMENT OF TRANSPORTATION (CONTINUED) DEFECT AND NONCOMPLIANCE NOTIFICATION § 577.10 Follow-up... manufacturer to send a follow-up notification in accordance with this section. The scope, timing, form,...

  16. 49 CFR 577.10 - Follow-up notification.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 49 Transportation 7 2012-10-01 2012-10-01 false Follow-up notification. 577.10 Section 577.10... ADMINISTRATION, DEPARTMENT OF TRANSPORTATION (CONTINUED) DEFECT AND NONCOMPLIANCE NOTIFICATION § 577.10 Follow-up... manufacturer to send a follow-up notification in accordance with this section. The scope, timing, form,...

  17. 49 CFR 382.311 - Follow-up testing.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... ALCOHOL USE AND TESTING Tests Required § 382.311 Follow-up testing. The requirements for follow-up testing must be performed in accordance with 49 CFR part 40, subpart O. ... 49 Transportation 5 2013-10-01 2013-10-01 false Follow-up testing. 382.311 Section...

  18. 49 CFR 577.10 - Follow-up notification.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 49 Transportation 7 2013-10-01 2013-10-01 false Follow-up notification. 577.10 Section 577.10... ADMINISTRATION, DEPARTMENT OF TRANSPORTATION (CONTINUED) DEFECT AND NONCOMPLIANCE NOTIFICATION § 577.10 Follow-up... manufacturer to send a follow-up notification in accordance with this section. The scope, timing, form,...

  19. 33 CFR 179.15 - Follow-up report.

    Code of Federal Regulations, 2013 CFR

    2013-07-01

    ... 33 Navigation and Navigable Waters 2 2013-07-01 2013-07-01 false Follow-up report. 179.15 Section...) BOATING SAFETY DEFECT NOTIFICATION § 179.15 Follow-up report. (a) Each manufacturer who makes an initial report required by § 179.13 shall submit a follow-up report to the Commandant by certified mail within...

  20. 33 CFR 179.15 - Follow-up report.

    Code of Federal Regulations, 2014 CFR

    2014-07-01

    ... 33 Navigation and Navigable Waters 2 2014-07-01 2014-07-01 false Follow-up report. 179.15 Section...) BOATING SAFETY DEFECT NOTIFICATION § 179.15 Follow-up report. (a) Each manufacturer who makes an initial report required by § 179.13 shall submit a follow-up report to the Commandant by certified mail within...

  1. 33 CFR 179.15 - Follow-up report.

    Code of Federal Regulations, 2011 CFR

    2011-07-01

    ... 33 Navigation and Navigable Waters 2 2011-07-01 2011-07-01 false Follow-up report. 179.15 Section...) BOATING SAFETY DEFECT NOTIFICATION § 179.15 Follow-up report. (a) Each manufacturer who makes an initial report required by § 179.13 shall submit a follow-up report to the Commandant by certified mail within...

  2. 49 CFR 577.10 - Follow-up notification.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 49 Transportation 7 2011-10-01 2011-10-01 false Follow-up notification. 577.10 Section 577.10... ADMINISTRATION, DEPARTMENT OF TRANSPORTATION (CONTINUED) DEFECT AND NONCOMPLIANCE NOTIFICATION § 577.10 Follow-up... manufacturer to send a follow-up notification in accordance with this section. The scope, timing, form,...

  3. 49 CFR 382.311 - Follow-up testing.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... ALCOHOL USE AND TESTING Tests Required § 382.311 Follow-up testing. The requirements for follow-up testing must be performed in accordance with 49 CFR part 40, subpart O. ... 49 Transportation 5 2012-10-01 2012-10-01 false Follow-up testing. 382.311 Section...

  4. 49 CFR 382.311 - Follow-up testing.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... ALCOHOL USE AND TESTING Tests Required § 382.311 Follow-up testing. The requirements for follow-up testing must be performed in accordance with 49 CFR part 40, subpart O. ... 49 Transportation 5 2011-10-01 2011-10-01 false Follow-up testing. 382.311 Section...

  5. 49 CFR 382.311 - Follow-up testing.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... ALCOHOL USE AND TESTING Tests Required § 382.311 Follow-up testing. The requirements for follow-up testing must be performed in accordance with 49 CFR part 40, subpart O. ... 49 Transportation 5 2014-10-01 2014-10-01 false Follow-up testing. 382.311 Section...

  6. 49 CFR 577.10 - Follow-up notification.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 49 Transportation 7 2014-10-01 2014-10-01 false Follow-up notification. 577.10 Section 577.10... ADMINISTRATION, DEPARTMENT OF TRANSPORTATION (CONTINUED) DEFECT AND NONCOMPLIANCE NOTIFICATION § 577.10 Follow-up... manufacturer to send a follow-up notification in accordance with this section. The scope, timing, form,...

  7. Broadband Electromagnetic Follow-up of Advanced LIGO Sources

    NASA Astrophysics Data System (ADS)

    Singer, Leo; LIGO Scientific Collaboration; Virgo Collaboration

    2016-03-01

    Advanced LIGO began observing in September 2015 with over 3 times the distance reach (27 times the sensitive volume) of its previous configuration. Some gravitational-wave sources, particularly neutron star binary mergers, are expected to produce broadband electromagnetic transients which may be crucial to understanding the astrophysical context of these events. We have assembled a consortium of over 60 ground- and space-based gamma-ray, x-ray, optical, infrared, and radio facilities collaborating to search for broadband electromagnetic counterparts of gravitational-wave sources. In this talk, we describe the LIGO/Virgo EM follow-up program and the astronomical facilities that participated during this first LIGO observing run. Then, we survey the multi-wavelength observing campaigns embarked upon for specific gravitational-wave events. Finally, we discuss lessons learned and the way forward for joint GW-EM observations in an era of increasingly sensitive GW detectors.

  8. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

    DOE PAGESBeta

    Abbott, B. P.

    2016-07-20

    This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. Here, we compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands.

  9. Can JWST Follow Up on Gravitational-Wave Detections?

    NASA Astrophysics Data System (ADS)

    Kohler, Susanna

    2016-02-01

    Bitten by the gravitational-wave bug? While we await Thursdays press conference, heres some food for thought: if LIGO were able to detect gravitational waves from compact-object mergers, how could we follow up on the detections? A new study investigates whether the upcoming James Webb Space Telescope (JWST) will be able to observe electromagnetic signatures of some compact-object mergers.Hunting for MergersStudying compact-object mergers (mergers of black holes and neutron stars) can help us understand a wealth of subjects, like high-energy physics, how matter behaves at nuclear densities, how stars evolve, and how heavy elements in the universe were created.The Laser Interferometer Gravitational-Wave Observatory (LIGO) is searching for the signature ripples in spacetime identifying these mergers, but gravitational waves are squirrelly: LIGO will only be able to localize wave sources to tens of square degrees. If we want to find out more about any mergers LIGO discovers in gravitational waves, well need a follow-up search for electromagnetic counterparts with other observatories.The Kilonova KeyOne possible electromagnetic counterpart is kilonovae, explosions that can be produced during a merger of a binary neutron star or a neutron starblack hole system. If the neutron star is disrupted during the merger, some of the hot mass is flung outward and shines brightly by radioactive decay.Kilonovae are especially promising as electromagnetic counterparts to gravitational waves for three reasons:They emit isotropically, so the number of observable mergers isnt limited by relativistic beaming.They shine for a week, giving follow-up observatories time to search for them.The source location can beeasily recovered.The only problem? We dont currently have any sensitive survey instruments in the near-infrared band (where kilonova emission peaks) that can provide coverage over tens of square degrees. Luckily, we will soon have just the thing: JWST, launching in 2018!JWSTs

  10. Follow up observations of SDSS and CRTS candidate cataclysmic variables

    SciTech Connect

    Szkody, Paula; Vasquez-Soltero, Stephanie; Everett, Mark E.; Silva, David R.; Howell, Steve B.; Landolt, Arlo U.; Bond, Howard E. E-mail: dsilva@noao.edu E-mail: landolt@rouge.phys.lsu.edu

    2014-10-01

    We present photometry and spectroscopy of 11 and 35 potential cataclysmic variables, respectively, from the Sloan Digital Sky Survey, the Catalina Real-Time Transient Survey, and vsnet alerts. The photometry results include quasi-periodic oscillations during the decline of V1363 Cyg, nightly accretion changes in the likely Polar (AM Herculis binary) SDSS J1344+20, eclipses in SDSS J2141+05 with an orbital period of 76 ± 2 minutes, and possible eclipses in SDSS J2158+09 at an orbital period near 100 minutes. Time-resolved spectra reveal short orbital periods near 80 minutes for SDSS J0206+20, 85 minutes for SDSS J1502+33, and near 100 minutes for CSS J0015+26, RXS J0150+37, SDSS J1132+62, SDSS J2154+15, and SDSS J2158+09. The prominent He II line and velocity amplitude of SDSS J2154+15 are consistent with a Polar nature for this object, while the absence of this line and a low velocity amplitude argue against this classification for RXS J0150+37. Single spectra of 10 objects were obtained near outburst and the rest near quiescence, confirming the dwarf novae nature of these objects.

  11. Early-onset schizophrenia: a 15-year follow-up.

    PubMed

    Röpcke, Bernd; Eggers, Christian

    2005-09-01

    The study describes the psychopathological and social outcome of patients treated for schizophrenia in adolescence (mean age at onset 16.0 years/SD 1.52) after a mean follow-up period of 15.4 years (10.2-21.2 years). Out of 55 patients consecutively admitted to hospital, 47 (85 %) could be traced and 39 (71 %) could be re-examined. At follow-up, 33/39 patients (85 %) had had at least one readmission. Full remission of global psychopathological symptoms [Clinical Global Impression (CGI) observed in 20/39 (51 %). The best predictor of global psychopathological and psychosocial outcome was type of onset (CGI: Beta=0.36, GAS: Beta=-0.37). A poor outcome was seen in 22 out of 25 cases with insidious onset. All predictors together explained 58% of the variance in the Positive and Negative Syndrome (PANSS) negative symptom ratings at follow-up. Gender, duration of first inpatient treatment and duration of untreated psychosis were of no predictive value for outcome. The nature of the diagnosis in the first episode strongly predicted the diagnosis given for the whole course after 15 years. In 26/37 cases (70 %), diagnosis at onset and overall diagnoses were the same. Our finding of an incidence of 61% insidious onset is similar to that in adult onset schizophrenia (AOS), but different to very early onset schizophrenia (VEOS), which shows a higher rate of insidious onset, cognitive impairment and poor outcome. Therefore, it seems that VEOS is a special group compared with early onset schizophrenia (EOS) and AOS. PMID:16220219

  12. Astrometric Follow-Up of Faint Near Earth Objects

    NASA Technical Reports Server (NTRS)

    Morgan, T. (Technical Monitor); Spahr, Timothy

    2004-01-01

    The observing program at Mt. Hopkins using the 48" reflector and funded by the Near- Earth Object Observation Program continues to excel. As in the past, all requested observing time was granted. Minor improvements continue to be made. For example, the telescope is set up to track and non-sidereal rates. This allows the user to track on the target object, rather than relying exclusively on the shift- and-stack technique. Other improvements made by the staff include automatic focus routines, automatic seeing-measurement routines, and improvement in dome seeing and mirror stabilization. The net result is better focus, better seeing, and the ability to expose longer in order to acquire the faintest and most important objects. During the proposal period, this program ranked again very high worldwide in terms of faint Near Earth Objects observed. During this latest proposal cycle, fewer objects were observed than previous cycles, but this was due to the strict targeting of only the faintest observable objects. The follow-up programs of observatory codes 926 (led by P. Holvorcem) and 291 (led by Dr. B. McMillan) have greatly increased their capacity, and as a result less bright objects are in urgent need of follow-up than in years past. Even with this new object selection and additional competition, code 696 still ranked second to code 291 in terms of objects observed fainter than V = 20. Minimal scripting is now in place to allow the telescope to run autonomously for 30-45 minutes at a time.

  13. A follow-up campaign for fast radio bursts

    NASA Astrophysics Data System (ADS)

    Petroff, Emily; Possenti, Andrea; Johnston, Simon; Kramer, Michael; Bailes, Matthew; Burke-Spolaor, Sarah; van Straten, Willem; Keane, Evan; Champion, David; Jameson, Andrew; Ng, Cherry; Barr, Ewan; Flynn, Chris; Caleb, Manisha

    2014-04-01

    Fast Radio Bursts (FRBs) are bright, millisecond-duration radio pulses hypothesized to originate at cosmological distances. To date, no counterpart sources have been associated with FRBs and their origins remain a puzzling mystery. Some have proposed FRBs come from Crab-like pulsar giant pulses or rare bursts from main sequence flare stars in our Galaxy. Both mechanisms would generate observable subsequent FRB-like events. In this proposal we directly test this hypothesis by conducting several follow-up observations on the eight FRBs from the High Time Resolution Universe Survey. This sample represents the majority of the dozen or so known FRB sources. With these observations we will set strict limits on any repetition of FRBs while using the 12 off-source beams of the multi-beam receiver as real-time FRB and transient detectors.

  14. Rothmund-Thomson Syndrome: A 13-Year Follow-Up

    PubMed Central

    Guerrero-González, Guillermo Antonio; Martínez-Cabriales, Sylvia Aideé; Hernández-Juárez, Aideé Alejandra; de Jesús Lugo-Trampe, José; Espinoza-González, Nelly Alejandra; Gómez-Flores, Minerva; Ocampo-Candiani, Jorge

    2014-01-01

    Rothmund-Thomson syndrome (RTS) is a rare autosomal recessive disorder presenting with poikiloderma and other clinical features, affecting the bones and eyes and, in type II RTS, presenting an increased risk for malignancy. With about 300 cases reported so far, we present a 13-year follow-up including clinical images, X-rays and genetic analysis. A 13-month-old female started with a facial rash with blisters on her cheeks and limbs at the age of 3 months along with congenital hypoplastic thumbs, frontal bossing and fine hair, eyebrows and eyelashes. The patient was lost to follow-up and returned 12 years later with palmoplantar hyperkeratotic lesions, short stature, disseminated poikiloderma and sparse scalp hair, with absence of eyelashes and eyebrows. Radiographic analysis showed radial ray defect, absence of the thumb and three wrist carpal bones, and reduced bone density. Gene sequencing for the RECQL4 helicase gene revealed a mutation on each allele. RTS is a rare disease, and in this patient we observed the evolution of her skin lesions and other clinical features, which were important for the classification of type II RTS. The next years will provide even more information on this rare disease. PMID:25120469

  15. Long-term follow-up of atomic bomb survivors.

    PubMed

    Sakata, Ritsu; Grant, Eric J; Ozasa, Kotaro

    2012-06-01

    The Life Span Study (LSS) is a follow-up study of atomic bomb (A-bomb) survivors to investigate the radiation effects on human health and has collected data for over 60 years. The LSS cohort consists of 93,741 A-bomb survivors and another 26,580 age and sex-matched subjects who were not in either city at the time of the bombing. Radiation doses have been computed based on individual location and shielding status at the time of the bombings. Age at death and cause of death are gathered through the Japanese national family registry system and cancer incidence data have been collected through the Hiroshima and Nagasaki cancer registries. Noncancer disease incidence and health information are collected through biannual medical examinations among a subset of the LSS. Radiation significantly increases the risks of death (22% at 1 Gy), cancer incidence (47% at 1 Gy), death due to leukemia (310% at 1 Gy), as well as the incidence of several noncancer diseases (e.g. thyroid nodules, chronic liver disease and cirrhosis, uterine myoma, and hypertension). Significant effects on maturity (e.g. growth reduction and early menopause) were also observed. Long-term follow-up studies of the A-bomb survivors have provided reliable information on health risks for the survivors and form the basis for radiation protection standards for workers and the public.

  16. Serial extraction: 20 years of follow-up.

    PubMed

    Almeida, Renato Rodrigues de; Almeida, Marcio Rodrigues de; Oltramari-Navarro, Paula Vanessa Pedron; Conti, Ana Cláudia de Castro Ferreira; Navarro, Ricardo de Lima; Souza, Karen Regina Siqueira de

    2012-01-01

    This paper reports a case treated by a serial extraction program at the mixed dentition stage followed by a corrective orthodontic treatment, with a long-term follow-up period. Twenty years after the interceptive treatment, a harmonious face was observed along with treatment stability in the anterior posterior direction, deep overbite (which has been mentioned as a disadvantage of the serial extraction program), and a small relapse of anterior tooth crowding. All these conditions have been regarded as normal occurrences for most orthodontic treatments with a long-term follow-up period. This case report demonstrated that the establishment of a serial extraction protocol determined relevant esthetic changes that afforded an improvement of the patient's self-esteem, with a positive social impact. Furthermore, the low cost of this protocol permits the use of this therapy with underprivileged populations. It is important to emphasize that an early correction of tooth crowding by this protocol does not guarantee stability, but small relapses do not invalidate its accomplishment.

  17. Serial extraction: 20 years of follow-up

    PubMed Central

    de ALMEIDA, Renato Rodrigues; de ALMEIDA, Marcio Rodrigues; OLTRAMARI-NAVARRO, Paula Vanessa Pedron; CONTI, Ana Cláudia de Castro Ferreira; NAVARRO, Ricardo de Lima; de SOUZA, Karen Regina Siqueira

    2012-01-01

    This paper reports a case treated by a serial extraction program at the mixed dentition stage followed by a corrective orthodontic treatment, with a long-term follow-up period. Twenty years after the interceptive treatment, a harmonious face was observed along with treatment stability in the anterior posterior direction, deep overbite (which has been mentioned as a disadvantage of the serial extraction program), and a small relapse of anterior tooth crowding. All these conditions have been regarded as normal occurrences for most orthodontic treatments with a long-term follow-up period. This case report demonstrated that the establishment of a serial extraction protocol determined relevant esthetic changes that afforded an improvement of the patient's self-esteem, with a positive social impact. Furthermore, the low cost of this protocol permits the use of this therapy with underprivileged populations. It is important to emphasize that an early correction of tooth crowding by this protocol does not guarantee stability, but small relapses do not invalidate its accomplishment. PMID:23032213

  18. Long-term follow-up of atomic bomb survivors.

    PubMed

    Sakata, Ritsu; Grant, Eric J; Ozasa, Kotaro

    2012-06-01

    The Life Span Study (LSS) is a follow-up study of atomic bomb (A-bomb) survivors to investigate the radiation effects on human health and has collected data for over 60 years. The LSS cohort consists of 93,741 A-bomb survivors and another 26,580 age and sex-matched subjects who were not in either city at the time of the bombing. Radiation doses have been computed based on individual location and shielding status at the time of the bombings. Age at death and cause of death are gathered through the Japanese national family registry system and cancer incidence data have been collected through the Hiroshima and Nagasaki cancer registries. Noncancer disease incidence and health information are collected through biannual medical examinations among a subset of the LSS. Radiation significantly increases the risks of death (22% at 1 Gy), cancer incidence (47% at 1 Gy), death due to leukemia (310% at 1 Gy), as well as the incidence of several noncancer diseases (e.g. thyroid nodules, chronic liver disease and cirrhosis, uterine myoma, and hypertension). Significant effects on maturity (e.g. growth reduction and early menopause) were also observed. Long-term follow-up studies of the A-bomb survivors have provided reliable information on health risks for the survivors and form the basis for radiation protection standards for workers and the public. PMID:22440534

  19. THE OPTICALLY UNBIASED GRB HOST (TOUGH) SURVEY. VI. RADIO OBSERVATIONS AT z {approx}< 1 AND CONSISTENCY WITH TYPICAL STAR-FORMING GALAXIES

    SciTech Connect

    Michalowski, M. J.; Dunlop, J. S.; Kamble, A.; Kaplan, D. L.; Hjorth, J.; Malesani, D.; Fynbo, J. P. U.; Kruehler, T.; Reinfrank, R. F.; Bonavera, L.; Ibar, E.; Garrett, M. A.; Jakobsson, P.; Levan, A. J.; Massardi, M.; Pal, S.; Sollerman, J.; Tanvir, N. R.; Van der Horst, A. J.; and others

    2012-08-20

    The objective of this paper is to determine the level of obscured star formation activity and dust attenuation in a sample of gamma-ray burst (GRB) hosts, and to test the hypothesis that GRB hosts have properties consistent with those of the general star-forming galaxy populations. We present a radio continuum survey of all z < 1 GRB hosts in The Optically Unbiased GRB Host (TOUGH) sample supplemented with radio data for all (mostly pre-Swift) GRB-SN hosts discovered before 2006 October. We present new radio data for 22 objects and have obtained a detection for three of them (GRB 980425, 021211, 031203; none in the TOUGH sample), increasing the number of radio-detected GRB hosts from two to five. The star formation rate (SFR) for the GRB 021211 host of {approx}825 M{sub Sun} yr{sup -1}, the highest ever reported for a GRB host, places it in the category of ultraluminous infrared galaxies. We found that at least {approx}63% of GRB hosts have SFR < 100 M{sub Sun} yr{sup -1} and at most {approx}8% can have SFR > 500 M{sub Sun} yr{sup -1}. For the undetected hosts the mean radio flux (<35 {mu}Jy 3{sigma}) corresponds to an average SFR < 15 M{sub Sun} yr{sup -1}. Moreover, {approx}> 88% of the z {approx}< 1 GRB hosts have ultraviolet dust attenuation A{sub UV} < 6.7 mag (visual attenuation A{sub V} < 3 mag). Hence, we did not find evidence for large dust obscuration in a majority of GRB hosts. Finally, we found that the distributions of SFRs and A{sub UV} of GRB hosts are consistent with those of Lyman break galaxies, H{alpha} emitters at similar redshifts, and of galaxies from cosmological simulations. The similarity of the GRB population with other star-forming galaxies is consistent with the hypothesis that GRBs, a least at z {approx}< 1, trace a large fraction of all star formation, and are therefore less biased indicators than once thought.

  20. The LCOGT near-Earth-object follow-up network

    NASA Astrophysics Data System (ADS)

    Lister, T.

    2014-07-01

    Las Cumbres Observatory Global Telescope (LCOGT) network is a planned homogeneous network that will eventually consist of over 35 telescopes at 6 locations in the northern and southern hemispheres [1]. This network is versatile and designed to respond rapidly to target of opportunity events and also to do long term monitoring of slowly changing astronomical phenomena. The global coverage of the network and the apertures of telescope available make the LCOGT network ideal for follow-up and characterization of a wide range of solar-system objects (e.g. asteroids, Kuiper-belt objects, comets) and in particular near-Earth objects (NEOs). There are 3 classes to the telescope resources: 2-meter aperture, 1-meter aperture and 0.4-meter aperture. We have been operating our two 2-meter telescopes since 2005 and began a specific program of NEO follow-up for the Pan-STARRS survey in October 2010. The combination of all-sky access, large aperture, rapid response, robotic operation and good site conditions allows us to provide time-critical follow-up astrometry and photometry on newly discovered objects and faint objects as they recede from the Earth, allowing the orbital arc to be extended and preventing loss of objects. These telescope resources have greatly increased as LCOGT has completed the first phase of the deployment, designated as ''Version 1.0'', with the installation, commissioning and ongoing operation of nine 1-meter telescopes. These are distributed among four sites with one 1-meter at McDonald Observatory (Texas), three telescopes at Cerro Tololo (Chile), three telescopes at SAAO (South Africa) and the final two telescope at Siding Spring Observatory (Australia). In addition to the 1-meter network, the scheduling and control system for the two 2-meter telescopes have been upgraded and unified with that of the 1-meter network to provide a coherent robotic telescopic network. The telescope network is now operating and observations are being executed remotely and

  1. GRB050525A : Multiband modelling of the afterglow

    NASA Astrophysics Data System (ADS)

    Resmi, Lekshmi; Misra, Kuntal; Castro-Tirado, Alberto

    2011-08-01

    The Swift era has posed a challenge to the standard blast-wave model of Gamma Ray Burst afterglows. The achromatic steepening of the afterglow lightcurves (`jet break') considered in the model as the signature of outflow collimation, has become almost rare. Several afterglows exhibited complex lightcurves that did not confirm by the predicted spectral--temporal `closure relations' of the blastwave model. Here we present optical observations and broadband modelling of the afterglow of GRB0505025A, a bright burst detected and followed up by Swift. We find that the overall evolution of the afterglow can not be explained by a single forward shock emission, though the late time evolution is compatible with the predictions of the standard afterglow model, including a jet break. We explain the afterglow evolution based on a two-component jet model and estimate the physical parameters.

  2. Submillimeter Follow-up of WISE-selected Hyperluminous Galaxies

    NASA Astrophysics Data System (ADS)

    Wu, Jingwen; Tsai, Chao-Wei; Sayers, Jack; Benford, Dominic; Bridge, Carrie; Blain, Andrew; Eisenhardt, Peter R. M.; Stern, Daniel; Petty, Sara; Assef, Roberto; Bussmann, Shane; Comerford, Julia M.; Cutri, Roc; Evans, Neal J., II; Griffith, Roger; Jarrett, Thomas; Lake, Sean; Lonsdale, Carol; Rho, Jeonghee; Stanford, S. Adam; Weiner, Benjamin; Wright, Edward L.; Yan, Lin

    2012-09-01

    We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of Wide-field Infrared Survey Explorer (WISE) selected, hyperluminous galaxies, the so-called W1W2-dropout galaxies. This is a rare (~1000 all-sky) population of galaxies at high redshift (peaks at z = 2-3), which are faint or undetected by WISE at 3.4 and 4.6 μm, yet are clearly detected at 12 and 22 μm. The optical spectra of most of these galaxies show significant active galactic nucleus activity. We observed 14 high-redshift (z > 1.7) W1W2-dropout galaxies with SHARC-II at 350-850 μm, with nine detections, and observed 18 with Bolocam at 1.1 mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 μm, as well as optical spectra of 12 targets, are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submillimeter ratios than other galaxy templates, suggesting a hotter dust temperature. We estimate their dust temperatures to be 60-120 K using a single-temperature model. Their infrared luminosities are well over 1013 L ⊙. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the universe. We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data.

  3. SUBMILLIMETER FOLLOW-UP OF WISE-SELECTED HYPERLUMINOUS GALAXIES

    SciTech Connect

    Wu Jingwen; Eisenhardt, Peter R. M.; Stern, Daniel; Assef, Roberto; Tsai, Chao-Wei; Cutri, Roc; Griffith, Roger; Jarrett, Thomas; Sayers, Jack; Bridge, Carrie; Benford, Dominic; Blain, Andrew; Petty, Sara; Lake, Sean; Bussmann, Shane; Comerford, Julia M.; Evans, Neal J. II; Lonsdale, Carol; Rho, Jeonghee; Stanford, S. Adam; and others

    2012-09-01

    We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of Wide-field Infrared Survey Explorer (WISE) selected, hyperluminous galaxies, the so-called W1W2-dropout galaxies. This is a rare ({approx}1000 all-sky) population of galaxies at high redshift (peaks at z = 2-3), which are faint or undetected by WISE at 3.4 and 4.6 {mu}m, yet are clearly detected at 12 and 22 {mu}m. The optical spectra of most of these galaxies show significant active galactic nucleus activity. We observed 14 high-redshift (z > 1.7) W1W2-dropout galaxies with SHARC-II at 350-850 {mu}m, with nine detections, and observed 18 with Bolocam at 1.1 mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 {mu}m, as well as optical spectra of 12 targets, are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submillimeter ratios than other galaxy templates, suggesting a hotter dust temperature. We estimate their dust temperatures to be 60-120 K using a single-temperature model. Their infrared luminosities are well over 10{sup 13} L{sub Sun }. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the universe. We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data.

  4. Submillimeter Follow-up of Wise-Selected Hyperluminous Galaxies

    NASA Technical Reports Server (NTRS)

    Wu, Jingwen; Tsai, Chao-Wei; Sayers, Jack; Benford, Dominic; Bridge, Carrie; Blain, Andrew; Eisenhardt, Peter R. M.; Stern, Daniel; Petty, Sara; Assef, Roberto; Bussmann, Shane; Comerford, Julia M.; Cutri, Roc; Evans, Neal J., II; Griffith, Roger; Jarrett, Thomas; Lake, Sean; Lonsdale, Carol; Rho, Jeonghee; Stanford, S. Adam

    2013-01-01

    We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of Wide-field Infrared Survey Explorer (WISE) selected, hyperluminous galaxies, the so-called W1W2-dropout galaxies. This is a rare (approximately 1000 all-sky) population of galaxies at high redshift (peaks at zeta = 2-3), which are faint or undetected by WISE at 3.4 and 4.6 micrometers, yet are clearly detected at 12 and 22 micrometers. The optical spectra of most of these galaxies show significant active galactic nucleus activity. We observed 14 high-redshift (zeta greater than 1.7) W1W2-dropout galaxies with SHARC-II at 350-850 micrometers, with nine detections, and observed 18 with Bolocam at 1.1 mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 micrometers, as well as optical spectra of 12 targets, are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submillimeter ratios than other galaxy templates, suggesting a hotter dust temperature.We estimate their dust temperatures to be 60-120 K using a single-temperature model. Their infrared luminosities are well over 10(exp 13) solar luminosity. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the universe.We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data.

  5. Submillimeter Follow-Up of WISE-Selected Hyperluminous Galaxies

    NASA Technical Reports Server (NTRS)

    Wu, Jingwen; Tsai, Chao-Wei; Sayers, Jack; Benford, Dominic; Bridge, Carrie; Blain, Andrew; Eisenhardt, Peter R.; Stern, Daniel; Petty, Sara; Assef, Roberto; Bussmann, Shane; Comerford, Julia M.; Cutri, Roc; Evans, Neal J., II; Griffith, Roger; Jarrett, Thomas; Lake, Sean; Lonsdale, Carol; Rho, Jeonghee; Stanford, S. Adam; Weiner, Benjamin; Wright, Edward L.; Yan, Lin

    2012-01-01

    We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of Wide-field Infrared Survey Explorer (WISE) selected, hyperluminous galaxies, the so-called W1W2-dropout galaxies. This is a rare (approx.1000 all-sky) population of galaxies at high redshift (peaks at z = 2-3), which are faint or undetected by WISE at 3.4 and 4.6 microns, yet are clearly detected at 12 and 22 microns. The optical spectra of most of these galaxies show significant active galactic nucleus activity. We observed 14 high-redshift (z > 1.7) W1W2-dropout galaxies with SHARC-II at 350-850 microns, with nine detections, and observed 18 with Bolocam at 1.1 mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 microns, as well as optical spectra of 12 targets, are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submillimeter ratios than other galaxy templates, suggesting a hotter dust temperature.We estimate their dust temperatures to be 60 C120 K using a single-temperature model. Their infrared luminosities are well over 10(exp 13) Stellar Luminosity. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the universe.We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data.

  6. High-Quality Early-Time Light Curves of GRB 060206: Implications for Gamma-Ray Burst Environments and Energetics

    NASA Astrophysics Data System (ADS)

    Monfardini, A.; Kobayashi, S.; Guidorzi, C.; Carter, D.; Mundell, C. G.; Bersier, D. F.; Gomboc, A.; Melandri, A.; Mottram, C. J.; Smith, R. J.; Steele, I. A.

    2006-09-01

    The 2 m robotic Liverpool Telescope (LT) reacted promptly to the high-redshift (z=4.048) gamma-ray burst GRB 060206. The afterglow was identified automatically, and the multicolor r'i'z' imaging program was triggered without human intervention. Combining our data with those obtained from later follow-ups provides a well-sampled optical light curve from 5 minutes to more than 2days after the gamma event. The light curve is highly structured, with at least three bumps evident in the first 75 minutes, including a major rebrightening (Δr'~-1.6 at t~3000 s), interpreted as late energy injection. At early time (t~440 s), we find evidence for fast (Δtrest<4 s<GRB (z<1) with similar intrinsic properties would have been interpreted completely differently, due to undersampling of the light curve in the rest frame at early times; the light-curve behavior of GRB 060206 should therefore not be considered peculiar. Finally, although the observed late-time steepening of the optical light curve resembles a jet break if taken in isolation, the lack of a corresponding change in the X-ray slope rules out a jet-break interpretation. Traditionally, GRB jet breaks have been inferred from optical data in the absence of simultaneous X-ray data. We therefore suggest that current estimates of the jet-opening angle distribution might be biased by events like GRB 060206. Consequently, the GRB explosion energy distribution and event rates may have to be revised.

  7. GRB 130427A: A Nearby Ordinary Monster

    NASA Technical Reports Server (NTRS)

    Maselli, A.; Melandri, A.; Nava, L.; Mundell, C. G.; Kawai, N.; Campana, S.; Covino, S.; Cummings, J. R.; Cusumano, G.; Evans, P. A.; Ghirlander, G.; Ghisellini, G.; Guidorzi, C.; Kobayashi, S.; Kuin, P.; La Parola, V.; Mangano, V.; Oates, S.; Barthelmy, S.; Gehrels, N.; Marshall, F.; Wiegand, B.

    2014-01-01

    Long-duration gamma-ray bursts (GRBs) are an extremely rare outcome of the collapse of massive stars and are typically found in the distant universe. Because of its intrinsic luminosity (L approx. 3 x 10(exp 53) ergs/s and its relative proximity (z = 0.34), GRB 130427A reached the highest fluence observed in the gamma-ray band. Here, we present a comprehensive multiwavelength view of GRB 130427A with Swift, the 2-meter Liverpool and Faulkes telescopes, and by other ground-based facilities, highlighting the evolution of the burst emission from the prompt to the afterglow phase. The properties of GRB 130427A are similar to those of the most luminous, high-redshift GRBs, suggesting that a common central engine is responsible for producing GRBs in both the contemporary and the early universe and over the full range of GRB isotropic energies.

  8. GRB 130427A: A Nearby Ordinary Monster

    NASA Astrophysics Data System (ADS)

    Maselli, A.; Melandri, A.; Nava, L.; Mundell, C. G.; Kawai, N.; Campana, S.; Covino, S.; Cummings, J. R.; Cusumano, G.; Evans, P. A.; Ghirlanda, G.; Ghisellini, G.; Guidorzi, C.; Kobayashi, S.; Kuin, P.; La Parola, V.; Mangano, V.; Oates, S.; Sakamoto, T.; Serino, M.; Virgili, F.; Zhang, B.-B.; Barthelmy, S.; Beardmore, A.; Bernardini, M. G.; Bersier, D.; Burrows, D.; Calderone, G.; Capalbi, M.; Chiang, J.; D'Avanzo, P.; D'Elia, V.; De Pasquale, M.; Fugazza, D.; Gehrels, N.; Gomboc, A.; Harrison, R.; Hanayama, H.; Japelj, J.; Kennea, J.; Kopac, D.; Kouveliotou, C.; Kuroda, D.; Levan, A.; Malesani, D.; Marshall, F.; Nousek, J.; O'Brien, P.; Osborne, J. P.; Pagani, C.; Page, K. L.; Page, M.; Perri, M.; Pritchard, T.; Romano, P.; Saito, Y.; Sbarufatti, B.; Salvaterra, R.; Steele, I.; Tanvir, N.; Vianello, G.; Weigand, B.; Wiersema, K.; Yatsu, Y.; Yoshii, T.; Tagliaferri, G.

    2014-01-01

    Long-duration gamma-ray bursts (GRBs) are an extremely rare outcome of the collapse of massive stars and are typically found in the distant universe. Because of its intrinsic luminosity (L ˜ 3 × 1053 ergs per second) and its relative proximity (z = 0.34), GRB 130427A reached the highest fluence observed in the γ-ray band. Here, we present a comprehensive multiwavelength view of GRB 130427A with Swift, the 2-meter Liverpool and Faulkes telescopes, and by other ground-based facilities, highlighting the evolution of the burst emission from the prompt to the afterglow phase. The properties of GRB 130427A are similar to those of the most luminous, high-redshift GRBs, suggesting that a common central engine is responsible for producing GRBs in both the contemporary and the early universe and over the full range of GRB isotropic energies.

  9. 49 CFR 219.211 - Analysis and follow-up.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... 49 Transportation 4 2013-10-01 2013-10-01 false Analysis and follow-up. 219.211 Section 219.211... Analysis and follow-up. (a) The laboratory designated in appendix B to this part undertakes prompt analysis... notification of the results of the toxicological analysis, any provision of collective bargaining...

  10. 49 CFR 219.211 - Analysis and follow-up.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... 49 Transportation 4 2014-10-01 2014-10-01 false Analysis and follow-up. 219.211 Section 219.211... Analysis and follow-up. (a) The laboratory designated in appendix B to this part undertakes prompt analysis... notification of the results of the toxicological analysis, any provision of collective bargaining...

  11. Leisure of Opiate Addicts at Posttreatment Follow-Up.

    ERIC Educational Resources Information Center

    Simpson, D. Dwayne; And Others

    1981-01-01

    Comparisons of self-reported leisure showed an overall shift toward more positive, socially accepted leisure activities at follow-up. More free time was spent with family and friends who did not use drugs. Positive leisure at follow-up was related to favorable outcomes on drug use, criminality, and productive activities. (Author)

  12. 49 CFR 219.211 - Analysis and follow-up.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... 49 Transportation 4 2012-10-01 2012-10-01 false Analysis and follow-up. 219.211 Section 219.211 Transportation Other Regulations Relating to Transportation (Continued) FEDERAL RAILROAD ADMINISTRATION... Analysis and follow-up. (a) The laboratory designated in appendix B to this part undertakes prompt...

  13. 49 CFR 219.211 - Analysis and follow-up.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... 49 Transportation 4 2011-10-01 2011-10-01 false Analysis and follow-up. 219.211 Section 219.211 Transportation Other Regulations Relating to Transportation (Continued) FEDERAL RAILROAD ADMINISTRATION... Analysis and follow-up. (a) The laboratory designated in appendix B to this part undertakes prompt...

  14. The LCOGT Near Earth Object (NEO) Follow-up Network

    NASA Astrophysics Data System (ADS)

    Lister, Tim; Gomez, Edward; Christensen, Eric; Larson, Steve

    2014-11-01

    Las Cumbres Observatory Global Telescope (LCOGT) network is a planned homogeneous network of over 35 telescopes at 6 locations in the northern and southern hemispheres. This network is versatile and designed to respond rapidly to target of opportunity events and also to do long term monitoring of slowly changing astronomical phenomena. The global coverage of the network and the apertures of telescope available make LCOGT ideal for follow-up and characterization of Solar System objects (e.g. asteroids, Kuiper Belt Objects, comets, Near-Earth Objects (NEOs)) and ultimately for the discovery of new objects.LCOGT has completed the first phase of the deployment with the installation and commissioning of nine 1-meter telescopes at McDonald Observatory (Texas), Cerro Tololo (Chile), SAAO (South Africa) and Siding Spring Observatory (Australia). The telescope network is now operating and observations are being executed remotely and robotically.I am using the LCOGT network to confirm newly detected NEO candidates produced by the major sky surveys such as Catalina Sky Survey (CSS), NEOWISE and PanSTARRS (PS1). Over 600 NEO candidates have been targeted so far this year with 250+ objects reported to the MPC, including 70 confirmed NEOs. An increasing amount of time is being spent to obtain follow-up astrometry and photometry for radar-targeted objects in order to improve the orbits and determine the rotation periods. This will be extended to obtain more light curves of other NEOs which could be Near-Earth Object Human Space Flight Accessible Targets Study (NHATS) or Asteroid Retrieval Mission (ARM) targets. Recent results have included the first period determination for the Apollo 2002 NV16 and our first NEO spectrum from the FLOYDS spectrographs on the LCOGT 2m telescopes obtained for 2012 DA14 during the February 2013 closepass.

  15. Broadband Electromagnetic Follow-up of Advanced LIGO Sources

    NASA Astrophysics Data System (ADS)

    Pound Singer, Leo

    2016-04-01

    Advanced LIGO began observing in September 2015 with over 3 times the distance reach (27 times the sensitive volume) of its previous configuration. Some gravitational-wave sources, particularly neutron star binary mergers, are expected to produce broadband electromagnetic transients which may be crucial to understanding the astrophysical context of these events. We have assembled a consortium of over 60 ground- and space-based gamma-ray, x-ray, optical, infrared, and radio facilities collaborating to search for broadband electromagnetic counterparts of gravitational-wave sources. In this talk, we describe the LIGO/Virgo EM follow-up program and the astronomical facilities that participated during this first LIGO observing run. Then, we survey the multi-wavelength observing campaigns embarked upon for specific gravitational-wave events. Finally, we discuss lessons learned and the way forward for joint GW-EM observations in an era of increasingly sensitive GW detectors.Submitted with The LIGO Scientific Collaboration and The Virgo Collaboration.

  16. GRB 081007 AND GRB 090424: THE SURROUNDING MEDIUM, OUTFLOWS, AND SUPERNOVAE

    SciTech Connect

    Jin Zhiping; Covino, Stefano; Fugazza, Dino; Melandri, Andrea; Campana, Sergio; D'Avanzo, Paolo; Della Valle, Massimo; Ferrero, Patrizia; Malesani, Daniele; Fynbo, Johan P. U.; Hjorth, Jens; Pian, Elena; Salvaterra, Ruben; Bersier, David; Cano, Zach; Castro-Tirado, Alberto J.; Gorosabel, Javier; Guidorzi, Cristiano; Haislip, Joshua B.; and others

    2013-09-10

    We discuss the results of the analysis of multi-wavelength data for the afterglows of GRB 081007 and GRB 090424, two bursts detected by Swift. One of them, GRB 081007, also shows a spectroscopically confirmed supernova, SN 2008hw, which resembles SN 1998bw in its absorption features, while the maximum magnitude may be fainter, up to 0.7 mag, than observed in SN 1998bw. Bright optical flashes have been detected in both events, which allows us to derive solid constraints on the circumburst-matter density profile. This is particularly interesting in the case of GRB 081007, whose afterglow is found to be propagating into a constant-density medium, yielding yet another example of a gamma-ray burst (GRB) clearly associated with a massive-star progenitor which did not sculpt the surroundings with its stellar wind. There is no supernova component detected in the afterglow of GRB 090424, likely due to the brightness of the host galaxy, comparable to the Milky Way. We show that the afterglow data are consistent with the presence of both forward- and reverse-shock emission powered by relativistic outflows expanding into the interstellar medium. The absence of optical peaks due to the forward shock strongly suggests that the reverse-shock regions should be mildly magnetized. The initial Lorentz factor of outflow of GRB 081007 is estimated to be {Gamma} {approx} 200, while for GRB 090424 a lower limit of {Gamma} > 170 is derived. We also discuss the prompt emission of GRB 081007, which consists of just a single pulse. We argue that neither the external forward-shock model nor the shock-breakout model can account for the prompt emission data and suggest that the single-pulse-like prompt emission may be due to magnetic energy dissipation of a Poynting-flux-dominated outflow or to a dissipative photosphere.

  17. The ECLAIRs micro-satellite mission for gamma-ray burst multi-wavelength observations

    NASA Astrophysics Data System (ADS)

    Schanne, S.; Atteia, J.-L.; Barret, D.; Basa, S.; Boer, M.; Casse, F.; Cordier, B.; Daigne, F.; Klotz, A.; Limousin, O.; Manchanda, R.; Mandrou, P.; Mereghetti, S.; Mochkovitch, R.; Paltani, S.; Paul, J.; Petitjean, P.; Pons, R.; Ricker, G.; Skinner, G.

    2006-11-01

    Gamma-ray bursts (GRB)—at least those with a duration longer than a few seconds—are the most energetic events in the Universe and occur at cosmological distances. The ECLAIRs micro-satellite, to be launched in 2009, will provide multi-wavelength observations of GRB, to study their astrophysics and to use them as cosmological probes. Furthermore, in 2009 ECLAIRs is expected to be the only space-borne instrument capable of providing a GRB trigger in near real-time with sufficient localization accuracy for GRB follow-up observations with the powerful ground-based spectroscopic telescopes available by then. A “Phase A study” of the ECLAIRs project has recently been launched by the French Space Agency CNES, aiming at a detailed mission design and selection for flight in 2006. The ECLAIRs mission is based on a CNES micro-satellite of the “Myriade” family and dedicated ground-based optical telescopes. The satellite payload combines a 2 sr field-of-view coded aperture mask gamma-camera using 6400 CdTe pixels for GRB detection and localization with 10 arcmin precision in the 4 50 keV energy band, together with a soft X-ray camera for onboard position refinement to 1 arcmin. The ground-based optical robotic telescopes will detect the GRB prompt/early afterglow emission and localize the event to arcsec accuracy, for spectroscopic follow-up observations.

  18. Bilateral sacrospinous fixation without hysterectomy: 18-month follow-up

    PubMed Central

    Şentürk, Mehmet Baki; Güraslan, Hakan; Çakmak, Yusuf; Ekin, Murat

    2015-01-01

    Objective The aim of this study was to evaluate the results of bilateral sacrospinous fixation (SSF), which was performed with surgical mesh interposition and bilateral vaginal repair. Material and Methods Twenty-two patients underwent SSF between 2010 and 2012, and the results were evaluated retrospectively. The results at preoperative and postoperative 6th, 12th, and 18th months of the pelvic organ prolapse quantification system (POP-Q) and the Pelvic Organ Prolapse/Urinary Incontinence Sexual Questionnaire-12 (PISQ-12) were compared using Friedman and Wilcoxon Signed Ranks tests. Values of p<0.05 and <0.01 were considered statistically significant. Results According to the POP-Q, significant healing was observed on all vaginal vault points (p=0.001), and no prolapse was observed until the 18-month follow-up stage. There were also prominent patients who felt satisfactory with respect to their sexual life according to PISQ-12 (p=0.001). Conclusion This technique appears to provide an adequate clinical resolution, and it may be the primary surgical option for women with pelvic organ prolapse. PMID:26097393

  19. Short-Term Follow-Up of Narcotic Addicts

    ERIC Educational Resources Information Center

    Swartz, June; Jabara, Raymond

    1974-01-01

    A follow-up questionnaire was mailed to 144 narcotic addict veterans approximately six months after termination from treatment at a multimodality drug program. It was found that 75 percent continued to use drugs, and 38 percent became readdicted. (Author)

  20. [Diagnosis of urethral stenosis and follow-up after Urethroplasty].

    PubMed

    Cogorno Wasylkowski, L; Ríos González, E; Martínez-Piñeiro Lorenzo, L

    2016-09-01

    This article presents a review of the different tests used for the evaluation and follow-up of urethral strictures. Because there is no consensus on how to assess urethral pathology, we reviewed each of the next follow-up tests: questionnaires, uroflowmetry, ultrasound, urethroscopy, urethrogram, CT scan and MRI, outlining their benefits and limitations in the diagnosis and follow-up of urethral stricture. Urethrogram and urethroscopy are the most commonly used tests, as they are those that give us more information on the evaluation of stenosis and for surgery planning. Questionnaires and uroflowmetry play a key role in the follow-up of these patients. Ultrasonography has high sensitivity and specificity for evaluating the spongiofibrosis, however it is not done routinely. The CT/MRI is recommended in the evaluation of pelvic trauma associated with fractures. PMID:27617551

  1. Outpatient follow-up for critical limb ischemia.

    PubMed

    Watch, Libby

    2014-09-01

    Outpatient follow-Up for critical limb ischemia offers the clinician the opportunity to monitor the patient for risk factor modification and wound healing. Routine surveillance following intervention will improve long-term patency.

  2. Follow-up Studies and Teacher Education Program Content.

    ERIC Educational Resources Information Center

    Schwanke, Dean

    1980-01-01

    This annotated bibliography deals with problem areas cited most frequently by educators. A brief review of follow-up research reveals that teachers' most frequent complaints about inadequate preparation relate to classroom management and discipline. (JN)

  3. Women with abnormal screening mammography lost to follow-up

    PubMed Central

    Kuo, Chia-Sheng; Chen, Guan-Ru; Hung, Shou-Hung; Liu, Yi-Lien; Huang, Kuo-Chin; Cheng, Shao-Yi

    2016-01-01

    Abstract Breast cancer has the highest incidence among all cancers for women in Taiwan. The current screening policy in Taiwan suggested a biennial mammography for all women 40 to 69 years of age. A recommendation for additional testing is recommended for women with a BI-RADS result of 0 or 4; a request made via postal mail. Approximately 20% of high-risk patients do not receive additional follow-up. Therefore, we aimed to explore the causes of these patients being lost to follow-up, despite an abnormal mammogram. Two questionnaires were designed separately according to the conceptual framework of the Health Belief Model. Study participants, women who received a screening mammography at the National Taiwan University Hospital in 2011 with a BI-RAD of 0 or 4, were interviewed via telephone. The dependent variable was receipt of follow-up or not. The analyses were performed by using χ2 tests and logistic regression models. In total, 528 women were enrolled in the study: 51.2% in BI-RADS 0 group and 56.6% in BI-RADS 4, respectively. In the BI-RADS 0 group, those patients who received a follow-up examination cited the most likely causes to be physician suggestion, health implications, and concerns regarding breast cancer. Patients who did not receive a follow-up examination cited a lack of time and a perception of good personal health as primary reasons. In the BI-RADS 4 group, those patients who received a follow-up examination cited the physician's recommendation and a recognition of the importance of follow-up examinations. Patients who did not receive a follow-up examination cited having received follow-up at another hospital and a desire for a second opinion. In the BI-RADS 0 group, multivariate analysis showed that patients with higher scores in the “perceived benefits” domain were statistically more likely to receive a follow-up examination. There was no significant difference in perceived threats, perceived barriers, action cues, or self-efficacy between

  4. Evaluating an outreach service for paediatric burns follow up.

    PubMed

    Cubitt, Jonathan J; Chesney, Amy; Brown, Liz; Nguyen, Dai Q

    2015-09-01

    Complications following paediatric burns are well documented and care needs to be taken to ensure the appropriate follow up of these patients. Historically this has meant follow up into adulthood however this is often not necessary. The centralisation of burns services in the UK means that patients and their parents may have to travel significant distances to receive this follow up care. To optimise our burns service we have introduced a burns outreach service to enable the patients to be treated closer to home. The aim of this study is to investigate the impact of the introduction of the burns outreach service and within this environment define the optimum length of time needed to follow up these patients. A retrospective analysis was carried out of 100 consecutive paediatric burns patients who underwent surgical management of their burn. During the follow up period there were 43 complications in 32 patients (32%). These included adverse scarring (either hypertrophic or keloid), delayed healing (taking >1 month to heal) and contractures (utilising either splinting or surgical correction). Fifty-nine percent of these complications occurred within 6 months of injury and all occurred within 18 months. Size of burn was directly correlated to the risk of developing a complication. The outreach service reduced the distance the patient needs to travel for follow up by more than 50%. There was also a significant financial benefit for the service as the follow up clinics were on average 50% cheaper with burns outreach than burns physician. Burns outreach is a feasible service that not only benefits the patients but also is cheaper for the burns service. The optimum length of follow up for paediatric burns in 18 months, after which if there have not been any complications they can be discharged. PMID:26036205

  5. Evaluating an outreach service for paediatric burns follow up.

    PubMed

    Cubitt, Jonathan J; Chesney, Amy; Brown, Liz; Nguyen, Dai Q

    2015-09-01

    Complications following paediatric burns are well documented and care needs to be taken to ensure the appropriate follow up of these patients. Historically this has meant follow up into adulthood however this is often not necessary. The centralisation of burns services in the UK means that patients and their parents may have to travel significant distances to receive this follow up care. To optimise our burns service we have introduced a burns outreach service to enable the patients to be treated closer to home. The aim of this study is to investigate the impact of the introduction of the burns outreach service and within this environment define the optimum length of time needed to follow up these patients. A retrospective analysis was carried out of 100 consecutive paediatric burns patients who underwent surgical management of their burn. During the follow up period there were 43 complications in 32 patients (32%). These included adverse scarring (either hypertrophic or keloid), delayed healing (taking >1 month to heal) and contractures (utilising either splinting or surgical correction). Fifty-nine percent of these complications occurred within 6 months of injury and all occurred within 18 months. Size of burn was directly correlated to the risk of developing a complication. The outreach service reduced the distance the patient needs to travel for follow up by more than 50%. There was also a significant financial benefit for the service as the follow up clinics were on average 50% cheaper with burns outreach than burns physician. Burns outreach is a feasible service that not only benefits the patients but also is cheaper for the burns service. The optimum length of follow up for paediatric burns in 18 months, after which if there have not been any complications they can be discharged.

  6. GRB 030329: 3 years of radio afterglow monitoring.

    PubMed

    van der Horst, A J; Kamble, A; Wijers, R A M J; Resmi, L; Bhattacharya, D; Rol, E; Strom, R; Kouveliotou, C; Oosterloo, T; Ishwara-Chandra, C H

    2007-05-15

    Radio observations of gamma-ray burst (GRB) afterglows are essential for our understanding of the physics of relativistic blast waves, as they enable us to follow the evolution of GRB explosions much longer than the afterglows in any other wave band. We have performed a 3-year monitoring campaign of GRB 030329 with the Westerbork Synthesis Radio Telescopes and the Giant Metrewave Radio Telescope. Our observations, combined with observations at other wavelengths, have allowed us to determine the GRB blast wave physical parameters, such as the total burst energy and the ambient medium density, as well as to investigate the jet nature of the relativistic outflow. Further, by modelling the late-time radio light curve of GRB 030329, we predict that the Low-Frequency Array (30-240 MHz) will be able to observe afterglows of similar GRBs, and constrain the physics of the blast wave during its non-relativistic phase.

  7. GRB 030329: 3 years of radio afterglow monitoring.

    PubMed

    van der Horst, A J; Kamble, A; Wijers, R A M J; Resmi, L; Bhattacharya, D; Rol, E; Strom, R; Kouveliotou, C; Oosterloo, T; Ishwara-Chandra, C H

    2007-05-15

    Radio observations of gamma-ray burst (GRB) afterglows are essential for our understanding of the physics of relativistic blast waves, as they enable us to follow the evolution of GRB explosions much longer than the afterglows in any other wave band. We have performed a 3-year monitoring campaign of GRB 030329 with the Westerbork Synthesis Radio Telescopes and the Giant Metrewave Radio Telescope. Our observations, combined with observations at other wavelengths, have allowed us to determine the GRB blast wave physical parameters, such as the total burst energy and the ambient medium density, as well as to investigate the jet nature of the relativistic outflow. Further, by modelling the late-time radio light curve of GRB 030329, we predict that the Low-Frequency Array (30-240 MHz) will be able to observe afterglows of similar GRBs, and constrain the physics of the blast wave during its non-relativistic phase. PMID:17293318

  8. Long-term follow-up of pediatric trachyonychia.

    PubMed

    Kumar, Monique G; Ciliberto, Heather; Bayliss, Susan J

    2015-01-01

    Pediatric trachyonychia is an acquired nail disease that can cause distress to families. It is a poorly understood disease, and long-term follow-up data are lacking. We present an institutional review of 11 children with isolated pediatric trachyonychia followed over time. Children with the diagnosis of pediatric trachyonychia were identified and invited to participate. Pictures were taken on follow-up and a questionnaire was answered. Exclusion criteria include having another diagnosis at the initial visit that causes nail dystrophy. Eleven patients with the diagnosis of pediatric trachyonychia were available for follow-up. The mean age of appearance was 2.7 years (range 2-7 yrs) and the average follow-up was 66 months (range 10-126 mos). Nine patients were treated with potent topical corticosteroids, one used only petrolatum, and one took vitamin supplements. One patient was found to have an additional skin and hair diagnosis of alopecia areata on follow-up. On follow-up, 82% noted improvement of the nails, whereas 18% noted no change. A majority of cases of pediatric trachyonychia are isolated and improve with time, regardless of treatment.

  9. Diagnosis, treatment and follow up of neonatal arrhythmias

    PubMed Central

    Binnetoğlu, Fatih Köksal; Babaoğlu, Kadir; Altun, Gürkan; Türker, Gülcan

    2014-01-01

    Summary Objective This study aimed to evaluate the aetiology, spectrum, course and outcomes of neonates with arrhythmias observed in a tertiary neonatal intensive care unit from 2007 to 2012. Methods Neonates with rhythm problems were included. The results of electrocardiography (ECG), Holter ECG, echocardiography and biochemical analysis were evaluated. The long-term results of follow up were reviewed. Results Forty-five patients were male (68%) and 21 (32%) were female. Fifty-five patients (83.3%) were term, 11 (16.6%) were preterm, and 34% were diagnosed in the prenatal period. Twenty cases (30.3%) had congenital heart disease. Twenty-three patients (34.8%) were diagnosed during the foetal period. The most common arrhythmias were supraventricular ectopic beats and supraventricular tachycardia (SVT) at 39.3 and 22.7%, respectively. SVT recurred in five patients after the neonatal period. Conclusion Supraventricular ectopic beats and SVT were the most common arrhythmias during the neonatal period. Although the prognosis of arrhythmias in the neonatal period is relatively good, regular monitoring is required. PMID:24844549

  10. Myxedema madness complicating postoperative follow-up of thyroid cancer.

    PubMed

    Morosán Allo, Yanina J; Rosmarin, Melanie; Urrutia, Agustina; Faingold, Maria Cristina; Musso, Carla; Brenta, Gabriela

    2015-08-01

    Although hypothyroidism is associated with an increased prevalence of psychiatric manifestations, myxedema madness is rarely observed. We report the case of a 62-year-old woman with no prior history of psychiatric disorders, who presented to the emergency department with psychomotor agitation 6 weeks after total thyroidectomy for papillary thyroid cancer. Serum thyroid stimulating hormone (TSH) on admission was 62.9 mIU/L and free T4 was < 0.35 ng/dL, indicating severe hypothyroidism. After ruling out other possible causes, the diagnosis of myxedema madness was considered; hence, antipsychotic drug treatment and intravenous levothyroxine were prescribed. Behavioral symptoms returned to normal within 4 days of presentation, while levels of thyroid hormones attained normal values 1 week after admission. Recombinant TSH (Thyrogen®) was used successfully to prevent new episodes of mania due to thyroid hormone withdrawal in further controls for her thyroid cancer. This case illustrates that myxedema madness can occur in the setting of acute hypothyroidism, completely reverting with levothyroxine and antipsychotic treatment. Recombinant TSH may be a useful tool to prevent myxedema madness or any severe manifestation of levothyroxine withdrawal for the follow-up of thyroid cancer. PMID:26331326

  11. Follow-up skeletal survey use by child abuse pediatricians.

    PubMed

    Harper, Nancy S; Lewis, Terri; Eddleman, Sonja; Lindberg, Daniel M

    2016-01-01

    Skeletal survey is frequently used to identify occult fractures in young children with concern for physical abuse. Because skeletal survey is relatively insensitive for some abusive fractures, a follow-up skeletal survey (FUSS) may be undertaken at least 10-14 days after the initial skeletal survey to improve sensitivity for healing fractures. This was a prospectively planned secondary analysis of a prospective, observational study of 2,890 children who underwent subspecialty evaluation for suspected child physical abuse at 1 of 19 centers. Our objective was to determine variability between sites in rates of FUSS recommendation, completion and fracture identification among the 2,049 participants who had an initial SS. Among children with an initial skeletal survey, the rate of FUSS recommendation for sites ranged from 20% to 97%; the rate of FUSS completion ranged from 10% to 100%. Among sites completing at least 10 FUSS, rates of new fracture identification ranged from 8% to 28%. Among completed FUSS, new fractures were more likely to be identified in younger children, children with higher initial level of concern for abuse, and those with a fracture or cutaneous injury identified in the initial evaluation. The current variability in FUSS utilization is not explained by variability in occult fracture prevalence. Specific guidelines for FUSS utilization are needed.

  12. Myxedema madness complicating postoperative follow-up of thyroid cancer.

    PubMed

    Morosán Allo, Yanina J; Rosmarin, Melanie; Urrutia, Agustina; Faingold, Maria Cristina; Musso, Carla; Brenta, Gabriela

    2015-08-01

    Although hypothyroidism is associated with an increased prevalence of psychiatric manifestations, myxedema madness is rarely observed. We report the case of a 62-year-old woman with no prior history of psychiatric disorders, who presented to the emergency department with psychomotor agitation 6 weeks after total thyroidectomy for papillary thyroid cancer. Serum thyroid stimulating hormone (TSH) on admission was 62.9 mIU/L and free T4 was < 0.35 ng/dL, indicating severe hypothyroidism. After ruling out other possible causes, the diagnosis of myxedema madness was considered; hence, antipsychotic drug treatment and intravenous levothyroxine were prescribed. Behavioral symptoms returned to normal within 4 days of presentation, while levels of thyroid hormones attained normal values 1 week after admission. Recombinant TSH (Thyrogen®) was used successfully to prevent new episodes of mania due to thyroid hormone withdrawal in further controls for her thyroid cancer. This case illustrates that myxedema madness can occur in the setting of acute hypothyroidism, completely reverting with levothyroxine and antipsychotic treatment. Recombinant TSH may be a useful tool to prevent myxedema madness or any severe manifestation of levothyroxine withdrawal for the follow-up of thyroid cancer.

  13. Asbestos and cancer: a cohort followed up to death.

    PubMed Central

    Enterline, P E; Hartley, J; Henderson, V

    1987-01-01

    The mortality experience of 1074 white men who retired from a United States asbestos company during the period 1941-67 and who were exposed to asbestos working as production and maintenance employees for the company is reported to the end of 1980 when 88% of this cohort was known to be dead. As noted in earlier reports the mortality for respiratory and gastrointestinal cancer was raised. A more detailed examination of causes of death shows that the excess in gastrointestinal cancer was largely due to a statistically significant excess in stomach cancer. A statistically significant excess was also noted for kidney cancer, cancer of the eye, and non-malignant respiratory disease. Eight deaths from malignant mesothelioma were observed, two of which were peritoneal. Asbestos exposures for these mesothelioma cases were low relative to other members of the cohort. Continuing follow up of this cohort shows a dose response relation for respiratory cancer that has become increasingly linear. Standardised mortality ratios peaked 10 to 15 years after retirement and were relatively constant at around 250 in each five year interval starting in 1950. This excess might have been detected as early as 1960 but certainly by 1965. The mortality experience of this cohort reflects the ultimate effects of asbestos since nearly all of the cohort has now died. PMID:3606968

  14. Familial cardiomyopathy--a 15-year follow-up.

    PubMed

    Rosenqvist, M; Biörck, G; de Faire, U; Freyschuss, U; Lindvall, K; Magnusson, B

    1980-01-01

    In 1961--1962 five families including 53 members with a familial form of cardiomyopathy (CMP) were examined. Fifteen years later a reinvestigation of the previously examined families was carried out using community registers; mortality as well as new family members were registered. Another 50 family members were thereby added. Three out of 6 young subjects who were diagnosed as having definite (2) or suspected (1) CMP at the initial examination died during the follow-up period. Four of the five families, totalling 39/41 members, were given a thorough noninvasive clinical examination including ECG, phonocardiogram exercise test, measurement of systolic time intervals and carotid arterial pulse curves, and echocardiography (Echo). A high number (17/39) of suspected or definite pathologic echocardiographic changes consistent with CMP was observed on reinvestigation. Eleven of these 17 were asymptomatic. Except for Echo, the non-invasive methods used in this study did not contribute to the diagnosis of CMP, but the non-Echo methods confirmed the Echo findings in those patients with symptoms of cardiac disease. The four reexamined families revealed a very heterogenous pattern of CMP, with both symmetric and asymmetric hypertrophy (ratio symmetric/asymmetric = 15 : 2). It may be questioned whether asymptomatic subjects with borderline changes, indicative of symmetric hypertrophy, will develop definite symmetric CMP or whether their symptoms constitute an early stage of asymmetric CMP. Echocardiographic findings may well fit with the theory of a dominant mode of inheritance.

  15. Follow up study of workers manufacturing chrysotile asbestos cement products.

    PubMed Central

    Gardner, M J; Winter, P D; Pannett, B; Powell, C A

    1986-01-01

    A cohort study has been carried out of 2167 subjects employed between 1941 and 1983 at an asbestos cement factory in England. The production process incorporated the use of chrysotile asbestos fibre only, except for a small amount of amosite during four months in 1976. Measured airborne fibre concentrations available since 1970 from personal samplers showed mean levels below 1 fibre/ml, although higher levels had probably occurred previously in certain areas of the factory. No excess of lung cancer was observed in the mortality follow up by comparison with either national or local death rates, and analyses of subgroups of the workforce by job, exposure level, duration of employment, duration since entry, or calendar years of employment gave no real suggestion of an asbestos related excess for this cause of death. There was one death from pleural mesothelioma and one with asbestosis mentioned as an associated cause on the death certificate, but neither is thought to be linked to asbestos exposure at this factory. Other suggested asbestos related cancers, such as laryngeal and gastrointestinal, did not show raised risks. Although the durations of exposure were short in this study, the findings are consistent with two other studies of workers exposed to low concentrations of chrysotile fibre in the manufacture of asbestos cement products which reported no excess mortality. PMID:3024695

  16. Surveys, Astrometric Follow-Up, and Population Statistics

    NASA Astrophysics Data System (ADS)

    Jedicke, R.; Granvik, M.; Micheli, M.; Ryan, E.; Spahr, T.; Yeomans, D. K.

    Asteroid surveys are the backbone of asteroid science, and with this in mind we begin with a broad review of the impact of asteroid surveys on our field. We then provide a brief history of asteroid discoveries so as to place contemporary and future surveys in perspective. Surveys in the United States (U.S.) have discovered the vast majority of the asteroids, and this dominance has been consolidated since the publication of Asteroids III. Our descriptions of the asteroid surveys that have been operational since that time are focused on those that have contributed the vast majority of asteroid observations and discoveries. We also provide some insight into upcoming next-generation surveys that are sure to alter our understanding of the small bodies in the inner solar system and provide evidence to untangle their complicated dynamical and physical histories. The Minor Planet Center, the nerve center of the asteroid discovery effort, has improved its operations significantly in the past decade so that it can manage the increasing discovery rate, and ensure that it is well-placed to handle the data rates expected in the next decade. We also consider the difficulties associated with astrometric follow-up of newly identified objects. It seems clear that both of these efforts must operate in new modes in order to keep pace with expected discovery rates of next-generation ground- and spacebased surveys.

  17. Searching for soft relativistic jets in core-collapse supernovae with the IceCube optical follow-up program

    NASA Astrophysics Data System (ADS)

    Abbasi, R.; Abdou, Y.; Abu-Zayyad, T.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Allen, M. M.; Altmann, D.; Andeen, K.; Auffenberg, J.; Bai, X.; Baker, M.; Barwick, S. W.; Bay, R.; Bazo Alba, J. L.; Beattie, K.; Beatty, J. J.; Bechet, S.; Becker, J. K.; Becker, K.-H.; Benabderrahmane, M. L.; Benzvi, S.; Berdermann, J.; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand, D.; Besson, D. Z.; Bindig, D.; Bissok, M.; Blaufuss, E.; Blumenthal, J.; Boersma, D. J.; Bohm, C.; Bose, D.; Böser, S.; Botner, O.; Brown, A. M.; Buitink, S.; Caballero-Mora, K. S.; Carson, M.; Chirkin, D.; Christy, B.; Clevermann, F.; Cohen, S.; Colnard, C.; Cowen, D. F.; Cruz Silva, A. H.; D'Agostino, M. V.; Danninger, M.; Daughhetee, J.; Davis, J. C.; de Clercq, C.; Degner, T.; Demirörs, L.; Descamps, F.; Desiati, P.; de Vries-Uiterweerd, G.; Deyoung, T.; Díaz-Vélez, J. C.; Dierckxsens, M.; Dreyer, J.; Dumm, J. P.; Dunkman, M.; Eisch, J.; Ellsworth, R. W.; Engdegård, O.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Fedynitch, A.; Feintzeig, J.; Feusels, T.; Filimonov, K.; Finley, C.; Fischer-Wasels, T.; Fox, B. D.; Franckowiak, A.; Franke, R.; Gaisser, T. K.; Gallagher, J.; Gerhardt, L.; Gladstone, L.; Glüsenkamp, T.; Goldschmidt, A.; Goodman, J. A.; Góra, D.; Grant, D.; Griesel, T.; Groß, A.; Grullon, S.; Gurtner, M.; Ha, C.; Haj Ismail, A.; Hallgren, A.; Halzen, F.; Han, K.; Hanson, K.; Heinen, D.; Helbing, K.; Hellauer, R.; Herquet, P.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Hoffmann, B.; Homeier, A.; Hoshina, K.; Huelsnitz, W.; Hülß, J.-P.; Hulth, P. O.; Hultqvist, K.; Hussain, S.; Ishihara, A.; Jacobi, E.; Jacobsen, J.; Japaridze, G. S.; Johansson, H.; Kampert, K.-H.; Kappes, A.; Karg, T.; Karle, A.; Kenny, P.; Kiryluk, J.; Kislat, F.; Klein, S. R.; Köhne, J.-H.; Kohnen, G.; Kolanoski, H.; Köpke, L.; Kopper, S.; Koskinen, D. J.; Kowalski, M.; Kowarik, T.; Krasberg, M.; Kroll, G.; Kurahashi, N.; Kuwabara, T.; Labare, M.; Laihem, K.; Landsman, H.; Larson, M. J.; Lauer, R.; Lünemann, J.; Madsen, J.; Marotta, A.; Maruyama, R.; Mase, K.; Matis, H. S.; Meagher, K.; Merck, M.; Mészáros, P.; Meures, T.; Miarecki, S.; Middell, E.; Milke, N.; Miller, J.; Montaruli, T.; Morse, R.; Movit, S. M.; Nahnhauer, R.; Nam, J. W.; Naumann, U.; Nygren, D. R.; Odrowski, S.; Olivas, A.; Olivo, M.; O'Murchadha, A.; Panknin, S.; Paul, L.; Pérez de Los Heros, C.; Petrovic, J.; Piegsa, A.; Pieloth, D.; Porrata, R.; Posselt, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.; Redl, P.; Resconi, E.; Rhode, W.; Ribordy, M.; Richman, M.; Rodrigues, J. P.; Rothmaier, F.; Rott, C.; Ruhe, T.; Rutledge, D.; Ruzybayev, B.; Ryckbosch, D.; Sander, H.-G.; Santander, M.; Sarkar, S.; Schatto, K.; Schmidt, T.; Schönwald, A.; Schukraft, A.; Schultes, A.; Schulz, O.; Schunck, M.; Seckel, D.; Semburg, B.; Seo, S. H.; Sestayo, Y.; Seunarine, S.; Silvestri, A.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Stezelberger, T.; Stokstad, R. G.; Stössl, A.; Strahler, E. A.; Ström, R.; Stüer, M.; Sullivan, G. W.; Swillens, Q.; Taavola, H.; Taboada, I.; Tamburro, A.; Ter-Antonyan, S.; Tilav, S.; Toale, P. A.; Toscano, S.; Tosi, D.; van Eijndhoven, N.; Vandenbroucke, J.; van Overloop, A.; van Santen, J.; Vehring, M.; Voge, M.; Walck, C.; Waldenmaier, T.; Wallraff, M.; Walter, M.; Weaver, Ch.; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Williams, D. R.; Wischnewski, R.; Wissing, H.; Wolf, M.; Wood, T. R.; Woschnagg, K.; Xu, C.; Xu, D. L.; Xu, X. W.; Yanez, J. P.; Yodh, G.; Yoshida, S.; Zarzhitsky, P.; Zoll, M.; IceCube Collaboration; Akerlof, C. W.; Pandey, S. B.; Yuan, F.; Zheng, W.; ROTSE Collaboration

    2012-03-01

    Context. Transient neutrino sources such as gamma-ray bursts (GRBs) and supernovae (SNe) are hypothesized to emit bursts of high-energy neutrinos on a time-scale of ≲100 s. While GRB neutrinos would be produced in high relativistic jets, core-collapse SNe might host soft-relativistic jets, which become stalled in the outer layers of the progenitor star leading to an efficient production of high-energy neutrinos. Aims: To increase the sensitivity to these neutrinos and identify their sources, a low-threshold optical follow-up program for neutrino multiplets detected with the IceCube observatory has been implemented. Methods: If a neutrino multiplet, i.e. two or more neutrinos from the same direction within 100 s, is found by IceCube a trigger is sent to the Robotic Optical Transient Search Experiment, ROTSE. The 4 ROTSE telescopes immediately start an observation program of the corresponding region of the sky in order to detect an optical counterpart to the neutrino events. Results: No statistically significant excess in the rate of neutrino multiplets has been observed and furthermore no coincidence with an optical counterpart was found. Conclusions: The search allows, for the first time, to set stringent limits on current models predicting a high-energy neutrino flux from soft relativistic hadronic jets in core-collapse SNe. We conclude that a sub-population of SNe with typical Lorentz boost factor and jet energy of 10 and 3 × 1051 erg, respectively, does not exceed 4.2% at 90% confidence.

  18. Searching for Soft Relativistic Jets in Core-Collapse Supernovae with the IceCube Optical Follow-up Program

    NASA Technical Reports Server (NTRS)

    Abbasi, R.; Abdou, Y.; Abu-Zayyad, T.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Allen, M. M.; Altmann, D.; Andeen, K.; Auffenberg, J.; Bai, X.; Baker, M.; Barwick, S. W.; Bay, R.; Bazo Alba, J. L.; Beattie, K.; Beatty, J. J.; Bechet, S.; Becker, J. K.; Becker, K. -H.; Benabderrahmane, M. L.; BenZvi, S.; Berdermann, J.; Stamatikos, M.

    2011-01-01

    Context. Transient neutrino sources such as Gamma-Ray Bursts (GRBs) and Supernovae (SNe) are hypothesized to emit bursts of high-energy neutrinos on a time-scale of < or approx.100 s. While GRB neutrinos would be produced in high relativistic jets, core-collapse SNe might host soft-relativistic jets, which become stalled in the outer layers of the progenitor star leading to an efficient production of high-energy neutrinos. Aims. To increase the sensitivity to these neutrinos and identify their sources, a low-threshold optical follow-up program for neutrino multiplets detected with the IceCube observatory has been implemented. Methods. If a neutrino multiplet, i.e. two or more neutrinos from the same direction within 100 s, is found by IceCube a trigger is sent to the Robotic Optical Transient Search Experiment, ROTSE. The 4 ROTSE telescopes immediately start an observation program of the corresponding region of the sky in order to detect an optical counterpart to the neutrino events. Results. No statistically significant excess in the rate of neutrino multiplets has been observed and furthermore no coincidence with an optical counterpart was found. Conclusions. The search allows, for the first time, to set stringent limits on current models predicting a high-energy neutrino flux from soft relativistic hadronic jets in core-collapse SNe. We conclude that a sub-population of SNe with typical Lorentz boost factor and jet energy of 10 and 3 x 10(exp 51) erg, respectively, does not exceed 4:2% at 90% confidence.

  19. Searching for High-energy Neutrinos from Supernovae with IceCube and an Optical Follow-up Program

    NASA Astrophysics Data System (ADS)

    Franckowiak, Anna

    2011-08-01

    In violent astrophysical processes high-energy neutrinos of TeV to PeV energies are expected to be produced along with the highest energy cosmic rays. The acceleration of nuclei to very high energies is assumed to takes place in astrophysical shocks and neutrinos are produced in the interaction of these cosmic rays with ambient baryons or photons. The neutrinos then escape the acceleration region and propagate through space without interaction, while the nuclei are deflected in magnetic fields and no longer carry information about their source position. Unlike gamma-rays, neutrinos are solely produced in hadronic processes and can therefore reveal the sources of charged cosmic rays. The IceCube neutrino detector, which is located at the geographical South Pole, has been build to detect these high-energy astrophysical neutrinos. The deep clear Antarctic ice is instrumented with light sensors on a grid, thus forming a Cherenkov particle detector, which is capable of detecting charged particles induced by neutrinos above 100 GeV. Transient neutrino sources such as Gamma-Ray Bursts (GRBs) and Supernovae (SNe) are hypothesized to emit bursts of high-energy neutrinos on a time-scale of = 100 s. While GRB neutrinos would be produced in the high relativistic jets driven by the central engine, corecollapse SNe might host soft-relativistic jets which become stalled in the outer layers of the progenitor star and lead to an efficient production of high-energy neutrinos. This work aims for an increased sensitivity for these neutrinos and for a possible identification of their sources. Towards this goal, a low-threshold optical follow-up program for neutrino multiplets detected with IceCube has been implemented. If a neutrino multiplet - i.e. two or more neutrinos from the same direction within 100 s - is found by IceCube a trigger is sent to the Robotic Optical Transient Search Experiment (ROTSE). The 4 ROTSE telescopes immediately start an observation program of the

  20. DISCOVERY AND REDSHIFT OF AN OPTICAL AFTERGLOW IN 71 deg{sup 2}: iPTF13bxl AND GRB 130702A

    SciTech Connect

    Singer, Leo P.; Brown, Duncan A.; Bradley Cenko, S.; Gehrels, Neil; McEnery, Julie; Kasliwal, Mansi M.; Mulchaey, John; Perley, Daniel A.; Kulkarni, S. R.; Bellm, Eric; Barlow, Tom; Cao, Yi; Horesh, Assaf; Ofek, Eran O.; Arcavi, Iair; Nugent, Peter E.; Bloom, Joshua S.; Corsi, Alessandra; Frail, Dale A.; Masci, Frank J.; and others

    2013-10-20

    We report the discovery of the optical afterglow of the γ-ray burst (GRB) 130702A, identified upon searching 71 deg{sup 2} surrounding the Fermi Gamma-ray Burst Monitor (GBM) localization. Discovered and characterized by the intermediate Palomar Transient Factory, iPTF13bxl is the first afterglow discovered solely based on a GBM localization. Real-time image subtraction, machine learning, human vetting, and rapid response multi-wavelength follow-up enabled us to quickly narrow a list of 27,004 optical transient candidates to a single afterglow-like source. Detection of a new, fading X-ray source by Swift and a radio counterpart by CARMA and the Very Large Array confirmed the association between iPTF13bxl and GRB 130702A. Spectroscopy with the Magellan and Palomar 200 inch telescopes showed the afterglow to be at a redshift of z = 0.145, placing GRB 130702A among the lowest redshift GRBs detected to date. The prompt γ-ray energy release and afterglow luminosity are intermediate between typical cosmological GRBs and nearby sub-luminous events such as GRB 980425 and GRB 060218. The bright afterglow and emerging supernova offer an opportunity for extensive panchromatic follow-up. Our discovery of iPTF13bxl demonstrates the first observational proof-of-principle for ∼10 Fermi-iPTF localizations annually. Furthermore, it represents an important step toward overcoming the challenges inherent in uncovering faint optical counterparts to comparably localized gravitational wave events in the Advanced LIGO and Virgo era.

  1. [Ambulatory control and follow-up of patients carrying a unicameral pacemaker].

    PubMed

    de Juan Montiel, J; Bardají, A; Vaño, J; Toda, R; Beret, T; Ridao, C

    1990-01-01

    The follow-up schedule after pacemaker implantation should be arranged to allow close monitoring during the immediate post-implant period, and frequent observations during the life of the system. Such follow-up has as major goals the evaluation of the electrical functions of the pacing system to detect malfunctions or imminent power source depletion and the evaluation of the patient cardiac status so that reprogramming can be accomplished. PMID:2236796

  2. Effect of Health Literacy on Research Follow-up

    PubMed Central

    Leak, Cardella; Goggins, Kathryn; Schildcrout, Jonathan S.; Theobald, Cecelia; Donato, Katharine M.; Bell, Susan P.; Schnelle, John; Kripalani, Sunil

    2016-01-01

    Previous research has not examined the effect of health literacy on research subjects' completion of scheduled research follow-up. This article evaluates patient factors associated with incomplete research follow-up at three time points after enrollment in a large, hospital-based prospective cohort study. Predictor variables included health literacy, age, race, gender, education, employment status, difficulty paying bills, hospital diagnosis, length of stay, self-reported global health status, depression, perceived health competence, medication adherence and healthcare system distrust. In a sample of 2042 patients, multivariable models demonstrated that lower health literacy and younger age were significantly associated with a lower likelihood of completing research follow-up interviews at 2-3 days, 30 days and 90 days after hospital discharge. Additionally, patients who had less education, were currently employed, and had moderate financial stress were less likely to complete 90-day follow-up. This study is the first to demonstrate that lower health literacy is a significant predictor of incomplete research follow-up. PMID:26513035

  3. [Telemedicine in pacemaker therapy and follow-up].

    PubMed

    Schuchert, A

    2009-12-01

    Present-day remote systems for cardiovascular implantable electronic devices (CIEDs) provide, in contrast to previous solutions, a broad range of data about the patient and the implanted device ("remote control"). Telemedicine includes remote monitoring as well as remote follow-up: Remote monitoring is the continual interrogation of the device to detect patient- or device-related adverse events earlier than with standard follow-up visits. Remote follow-up aims to replace scheduled and unscheduled face-to-face follow-up visits due to the interrogation of the automatic pacemaker functions. Currently available remote systems, such as Home Monitoring, CareLink, Merlin.net, and Latitude, have in common that they interrogate the device, send these data to a server, and provide the data to the physician on a secured web site. Automatic wireless interrogation of the device is the preferred solution; however, the devices must have been equipped with a micro-antenna, which is usually restricted to more recent pacemaker models. Knowledge about remote control in pacemaker patients is limited, because most remote applications were evaluated in ICD and CRT patients. While the most frequently reported clinical event in pacemaker patients is atrial fibrillation, the impact in routine clinical follow-up still has to be evaluated in detail. Device-related adverse events are rare. Large, long-term, randomized trials are comparing remote and conventional approaches with the aim of demonstrating the benefits of telemedicine in this patient group.

  4. Cohort follow-up: the 21st century procedures.

    PubMed

    Bahr, Debra E; Hughes, Therese; Aldrich, Timothy E; Silver, Kenneth Z; Brion, Gall M

    2009-01-01

    The basic logic of designing an occupational cohort study has changed little since William R. Gaffey outlined the issues of follow-up, measurement of exposure, and analysis of data. However, many new avenues of tracking workers for epidemiological studies have been developed since Gaffey wrote his paper in 1973. Many disease registries also perform follow-up of subjects for vital status determination, so the procedures used with this process are common to the two applications. This article speaks to cohort construction for this occupational research as well as describes the 2007 methods for vital status follow-up. Rises in concern about work-related disease risks and the scientific resources for performing these studies coincided with the computer revolution. Government and private sources of data on vital status have changed in several ways over the 35 years since Gaffey's seminal paper. Some systems make the process of follow-up more rapid and productive, and some barriers have been imposed as societal concerns for privacy have risen. We describe the process of linking 5 sources of data to compile a roster of 6,820 workers employed at the Paducah Gaseous Diffusion Plant from 1953 to 2003. The record linkage processes achieved a final death cohort of 1672 deaths--the ascertainment of these deaths (by time period) was 1379 (1979-2003) and 293 (1953-1978); follow-up then was 100% for this cohort.

  5. Molecular hydrogen in the damped Lyman α system towards GRB 120815A at z = 2.36

    NASA Astrophysics Data System (ADS)

    Krühler, T.; Ledoux, C.; Fynbo, J. P. U.; Vreeswijk, P. M.; Schmidl, S.; Malesani, D.; Christensen, L.; De Cia, A.; Hjorth, J.; Jakobsson, P.; Kann, D. A.; Kaper, L.; Vergani, S. D.; Afonso, P. M. J.; Covino, S.; de Ugarte Postigo, A.; D'Elia, V.; Filgas, R.; Goldoni, P.; Greiner, J.; Hartoog, O. E.; Milvang-Jensen, B.; Nardini, M.; Piranomonte, S.; Rossi, A.; Sánchez-Ramírez, R.; Schady, P.; Schulze, S.; Sudilovsky, V.; Tanvir, N. R.; Tagliaferri, G.; Watson, D. J.; Wiersema, K.; Wijers, R. A. M. J.; Xu, D.

    2013-09-01

    We present the discovery of molecular hydrogen (H2), including the presence of vibrationally-excited H2* in the optical spectrum of the afterglow of GRB 120815A at z = 2.36 obtained with X-shooter at the VLT. Simultaneous photometric broad-band data from GROND and X-ray observations by Swift/XRT place further constraints on the amount and nature of dust along the sightline. The galactic environment of GRB 120815A is characterized by a strong DLA with log(N(H i)/cm-2) = 21.95 ± 0.10, prominent H2 absorption in the Lyman-Werner bands (log (N(H2)/cm-2) = 20.54 ± 0.13) and thus a molecular gas fraction log f(H2) = -1.14 ± 0.15. The distance d between the absorbing neutral gas and GRB 120815A is constrained via photo-excitation modeling of fine-structure and meta-stable transitions of Fe ii and Ni ii to d = 0.5 ± 0.1 kpc. The DLA metallicity ([Zn/H] = -1.15 ± 0.12), visual extinction (AV ≲ 0.15 mag) and dust depletion ([Zn/Fe] = 1.01 ± 0.10) are intermediate between the values of well-studied, H2-deficient GRB-DLAs observed at high spectral resolution, and the approximately solar metallicity, highly-obscured and H2-rich GRB 080607 sightline. With respect to N(H i), metallicity, as well as dust-extinction and depletion, GRB 120815A is fairly representative of the average properties of GRB-DLAs. This demonstrates that molecular hydrogen is present in at least a fraction of the more typical GRB-DLAs, and H2 and H2* are probably more wide-spread among GRB-selected systems than the few examples of previous detections would suggest. Because H2* transitions are located redwards of the Lyman α absorption, H2* opens a second route for positive searches for molecular absorption also in GRB afterglows at lower redshifts and observed at lower spectral resolution. Further detections of molecular gas in GRB-DLAs would allow statistical studies, and, coupled with host follow-up and sub-mm spectroscopy, provide unprecedented insights into the process and conditions of star

  6. Search for VHE emission from GRB with Milagro

    SciTech Connect

    Saz Parkinson, P.M.

    2005-02-21

    The Milagro gamma-ray observatory employs a water Cherenkov detector to observe extensive air showers produced by high-energy particles impacting in the Earth's atmosphere. Milagro is uniquely capable of searching for very high-energy emission from gamma-ray bursts (GRB) during the prompt emission phase because of its wide field of view and high duty cycle, monitoring the northern sky almost continuously in the 100 GeV to 100 TeV energy range. 33 satellite-triggered GRB have occurred within the field of view of Milagro between January 2000 and December 2003. We have searched for counterparts to these GRB and found no significant emission from any of these burst positions. In the case of GRB 010921, the redshift is low enough (0.45) that our upper limit on the fluence places an observational constraint on potential GRB models.

  7. Posttreatment Follow-Up of Brucellosis by PCR Assay

    PubMed Central

    Morata, Pilar; Queipo-Ortuño, María Isabel; Reguera, José María; García-Ordoñez, Miguel Angel; Pichardo, Cristina; Colmenero, Juan de Dios

    1999-01-01

    In order to evaluate the usefulness of a peripheral blood PCR assay in the posttreatment follow-up of brucellosis, a cohort of 30 patients was studied by means of blood cultures, rose Bengal, seroagglutination, Coombs' antibrucella tests, and PCR assay at the time of diagnosis, at the end of treatment, and 2, 4, and 6 months later. Of the 29 patients whose PCR assays were initially positive, 28 (96.5%) were negative at the conclusion of the treatment. PCR was positive for the two patients who had relapses and negative for another four who had suspected but unconfirmed relapses. PCR was negative for 98.3% of the follow-up samples from those patients who had a favorable evolution. In conclusion, PCR appears to be a very useful technique, not only for the initial diagnosis of the disease, but also for posttreatment follow-up and the early detection of relapses. PMID:10565954

  8. Suicide Prevention and Follow-Up Services: A Narrative Review

    PubMed Central

    Ghanbari, Behrooz; Malakouti, Seyed Kazem; Nojomi, Marzieh; Alavi, Kaveh; Khaleghparast, Shiva

    2016-01-01

    Previous suicide attempt is the most important predictor of death by suicide. Thus preventive interventions after attempting to suicide is essential to prevent reattempts. This paper attempts to determine whether phone preventive interventions or other vehicles (postal cards, email and case management) are effective in reattempt prevention and health promotion after discharge by providing an overview of studies on suicide reattempts. The research investigated in this review conducted from 1995 to 2014. A total of 26 cases related to the aim of this research were derived from 36 English articles with the aforementioned keywords Research shows that providing comprehensive aids, social support, and follow-up after discharge can significantly prevent suicide reattempts. Several studies showed that follow-up support (phone calls, crisis cards, mails, postal cards.) after discharge can significantly decrease the risk of suicide. More randomized controlled trials (RCT) are required to determine what factors of follow-up are more effective than other methods. PMID:26652085

  9. Tracking and follow-up of marginalized populations: a review.

    PubMed

    McKenzie, M; Tulsky, J P; Long, H L; Chesney, M; Moss, A

    1999-11-01

    Maintaining study cohorts is a key element of longitudinal research. Participant attrition introduces the possibility of bias and limits the generalizability of a study's findings, but with appropriate planning it is possible to sustain contact with even the most transient participants. This paper reviews the essential elements of tracking and follow-up of marginalized populations, which are (1) collection of contact information, (2) thorough organization of tracking efforts, (3) attention to staff training and support, (4) use of phone and mail follow-up, (5) use of incentives, (6) establishing rapport with participants, (7) assurance of confidentiality, (8) use of agency tracking, (9) use of field tracking, and (10) attention to safety concerns. Diligent application of these tracking strategies allows researchers to achieve follow-up rates of 75 percent to 97 percent with vulnerable populations such as homeless, mentally ill adults, injection drug users, and runaway youth.

  10. Suicide Prevention and Follow-Up Services: A Narrative Review.

    PubMed

    Ghanbari, Behrooz; Malakouti, Seyed Kazem; Nojomi, Marzieh; Alavi, Kaveh; Khaleghparast, Shiva

    2015-09-28

    Previous suicide attempt is the most important predictor of death by suicide. Thus preventive interventions after attempting to suicide is essential to prevent reattempts. This paper attempts to determine whether phone preventive interventions or other vehicles (postal cards, email and case management) are effective in reattempt prevention and health promotion after discharge by providing an overview of studies on suicide reattempts. The research investigated in this review conducted from 1995 to 2014. A total of 26 cases related to the aim of this research were derived from 36 English articles with the aforementioned keywords Research shows that providing comprehensive aids, social support, and follow-up after discharge can significantly prevent suicide reattempts. Several studies showed that follow-up support (phone calls, crisis cards, mails, postal cards.) after discharge can significantly decrease the risk of suicide. More randomized controlled trials (RCT) are required to determine what factors of follow-up are more effective than other methods.

  11. Suicide Prevention and Follow-Up Services: A Narrative Review.

    PubMed

    Ghanbari, Behrooz; Malakouti, Seyed Kazem; Nojomi, Marzieh; Alavi, Kaveh; Khaleghparast, Shiva

    2016-01-01

    Previous suicide attempt is the most important predictor of death by suicide. Thus preventive interventions after attempting to suicide is essential to prevent reattempts. This paper attempts to determine whether phone preventive interventions or other vehicles (postal cards, email and case management) are effective in reattempt prevention and health promotion after discharge by providing an overview of studies on suicide reattempts. The research investigated in this review conducted from 1995 to 2014. A total of 26 cases related to the aim of this research were derived from 36 English articles with the aforementioned keywords Research shows that providing comprehensive aids, social support, and follow-up after discharge can significantly prevent suicide reattempts. Several studies showed that follow-up support (phone calls, crisis cards, mails, postal cards.) after discharge can significantly decrease the risk of suicide. More randomized controlled trials (RCT) are required to determine what factors of follow-up are more effective than other methods. PMID:26652085

  12. Fermi Observations of GRB 090510: A Short-Hard Gamma-ray Burst with an Additional, Hard Power-law Component from 10 keV TO GeV Energies

    NASA Astrophysics Data System (ADS)

    Ackermann, M.; Asano, K.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Ballet, J.; Barbiellini, G.; Baring, M. G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Bhat, P. N.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Briggs, M. S.; Brigida, M.; Bruel, P.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Carrigan, S.; Casandjian, J. M.; Cecchi, C.; Çelik, Ö.; Charles, E.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Connaughton, V.; Conrad, J.; Dermer, C. D.; de Palma, F.; Dingus, B. L.; Silva, E. do Couto e.; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Finke, J.; Focke, W. B.; Frailis, M.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giglietto, N.; Giordano, F.; Glanzman, T.; Godfrey, G.; Granot, J.; Grenier, I. A.; Grondin, M.-H.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hays, E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, W. N.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kawai, N.; Kippen, R. M.; Knödlseder, J.; Kocevski, D.; Kouveliotou, C.; Kuss, M.; Lande, J.; Latronico, L.; Lemoine-Goumard, M.; Llena Garde, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Makeev, A.; Mazziotta, M. N.; McEnery, J. E.; McGlynn, S.; Meegan, C.; Mészáros, P.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Moiseev, A. A.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nakajima, H.; Nakamori, T.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohno, M.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, M.; Paciesas, W. S.; Paneque, D.; Panetta, J. H.; Parent, D.; Pelassa, V.; Pepe, M.; Pesce-Rollins, M.; Piron, F.; Preece, R.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Ritz, S.; Rodriguez, A. Y.; Roth, M.; Ryde, F.; Sadrozinski, H. F.-W.; Sander, A.; Scargle, J. D.; Schalk, T. L.; Sgrò, C.; Siskind, E. J.; Smith, P. D.; Spandre, G.; Spinelli, P.; Stamatikos, M.; Stecker, F. W.; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, T.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Toma, K.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Uehara, T.; Usher, T. L.; van der Horst, A. J.; Vasileiou, V.; Vilchez, N.; Vitale, V.; von Kienlin, A.; Waite, A. P.; Wang, P.; Wilson-Hodge, C.; Winer, B. L.; Wu, X. F.; Yamazaki, R.; Yang, Z.; Ylinen, T.; Ziegler, M.

    2010-06-01

    We present detailed observations of the bright short-hard gamma-ray burst GRB 090510 made with the Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) on board the Fermi observatory. GRB 090510 is the first burst detected by the LAT that shows strong evidence for a deviation from a Band spectral fitting function during the prompt emission phase. The time-integrated spectrum is fit by the sum of a Band function with E peak = 3.9 ± 0.3 MeV, which is the highest yet measured, and a hard power-law component with photon index -1.62 ± 0.03 that dominates the emission below ≈20 keV and above ≈100 MeV. The onset of the high-energy spectral component appears to be delayed by ~0.1 s with respect to the onset of a component well fit with a single Band function. A faint GBM pulse and a LAT photon are detected 0.5 s before the main pulse. During the prompt phase, the LAT detected a photon with energy 30.5+5.8 -2.6 GeV, the highest ever measured from a short GRB. Observation of this photon sets a minimum bulk outflow Lorentz factor, Γgsim 1200, using simple γγ opacity arguments for this GRB at redshift z = 0.903 and a variability timescale on the order of tens of ms for the ≈100 keV-few MeV flux. Stricter high confidence estimates imply Γ >~ 1000 and still require that the outflows powering short GRBs are at least as highly relativistic as those of long-duration GRBs. Implications of the temporal behavior and power-law shape of the additional component on synchrotron/synchrotron self-Compton, external-shock synchrotron, and hadronic models are considered.

  13. Kepler Data Validation and Follow-up Programs

    NASA Technical Reports Server (NTRS)

    William, Borucki J.

    2009-01-01

    The approach that the Kepler Mission uses to remove false positive events and to validate the discoveries consists of two parts; data validation (DPI) and follow up observations program (FOP). DV consists of several methods of examining the data from the spacecraft observations. First, to rule out statistical fluctuations in the data, accept only signals that show 3 or more transits and that have a total signal-to-noise ratio that exceeds 7 sigma. Second. to identify small stellar companions to the target star, we check for secondary eclipses and determine if the transit characteristics are appropriate for a planetary companion. Third, check for background binaries that are in the target aperture. Here we measure the movement of the image centroid before, during, and after the transit. If the target is producing the signal, a dimming wi11 move the image centroid in a known direction and magnitude. If the signal comes from a nearby star, the amplitude and direction of the motion wi11 be different, This test is expected to rule out the hundreds of binary signals expected from background stars. The precision of the measurement depends on the stellar fluxes and positions but can be better than 0.01 pixel; i.e., 0.04". Those candidates that pass these tests are examined using ground-based telescopes and radial velocity spectrometers. First medium precision RV is used to rule out any remaining stellar companions. Then high spatial resolution imaging is used to check for nearby stars that are in the aperture- (The Kepler apertures depend on magnitude but are of order 36 sq are sec in area.) If no stars are present that quid generate the observed signal, then the candidate goes to a large telescope such as Keck, HET, or Wi1lilam Herschel for high precision observations to get the planet mass or an upper limit to it, if there are some stars in the aperture, then the photometric observations are employed to look for the transit by cane of the confounding stars. If none are

  14. Acromegalic patients lost to follow-up: a pilot study.

    PubMed

    Kasuki, Leandro; Marques, Nelma Verônica; Nuez, Maria José Braga La; Leal, Vera Lucia Gomes; Chinen, Renata N; Gadelha, Mônica R

    2013-06-01

    Approximately 50 % of all acromegalic patients will require lifelong medical treatment to normalize mortality rates and reduce morbidity. Thus, adherence to therapy is essential to achieve treatment goals. To date, no study has evaluated the frequency and reasons for loss to follow-up in the acromegalic population. The current study aimed at evaluating the frequency of acromegalic patient loss to follow-up in three reference centers and the reasons responsible for their low compliance with treatment. All of the files for the acromegalic patients in the three centers were reviewed. Those patients, who had not followed up with the hospital for more than a year, were contacted via phone and/or mail and invited to participate. Patients who agreed to participate were interviewed, and blood samples were collected. A total of 239 files were reviewed; from these 42 patients (17.6 %) were identified who were lost to follow-up. It was possible to contact 27 of these patients, 10 of whom did not attend the appointments for more than one time and 17 of whom agreed to participate in the study. Fifteen of these 17 patients had active disease (88.2 %), and all of the patients restarted treatment in the original centers. The main reason for loss to follow-up was an absence of symptoms. High-quality follow-up is important in acromegaly to successfully achieve the aims of the treatment. An active search for patients may allow the resumption of treatment in a significant proportion of these cases, contributing to reduced morbidity and mortality in this patient population.

  15. Clinical follow up of uniparental disomy 16: First data

    SciTech Connect

    Dworniczak, B.; Koppers, B.; Bogdanova, N.

    1994-09-01

    Following the introduction of the concept of uniparental disomy (UPD) in 1980 by Engel this segregational anomaly is reported in an ever increasing number of patients. So far, several groups of individuals with an increased risk for UPD have been identified including abnormal carriers of familial balanced translocations or centric fusions, carriers of mosaic trisomies, and fetuses after prenatal diagnosis of confined placental mosaicism. A major pathogenetic mechanism appears to be post-meiotic chromosome loss in trisomic conceptuses. UPD was repeatedly observed in the fetus after diagnosis of mosaic or non-mosaic trisomies in the placenta which are usually considered {open_quotes}lethal{close_quotes} (i.e. trisomies 15 and 16). In an ongoing study to determine the incidence and clinical consequences of UPD we investigated the parental origin of chromosomes in the disomic cell line after prenatal diagnosis of mosaicism for various trisomies (e.g. 2, 7, 14, 15, and 16). At present, two maternal disomies 16 and one maternal disomy 15 were identified. Severe intrauterine growth retardation was a common symptome which, however, was also present in some but not all mosaics with a biparental origin of the chromosomes in question. While prognosis is clear in some instances (i.e. UPD 15) counseling can be extremely difficult in others, when imprinting effects and homozygosity for unknown recessive traits present in a parent have to be considered. To assess the clinical significance, detailed follow-up studies of proven cases of uniparental disomies are essential. First data of two cases with UPD 16 are presented.

  16. Preparing for LSST with the LCOGT NEO Follow-up Network

    NASA Astrophysics Data System (ADS)

    Greenstreet, Sarah; Lister, Tim; Gomez, Edward

    2016-10-01

    The Las Cumbres Observatory Global Telescope Network (LCOGT) provides an ideal platform for follow-up and characterization of Solar System objects (e.g. asteroids, Kuiper Belt Objects, comets, Near-Earth Objects (NEOs)) and ultimately for the discovery of new objects. The LCOGT NEO Follow-up Network is using the LCOGT telescope network in addition to a web-based system developed to perform prioritized target selection, scheduling, and data reduction to confirm NEO candidates and characterize radar-targeted known NEOs.In order to determine how to maximize our NEO follow-up efforts, we must first define our goals for the LCOGT NEO Follow-up Network. This means answering the following questions. Should we follow-up all objects brighter than some magnitude limit? Should we only focus on the brightest objects or push to the limits of our capabilities by observing the faintest objects we think we can see and risk not finding the objects in our data? Do we (and how do we) prioritize objects somewhere in the middle of our observable magnitude range? If we want to push to faint objects, how do we minimize the amount of data in which the signal-to-noise ratio is too low to see the object? And how do we find a balance between performing follow-up and characterization observations?To help answer these questions, we have developed a LCOGT NEO Follow-up Network simulator that allows us to test our prioritization algorithms for target selection, confirm signal-to-noise predictions, and determine ideal block lengths and exposure times for observing NEO candidates. We will present our results from the simulator and progress on our NEO follow-up efforts.In the era of LSST, developing/utilizing infrastructure, such as the LCOGT NEO Follow-up Network and our web-based platform for selecting, scheduling, and reducing NEO observations, capable of handling the large number of detections expected to be produced on a daily basis by LSST will be critical to follow-up efforts. We hope our

  17. The Ultraluminous GRB 110918A

    NASA Astrophysics Data System (ADS)

    Frederiks, D. D.; Hurley, K.; Svinkin, D. S.; Pal'shin, V. D.; Mangano, V.; Oates, S.; Aptekar, R. L.; Golenetskii, S. V.; Mazets, E. P.; Oleynik, Ph. P.; Tsvetkova, A. E.; Ulanov, M. V.; Kokomov, A. A.; Cline, T. L.; Burrows, D. N.; Krimm, H. A.; Pagani, C.; Sbarufatti, B.; Siegel, M. H.; Mitrofanov, I. G.; Golovin, D.; Litvak, M. L.; Sanin, A. B.; Boynton, W.; Fellows, C.; Harshman, K.; Enos, H.; Starr, R.; von Kienlin, A.; Rau, A.; Zhang, X.; Goldstein, J.

    2013-12-01

    GRB 110918A is the brightest long gamma-ray burst (GRB) detected by Konus-WIND during its almost 19 yr of continuous observations and the most luminous GRB ever observed since the beginning of the cosmological era in 1997. We report on the final Interplanetary Network localization of this event and its detailed multiwavelength study with a number of space-based instruments. The prompt emission is characterized by a typical duration, a moderate peak energy of the time-integrated spectrum, and strong hard-to-soft evolution. The high observed energy fluence yields, at z = 0.984, a huge isotropic-equivalent energy release E iso = (2.1 ± 0.1) × 1054 erg. The record-breaking energy flux observed at the peak of the short, bright, hard initial pulse results in an unprecedented isotropic-equivalent luminosity L iso = (4.7 ± 0.2) × 1054 erg s-1. A tail of the soft γ-ray emission was detected with temporal and spectral behavior typical of that predicted by the synchrotron forward-shock model. The Swift/X-Ray Telescope and the Swift/Ultraviolet Optical Telescope observed the bright afterglow from 1.2 to 48 days after the burst and revealed no evidence of a jet break. The post-break scenario for the afterglow is preferred from our analysis, with a hard underlying electron spectrum and interstellar-medium-like circumburst environment implied. We conclude that, among the multiple reasons investigated, the tight collimation of the jet must have been a key ingredient to produce this unusually bright burst. The inferred jet opening angle of 1.°7-3.°4 results in reasonable values of the collimation-corrected radiated energy and the peak luminosity, which, however, are still at the top of their distributions for such tightly collimated events. We estimate a detection horizon for a similar ultraluminous GRB of z ~ 7.5 for Konus-WIND and z ~ 12 for the Swift/Burst Alert Telescope, which stresses the importance of GRBs as probes of the early Universe.

  18. The ultraluminous GRB 110918A

    SciTech Connect

    Frederiks, D. D.; Svinkin, D. S.; Pal'shin, V. D.; Aptekar, R. L.; Golenetskii, S. V.; Mazets, E. P.; Oleynik, Ph. P.; Tsvetkova, A. E.; Ulanov, M. V.; Kokomov, A. A.; Hurley, K.; Mangano, V.; Burrows, D. N.; Sbarufatti, B.; Siegel, M. H.; Oates, S.; Cline, T. L.; Krimm, H. A.; Pagani, C.; Mitrofanov, I. G. [Space Research Institute, Profsoyuznaya 84 and others

    2013-12-20

    GRB 110918A is the brightest long gamma-ray burst (GRB) detected by Konus-WIND during its almost 19 yr of continuous observations and the most luminous GRB ever observed since the beginning of the cosmological era in 1997. We report on the final Interplanetary Network localization of this event and its detailed multiwavelength study with a number of space-based instruments. The prompt emission is characterized by a typical duration, a moderate peak energy of the time-integrated spectrum, and strong hard-to-soft evolution. The high observed energy fluence yields, at z = 0.984, a huge isotropic-equivalent energy release E {sub iso} = (2.1 ± 0.1) × 10{sup 54} erg. The record-breaking energy flux observed at the peak of the short, bright, hard initial pulse results in an unprecedented isotropic-equivalent luminosity L {sub iso} = (4.7 ± 0.2) × 10{sup 54} erg s{sup –1}. A tail of the soft γ-ray emission was detected with temporal and spectral behavior typical of that predicted by the synchrotron forward-shock model. The Swift/X-Ray Telescope and the Swift/Ultraviolet Optical Telescope observed the bright afterglow from 1.2 to 48 days after the burst and revealed no evidence of a jet break. The post-break scenario for the afterglow is preferred from our analysis, with a hard underlying electron spectrum and interstellar-medium-like circumburst environment implied. We conclude that, among the multiple reasons investigated, the tight collimation of the jet must have been a key ingredient to produce this unusually bright burst. The inferred jet opening angle of 1.°7-3.°4 results in reasonable values of the collimation-corrected radiated energy and the peak luminosity, which, however, are still at the top of their distributions for such tightly collimated events. We estimate a detection horizon for a similar ultraluminous GRB of z ∼ 7.5 for Konus-WIND and z ∼ 12 for the Swift/Burst Alert Telescope, which stresses the importance of GRBs as probes of the early

  19. 10 CFR 1022.17 - Follow-up.

    Code of Federal Regulations, 2010 CFR

    2010-01-01

    ... ENERGY (GENERAL PROVISIONS) COMPLIANCE WITH FLOODPLAIN AND WETLAND ENVIRONMENTAL REVIEW REQUIREMENTS Procedures for Floodplain and Wetland Reviews § 1022.17 Follow-up. For those DOE actions taken in a floodplain or wetland, DOE shall verify that the implementation of the selected alternative,...

  20. 10 CFR 1022.17 - Follow-up.

    Code of Federal Regulations, 2011 CFR

    2011-01-01

    ... ENERGY (GENERAL PROVISIONS) COMPLIANCE WITH FLOODPLAIN AND WETLAND ENVIRONMENTAL REVIEW REQUIREMENTS Procedures for Floodplain and Wetland Reviews § 1022.17 Follow-up. For those DOE actions taken in a floodplain or wetland, DOE shall verify that the implementation of the selected alternative,...

  1. 10 CFR 1022.17 - Follow-up.

    Code of Federal Regulations, 2013 CFR

    2013-01-01

    ... ENERGY (GENERAL PROVISIONS) COMPLIANCE WITH FLOODPLAIN AND WETLAND ENVIRONMENTAL REVIEW REQUIREMENTS Procedures for Floodplain and Wetland Reviews § 1022.17 Follow-up. For those DOE actions taken in a floodplain or wetland, DOE shall verify that the implementation of the selected alternative,...

  2. 10 CFR 1022.17 - Follow-up.

    Code of Federal Regulations, 2012 CFR

    2012-01-01

    ... ENERGY (GENERAL PROVISIONS) COMPLIANCE WITH FLOODPLAIN AND WETLAND ENVIRONMENTAL REVIEW REQUIREMENTS Procedures for Floodplain and Wetland Reviews § 1022.17 Follow-up. For those DOE actions taken in a floodplain or wetland, DOE shall verify that the implementation of the selected alternative,...

  3. 10 CFR 1022.17 - Follow-up.

    Code of Federal Regulations, 2014 CFR

    2014-01-01

    ... ENERGY (GENERAL PROVISIONS) COMPLIANCE WITH FLOODPLAIN AND WETLAND ENVIRONMENTAL REVIEW REQUIREMENTS Procedures for Floodplain and Wetland Reviews § 1022.17 Follow-up. For those DOE actions taken in a floodplain or wetland, DOE shall verify that the implementation of the selected alternative,...

  4. Three Year Follow-Up of 1974 Graduates.

    ERIC Educational Resources Information Center

    Baratta, Mary Kathryne

    To evaluate the long-term benefits of attendance at Moraine Valley Community College (MVCC), a three-year follow-up study was conducted of the 620 1974 graduates (324 transfer and 296 occupational students). Each graduate was sent a questionnaire collecting information on involvement with MVCC after graduation, present educational status,…

  5. Employer Follow-Up Survey, February-March 1994.

    ERIC Educational Resources Information Center

    Adams, Judith

    In February 1994, a study was conducted by Macomb Community College (MCC), in Michigan, to determine the extent to which the training received by MCC graduates met the needs of area employers. In conjunction with a follow-up study of MCC completers from 1992-93, respondents were requested to complete release of information forms for their…

  6. Employer Follow-Up, 1978. Research Report Number 20.

    ERIC Educational Resources Information Center

    Nespoli, Lawrence A.; Nair, P. C.

    An employer follow-up study was conducted by Howard Community College (HCC) in May, 1979, to determine the job performance of the HCC 1978 occupational program graduates. Only the employers of occupational graduates in full-time jobs related to their program of study were involved. These employers were asked, on a specially prepared questionnaire,…

  7. Follow-Up of 1978 Entrants. Research Report Number 32.

    ERIC Educational Resources Information Center

    Nespoli, Lawrence A.; Radcliffe, Susan K.

    A follow-up study of students entering Howard Community College (HCC) in 1978 was conducted to obtain information on student outcomes three and one-half years after enrollment. A questionnaire developed by the Maryland Community College Research Group and the Maryland State Board for Community Colleges was sent to 592 students who entered HCC in…

  8. Follow-Up of 1981 Graduates. Research Report Number 33.

    ERIC Educational Resources Information Center

    Nespoli, Lawrence A.; Radcliffe, Susan K.

    A follow-up study of 1981 graduates of Howard Community College (HCC) was conducted to obtain demographic data, determine students' employment and educational status 6 months after graduation, and to assess graduates' satisfaction with HCC's classroom instruction and preparation for transfer/employment. Study findings, based on survey responses…

  9. Follow-Up of 1984 Entrants. Research Report Number 60.

    ERIC Educational Resources Information Center

    Seboda, Barbara L.

    In 1988, a follow-up mail survey was conducted of 1984 entrants at Howard Community College (HCC) in Maryland to determine their educational and career achievements subsequent to their community college experience and to assess the effectiveness of the college from the students' perspective. Questionnaires were sent to all 1,160 student who…

  10. Trident Technical College 1998 Graduate Follow-Up.

    ERIC Educational Resources Information Center

    Trident Technical Coll., Charleston, SC.

    Presents the results of South Carolina's Trident Technical College's (TTC's) 1998 graduate follow-up survey report of 915 TTC graduates. Graduates were surveyed and results were obtained for the following items: graduate goals, employment, placement rates, graduates in related fields, when job were obtained, job finding methods, job locations, job…

  11. Trident Technical College 1999 Graduate Follow-Up Report.

    ERIC Educational Resources Information Center

    Trident Technical Coll., Charleston, SC.

    Presents the results of South Carolina's Trident Technical College's (TTC's) 1999 graduate follow-up survey report. Graduates were surveyed and results were obtained for the following items: graduate goals, employment, placement rates, graduates in related fields, when job obtained, job finding methods, job locations, job satisfaction, job…

  12. 38 CFR 41.315 - Audit findings follow-up.

    Code of Federal Regulations, 2010 CFR

    2010-07-01

    ... 38 Pensions, Bonuses, and Veterans' Relief 2 2010-07-01 2010-07-01 false Audit findings follow-up. 41.315 Section 41.315 Pensions, Bonuses, and Veterans' Relief DEPARTMENT OF VETERANS AFFAIRS (CONTINUED) AUDITS OF STATES, LOCAL GOVERNMENTS, AND NON-PROFIT ORGANIZATIONS Auditees § 41.315...

  13. Hospitalization patterns in schizophrenia. A 13-year follow-up.

    PubMed

    Munk-Jørgensen, P; Mortensen, P B; Machón, R A

    1991-01-01

    All first admitted patients in 1972 from a catchment area of 582,000 inhabitants aged 15 years or more who were diagnosed as schizophrenic at least once from 1972 until September 1983 (n = 53) were followed-up on average 13 years after first admission. About 20% of the cohort was hospitalized on any given day throughout the length of the follow-up period. The duration of hospitalization decreased from a mean of 8.2 months for the first admission to 1.7 months for the tenth or later admission. The readmission risk increased as a function of the number of previous admissions. Patients with income from occupation or from grants for education had shorter duration of first in-patient period. If the patients were diagnosed as schizophrenics already during the first hospitalization the risk for prolonged duration of the first in-patient period was increased but the readmission risk diminished. Furthermore, readmission risk after the first discharge was diminished by own income and by out-patient treatment and increased by low social status. High proportion of follow-up time in hospital (greater than or equal to 30%) was correlated to affective flattening present at first admission. Of the cohorts' total number of admissions (n = 493) 12% were involuntary. Involuntary admissions were more frequent in the first half of the follow-up period and were correlated to a previous involuntary admission. PMID:2009251

  14. 33 CFR 179.15 - Follow-up report.

    Code of Federal Regulations, 2012 CFR

    2012-07-01

    ... 33 Navigation and Navigable Waters 2 2012-07-01 2012-07-01 false Follow-up report. 179.15 Section 179.15 Navigation and Navigable Waters COAST GUARD, DEPARTMENT OF HOMELAND SECURITY (CONTINUED...) A positive identification of the initial report; (2) The number of units in which the defect...

  15. Extended Follow-Up | Division of Cancer Prevention

    Cancer.gov

    NCI supports the continued follow-up of participants in the Prostate, Lung, Colorectal, and Ovarian Cancer Screening Trial (PLCO) to strengthen the PLCO as a valuable resource for molecular epidemiologic research as well as provide long-term data on the trial’s primary endpoints. |

  16. Brevard District Plan for Placement and Follow-Up.

    ERIC Educational Resources Information Center

    Thomas, Olive W.

    The Brevard District Plan for placement and follow-up is intended for all secondary students, including dropouts, disadvantaged, adult students, and graduates. The areas of placement may be in gainful employment, educational institutions, or a combination of both. The plan specifies procedures for implementing placement and stipulates the type of…

  17. Wide Angle Mobility Light (WAML) Follow-up.

    ERIC Educational Resources Information Center

    Shull, L. E.; Kuyk, T.

    1990-01-01

    A follow-up study of an earlier report on the Wide Angle Mobility Light (WAML) was conducted to analyze the various applications of the device and its reliability. Results indicate high client satisfaction with WAML among test subjects (26 blind male veterans with night blindness, age 32 to 68). (Author/PB)

  18. Loss to Follow-Up: Issues and Recommendations

    ERIC Educational Resources Information Center

    Hoffman, Jeff; Munoz, Karen F.; Bradham, Tamala S.; Nelson, Lauri

    2011-01-01

    State coordinators of early hearing detection and intervention (EHDI) programs completed a strengths, weaknesses, opportunities, and threats, or SWOT, analysis that examined 12 areas within state EHDI programs. Related to how EHDI programs address loss to follow-up, 47 coordinators responded with 277 items, and themes were identified in each…

  19. Follow-Up of the Fall 1990 FTIC Cohort.

    ERIC Educational Resources Information Center

    Windham, Patricia

    Drawing from data provided by the Florida Education and Training Placement Information Program (FETPIP), this series of reports provides follow-up information on FTIC students entering Tallahassee Community College (TCC) in fall 1990. The four reports compare students based on race, entry level test pass rates, full-/part-time status, and grade…

  20. Graduate Follow-Up Study, 1997-98.

    ERIC Educational Resources Information Center

    Wisconsin Technical Coll. System Board, Madison.

    The Graduate Follow-up Survey is conducted annually by the Wisconsin Technical College System board to gather data regarding the activities and perceptions of recent technical college graduates. The 1997-98 survey identifies graduates' current activities, determines the extent to which these activities are related to the graduates' educational…

  1. Sexually Abstinent Adolescents: An 18-Month Follow-Up

    ERIC Educational Resources Information Center

    Blinn-Pike, Lynn; Berger, Thomas J.; Hewett, John; Oleson, Jacob

    2004-01-01

    This study was a longitudinal follow-up of 697 early adolescents from 20 schools in Missouri, investigating students who, in 1997, indicated on a survey of sexual attitudes and behaviors that they had not had sexual intercourse. They completed the Reasons for Abstinence Scale (RAS) by identifying those items that were reasons why they had not had…

  2. Screening and follow up of vulval skin disorders.

    PubMed

    Eva, Lois J

    2012-04-01

    Vulval squamous cell carcinoma is relatively rare; however, up to 20% of women have significant vulval symptoms during their lifetime. Formal screening programmes for vulval disease have not been established. The evidence for the use of vulval cytology and vulvoscopy is reviewed. No randomised-controlled trials have compared follow-up regimens, and although a few consensus documents have been published, formal guidelines are lacking in Grade A evidence. With increasing pressure on healthcare resources, the possibility of identifying high-risk groups to optimise the use of follow up in specialist clinics is explored. Vulval disease is uncommon and there is no evidence that screening would decrease incidence. If high-risk groups can be identified, follow up should take place in specialised vulval clinics with experienced clinicians who are trained in vulval disease. Women with uncomplicated vulval conditions should be discharged to patient-initiated follow up or primary care. Central to the reduction of mortality and morbidity is increased awareness of vulval conditions among women and improved education of healthcare professionals, with particular understanding of the importance of physical examination.

  3. A Follow-up Study of Secretarial Students.

    ERIC Educational Resources Information Center

    Gell, Robert L.; Bleil, David F.

    To determine how effectively the Secretarial Studies Department's program was meeting the needs of its students, a follow-up study was conducted of former Montgomery Community College Secretarial Studies students. The survey sought to determine, in particular, if the students had secured employment that was related to their course work at the…

  4. Prediction of Marital Distress: A 5-Year Follow-Up.

    ERIC Educational Resources Information Center

    Markman, Howard J.

    1981-01-01

    Couples planning marriage participated in a longitudinal study examining the predictive power of communication ratings. Intact couples (N=9) completed data at three follow-up points. Results indicated the more positively premarital couples rated their communication, the more satisfied they were with their relationship five-and-a-half-years later.…

  5. Three-Year Follow-Up Data in Overweight Treatment.

    ERIC Educational Resources Information Center

    Hautzinger, Martin

    1980-01-01

    The body weight of former participants to control long-term efficiency of behavior-oriented weight reduction programs was rechecked. Only 4 of the 21 available subjects regained weight over the three-year period. On an average, subjects lost 4.4 kilograms over the follow-up period. (Author)

  6. Matching Methods for Selection of Participants for Follow-Up

    ERIC Educational Resources Information Center

    Stuart, Elizabeth A.; Lalongo, Nicholas S.

    2010-01-01

    This work examines ways to make the best use of limited resources when selecting individuals to follow up in a longitudinal study estimating causal effects. In the setting under consideration, covariate information is available for all individuals but outcomes have not yet been collected and may be expensive to gather, and thus only a subset of…

  7. Factors Associated with Adherence to Follow-up Colposcopy

    ERIC Educational Resources Information Center

    Fish, Laura J.; Moorman, Patricia G.; Wordlaw-Stintson, Lashawn; Vidal, Adriana; Smith, Jennifer S.; Hoyo, Cathrine

    2013-01-01

    Background: Understanding the gaps in knowledge about human papilloma virus (HPV) infection, transmission, and health consequences and factors associated with the knowledge gap is an essential first step for the development of interventions to improve adherence to follow-up among women with abnormal Pap smears. Purpose: To examine the relationship…

  8. Photohadronic Instability Model for GRB Prompt Emission

    NASA Astrophysics Data System (ADS)

    Dimitrakoudis, S.

    2013-09-01

    Τhe mechanisms behind gamma-ray bursts (GRBs) are not yet well understood. Here we investigate a model where a spectral energy distribution (SED) that looks surprisingly like a typical GRB prompt emission is generated starting with merely high energy protons and a magnetic field. Using a selfconsistent, time-dependent code we show that when the density of such protons exceeds a certain threshold their energy is converted explosively to lower energy photons through a series of positive feedback loops. At even higher densities, Compton scattering of cold electrons shapes the low energy part of the SED into the familiar Band function, a distinctive peak between 1-10 keV (in the comoving frame) in GRB observations. This approach, although similar to the photospheric GRB model, also allows us to investigate the neutrino emission, which can be compared with recent ICECUBE limits.

  9. Search for TeV Gamma-ray Emission from GRB 100621A, an extremely bright GRB in X-rays, with H.E.S.S.

    NASA Astrophysics Data System (ADS)

    H.E.S.S. Collaboration; Abramowski, A.; Aharonian, F.; Ait Benkhali, F.; Akhperjanian, A. G.; Angüner, E.; Anton, G.; Balenderan, S.; Balzer, A.; Barnacka, A.; Becherini, Y.; Becker Tjus, J.; Bernlöhr, K.; Birsin, E.; Bissaldi, E.; Biteau, J.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bordas, P.; Brucker, J.; Brun, F.; Brun, P.; Bulik, T.; Carrigan, S.; Casanova, S.; Cerruti, M.; Chadwick, P. M.; Chalme-Calvet, R.; Chaves, R. C. G.; Cheesebrough, A.; Chrétien, M.; Colafrancesco, S.; Cologna, G.; Conrad, J.; Couturier, C.; Dalton, M.; Daniel, M. K.; Davids, I. D.; Degrange, B.; Deil, C.; deWilt, P.; Dickinson, H. J.; Djannati-Ataï, A.; Domainko, W.; O'C. Drury, L.; Dubus, G.; Dutson, K.; Dyks, J.; Dyrda, M.; Edwards, T.; Egberts, K.; Eger, P.; Espigat, P.; Farnier, C.; Fegan, S.; Feinstein, F.; Fernandes, M. V.; Fernandez, D.; Fiasson, A.; Fontaine, G.; Förster, A.; Füßling, M.; Gajdus, M.; Gallant, Y. A.; Garrigoux, T.; Giebels, B.; Glicenstein, J. F.; Grondin, M.-H.; Grudzińska, M.; Häffner, S.; Hahn, J.; Harris, J.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hervet, O.; Hillert, A.; Hinton, J. A.; Hofmann, W.; Hofverberg, P.; Holler, M.; Horns, D.; Jacholkowska, A.; Jahn, C.; Jamrozy, M.; Janiak, M.; Jankowsky, F.; Jung, I.; Kastendieck, M. A.; Katarzyński, K.; Katz, U.; Kaufmann, S.; Khélifi, B.; Kieffer, M.; Klepser, S.; Klochkov, D.; Kluźniak, W.; Kneiske, T.; Kolitzus, D.; Komin, Nu.; Kosack, K.; Krakau, S.; Krayzel, F.; Krüger, P. P.; Laffon, H.; Lamanna, G.; Lefaucheur, J.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J.-P.; Lennarz, D.; Lohse, T.; Lopatin, A.; Lu, C.-C.; Marandon, V.; Marcowith, A.; Marx, R.; Maurin, G.; Maxted, N.; Mayer, M.; McComb, T. J. L.; Méhault, J.; Menzler, U.; Meyer, M.; Moderski, R.; Mohamed, M.; Moulin, E.; Murach, T.; Naumann, C. L.; de Naurois, M.; Niemiec, J.; Nolan, S. J.; Oakes, L.; O'Brien, P. T.; Ohm, S.; de Oña Wilhelmi, E.; Opitz, B.; Ostrowski, M.; Oya, I.; Panter, M.; Parsons, R. D.; Paz Arribas, M.; Pekeur, N. W.; Pelletier, G.; Perez, J.; Petrucci, P.-O.; Peyaud, B.; Pita, S.; Poon, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Raue, M.; Reimer, A.; Reimer, O.; Renaud, M.; de los Reyes, R.; Rieger, F.; Rob, L.; Romoli, C.; Rosier-Lees, S.; Rowell, G.; Rudak, B.; Rulten, C. B.; Sahakian, V.; Sanchez, D. A.; Santangelo, A.; Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schwanke, U.; Schwarzburg, S.; Schwemmer, S.; Sol, H.; Spengler, G.; Spies, F.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Stinzing, F.; Stycz, K.; Sushch, I.; Szostek, A.; Tam, P. H. T.; Tavernet, J.-P.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tluczykont, M.; Trichard, C.; Valerius, K.; van Eldik, C.; Vasileiadis, G.; Venter, C.; Viana, A.; Vincent, P.; Völk, H. J.; Volpe, F.; Vorster, M.; Wagner, S. J.; Wagner, P.; Ward, M.; Weidinger, M.; Weitzel, Q.; White, R.; Wierzcholska, A.; Willmann, P.; Wörnlein, A.; Wouters, D.; Zacharias, M.; Zajczyk, A.; Zdziarski, A. A.; Zech, A.; Zechlin, H.-S.

    2014-05-01

    The long gamma-ray burst (GRB) 100621A, at the time the brightest X-ray transient ever detected by Swift-XRT in the 0.3-10 keV range, has been observed with the H.E.S.S. imaging air Cherenkov telescope array, sensitive to gamma radiation in the very-high-energy (VHE, >100 GeV) regime. Due to its relatively small redshift of z ~ 0.5, the favourable position in the southern sky and the relatively short follow-up time (<700 s after the satellite trigger) of the H.E.S.S. observations, this GRB could be within the sensitivity reach of the H.E.S.S. instrument. The analysis of the H.E.S.S. data shows no indication of emission and yields an integral flux upper limit above ~380 GeV of 4.2 × 10-12 cm-2 s-1 (95% confidence level), assuming a simple Band function extension model. A comparison to a spectral-temporal model, normalised to the prompt flux at sub-MeV energies, constraints the existence of a temporally extended and strong additional hard power law, as has been observed in the other bright X-ray GRB 130427A. A comparison between the H.E.S.S. upper limit and the contemporaneous energy output in X-rays constrains the ratio between the X-ray and VHE gamma-ray fluxes to be greater than 0.4. This value is an important quantity for modelling the afterglow and can constrain leptonic emission scenarios, where leptons are responsible for the X-ray emission and might produce VHE gamma rays.

  10. A retrospective follow-up study of body dysmorphic disorder#

    PubMed Central

    Phillips, Katharine A.; Grant, Jon E.; Siniscalchi, Jason M.; Stout, Robert; Price, Lawrence H.

    2006-01-01

    Background Although research on body dysmorphic disorder (BDD) is increasing, no follow-up studies of this disorder’s course of illness have been published. Methods The status of 95 outpatients with BDD treated in a clinical practice was assessed by chart review. Standard scales were used to rate subjects at baseline and the most recent clinic visit (mean duration of follow-up, 1.7 ± 1.1; range, 0.5–6.4 years). Ratings were also done at 6-month intervals over the first 4 years of follow-up. Results Allowing for censoring, life table analysis estimated that the proportion of subjects who achieved full remission from BDD at the 6-month and/or 12-month assessment was 24.7%; the proportion who attained partial or full remission at 6 months and/or 12 months was 57.8%. After 4 years of follow-up, 58.2% had experienced full remission, and 83.8% had experienced partial or full remission, at one or more 6-month assessment points. Of those subjects who attained partial or full remission at one or more assessment points, 28.6% subsequently relapsed. Between baseline and the most recent assessment, BDD severity and functioning significantly improved: at the most recent assessment, 16.7% of subjects were in full remission, 37.8% were in partial remission, and 45.6% met full criteria for BDD. Greater severity of BDD symptoms and the presence of major depression or social phobia at baseline were associated with more severe BDD symptoms at study end point. All subjects received at least one medication trial, and 34.3% received some type of therapy during the follow-up period. Conclusions A majority of treated patients with BDD improved, although improvement was usually partial. Prospective longitudinal studies are needed to further elucidate the course of BDD. PMID:16122530

  11. Hyperlipidaemia in general practice: three year follow up of an opportunistic screening project.

    PubMed Central

    Mann, J I; Morgan, B; Ball, M; Mant, D; Jones, L; Robertson, I

    1990-01-01

    As part of the national lipid screening project 927 people with a plasma cholesterol level greater than 6.5 mM were detected by screening 4006 men and women aged 25-59 years. Three years later 801 of the 878 patients eligible for a follow-up study (91%) had been followed up at least once. The median number of follow-up visits was two. The bulk of the workload fell on the nursing staff. The mean decrease in cholesterol level was 8-14% in those receiving dietary advice only, 15-25% in those receiving additional drug treatment and 12% for all patients. A proportion of this decrease must be attributable to regression to the mean, loss to follow up when patients were doing well, and the patients' knowledge of their follow-up date. Data on a group of patients not attending for regular follow up suggest that regression to the mean could account for up to 7% of the cholesterol reduction observed. Screening for hyperlipidaemia in general practice is feasible when the necessary infrastructure is provided, but even with a fairly conservative protocol 3% of those screened received drug treatment. PMID:2271263

  12. GRB Studies with Fermi

    NASA Technical Reports Server (NTRS)

    Meegan, Charles A.

    2008-01-01

    This slide presentation reviews the studies of Gamma Ray Bursts (GRB) with the Fermi Gamma Ray Space Telescope. Included are pictures of the observatory, with illustrations of the Large Area Telescope (LAT), and the Gamma-ray Burst Monitor (GBM) including information about both their capabilities. Graphs showing the GBM count rate over time after the GBM trigger for three GRBs, preliminary charts showing the multiple detector light curves the spectroscopy of the main LAT peak and the spectral evolution of GRB 080916C Burst Temporally-extended LAT emission.

  13. GRB 091127: The Cooling Break Race on Magnetic Fuel

    NASA Technical Reports Server (NTRS)

    Filgas, R.; Greiner, J.; Schady, P.; Kruhler, T.; Updike, A. C.; Klose, S.; Nardini, M.; Kann, D. A.; Rossi, A.; Sudilovsky, V.; Afonso, P. M. J.; Clemens, C.; Elliott, J.; Nicuesa Guelbenzu, A.; Olivares, F.; Rau, A.

    2011-01-01

    Using high-quality, broad-band afterglow data for GRB 091127, we investigate the validity of the synchrotron fireball model for gamma-ray bursts, and infer physical parameters of the ultra-relativistic outflow. Methods. We used multi-wavelength (NIR to X-ray) follow-up observations obtained with GROND simultaneously in the g' r' t' i' z' JH filters and the XRT onboard the Swift satellite in the 0.3 to 10 keY energy range. The resulting afterglow light curve is of excellent accuracy with relative photometric errors as low as 1 %, and the spectral energy distribution (SED) is well-sampled over 5 decades in energy. These data present one of the most comprehensive observing campaigns for a single GRB afterglow and allow us to test several proposed emission models and outflow characteristics in unprecedented detail. Results. Both the multi-color light curve and the broad-band SED of the afterglow of GRB 091127 show evidence of a cooling break moving from high to lower energies. The early light curve is well described by a broken power-law, where the initial decay in the optical/NlR wavelength range is considerably flatter than at X-rays. Detailed fitting of the time-resolved SED shows that the break is very smooth with a sharpness index of 2.2 +/- 0.2, and evolves towards lower frequencies as a power-law with index -1.23 +/- 0.06. These are the first accurate and contemporaneous measurements of both the sharpness of the spectral break and its time evolution. Conclusions. The measured evolution of the cooling break (V(sub c) varies as t(sup -1.2) is not consistent with the predictions of the standard model, wherein V(sub c) varies as t(sup -05) is expected. A possible explanation for the observed behavior is a time dependence of the microphysical parameters, in particular the fraction of the total energy in the magnetic field epsilon(sub Beta). This conclusion provides further evidence that the standard fireball model is too simplistic, and time-dependent micro

  14. [Densitometric follow-up of algodystrophy using computerized tomography].

    PubMed

    Lindecken, K D; Krawzak, H W; Strosche, H; Kukulies, R; Schmidt, W G

    1987-01-01

    Clinical and radiological findings obtained from diagnosis and follow-up examination of post-traumatic algodystrophy (Morbus Sudeck) are very much open to subjective interpretation. Decisive importance is attributed not only to alteration of soft tissue but also to typical distribution patterns and severity of bone demineralisation. No objectifiable and quantifiable have so far become available for proper assessment but are urgently desirable in view of the great number of therapeutic approaches. Densitometry integrated with computed tomography was applied to nine patients with algodystrophy of hand or foot in the region of spongy bones to determine absorption values which were then compared with those on the clinically intact side. Significant differences between sides proved to be objectifiable and were quantifiable measures by which demineralisation of the effected extremity could be assessed. Repeated examinations were undertaken for follow-up through a period up to nine months. PMID:3630448

  15. Is follow-up capacity the current NHS bottleneck?

    PubMed

    Allder, Steven; Walley, Paul; Silvester, Kate

    2011-02-01

    Capacity and demand theory suggests that the presence of a queue is not necessarily an indication of a shortage of capacity in a system. It is much more likely that either there is a demand and capacity variation that creates queues or there is a delay designed into the system. A shortage of capacity is only really indicated where a backlog is not stable and continues to grow. In this article, data are taken from one NHS trust that provides evidence for a continually growing backlog for follow-up outpatient services. It is believed that these data are representative of most locations within the NHS in England and therefore suggest an immediate shortage in effective follow-up capacity. To avoid compromise to patient care, the problem will have to be addressed before the situation becomes unmanageable. The paper highlights options to reduce or deflect demand or to increase effective capacity.

  16. Discharge planning and follow-up care: the asphyxiated infant.

    PubMed

    Parker, L

    1991-01-01

    Discharge planning and follow-up care of the asphyxiated infant is a complex process. Models of discharge planning, team member responsibilities, and teaching responsibilities are components of hospital discharge plans. Special care needs of these infants may include vision, hearing, immunizations, seizures, medications, and feeding. Families and health care professionals need to be familiar with programs providing financial resources for care of the infant such as private insurance, prepaid health care, Medicaid, Medical Needy program, Children with Special Health Care Needs (CSHCN), federal legislation mandating education and services for high-risk infants (PL 99-142 and PL 99-457) and intervention programs. Families returning to Newborn Follow-up programs become acquainted with a variety of professionals and types of neonatal and infant assessments. Providing teaching materials and information regarding special health problems, services and outcome, as it becomes known, is the responsibility of the extended health care team of nurses, physicians, home health services, psychologists, and therapists.

  17. From themes to hypotheses: following up with quantitative methods.

    PubMed

    Morgan, David L

    2015-06-01

    One important category of mixed-methods research designs consists of quantitative studies that follow up on qualitative research. In this case, the themes that serve as the results from the qualitative methods generate hypotheses for testing through the quantitative methods. That process requires operationalization to translate the concepts from the qualitative themes into quantitative variables. This article illustrates these procedures with examples that range from simple operationalization to the evaluation of complex models. It concludes with an argument for not only following up qualitative work with quantitative studies but also the reverse, and doing so by going beyond integrating methods within single projects to include broader mutual attention from qualitative and quantitative researchers who work in the same field.

  18. [Follow-up of newborns with hypoxic-ischaemic encephalopathy].

    PubMed

    Martínez-Biarge, M; Blanco, D; García-Alix, A; Salas, S

    2014-07-01

    Hypothermia treatment for newborn infants with hypoxic-ischemic encephalopathy reduces the number of neonates who die or have permanent neurological deficits. Although this therapy is now standard of care, neonatal hypoxic-ischaemic encephalopathy still has a significant impact on the child's neurodevelopment and quality of life. Infants with hypoxic-ischaemic encephalopathy should be enrolled in multidisciplinary follow-up programs in order to detect impairments, to initiate early intervention, and to provide counselling and support for families. This article describes the main neurodevelopmental outcomes after term neonatal hypoxic-ischaemic encephalopathy. We offer recommendations for follow-up based on the infant's clinical condition and other prognostic indicators, mainly neonatal neuroimaging. Other aspects, such as palliative care and medico-legal issues, are also briefly discussed.

  19. [Diagnosis, therapy and follow up of diabetic eye disease].

    PubMed

    Stur, Michael; Egger, Stefan; Haas, Anton; Kieselbach, Gerhard; Mennel, Stefan; Michl, Reinhard; Roden, Michael; Stolba, Ulrike; Wedrich, Andreas

    2012-12-01

    Diabetes mellitus causes diabetic retinopathy, diabetic macular edema, optic neuropathy, cataract or dysfunction of the eye muscles. The incidence of these defects correlates with disease duration and quality of the metabolic control. The recommendations of the Austrian Diabetes Association for the diagnosis, the therapeutic procedures and requirements for adequate follow up depending on the stages of the different forms of diabetic eye disease are summarized.

  20. Ute Unit: Study Guide and Follow Up Activities.

    ERIC Educational Resources Information Center

    North Conejos School District, Capulin, CO.

    The study guide and follow-up activities were designed primarily to give students a feeling of Ute life in the San Luis Valley in Colorado. The unit begins with six Southern Ute stories about the wolf and coyote, the race between the skunk and the coyote, the frog and the eagle, why the frog croaks, the bear (Que Ye Qat), and the two Indian…

  1. A Follow-up Study: The Registered Nurses Program, 1977.

    ERIC Educational Resources Information Center

    Kondwros, Jerry M.

    Twenty-seven (77.1%) of the thirty-five 1977 graduates of the South Georgia Colleges' Division of Nursing responded to a follow-up survey, producing the following information: (1) 17 were employed full-time, two were employed part-time, and eight were unemployed; (2) 88.9% agreed they were prepared adequately for the state board examination; (3)…

  2. Idiopathic hypertrophic cranial pachymenigitis - A long follow-up needed.

    PubMed

    Hashmi, M A; Gautam, G; Sengupta, P; Singh, H; Haque, N

    2011-07-01

    Idiopathic hypertrophic cranial pachymenigitis is a rare clinical condition caused by localized or diffuse inflammatory thickening of dura matter. Described here is a person having diffuse thickening of dura matter of base of skull and he was on follow-up treatment for 5 years with us. Diagnosis was done by excluding other conditions and with biopsy. The patient responded to steroid and the MRI picture, which is given serially, shows improvement. PMID:22347338

  3. Benign recurrent intrahepatic cholestasis--25 years of follow-up.

    PubMed Central

    Putterman, C.; Keidar, S.; Brook, J. G.

    1987-01-01

    Only 70 cases of recurrent intrahepatic cholestasis have been reported in the literature since the original description of this entity in 1959. The benign nature of the disease has been questioned, some authors suggesting progression to biliary cirrhosis. We report our follow-up of one such patient for over 25 years with no adverse physical consequences or histological deterioration. Sequential liver biopsies were obtained during this period. A conservative approach to diagnosis and treatment is therefore indicated. PMID:3684838

  4. Follow-up study of respiratory function in hemp workers.

    PubMed

    Zuskin, E; Mustajbegovic, J; Schachter, E N

    1994-07-01

    A 3-year follow-up study was performed on 38 women and 28 men from the originally studied textile workers employed in a soft hemp processing mill. Acute and chronic respiratory symptoms and ventilatory capacity were recorded during the cross-sectional and the follow-up studies. Maximum expiratory flow-volume (MEFV) curves were obtained on these workers, and forced vital capacity (FVC), 1-second forced expiratory volume (FEV1) and flow rates at 50% and at 25% of the VC (FEF50, FEF25) were measured. High prevalences of acute and chronic respiratory symptoms persisted at the follow-up study. In particular, high prevalences of byssinosis were documented at both studies (women: 47.4% and 47.4%; men: 64.3% and 67.9%, respectively). Statistically significant mean across-shift reductions were recorded for all ventilatory capacity tests at the initial study. A large mean annual decline was calculated for FEV1 in women and for all ventilatory capacity parameters in men; these declines were greater for workers with symptoms of byssinosis than for those without. The accelerated decline in FEV1 noted in the women workers, who were predominantly nonsmokers, suggests an independent hemp effect. Exposures in the work environment were measured with Hexhlet filters and revealed very high dust concentrations (mean total: 21.4 mg/m3, 22.4 mg/m3; respirable: 8.4 mg/m3, 9.9 mg/m3) at both initial and follow-up studies. These levels are much higher than those found in mills processing organic materials in North America. Our data demonstrate that work in the hemp industry, particularly in small poorly regulated mills, continues to have deleterious effects on respiratory function.

  5. A follow-up study of attempted railway suicides.

    PubMed

    O'Donnell, I; Arthur, A J; Farmer, R D

    1994-02-01

    This paper reports the subsequent mortality of 94 persons who attempted suicide by jumping in front of London Underground trains between 1977 and 1979. The follow-up period was 10 yr. Despite the apparent seriousness of the method, completion of suicide was not found to be higher than in previous studies of attempted suicide by other methods. By the end of the follow-up period 18 persons had died, nine of natural causes. Coroners' inquests were held for the unnatural deaths. Seven verdicts of suicide and two of accidental death were recorded. Of the nine unnatural deaths four were from multiple injuries, three from drowning, one from asphyxia and one from acute narcotic poisoning. All four multiple injury deaths were women, three of these were from repeated incidents involving London Underground trains. The time interval between the index attempt and eventual death for the suicide/accident group ranged from 1 day to 43 months. For ethical reasons it was not possible to follow-up attempted suicides who were presumed to have remained alive. PMID:8153748

  6. Health fair glaucoma screening: follow-up evaluation.

    PubMed

    Skorin, L; Multack, R F; Holtzman, J N

    1991-07-01

    Glaucoma screening is a standard procedure at many health fairs. Information on correct screening techniques, instrumentation, and target populations has been available. However, a scarcity of information exists concerning the success of efforts to follow up on abnormal results. This study reports on the findings of a long-term (6-month) follow-up of all individuals with abnormal tonometric results screened at an inner-city osteopathic hospital. Of the 218 subjects screened, 15 were found to have abnormal tonometric results. Seven of the 15 subjects were actually reached at the 6-month follow-up interval. Four of the seven had not sought any further eye care; two had sought nonmedical evaluation; only one had sought medical ocular care, and that subject was later found to have glaucoma. The results presented in this article indicate that compliance by this population is inadequate. Inner-city participants require more education. We encourage physicians to promptly refer such patients for appropriate medical ocular care.

  7. Follow-up of permanent hearing impairment in childhood.

    PubMed

    Della Volpe, A; De Lucia, A; Pastore, V; Bracci Laudiero, L; Buonissimo, I; Ricci, G

    2016-02-01

    Programmes for early childhood childhood hearing impairment identification allows to quickly start the appropriate hearing aid fitting and rehabilitation process; nevertheless, a large number of patients do not join the treatment program. The goal of this article is to present the results of a strategic review of the strengths, weaknesses, opportunities and threats connected with the audiologic/prosthetic/language follow-up process of children with bilateral permanent hearing impairment. Involving small children, the follow-up includes the involvement of specialised professionals of a multidisciplinary team and a complex and prolonged multi-faced management. Within the framework of the Italian Ministry of Health project CCM 2013 "Preventing Communication Disorders: a Regional Program for Early Identification, Intervention and Care of Hearing Impaired Children", the purpose of this analysis was to propose recommendations that can harmonise criteria for outcome evaluation and provide guidance on the most appropriate assessment methods to be used in the follow-up course of children with permanent hearing impairment. PMID:27054392

  8. Complications and Follow-up after Unprotected Carotid Artery Stenting

    SciTech Connect

    Hauth, Elke A.M. Drescher, Robert; Jansen, Christian; Gissler, H. Martin; Schwarz, Michael; Forsting, Michael; Jaeger, Horst J.; Mathias, Klaus D.

    2006-08-15

    Purpose. This prospective study was undertaken to determine the success rate, complications, and outcome of carotid artery stenting (CAS) without the use of cerebral protection devices. Methods. During 12 months, 94 high-grade stenoses of the carotid artery in 91 consecutive patients were treated. Sixty-six (70%) of the stenoses were symptomatic and 28 (30%) were asymptomatic. Results. In all 94 carotid stenoses CAS was successfully performed. During the procedure and within the 30 days afterwards, there were 2 deaths and 3 major strokes in the 66 symptomatic patients, resulting in a combined death and stroke rate of 5 of 66 (7%). Only one of these complications, a major stroke, occurred during the procedure. In the 6-month follow-up, one additional major stroke occurred in a originally symptomatic patient resulting in a combined death and stroke rate of 6 of 66 (10%) for symptomatic patients at 6 months. No major complications occurred in asymptomatic patients during the procedure or in the 6-month follow-up period. At 6 months angiographic follow-up the restenosis rate with a degree of >50% was 3 of 49 (6%) and the rate with a degree of {>=}70% was 1 of 49 (2%). Conclusions. Cerebral embolization during CAS is not the only cause of the stroke and death rate associated with the procedure. The use of cerebral protection devices during the procedure may therefore not prevent all major complications following CAS.

  9. Follow-up of permanent hearing impairment in childhood.

    PubMed

    Della Volpe, A; De Lucia, A; Pastore, V; Bracci Laudiero, L; Buonissimo, I; Ricci, G

    2016-02-01

    Programmes for early childhood childhood hearing impairment identification allows to quickly start the appropriate hearing aid fitting and rehabilitation process; nevertheless, a large number of patients do not join the treatment program. The goal of this article is to present the results of a strategic review of the strengths, weaknesses, opportunities and threats connected with the audiologic/prosthetic/language follow-up process of children with bilateral permanent hearing impairment. Involving small children, the follow-up includes the involvement of specialised professionals of a multidisciplinary team and a complex and prolonged multi-faced management. Within the framework of the Italian Ministry of Health project CCM 2013 "Preventing Communication Disorders: a Regional Program for Early Identification, Intervention and Care of Hearing Impaired Children", the purpose of this analysis was to propose recommendations that can harmonise criteria for outcome evaluation and provide guidance on the most appropriate assessment methods to be used in the follow-up course of children with permanent hearing impairment.

  10. [Guidelines for the follow up of patients with bronchopulmonary dysplasia].

    PubMed

    Pérez Tarazona, S; Rueda Esteban, S; Alfonso Diego, J; Barrio Gómez de Agüero, M I; Callejón Callejón, A; Cortell Aznar, I; de la Serna Blázquez, O; Domingo Miró, X; García García, M L; García Hernández, G; Luna Paredes, C; Mesa Medina, O; Moreno Galdó, A; Moreno Requena, L; Pérez Pérez, G; Salcedo Posadas, A; Sánchez Solís de Querol, M; Torrent Vernetta, A; Valdesoiro Navarrete, L; Vilella Sabaté, M

    2016-01-01

    Bronchopulmonary dysplasia (BPD) is the most common complication of preterm birth, and remains a major problem in pediatric pulmonology units. The decision of discharging from the Neonatal Unit should be based on a thorough assessment of the condition of the patient and compliance with certain requirements, including respiratory and nutritional stability, and caregiver education on disease management. For proper control of the disease, a schedule of visits and complementary tests should be established prior to discharge, and guidelines for prevention of exacerbations and appropriate treatment should be applied. In this paper, the Working Group in Perinatal Respiratory Diseases of the Spanish Society of Pediatric Pulmonology proposes a protocol to serve as a reference for the follow up of patients with BPD among different centers and health care settings. Key factors to consider when planning discharge from the Neonatal Unit and during follow up are reviewed. Recommendations on treatment and prevention of complications are then discussed. The final section of this guide aims to provide a specific schedule for follow-up and diagnostic interventions to be performed in patients with BPD.

  11. Follow-up after treatment for breast cancer

    PubMed Central

    Sisler, Jeffrey; Chaput, Genevieve; Sussman, Jonathan; Ozokwelu, Emmanuel

    2016-01-01

    Objective To offer FPs a summary of evidence-based recommendations to guide their follow-up survivorship care of women treated for breast cancer. Quality of evidence A literature search was conducted in MEDLINE from 2000 to 2016 using the search words breast cancer, survivorship, follow-up care, aftercare, guidelines, and survivorship care plans, with a focus on review of recent guidelines published by national cancer organizations. Evidence ranges from level I to level III. Main message Survivorship care involves 4 main tasks: surveillance and screening, management of long-term effects, health promotion, and care coordination. Surveillance for recurrence involves only annual mammography, and screening for other cancers should be done according to population guidelines. Management of the long-term effects of cancer and its treatment addresses common issues of pain, fatigue, lymphedema, distress, and medication side effects, as well as longer-term concerns for cardiac and bone health. Health promotion emphasizes the benefits of active lifestyle change in cancer survivors, with an emphasis on physical activity. Survivorship care is enhanced by the involvement of various health professionals and services, and FPs play an important role in care coordination. Conclusion Family physicians are increasingly the main providers of follow-up care after breast cancer treatment. Breast cancer should be viewed as a chronic medical condition even in women who remain disease free, and patients benefit from the approach afforded other chronic conditions in primary care. PMID:27737976

  12. Discovery and Follow-up of High Energy Transients with Swift

    NASA Astrophysics Data System (ADS)

    Gehrels, Neil; Swift Team

    2013-01-01

    The Swift mission lives in the time domain, observing transients every day. It is an international space mission from the US, UK and Italy that detects transients in the hard X-ray band and autonomously slews for sensitive X-ray and optical follow-up. Source coordinates can also be rapidly sent up to the satellite for follow-up of transients detected by other observatories. Targets of interest include GRBs, supernovae, tidal disruption events, AGN flares, galactic transients and flare stars. Much is being learned about these sources. Also interesting are the odd-ball events observed every year that defy classification.

  13. The 'Supercritical Pile' GRB Model: Afterglows and GRB, XRR, XRF Unification

    NASA Technical Reports Server (NTRS)

    Kazanas, D.

    2007-01-01

    We present the general notions and observational consequences of the "Supercritical Pile" GRB model; the fundamental feature of this model is a detailed process for the conversion of the energy stored in relativistic protons in the GRB Relativistic Blast Waves (RBW) into relativistic electrons and then into radiation. The conversion is effected through the $p \\, \\gamma \\rightarrow p \\, e circumflex + e circumflex -$ reaction, whose kinematic threshold is imprinted on the GRB spectra to provide a peak of their emitted luminosity at energy \\Ep $\\sim 1$ MeV in the lab frame. We extend this model to include, in addition to the (quasi--)thermal relativistic post-shock protons an accelerated component of power law form. This component guarantees the production of $e circumflex +e circumflex- - $pairs even after the RBW has slowed down to the point that its (quasi-) thermal protons cannot fulfill the threshold of the above reaction. We suggest that this last condition marks the transition from the prompt to the afterglow GRB phase. We also discuss conditions under which this transition is accompanied by a significant drop in the flux and could thus account for several puzzling, recent observations. Finally, we indicate that the same mechanism applied to the late stages of the GRB evolution leads to a decrease in \\Ep $\\propto \\Gamma circumflex 2(t)\\propto t circumflex {-3/4}$, a feature amenable to future observational tests.

  14. Pi of the Sky preparations for LSC-Virgo's electromagnetic follow-up project

    NASA Astrophysics Data System (ADS)

    ZadroŻny, Adam; Sokołowski, Marcin; Majcher, Ariel; Opiela, Rafał; Obara, Łukasz

    2015-09-01

    The presentation focuses on plans of the Pi of the Sky collaboration to participate in the future LSC-Virgo's Electromagnetic (EM) Follow-up campaigns. Pi of the Sky telescope participated in the first "EM Follow-up project", called Looc-Up1-3 2009-2010 organized by LSC-Virgo collaboration. Pi of the Sky brought to the project an instrument with the biggest field of view and with a very high time resolution. Recently Pi of the Sky has signed an Memorandum of Understanding (MOU) with LSC-Virgo for EM Follow-up observations in the Advanced Detector Era (ADE). Plans of the Pi of the Sky telescope for joint observations with advanced LIGO and Virgo detectors will be also outlined.

  15. Appraising the value of independent EIA follow-up verifiers

    SciTech Connect

    Wessels, Jan-Albert

    2015-01-15

    Independent Environmental Impact Assessment (EIA) follow-up verifiers such as monitoring agencies, checkers, supervisors and control officers are active on various construction sites across the world. There are, however, differing views on the value that these verifiers add and very limited learning in EIA has been drawn from independent verifiers. This paper aims to appraise how and to what extent independent EIA follow-up verifiers add value in major construction projects in the developing country context of South Africa. A framework for appraising the role of independent verifiers was established and four South African case studies were examined through a mixture of site visits, project document analysis, and interviews. Appraisal results were documented in the performance areas of: planning, doing, checking, acting, public participating and integration with other programs. The results indicate that independent verifiers add most value to major construction projects when involved with screening EIA requirements of new projects, allocation of financial and human resources, checking legal compliance, influencing implementation, reporting conformance results, community and stakeholder engagement, integration with self-responsibility programs such as environmental management systems (EMS), and controlling records. It was apparent that verifiers could be more creatively utilized in pre-construction preparation, providing feedback of knowledge into assessment of new projects, giving input to the planning and design phase of projects, and performance evaluation. The study confirms the benefits of proponent and regulator follow-up, specifically in having independent verifiers that disclose information, facilitate discussion among stakeholders, are adaptable and proactive, aid in the integration of EIA with other programs, and instill trust in EIA enforcement by conformance evaluation. Overall, the study provides insight on how to harness the learning opportunities

  16. Automated Telecommunication to Obtain Longitudinal Follow-up in a Multicenter Cross-sectional COPD Study

    PubMed Central

    Stewart, Jeffrey I.; Moyle, Sarah; Criner, Gerard J.; Wilson, Carla; Tanner, Ron; Bowler, Russell P.; Crapo, James D.; Zeldin, Robert K.; Make, Barry J.; Regan, Elizabeth A.

    2013-01-01

    Background It can be challenging to maintain longitudinal follow-up of subjects in clinical studies. COPDGene is a multicenter, observational study designed to identify genetic factors associated with COPD and to characterize COPD-related phenotypes. To obtain follow-up data on patient's vital status and outcomes, the COPDGene Longitudinal Follow-up (LFU) Program was developed to supplement its parent study. Methods/Results We used a telecommunication system that employed automated telephone contact or web-based questions to obtain longitudinal follow-up data in our subjects. A branching questionnaire asked about exacerbations, new therapies, smoking status, development of co-morbid conditions, and general health status. Study coordinators contacted subjects who did not respond to one of the automated methods. We enrolled 10,383 subjects in the COPDGene study. As of August 29, 2011, 7,959 subjects completed 19,955 surveys. On the first survey, 68.8% of subjects who completed their survey did so by electronic means, while 31.3% required coordinator phone follow-up. On each subsequent survey the number of subjects who completed their survey by electronic means increased, while the number of subjects who required coordinator follow-up decreased. Despite many of the patients in the cohort being chronically ill and elderly, there was broad acceptance of the system with over half the cohort using electronic response methods. Conclusions The COPDGene LFU Study demonstrated that telecommunications was an effective way to obtain longitudinal follow-up of subjects in a large multicenter study. Web-based and automated phone contacts are accepted by research subjects and could serve as a model for LFU in future studies. PMID:22676387

  17. AN IMAGING AND SPECTROSCOPIC STUDY OF FOUR STRONG Mg II ABSORBERS REVEALED BY GRB 060418

    SciTech Connect

    Pollack, L. K.; Prochaska, J. X.; Chen, H.-W.; Bloom, J. S.

    2009-08-20

    We present results from an imaging and spectroscopic study of four strong Mg II absorbers of W(2796) {approx}> 1 A revealed by the afterglow of GRB 060418 at z{sub GRB} = 1.491. These absorbers, at z = 0.603, 0.656, 1.107, and z {sub GRB}, exhibit large ion abundances that suggest neutral gas columns characteristic of damped Ly{alpha} systems. The imaging data include optical images obtained using Low-Resolution Imaging Spectrometer (LRIS) on the Keck I telescope and using Advanced Camera for Surveys on board Hubble Space Telescope, and near-infrared H-band images obtained using Persson's Auxiliary Nasmyth Infrared Camera on the Magellan Baade Telescope and K'-band images obtained using NIRC2 with laser guide star adaptive optics on the Keck II telescope. These images reveal six distinct objects at {delta} {theta} {approx}< 3.''5 of the afterglow's position, two of which exhibit well-resolved mature disk morphology, one shows red colors, and three are blue compact sources. Follow-up spectroscopic observations using LRIS confirm that one of the disk galaxies coincides with the Mg II absorber at z = 0.656. The observed broadband spectral energy distributions of the second disk galaxy and the red source indicate that they are associated with the absorbers at z = 0.603 and z = 1.107, respectively. These results show that strong Mg II absorbers identified in gamma-ray burst (GRB) afterglow spectra are associated with typical galaxies of luminosity {approx}0.1 - 1 L{sub *} at impact parameter of {rho} {approx}< 10 h {sup -1} kpc. The close angular separation would preclude easy detections toward a bright quasar. Finally, we associate the remaining three blue compact sources with the GRB host galaxy, noting that they are likely star-forming knots located at projected distances of {rho} = 2 - 12 h {sup -1} kpc from the afterglow. At the afterglow's position, we derive a 2{sigma} upper limit to the underlying star-formation rate intensity of 0.0074 M{sub sun} yr{sup -1} kpc

  18. A follow-up study of neurobehavioral functions in welders exposed to manganese.

    PubMed

    Ellingsen, Dag G; Chashchin, Maxim; Bast-Pettersen, Rita; Zibarev, Evgenij; Thomassen, Yngvar; Chashchin, Valery

    2015-03-01

    Welders may be exposed to high amounts of manganese (Mn). In this study 63 welders and 65 referents were followed up with neurobehavioral tests approximately 6 years after the initial examination at baseline. The welders were exposed to the geometric mean (GM) Mn concentration of 116μg/m(3) at baseline and 148μg/m(3) at follow-up. Their mean duration of employments as welders was 19.5 years at follow-up. Being exposed as a welder was associated with a decline between baseline and follow-up in the performance on the Static Steadiness Test, Finger Tapping Test and Grooved Pegboard Test. However, the decline was also associated with having high concentrations of carbohydrate deficient transferrin in serum (sCDT), indicating high alcohol consumption. When subjects with sCDT above the upper reference limit of the laboratory (≥1.7%) were excluded from the analyses, no difference in the decline in performance was observed between welders and referents for any of the applied neurobehavioral tests. Three welders had developed bradykinesia at follow-up, as assessed by a substantial decline in their Finger Tapping Test performance. They had also experienced a severe decline in Foot Tapping, Grooved Pegboard and Postural Sway Test scores (while blindfolded), while postural tremor as assessed with the CATSYS Tremor 7.0 was normal. Their neurobehavioral test performance at baseline 6 years previously had been normal.

  19. Follow-up of patients with epidemic poststreptococcal glomerulonephritis.

    PubMed

    Pinto, S W; Sesso, R; Vasconcelos, E; Watanabe, Y J; Pansute, A M

    2001-08-01

    In 1998 there was a large outbreak of acute glomerulonephritis (GN) in Nova Serrana, Brazil, caused by group C Streptococcus zooepidemicus and linked to the consumption of contaminated cheese produced with unpasteurized milk. This study describes the follow-up of these patients after a mean of 2 years following the acute episode. Of 134 patients identified in 1998, 69 patients were reexamined and underwent measurements of blood pressure, 24-hour creatinine clearance, microalbuminuria (radioimmunoassay), and urine sediment analysis. Of the original group of 134 patients, 3 patients died in the acute phase and 5 patients (3.7%) required chronic dialysis. Of 69 patients reevaluated, 65 patients (94%) were adults (mean age, 39 +/- 2 [SE] years) and 47 patients (68%) were women. At the follow-up examination, we found arterial hypertension in 42% of subjects (27 of 64 subjects), serum creatinine levels greater than 1.2 mg/dL in 12% (10 of 68 subjects), reduced creatinine clearance (<80 mL/min/1.73 m(2)) in 30% (20 of 67 subjects, 2 of them on chronic dialysis therapy), and increased microalbuminuria (>20 microg/min) in 34% (22 of 65 subjects). Increased microalbuminuria and/or reduced creatinine clearance were detected in 48% of the subjects (31 of 65 subjects). Patients with microalbuminuria had greater diastolic blood pressure than those without microalbuminuria (mean, 98 +/- 4 versus 88 +/- 2 mm Hg; P = 0.02). In conclusion, after a mean of 2 years, patients with epidemic poststreptococcal GN caused by S zooepidemicus present a high rate of hypertension and frequent abnormalities of renal function, with some having reached end-stage renal disease. Longer follow-up will be important to define the prognosis of these patients.

  20. Shillapoo Wildlife Area 2007 Follow-up HEP Report.

    SciTech Connect

    Ashley, Paul R.

    2008-03-01

    In April and May 2007 the Regional HEP Team (RHT) conducted a follow-up HEP analysis on the Egger (612 acres) and Herzog (210 acres) parcels located at the north end of the Shillapoo Wildlife Area. The Egger and Herzog parcels have been managed with Bonneville Power Administration funds since acquired in 1998 and 2001 respectively. Slightly more than 936 habitat units (936.47) or 1.14 HUs per acre was generated as an outcome of the 2007 follow-up HEP surveys. Results included 1.65 black-capped chickadee HUs, 280.57 great blue heron HUs, 581.45 Canada goose HUs, 40 mallard HUs, and 32.80 mink HUs. Introduction A follow-up Habitat Evaluation Procedures (HEP) (USFWS 1980) analysis was conducted by the Columbia Basin Fish and Wildlife Authority's (CBFWA) Regional HEP Team (RHT) during April and May 2007 to document changes in habitat quality and to determine the number of habitat units (HUs) to credit Bonneville Power Administration (BPA) for providing operation and maintenance (O&M) funds since WDFW acquired the parcels. The 2007 follow-up HEP evaluation was limited to Shillapoo Wildlife Area (SWA) parcels purchased with Bonneville Power Administration funds. D. Budd (pers. comm.) reported WDFW purchased the 612 acre Egger Farms parcel on November 2, 1998 for $1,737,0001 and the 210 acre Herzog acquisition on June 21, 2001 for $500,000 with Memorandum of Agreement funds (BPA and WDFW 1996) as partial fulfillment of BPA's wildlife mitigation obligation for construction of Bonneville and John Day Dams (Rasmussen and Wright 1989). Anticipating the eventual acquisition of the Egger and Herzog properties, WDFW conducted HEP surveys on these lands in 1994 to determine the potential number of habitat units to be credited to BPA. As a result, HEP surveys and habitat unit calculations were completed as much as seven years prior to acquiring the sites. The term 'Shillapoo Wildlife Area' will be used to describe only the Herzog and Egger parcels in this document. Details and

  1. Follow-up problems with fixed appliances in pediatric dentistry.

    PubMed

    Ari, Timucin

    2015-03-01

    Fixed appliances are commonly used in managing early orthodontic problems. Despite their widespread use, they have the potential to impinge on the soft tissues, interfere with the eruption of adjacent teeth and become dislodged or broken. These two case reports present the poor outcomes of fixed appliance treatments if the patient fails to attend follow-up appointments. A successful outcome of treatment with fixed appliances depends upon proper patient selection and the communication skills of the dentist to help patients/parents understand the importance of regular checkups. PMID:25928968

  2. [Ataxia telangiectasia. Diagnosis and follow-up in 4 cases].

    PubMed

    Monterrubio Ledezma, César Eduardo; Corona Rivera, Alfredo; Corona Rivera, Jorge Román; Rodríguez Casillas, Lourdes Jocelyn; Hernández Rocha, Juan; Barros Nuñez, Patricio; Bobadilla Morales, Lucina

    2013-01-01

    Ataxia telangiectasia (AT) is a chromosomal instability syndrome with autosomal recessive inheritance, it is caused by more than 500 mutations of the ATM gene, which is involved in the cellular response to DNA damage. The diagnosis becomes difficult due to the evolution of the disease, their poor knowledge, and limited access to diagnostic tests. Chromosomal damage induced by ionizing radiation (IR) assay is still a sensitive method for early diagnosis, and it is essential for better management and genetic counseling. This paper shows diagnosis and follow-up in four cases with AT. PMID:23999637

  3. The Achromatic Light Curve of the Optical Afterglow of GRB 030226 at a Redshift of z Approximately 2

    NASA Technical Reports Server (NTRS)

    Klose, S.; Greiner, J.; Rau, A.; Henden, A. A.; Hartmann, D. H.; Zeh, A.; Masetti, N.; Guenther, E.; Stecklum, B.; Lindsay, K.

    2003-01-01

    Abstract. We report on optical and near-infrared (NIR) follow-up observations of the afterglow of GRB 030226, mainly performed with the telescopes at ESO La Silla and Paranal, with additional data obtained at other places. Our first observations started 0.2 days after the burst when the afterglow was at a magnitude of R approximately equal to 19 . One week later the magnitude of the afterglow had fallen to R=25, and at two weeks after the burst it could no longer be detected (R > 26). Our VLT blueband spectra show two absorption line systems at redshifts z = 1.962 +/- 0.001 and at z = 1.986 +/- 0.001, placing the redshift of the burster close to 2. Within our measurement errors no evidence for variations in the line strengths has been found between 0.2 and 1.2 days after the burst. An overabundance of alpha-group elements might indicate that the burst occurred in a chemically young interstellar region shaped by the nucleosynthesis from type II supernovae. The spectral slope of the afterglow shows no signs for cosmic dust along the line of sight in the GRB host galaxy, which itself remained undetected (R > 26.2). At the given redshift no supernova component affected the light from the GRB afterglow, so that the optical transient was essentially only powered by the radiation from the GRB fireball, allowing for a detailed investigation of the color evolution of the afterglow light. In our data set no obvious evidence for color changes has been found before, during, or after the smooth break in the light curve approximately 1 day after the burst. In comparison with investigations by others, our data favor the interpretation that the afterglow began to develop into a homogeneous interstellar medium before the break in the light curve became apparent.

  4. Liverpool Telescope follow-up of candidate electromagnetic counterparts during the first run of Advanced LIGO

    NASA Astrophysics Data System (ADS)

    Copperwheat, C. M.; Steele, I. A.; Piascik, A. S.; Bersier, D.; Bode, M. F.; Collins, C. A.; Darnley, M. J.; Galloway, D. K.; Gomboc, A.; Kobayashi, S.; Lamb, G. P.; Levan, A. J.; Mazzali, P. A.; Mundell, C. G.; Pian, E.; Pollacco, D.; Steeghs, D.; Tanvir, N. R.; Ulaczyk, K.; Wiersema, K.

    2016-11-01

    The first direct detection of gravitational waves was made in 2015 September with the Advanced LIGO detectors. By prior arrangement, a worldwide collaboration of electromagnetic follow-up observers were notified of candidate gravitational wave events during the first science run, and many facilities were engaged in the search for counterparts. Three alerts were issued to the electromagnetic collaboration over the course of the first science run, which lasted from 2015 September to 2016 January. Two of these alerts were associated with the gravitational wave events since named GW150914 and GW151226. In this paper we provide an overview of the Liverpool Telescope contribution to the follow-up campaign over this period. Given the hundreds of square degree uncertainty in the sky position of any gravitational wave event, efficient searching for candidate counterparts required survey telescopes with large (˜degrees) fields of view. The role of the Liverpool Telescope was to provide follow-up classification spectroscopy of any candidates. We followed candidates associated with all three alerts, observing 1, 9 and 17 candidates respectively. We classify the majority of the transients we observed as supernovae. No counterparts were identified, which is in line with expectations given that the events were classified as black hole-black hole mergers. However these searches laid the foundation for similar follow-up campaigns in future gravitational wave detector science runs, in which the detection of neutron star merger events with observable electromagnetic counterparts is much more likely.

  5. Photometric Follow-Up of A Likely Galactic Nova ASASSN-16kt: Almost Naked Eye

    NASA Astrophysics Data System (ADS)

    Chen, Ping; Dong, Subo; Bose, S.; Stanek, K. Z.; Kochanek, C. S.; Brown, J. S.; Holoien, T. W.-S.; Shields, J.; Shappee, B. J.; Prieto, J. L.; Bersier, D.; Chomiuk, L.; Strader, J.; Brimacombe, J.

    2016-09-01

    We obtained follow-up photometric observations of ASASSN-16kt (ATel #9538 & ATel #9539) with LCOGT 1m telescope at Sutherland, South Africa (SAAO). We performed aperture photometry on the images using the IRAF apphot package and calibrated the results using the AAVSO Photometric All-Sky Survey (APASS; Henden et al. 2015).

  6. Radio Follow-up of Gravitational-wave Triggers during Advanced LIGO O1

    NASA Astrophysics Data System (ADS)

    Palliyaguru, N. T.; Corsi, A.; Kasliwal, M. M.; Cenko, S. B.; Frail, D. A.; Perley, D. A.; Mishra, N.; Singer, L. P.; Gal-Yam, A.; Nugent, P. E.; Surace, J. A.

    2016-10-01

    We present radio follow-up observations carried out with the Karl G. Jansky Very Large Array during the first observing run (O1) of the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO). A total of three gravitational-wave triggers were followed-up during the ≈ 4 months of O1, from 2015 September to 2016 January. Two of these triggers, GW150914 and GW151226, are binary black hole (BH) merger events of high significance. A third trigger, G194575, was subsequently declared as an event of no interest (i.e., a false alarm). Our observations targeted selected optical transients identified by the intermediate Palomar Transient Factory in the Advanced LIGO error regions of the three triggers, and a limited region of the gravitational-wave localization area of G194575 not accessible to optical telescopes due to Sun constraints, where a possible high-energy transient was identified. No plausible radio counterparts to GW150914 and GW151226 were found, in agreement with expectations for binary BH mergers. We show that combining optical and radio observations is key to identifying contaminating radio sources that may be found in the follow-up of gravitational-wave triggers, such as emission associated with star formation and active galactic nuclei. We discuss our results in the context of the theoretical predictions for radio counterparts to gravitational-wave transients, and describe our future plans for the radio follow-up of Advanced LIGO (and Virgo) triggers.

  7. Follow-up Photometry of the Galactic Nova ASASSN-16kt

    NASA Astrophysics Data System (ADS)

    Prieto, J. L.

    2016-09-01

    We obtained follow-up photometry of the Galactic Nova ASASSN-16kt (ATel #9538, #9539, #9550; CBET #4322) with a Celestron NexStar 4" telescope and a Canon EOS 300D camera observing from downtown Santiago (Chile), through variable clouds, on UT 2016 September 28.98 (JD = 2457660.47986).

  8. How Can The SN-GRB Time Delay Be Measured?

    NASA Technical Reports Server (NTRS)

    Norris, J. P.; Bonnell, J. T.

    2003-01-01

    The connection between SNe and GRBs, launched by SN 1998bw / GRB 980425 and clinched by SN 2003dh / GRB 030329-with the two GRBs differing by a factor of approximately 50000 in luminosity-so far suggests a rough upper limit of approximately 1-2 days for the delay between SN and GRB. Only four SNe have had nonnegligible coverage in close coincidence with the initial explosion, near the W shock breakout: two Qpe II, and two Type IC, SN 1999ex and SN 1998bw. For the latter, only a hint of the minimum between the UV maximum and the radioactivity bump served to help constrain the interval between SN and GRB. Swift GRB alerts may provide the opportunity to study many SNe through the UV breakout phase: GRB 980425 look dikes -apparently nearby, low- luminosity, soft-spectrum, long-lag GRBs-accounted for half of BATSE bursts near threshold, and may dominate the Swift yield near threshold, since it has sensitivity to lower energies than did BATSE. The SN to GRB delay timescale should be better constrained by prompt UV/optical observations alerted by these bursts. Definitive delay measurements may be obtained if long-lag bursters are truly nearby: The SNe/GRBs could emit gravitational radiation detectable by LIGO-II if robust non-axisymmetric bar instabilities develop during core collapse, and/or neutrino emission may be detectable as suggested by Meszaros et al.

  9. What Happens in Classrooms after Earth Science Fieldwork? Supporting Student Learning Processes during Follow-Up Activities

    ERIC Educational Resources Information Center

    Remmen, Kari Beate; Frøyland, Merethe

    2015-01-01

    Follow-up activities after fieldwork are recommended, yet little research has been conducted in this area. This study investigates six cases of follow-up work carried out by three teachers and their students in three upper secondary schools in Norway. The data comprises video observations of teachers and students, instructional artifacts,…

  10. Follow-up of children of drug-addicted mothers.

    PubMed Central

    Sardemann, H; Madsen, K S; Friis-Hansen, B

    1976-01-01

    During a period of 2 years (1971-72) 19 newborn infants were admitted to hospital because their mothers were drug addicts. To evaluate the prognosis in these children, 17 were followed up by a social adviser, a psychologist, and a paediatrician. During the neonatal period 16 of the infants had withdrawal symptoms, for which 11 required medical treatment. One infant died of congenital malformations. Of the surviving 18 infants 14 were discharged to their mothers and 4 went to a children's home. During follow-up, which varied from up to 2 months to up to 2 years 8 months of age, 10 of the children had to be placed in a children's home for a period. No physical abnormalities were found in the children. Motor and perceptual development were normal in 12 but in 3 speech development was delayed. Five mothers ceased to take drugs after delivery and 2 had done so during early pregnancy. The pre- and perinatal complications and the undesirable environment in which the children grow up show the need for a comprehensive treatment programme. PMID:1259458

  11. Gastric and Duodenal Stents: Follow-Up and Complications

    SciTech Connect

    Pinto Pabon, Isabel Teresa; Paul Diaz, Laura; Ruiz de Adana, Juan Carlos; Lopez Herrero, Julio

    2001-05-15

    Purpose: To assess the efficacy of self-expanding metallic stents in treating inoperable gastric and duodenal stenoses during follow-up and to evaluate the complications encountered.Methods: A total of 31 patients suffering from gastroduodenal obstruction (29 malignant, 2 benign) were treated with a self-expanding metallic stent (Wallstent). In 24 cases insertion was by the peroral route, in seven cases via gastrostomy.Results: All the strictures were successfully negotiated under fluoroscopic guidance without having to resort to endoscopy. A total of 27 patients (87%) were able to resume a regular diet, a soft diet, or a liquid diet orally. Complications included one case of stent malpositioning, one case of leakage of ascitic fluid through the gastrostomy orifice, one case of perforation and fistula to the biliary tree, and two cases of hematemesis. In two patients (6%) additional stents were implanted to improve patency. In all patients follow-up was maintained until death. Recurrence of symptoms immediately before death occurred in seven cases (23%). Mean survival time of patients was 13.3 weeks (SE {+-} 4.6).Conclusions: The deployment of gastroduodenal stents resulted in good palliation of inoperable gastric and duodenal stenoses. Certain technical aspects, e.g., adaptation of stents to bowel morphology, is critical to proper stent function and avoidance of complications.

  12. [The follow up of patients with bronchial carcinoma (author's transl)].

    PubMed

    Wilde, J

    1980-01-01

    The aims of follow up of patients with bronchial carcinoma are: 1. Complete use of all therapeutical possibilities. 2. Avoidance of preventable complications of therapeutical prescriptions. 3. Prevention of sicknesses beside the basic complaint. 4. The rehabilitation of the patient. The medical structure for realizing these aims, we suppose in the cooperation of the doctor of the family or the factory, who will see the patient in intervals of four weeks, and the ambulant working pulmologist, who will see the patient in intervals of 3 months, and the thorax-centre, what the patient will consult once or twice the year, and the centre for rehabilitation, where patients with limited cardiorespiratoric function will get an appropriated training of condition. Two cure-places with this special direction will satisfy the require in the GDR. The oncologist of the district where the patient lives will be the coordinator of all parts of this system and the controller to keep its function. The effectivity of follow up will be realised by clear and proofed recommendations by the therapeutical centres and the continued consultations on actual problem cases with the shared doctors. The data processing can do an useful help in this cooperation. PMID:6261467

  13. The AAVSO International GRB Network

    NASA Astrophysics Data System (ADS)

    Price, Aaron

    2003-04-01

    The AAVSO International GRB Network provides services to both amateurs and professionals to help detect GRB afterglows. The network leverages the unique abilities of amateur astronomers to offer global coverage to eliminate geographic and climatic restrictions to GRB alert reaction times. Additionally, public outreach is a critical component of the network and automated online chart making procedures have made it a useful tool for professionals. The financial support of NASA and the Curry Foundation is gratefully appreciated.

  14. Improving pediatric Inflammatory Bowel Disease (IBD) follow-up.

    PubMed

    Dykes, Dana; Williams, Elizabeth; Margolis, Peter; Ruschman, Jennifer; Bick, Julianne; Saeed, Shehzad; Opipari, Lisa

    2016-01-01

    Standardization of Inflammatory Bowel Disease (IBD) care through participation in the ImproveCareNow (ICN) Network has improved outcomes for pediatric patients with IBD, but under the current care model, our improvements have plateaued. Current ICN model care guidelines recommend health supervision visits every six months. We identified a gap in our practice's ability to ensure either a routine six month follow-up or a rapid follow-up after a disease flare, and a significant number of patients with active disease status during a six month period lacked timely reassessment after interventions or medication changes. Telemedicine provides an alternative method of care delivery to address these gaps, but has had limited use in patients with IBD. A multi-step approach to offer alternative follow-up care options via telemedicine was developed with potential impact on remission rates and quality of life. Short term goals of the pilot were to improve telemedicine access for patients with IBD were to 1) increase the percent of patients with active disease with a follow-up completed within two months of a visit from 40% to 70%, 2) increase the percent of patients with a visit scheduled within two months of their last sick visit from 20% to 70% (interim measure), 3) increase the number of eVisits from zero visits per month to two visits per month during pilot phase, 4) increase electronic communication with patients from zero messages per month to 200 messages per month, 5) no change in complications or adverse events (defined as an unplanned visit or ED (emergency department) encounter within 30 days of an eVisit. The expected outcomes of the e-visit model were to: maintain baseline care standards and health screening capabilities, improve access to care, and provide equivalent care delivery (no increase in the number of unplanned clinical encounters). Using the IHI model for improvement (Plan-Do-Study-Act) we have seen a progressive increase in the rate of patient signups

  15. Improving pediatric Inflammatory Bowel Disease (IBD) follow-up

    PubMed Central

    Dykes, Dana; Williams, Elizabeth; Margolis, Peter; Ruschman, Jennifer; Bick, Julianne; Saeed, Shehzad; Opipari, Lisa

    2016-01-01

    Standardization of Inflammatory Bowel Disease (IBD) care through participation in the ImproveCareNow (ICN) Network has improved outcomes for pediatric patients with IBD, but under the current care model, our improvements have plateaued. Current ICN model care guidelines recommend health supervision visits every six months. We identified a gap in our practice's ability to ensure either a routine six month follow-up or a rapid follow-up after a disease flare, and a significant number of patients with active disease status during a six month period lacked timely reassessment after interventions or medication changes. Telemedicine provides an alternative method of care delivery to address these gaps, but has had limited use in patients with IBD. A multi-step approach to offer alternative follow-up care options via telemedicine was developed with potential impact on remission rates and quality of life. Short term goals of the pilot were to improve telemedicine access for patients with IBD were to 1) increase the percent of patients with active disease with a follow-up completed within two months of a visit from 40% to 70%, 2) increase the percent of patients with a visit scheduled within two months of their last sick visit from 20% to 70% (interim measure), 3) increase the number of eVisits from zero visits per month to two visits per month during pilot phase, 4) increase electronic communication with patients from zero messages per month to 200 messages per month, 5) no change in complications or adverse events (defined as an unplanned visit or ED (emergency department) encounter within 30 days of an eVisit. The expected outcomes of the e-visit model were to: maintain baseline care standards and health screening capabilities, improve access to care, and provide equivalent care delivery (no increase in the number of unplanned clinical encounters). Using the IHI model for improvement (Plan-Do-Study-Act) we have seen a progressive increase in the rate of patient signups

  16. Long-Term Follow-Up of Iliac Wallstents

    SciTech Connect

    Reyes, Ricardo; Carreira, Jose Martin Gude, Francisco; Gorriz, Elias; Gallardo, Laura; Pardo, Maria Dolores; Hermida, Maria

    2004-11-15

    We evaluated the long-term results of the iliac artery stent placement for the treatment of patients with intermittent claudication. From November 1988 to December 1998, 303 legs were treated with metal stents in 259 patients with iliac occlusive arterial disease in a follow-up study approved by the institutional review board. Stenoses (n = 162) were treated after failed angioplasty and occlusions (n = 141) were treated with primary stent placement. According to Fontaine's clinical classification of chronic ischemia, 266 (88%) legs presented stage IIB, 14 (5%) stage III, and 23 (7%) stage IV. In all legs, self-expandable stents (Wallstent) were implanted. The patients were followed up with clinical examination, ankle brachial- index examination measurement and intravenous angiography. The data were analyzed using the univariate analysis (Kaplan-Meier method) and multivariate analysis (Cox proportional model). The primary endpoint of the study was the identification of restenosis or reoclusion of the stenting arterial segment and a secondary endpoint that was an identification of the risk factors of restenosis and reoclusion. The mean {+-} SD ankle-brachial index pre-, post-procedure, and in the last control was 0.58 {+-} 0.18, 0.90 {+-} 0.23, and 0.86 {+-} 0.24, respectively. Primary cumulative patency rates were 70% {+-} 4 after 5 years, and 65% {+-} 5 after 7 years, and secondary patency rates were 92% {+-} 2 after 5 years, and 87% {+-} 4 after 9 years. Immediate complications in the first 24 hours appeared in 12 (4%) legs, thrombosis in 5 legs, 3 legs presented with distal embolism, 2 thrombi at the access site and pseudo aneurysm and artery rupture in 1 leg. A patient died in the first 24 hours. Within 30 days after the procedure seven complications, 3 thromboses and 4 stenosis appeared. During follow-up, 42 (16%) patients died of other causes. The main causes of death were cardiac disease (39%), cerebrovascular disease (15%), cancer (7%), respiratory diseases

  17. CONSTRAINING GAMMA-RAY BURST EMISSION PHYSICS WITH EXTENSIVE EARLY-TIME, MULTIBAND FOLLOW-UP

    SciTech Connect

    Cucchiara, A.; Cenko, S. B.; Bloom, J. S.; Morgan, A.; Perley, D. A.; Li, W.; Butler, N. R.; Filippenko, A. V.; Melandri, A.; Kobayashi, S.; Smith, R. J.; Mundell, C. G.; Steele, I. A.; Hora, J. L.; Da Silva, R. L.; Prochaska, J. X.; Worseck, G.; Fumagalli, M.; Cobb, B.; and others

    2011-12-20

    Understanding the origin and diversity of emission processes responsible for gamma-ray bursts (GRBs) remains a pressing challenge. While prompt and contemporaneous panchromatic observations have the potential to test predictions of the internal-external shock model, extensive multiband imaging has been conducted for only a few GRBs. We present rich, early-time, multiband data sets for two Swift events, GRB 110205A and GRB 110213A. The former shows optical emission since the early stages of the prompt phase, followed by the steep rising in flux up to {approx}1000 s after the burst (t{sup -{alpha}} with {alpha} = -6.13 {+-} 0.75). We discuss this feature in the context of the reverse-shock scenario and interpret the following single power-law decay as being forward-shock dominated. Polarization measurements, obtained with the RINGO2 instrument mounted on the Liverpool Telescope, also provide hints on the nature of the emitting ejecta. The latter event, instead, displays a very peculiar optical to near-infrared light curve, with two achromatic peaks. In this case, while the first peak is probably due to the onset of the afterglow, we interpret the second peak to be produced by newly injected material, signifying a late-time activity of the central engine.

  18. A Bulk Comptonization Model for the Prompt GRB Emission and its Relation to the Fermi GRB Spectra

    NASA Technical Reports Server (NTRS)

    Kazanas, Demosthenes

    2010-01-01

    We present a model in which the GRB prompt emission at E E(sub peak) is due to bulk Comptonization by the relativistic blast wave motion of either its own synchrotron photons of ambient photons of the stellar configuration that gave birth to the GRB. The bulk Comptonization process then induces the production of relativistic electrons of Lorentz factor equal to that of the blast wave through interactions with its ambient protons. The inverse compton emission of these electrons produces a power law component that extends to multi GeV energies in good agreement with the LAT GRB observations.

  19. ALMA SUBMILLIMETER CONTINUUM IMAGING OF THE HOST GALAXIES OF GRB 021004 AND GRB 080607

    SciTech Connect

    Wang, Wei-Hao; Huang, Kui-Yun; Chen, Hsiao-Wen

    2012-12-20

    We report 345 GHz continuum observations of the host galaxies of gamma-ray bursts (GRBs) 021004 and 080607 at z > 2 using the Atacama Large Millimeter/Submillimeter Array (ALMA) in Cycle 0. Of the two bursts, GRB 021004 is one of the few GRBs that originate in a Lyman limit host, while GRB 080607 is classified as a 'dark burst' and its host galaxy is a candidate of dusty star-forming galaxy at z {approx} 3. With an order of magnitude improvement in the sensitivities of the new imaging searches, we detect the host galaxy of GRB 080607 with a flux of S{sub 345} = 0.31 {+-} 0.09 mJy and a corresponding infrared luminosity of L{sub IR} = (2.4-4.5) Multiplication-Sign 10{sup 11} L{sub Sun }. However, the host galaxy of GRB 021004 remains undetected and the ALMA observations allow us to place a 3{sigma} upper limit of L{sub IR} < 3.1 Multiplication-Sign 10{sup 11} L{sub Sun} for the host galaxy. The continuum imaging observations show that the two galaxies are not ultraluminous infrared galaxies, but are at the faintest end of the dusty galaxy population that gives rise to the submillimeter extragalactic background light. The derived star formation rates of the two GRB host galaxies are less than 100 M{sub Sun} yr{sup -1}, which are broadly consistent with optical measurements. The result suggests that the large extinction (A{sub V} {approx} 3) in the afterglow of GRB 080607 is confined along its particularly dusty sight line, and not representative of the global properties of the host galaxy.

  20. Follow-up of adolescent oral contraceptive users.

    PubMed

    Delmore, T; Kalagian, W F; Loewen, I R

    1991-01-01

    Clients in birth control centers (St. Catharines, Niagara Falls, and Welland) in Ontario, Canada were profiled in 1989; factors affecting compliance with the use of oral contraceptives (OCs) were investigated. Compliance was assessed for those 16 years and after 3 months of OC use. A control group and 2 study groups were randomly formed. 1 group was told about a follow up telephone call if the 3-month checkup appointment was not kept and the other not told. Compliance was determined by keeping the follow-up appointment and taking the pill as directed. Self-administered questionnaires were obtained at the 1st appointment and the 2nd study group was interviewed at the 3-month appointment time. Of the 334 intake interviews, 28.4% were adolescents 16 years old. Information on birth control came most frequently from friends (78.7%; then high school classmates, 61.4% grade school classmates, 61.4%; and family, 38.0%). 94.3% had a boyfriend, primarily a steady one. 82.4% were sexually active before the Center visit. 21.3% had had sex when 15 years old. 9.2% of those sexually active had never used birth control. 85.2% of those using contraception had used a condom at least once, and 33.9% used withdrawal. In the preceding month, birth control was used 60% of the time. 46% of mothers and 25% of fathers were considered supportive of birth control. 228 16 years participated in the compliance study. The 2 study groups and the control group were not significantly different in their compliance. The only statistically significant predictor of compliance (from the intake interview) was the previous use of the condom. Those more likely to be compliant were the 10.9% sexually active who had never used a condom. Continuing with the family doctor, not sexually active, advice to stop, side effects concerns, and remembering to take the pill were the most common reasons for noncompliance. The implication for health and sex education is that emphasis needs to the placed on the risks taken

  1. Long-term Follow-up After Bariatric Surgery

    PubMed Central

    Puzziferri, Nancy; Roshek, Thomas B.; Mayo, Helen G.; Gallagher, Ryan; Belle, Steven H.; Livingston, Edward H.

    2015-01-01

    IMPORTANCE Bariatric surgery is an accepted treatment for obesity. Despite extensive literature, few studies report long-term follow-up in cohorts with adequate retention rates. OBJECTIVE To assess the quality of evidence and treatment effectiveness 2 years after bariatric procedures for weight loss, type 2 diabetes, hypertension, and hyperlipidemia in severely obese adults. EVIDENCE REVIEW MEDLINE and Cochrane databases were searched from 1946 through May 15, 2014. Search terms included bariatric surgery, individual bariatric procedures, and obesity. Studies were included if they described outcomes for gastric bypass, gastric band, or sleeve gastrectomy performed on patients with a body mass index of 35 or greater, had more than 2 years of outcome information, and had follow-up measures for at least 80% of the initial cohort. Two investigators reviewed each study and a third resolved study inclusion disagreements. FINDINGS Of 7371 clinical studies reviewed, 29 studies (0.4%, 7971 patients) met inclusion criteria. All gastric bypass studies (6 prospective cohorts, 5 retrospective cohorts) and sleeve gastrectomy studies (2 retrospective cohorts) had 95% confidence intervals for the reported mean, median, or both exceeding 50% excess weight loss. This amount of excess weight loss occurred in 31% of gastric band studies (9 prospective cohorts, 5 retrospective cohorts). The mean sample-size–weighted percentage of excess weight loss for gastric bypass was 65.7% (n = 3544) vs 45.0% (n = 4109) for gastric band. Nine studies measured comorbidity improvement. For type 2 diabetes (glycated hemoglobin <6.5% without medication), sample-size–weighted remission rates were 66.7% for gastric bypass (n = 428) and 28.6% for gastric band (n = 96). For hypertension (blood pressure <140/90 mm Hg without medication), remission rates were 38.2% for gastric bypass (n = 808) and 17.4% for gastric band (n = 247). For hyperlipidemia (cholesterol <200 mg/dL, high-density lipoprotein >40

  2. Factors Associated with Follow-Up Attendance among Rape Victims Seen in Acute Medical Care

    PubMed Central

    Darnell, Doyanne; Peterson, Roselyn; Berliner, Lucy; Stewart, Terri; Russo, Joan; Whiteside, Lauren; Zatzick, Douglas

    2016-01-01

    Objective Rape is associated with Posttraumatic Stress Disorder and related comorbidities. Most victims do not obtain treatment for these conditions. Acute care medical settings are well-positioned to link patients to services; however, difficulty engaging victims and low attendance at provided follow-up appointments is well documented. Identifying factors associated with follow-up can inform engagement and linkage strategies. Method Administrative, patient self-report, and provider observational data from Harborview Medical Center were combined for the analysis. Using logistic regression, we examined factors associated with follow-up health service utilization after seeking services for rape in the emergency department. Results Of the 521 diverse female (n=476) and male (n=45) rape victims, 28% attended the recommended medical/counseling follow-up appointment. In the final (adjusted) logistic regression model, having a developmental or other disability (OR=0.40, 95% CI=0.21-0.77), having a current mental illness (OR=0.25, 95% CI=0.13-0.49), and being assaulted in public (OR=0.50, 95% CI=0.28-0.87) were uniquely associated with reduced odds of attending the follow-up. Having a prior mental health condition (OR= 3.02 95% CI=1.86-4.91), a completed SANE examination (OR=2.97, 95% CI=1.84-4.81), and social support available to help cope with the assault (OR=3.54, 95% CI=1.76-7.11) were associated with an increased odds of attending the follow-up. Conclusions Findings point to relevant characteristics ascertained at the acute care medical visit for rape that may be used to identify victims less likely to obtain posttraumatic medical and mental health services. Efforts to improve service linkage among these patients is warranted and may require alternative models to engage these patients to support posttraumatic recovery. PMID:26168030

  3. GRB 070724B: the first Gamma Ray Burst localized by SuperAGILE

    SciTech Connect

    Del Monte, E.; Costa, E.; Donnarumma, I.; Feroci, M.; Lapshov, I.; Lazzarotto, F.; Soffitta, P.; Argan, A.; Pucella, G.; Trois, A.; Vittorini, V.; Evangelista, Y.; Rapisarda, M.; Barbiellini, G.; Longo, F.; Basset, M.; Foggetta, L.; Vallazza, E.; Bulgarelli, A.; Di Cocco, G.

    2008-05-22

    GRB070724B is the first Gamma Ray Burst localized by the SuperAGILE instrument aboard the AGILE space mission. The SuperAGILE localization has been confirmed after the after-glow observation by the XRT aboard the Swift satellite. No significant gamma ray emission above 50 MeV has been detected for this GRB. In this paper we describe the SuperAGILE capabilities in detecting Gamma Ray Burst and the AGILE observation of GRB 070724B.

  4. Hydrotherapy after total knee arthroplasty. A follow-up study.

    PubMed

    Giaquinto, S; Ciotola, E; Dall'Armi, V; Margutti, F

    2010-01-01

    The study evaluated the subjective functional outcome following total knee arthroplasty (TKA) in participants who underwent hydrotherapy (HT) six months after discharge from a rehabilitation unit. A total of 70 subjects, 12 of which were lost at follow-up, were randomly assigned to either a conventional gym treatment (N=30) or HT (N=28). A prospective design was performed. Participants were interviewed with Western-Ontario McMasters Universities Osteoarthritis Index (WOMAC) at admission, at discharge and six months later. Kruskal-Wallis and Wilcoxon tests were applied for statistical analysis. Both groups improved. The WOMAC subscales, namely pain, stiffness and function, were all positively affected. Statistical analysis indicates that scores on all subscales were significantly lower for the HT group. The benefits gained by the time of discharge were still found after six months. HT is recommended after TKA in a geriatric population.

  5. [Neuromuscular disease: respiratory clinical assessment and follow-up].

    PubMed

    Martínez Carrasco, C; Villa Asensi, J R; Luna Paredes, M C; Osona Rodríguez de Torres, F B; Peña Zarza, J A; Larramona Carrera, H; Costa Colomer, J

    2014-10-01

    Patients with neuromuscular disease are an important group at risk of frequently suffering acute or chronic respiratory failure, which is their main cause of death. They require follow-up by a pediatric respiratory medicine specialist from birth or diagnosis in order to confirm the diagnosis and treat any respiratory complications within a multidisciplinary context. The ventilatory support and the cough assistance have improved the quality of life and long-term survival for many of these patients. In this paper, the authors review the pathophysiology, respiratory function evaluation, sleep disorders, and the most frequent respiratory complications in neuromuscular diseases. The various treatments used, from a respiratory medicine point of view, will be analyzed in a next paper.

  6. [The follow up of the women vaccinated against HPV].

    PubMed

    Riethmuller, D; Ramanah, R; Carcopino, X; Levêque, J

    2013-10-01

    HPV vaccine decreases significantly the risk of cervical cancer in women. However, continuing screening strategies in vaccinated women remains relevant as there is a small residual risk of cancer and pre-cancerous lesions even after prophylactic vaccination. The follow-up strategy to adopt has been the object of reflection by many experts, and especially since the vaccination catch-up population concerning women until 23 years of age will soon become the target screening population following recent guidelines. Finally, the arrival of HPV vaccines forces us to think about screening organization and optimization in a broader way so as it benefits all women concerned, whether vaccinated or not, and not only barely half of them as is the case now. The aim of this work was to clarify the issue and to make proposals for management.

  7. Follow-up studies of suspicious choroidal nevi.

    PubMed

    Mims, J L; Shields, J A

    1978-09-01

    The fundus photographs and fluorescein angiograms of 255 consecutive cases of choroidal nevi were reviewed. Sixty-one cases (24%) were selected as suspicious on the basis of strict preestablished criteria including greatest single diameter, elevation, degree of disruption of the retinal pigment epithelium, and presence of subretinal fluid. Fifty of these 61 had adequate four-year follow-up. The remaining 194 cases, labeled as nonsuspicious, were usually small, relatively flat, slate-grey nevi which failed to meet the criteria for being suspicious. Of the 50 suspicious choroidal nevi followed four years, five (10%) showed photographic evidence of growth 4 to 30 months after the last examination. In contrast, none of the 194 nonsuspicious cases demonstrated growth. On the basis of these results, recommendations are made for the management of suspicious choroidal nevi.

  8. Electro-clinical follow-up of shunted hydrocephalic children.

    PubMed

    Varfis, G; Berney, J; Beaumanoir, A

    1977-01-01

    In a survey of 29 hydrocephalic children treated by ventriculoatrial shunt (Holter valve) with a follow-up of 4 years, EEG records before the operation and at least once a year thereafter, the authors can support the view that an epileptogenic focus has developed around the place of insertion of the ventricular catheter in 19 cases, leading to epileptic seizures in 17 up to now. Thus the incidence of convulsions in this particular group of patients is 0.59 (17/29), the limits of confidence 95% being 0.39-0.76. The irritative abnormalities occur usually during the second year after the operation and the delay for the onset of clinical seizures is variable. The age at operation seems to influence the occurrence of the epileptogenic scar. The type of hydrocephalus and especially the presence of an associated cerebral focal lesion can be of importance in the development of clinical seizures. PMID:405183

  9. Action fluency in Parkinson's disease: a follow-up study.

    PubMed

    Signorini, Matteo; Volpato, Chiara

    2006-04-01

    The impairment in action fluency task present in Parkinson's disease (PD) patients has been previously interpreted as an indicator of conversion from PD to PD with dementia or as a grammatical deficit for verbs and ascribed to a frontostriatal loop pathophysiology. In the present study, 20 patients with PD without dementia were longitudinally tested with overall cognitive decline scales and semantic, letter, and action fluency tasks in a 24-month follow-up study. In comparison with healthy age-matched controls, PD patients showed a stable and consistent impairment on action fluency without any sign of cognitive decline. Our findings suggest that action fluency task may be an early sign of impairment of frontostriatal circuits in PD and it cannot be considered an indicator of conversion from PD to PD with dementia.

  10. [Neuromuscular disease: respiratory clinical assessment and follow-up].

    PubMed

    Martínez Carrasco, C; Villa Asensi, J R; Luna Paredes, M C; Osona Rodríguez de Torres, F B; Peña Zarza, J A; Larramona Carrera, H; Costa Colomer, J

    2014-10-01

    Patients with neuromuscular disease are an important group at risk of frequently suffering acute or chronic respiratory failure, which is their main cause of death. They require follow-up by a pediatric respiratory medicine specialist from birth or diagnosis in order to confirm the diagnosis and treat any respiratory complications within a multidisciplinary context. The ventilatory support and the cough assistance have improved the quality of life and long-term survival for many of these patients. In this paper, the authors review the pathophysiology, respiratory function evaluation, sleep disorders, and the most frequent respiratory complications in neuromuscular diseases. The various treatments used, from a respiratory medicine point of view, will be analyzed in a next paper. PMID:24709048

  11. Detection of GRB 060927 at zeta = 5.47: Implications for the Use of Gamma-Ray Bursts as Probes of the End of the Dark Ages

    NASA Technical Reports Server (NTRS)

    Ruiz-Velasco, A. E.; Swan, H.; Troja, E.; Malesani, D.; Fynbo, J. P. U.; Sterling, R. L. C.; Xu, D.; Aharonian, F.; Akerlof, C.; Andersen, M. I.; Ashley, M. C. B.; Barthelmy, S. D.; Bersier, D.; CastroCeron, J. M.; Castro-Tirado, A. J.; Gehrels, N.; Gogus, E.; Gorosabel, J.; Guidorzi, C.; Guver, T.; Hjorth, J.; Horns, D.; Huang, K. Y.; Jakobsson, P.; Jensen, B. L.

    2007-01-01

    We report on follow-up observations of the gamma-ray burst GRB 060927 using the robotic ROTSE-IIIa telescope and a suite of larger aperture groundbased telescopes. An optical afterglow was detected 20 s after the burst, the earliest rest-frame detection of optical emission from any GRB. Spectroscopy performed with the VLT about 13 hours after the trigger shows a continuum break at lambda approx. equals 8070 A, produced by neutral hydrogen absorption at zeta = 5.6. We also detect an absorption line at 8158 A which we interpret as Si II lambda 1260 at zeta = 5.467. Hence, GRB 060927 is the second most distant GRB with a spectroscopically measured redshift. The shape of the red wing of the spectral break can be fitted by a damped Ly(alpha) profile with a column density with log(N(sub HI)/sq cm) = 22.50 +/- 0.15. We discuss the implications of this work for the use of GRBs as probes of the end of the dark ages and draw three main conclusions: i) GRB afterglows originating from zeta greater than or approx. equal to 6 should be relatively easy to detect from the ground, but rapid near-infrared monitoring is necessary to ensure that they are found; ii) The presence of large H I column densities in some GRBs host galaxies at zeta > 5 makes the use of GRBs to probe the reionization epoch via spectroscopy of the red damping wing challenging; iii) GRBs appear crucial to locate typical star-forming galaxies at zeta > 5 and therefore the type of galaxies responsible for the reionization of the universe.

  12. Digital dermoscopic follow-up of 1544 melanocytic nevi.

    PubMed

    Rotaru, Maria; Nati, Angelica-Elena; Avrămoiu, Ioan; Grosu, Florin; Mălăescu, Gheorghe Dan

    2015-01-01

    The use of dermatoscopy increases melanocytic nevi diagnostic accuracy, and is important for dermoscopic monitoring of atypical lesions, allowing to find significant changes in the earliest stage. Dermoscopic diagnosis of melanocytic nevi type in a group of patients and their follow-up with the assessment of changes occurred during dermoscopic monitoring. Dermoscopically, we followed the nevic size and pattern, the color and pigment distribution. Follow-up visits were scheduled depending on the type of the melanocytic lesions and the patient's compliance. The nevi that have shown significant dermoscopic changes were excised and histopathologically examined. The study was performed on a group of 92 patients, mostly females (56.5%), mean age of 29.1 years. Of the total of 1544 melanocytic nevi examined, 27.4% were atypical and 72.6% common nevi. The average dermoscopic examination interval was 14.1 months. During monitoring, 35.5% atypical nevi and 22.5% common nevi have modified, especially changes in pigmentation and color (31% atypical nevi and 9.9% common nevi) and the appearance of new dermoscopic structures (12.7% atypical nevi and common nevi 8.5%). Of the total nevi monitored, 3% showed significant changes and were excised and examined pathologically, without diagnose of any malignant transformation. In our study, dermoscopic changes appeared in atypical as well as in common nevi. The dermoscopic monitoring of melanocytic-pigmented lesions remains an accessible method of assessment the evolution of nevi and can reduce the risk of appearance of malignant melanoma in the general population.

  13. Male sexual dysfunctions and multimedia immersion therapy (follow-up).

    PubMed

    Optale, Gabriele; Marin, Silvia; Pastore, Massimiliano; Nasta, Alberto; Pianon, Carlo

    2003-06-01

    The aim of the study was to evaluate the efficiency, after 1 year, of combined use of psychodynamic psychotherapy integrating virtual reality (VR) for the treatment of erectile dysfunction (ED) and premature ejaculation (PE) in 160 heterosexual males who had neither any prior sexual therapy nor had made use (either before, during or after therapy) of any specific pharmaceuticals for the treatment of primary sexual dysfunction. All subjects had given their informed consent. After a clinical diagnosis in an andrologic center, 50 presumably psychological ED (average age 43.7 years), 60 mixed ED (53.9 years) and 50 primary PE (39 years) who suffered these problems over 6 months were undergoing a cycle of 12 sessions, over a 25-week period, of psychotherapy, integrating an audio CD and helmet with miniature television screens that projected specially designed CD-ROM program on the ontogenetic development of male sexual identity. The clinical follow up was done after 6 and 12 months after the cycle. After one year, the overall partial (two times out of three) and complete positive response rate for psychological ED was 75%, for mixed ED was 47% and for PE was 54%. We considered drop-out cases as only before the 7th session of the treatment cycle, the drop-outs after session 7 and the patients that did not show up for follow-up are counted as negative results. Two patients reported nausea and one, vertigo during the first 15-min virtual reality experience. Considering the particular way that full-immersion virtual reality involves the subject who experiences it, we hypothesized that this methodological approach could speed up the therapeutic process. The evidence that positive results persist over time allows us to hypothesize that certain changes in cerebral function can be possible and that these changes are correlated to favorable sexual performance in the male.

  14. Hallucinations in Parkinson's disease: a follow-up study.

    PubMed

    de Maindreville, Anne Doé; Fénelon, Gilles; Mahieux, Florence

    2005-02-01

    To study prevalence of hallucinations in patients with Parkinson's disease (PD) during a 1-year period, and identify factors predictive of the onset of hallucinations in patients who were hallucination-free at baseline, 141 unselected outpatients with PD were evaluated prospectively for a set of demographic, clinical, and therapeutic variables and the presence of hallucinations during the previous 3 months. Patient groups were compared with nonparametric tests, and logistic regression was applied to significant data. Follow-up data were available for 127 patients. The hallucination prevalence rates (%) at the first and second evaluation were, respectively, 41.7 and 49.6 for hallucinations of all types (NS), 29.1 and 40.2 for minor hallucinations (i.e., presence or passage hallucinations, and illusions) (P = 0.02), 22.8 and 21.2 for formed visual hallucinations (NS), and 8.7 and 8.7 for auditory hallucinations (NS). Hallucinations rarely started or ceased during the study. The most labile forms were minor hallucinations, which developed in 20% of patients and ceased in 9%. During follow-up, 15% of patients started to hallucinate. Three factors, all present at the first evaluation, independently predicted the onset of hallucinations in patients previously free of hallucinations at baseline (odds ratio; 95% confidence interval): severe sleep disturbances (14.3; 2.5-80.9), ocular disorders (9.1; 1.6-52.0), and a high axial motor score (5.7; 1.2-27.4). Hallucinations have a chronic course in most parkinsonian patients. Factors predicting the onset of hallucinations point to a role of extranigral brainstem involvement and a nonspecific, facilitating role of ocular disorders.

  15. Asthma after childhood pneumonia: six year follow up study

    PubMed Central

    Clark, Christopher E; Coote, Jacqueline M; Silver, David A T; Halpin, David M G

    2000-01-01

    Objective To establish the long term cumulative prevalence of asthma in children admitted to hospital with pneumonia and to examine the hypothesis that some children admitted to hospital with pneumonia may be presenting with undiagnosed asthma. Design Prospective study of a cohort of children previously admitted to hospital with pneumonia, followed up by postal questionnaires to their general practitioners and the children or their parents. Setting General practices in southwest England. Participants 78 children admitted to the Royal Devon and Exeter Hospital between 1989 and 1991 with a diagnosis of pneumonia confirmed on independent review of x ray films. Main outcome measures Any diagnosis of asthma, use of any treatment for asthma, and asthma symptom scores. Results On the basis of a 100% response rate from general practitioners and 86% from patients or parents, the cumulative prevalence of asthma was 45%. A diagnosis of asthma was associated with a family history of asthma (odds ratio 11.23; 95% confidence interval 2.57 to 56.36; P=0.0002). Mean symptom scores were higher for all children with asthma (mean score 2.4; χ2=14.88; P=0.0001) and for children with asthma not being treated (mean 1.4; χ2=6.2; P=0.01) than for those without asthma (mean 0.2) . Conclusions A considerable proportion of children presenting to a district general hospital with pneumonia either already have unrecognised asthma or subsequently develop asthma. The high cumulative prevalence of asthma suggests that careful follow up of such children is worth while. Asthma is undertreated in these children; a structured symptom questionnaire may help to identify and reduce morbidity due to undertreatment. PMID:10834897

  16. Digital dermoscopic follow-up of 1544 melanocytic nevi.

    PubMed

    Rotaru, Maria; Nati, Angelica-Elena; Avrămoiu, Ioan; Grosu, Florin; Mălăescu, Gheorghe Dan

    2015-01-01

    The use of dermatoscopy increases melanocytic nevi diagnostic accuracy, and is important for dermoscopic monitoring of atypical lesions, allowing to find significant changes in the earliest stage. Dermoscopic diagnosis of melanocytic nevi type in a group of patients and their follow-up with the assessment of changes occurred during dermoscopic monitoring. Dermoscopically, we followed the nevic size and pattern, the color and pigment distribution. Follow-up visits were scheduled depending on the type of the melanocytic lesions and the patient's compliance. The nevi that have shown significant dermoscopic changes were excised and histopathologically examined. The study was performed on a group of 92 patients, mostly females (56.5%), mean age of 29.1 years. Of the total of 1544 melanocytic nevi examined, 27.4% were atypical and 72.6% common nevi. The average dermoscopic examination interval was 14.1 months. During monitoring, 35.5% atypical nevi and 22.5% common nevi have modified, especially changes in pigmentation and color (31% atypical nevi and 9.9% common nevi) and the appearance of new dermoscopic structures (12.7% atypical nevi and common nevi 8.5%). Of the total nevi monitored, 3% showed significant changes and were excised and examined pathologically, without diagnose of any malignant transformation. In our study, dermoscopic changes appeared in atypical as well as in common nevi. The dermoscopic monitoring of melanocytic-pigmented lesions remains an accessible method of assessment the evolution of nevi and can reduce the risk of appearance of malignant melanoma in the general population. PMID:26743296

  17. An Off-Axis Model for GRB 031203

    NASA Technical Reports Server (NTRS)

    Ramirez-Ruiz, Enrico; Granot, Jonathan; Kouveliotou, Chryssa; Woosley, S. E.; Patel, Sandy K.; Mazzali, Paolo A.

    2004-01-01

    The low luminosity radio emission of the unusually faint GRB 031203 has been argued to support the idea of a class of intrinsically sub-energetic gamma-ray bursts (GRBs), currently comprising two members. While low energy GRBs probably exist, we show that the collective prompt and multiwavelength observations of the afterglow of GRB 031203, do not necessarily require a sub-energetic nature for that event. In fact, the data are more consistent with a typical, powerful GRB seen at an angle of about twice the opening angle of the central jet. The (redshift corrected) peak energy, E(sub p), of GRB 031203 then becomes approximately 2 MeV, similar to many other GRBs.

  18. A Broader Perspective on the GRB-SN Connection

    NASA Astrophysics Data System (ADS)

    Soderberg, Alicia M.

    2006-05-01

    Over the last few years our understanding of local Type Ibc supernovae and their connection to long-duration gamma-ray bursts has been revolutionized. Recent discoveries have shown that the emerging picture for core-collapse explosions is one of diversity. Compiling data from our dedicated radio survey of SNe Ibc and our comprehensive HST survey of GRB-SNe together with ground-based follow-up campaigns, I review our current understanding of the GRB-SN connection. In particular, I compare local SNe Ibc with GRB-SNe based on the following criteria: (1) the distribution of optical peak magnitudes which serve as a proxy for the mass of 56Ni produced in the explosion, (2) radio luminosity at early time (few days to weeks) which provides a measure of the energy coupled to on-axis relativistic ejecta, and (3) radio luminosity at late time (several years) which constrains the emission from GRB jets initially directed away from our line-of-sight. By focusing on these three points, I will describe the complex picture of stellar death that is emerging.

  19. Long-term follow-up of thyroid nodule growth.

    PubMed

    Quadbeck, B; Pruellage, J; Roggenbuck, U; Hirche, H; Janssen, O E; Mann, K; Hoermann, R

    2002-10-01

    Benign thyroid nodules are common in iodine deficient countries. Although many recent studies have addressed the molecular basis and short-term outcome of treatment in nodular thyroid disease, data on the long-term follow-up of thyroid nodule growth are widely lacking. The aim of the present study was to evaluate the long-term behaviour of benign thyroid nodules growth. We followed 109 consecutive patients seen at yearly intervals in our Outpatient Clinic for at least 3 years (range 3-12 years, mean 4.9 +/- 2.6 years) presenting with 139 benign nodules in uni- or multinodular goiters. The size of the nodules and thyroid glands was analysed retrospectively. The study included a spectrum of benign thyroid nodules, 86 functioning and 53 non-functioning. 27 patients were treated with levothyroxine, 8 with iodide and 16 with a combination of both. 58 patients were not treated mainly because of thyroid functional autonomy. Patients with overt hyperthyroidism or suspected malignancy by fine-needle aspiration were excluded from the study. The nodules and glands were assessed by ultrasonography at yearly intervals and documented by photoprints. Relevant growth was defined as an increase in nodule volume of at least 30%. For statistical analyses, Cox Proportional Hazard Model and life-table analyses according to Kaplan-Meier were performed. Most thyroid nodules grew slowly but continuously during follow-up. After about 3 years, half of the nodules had increased their volume by at least 30%. Growth of the nodules was significantly faster than of the corresponding thyroid glands (p < 0.0001). Age and sex of the patients and size or function of the nodules at initial presentation were not significantly related to their growth. Suppression of TSH did not affect growth of the nodules irrespective of the source of thyroid hormones, endogenous or by administration of levothyroxine. In conclusion, benign thyroid nodules have a slow intrinsic growth potential, which is apparently

  20. Initial Follow-up of Pulsar Discoveries from the HTRU Galactic Plane Survey

    NASA Astrophysics Data System (ADS)

    Ng, Cherry; Possenti, Andrea; Johnston, Simon; Kramer, Michael; Burgay, Marta; Bailes, Matthew; Bhat, Ramesh; Keith, Michael; Burke-Spolaor, Sarah; van Straten, Willem; Stappers, Benjamin; Bates, Samuel; Keane, Evan; Levin, Lina; Champion, David; Jameson, Andrew; Tiburzi, Caterina; Petroff, Emily; Barr, Ewan; Flynn, Chris

    2014-10-01

    This is a request for observing time for the initial follow-up of pulsar discoveries from the low-latitude Galactic plane section of the HTRU survey (P630). We have already discovered (50 pulsars from just 40% of processed data. Extrapolation and population synthesis show that the Galactic plane survey will result in at least a further 100 discoveries. Currently, with data processing on-going employing all available computing resources, we expect about 20 new discoveries per semester. The discovery of pulsars is just a first step and interesting science can usually only be revealed when a follow-up timing campaign is carried out. One year of initial timing is the minimal timespan required to fully-characterise any newly-discovered pulsars, essential for deriving pulsar parameters such as the characteristic age, magnetic field strength, spin-down rate, as well as to detect any unexpected behaviour of the pulsar which might result from emission instabilities. This follow-up timing project is necessary for identifying any individual interesting pulsar systems discovered from the HTRU Galactic plane survey. Since all of the pulsars on the observing list here are followed-up for the first time, they will produce completely new and exciting results. In addition, this timing project will enable a large-scale examination of the Galactic plane pulsar population, exploring the true boundaries of pulsar phase space. Given the large number of discoveries expected and the long integration length required, this dedicated follow-up timing campaign is vital for achieving our science goals.

  1. Initial Follow-up of Pulsar Discoveries from the HTRU Galactic Plane Survey

    NASA Astrophysics Data System (ADS)

    Ng, Cherry; Possenti, Andrea; Johnston, Simon; Kramer, Michael; Burgay, Marta; Bailes, Matthew; Bhat, Ramesh; Keith, Michael; Burke-Spolaor, Sarah; van Straten, Willem; Stappers, Benjamin; Bates, Samuel; Keane, Evan; Levin, Lina; Champion, David; Jameson, Andrew; Tiburzi, Caterina; Petroff, Emily; Barr, Ewan; Flynn, Chris

    2014-04-01

    This is a request for observing time for the initial follow-up of pulsar discoveries from the low-latitude Galactic plane section of the HTRU survey (P630). We have already discovered 40 pulsars from just 30% of processed data. Extrapolation and population synthesis show that the Galactic plane survey will result in at least a further 120 discoveries. Currently, with data processing on-going employing all available computing resources, we expect about 20 new discoveries per semester. The discovery of pulsars is just a first step and interesting science can usually only be revealed when a follow-up timing campaign is carried out. One year of initial timing is the minimal timespan required to fully-characterise any newly-discovered pulsars, essential for deriving pulsar parameters such as the characteristic age, magnetic field strength, spin-down rate, as well as to detect any unexpected behaviour of the pulsar which might result from emission instabilities. This follow-up timing project is necessary for identifying any individual interesting pulsar systems discovered from the HTRU Galactic plane survey. Since all of the pulsars on the observing list here are followed-up for the first time, they will produce completely new and exciting results. In addition, this timing project will enable a large-scale examination of the Galactic plane pulsar population, exploring the true boundaries of pulsar phase space. Given the large number of discoveries expected and the long integration length required, this dedicated follow-up timing campaign is vital for achieving our science goals.

  2. Long-term follow-up study of radial forearm free flap reconstruction after hemiglossectomy.

    PubMed

    Akashi, Masaya; Hashikawa, Kazunobu; Sakakibara, Akiko; Komori, Takahide; Terashi, Hiroto

    2015-01-01

    Previous studies on postoperative long-term results in patients who underwent reconstructive free flap transfer following hemiglossectomy had some issues, including the heterogeneity of the patient population and the observation period. The present study aimed to evaluate changes of reconstructed tongues in patients who underwent radial forearm free flap (RFFF) after hemiglossectomy with long-term follow-up. We enrolled 23 patients who underwent RFFF after hemiglossectomy with a postoperative follow-up of 5 years or more. Postoperative status (eating, speech, sensation function) was assessed by concise medical inquiries. Morphological changes of flaps were evaluated by reviewing clinical photographs. Hemiglossectomy involving the base of the tongue was performed in 4 cases (17.4%) and was limited to the mobile tongue in 19 cases (82.6%). The mean follow-up was 85.4 months (range, 60-122 months). All patients experienced gradually improved postoperative status. The most significant improvement was found between 1 and 5 years after surgery (P = 0.007), but not between 1 and 3 years (P = 0.075) or between 3 and 5 years (P = 0.530). In almost all of the flaps, there were few morphological changes throughout the follow-up period. Postoperative status in patients who underwent reconstructive RFFF following hemiglossectomy improved sequentially.

  3. Study Protocol, Sample Characteristics, and Loss to Follow-Up: The OPPERA Prospective Cohort Study

    PubMed Central

    Bair, Eric; Brownstein, Naomi C.; Ohrbach, Richard; Greenspan, Joel D.; Dubner, Ron; Fillingim, Roger B.; Maixner, William; Smith, Shad; Diatchenko, Luda; Gonzalez, Yoly; Gordon, Sharon; Lim, Pei-Feng; Ribeiro-Dasilva, Margarete; Dampier, Dawn; Knott, Charles; Slade, Gary D.

    2013-01-01

    When studying incidence of pain conditions such as temporomandibular disorders (TMDs), repeated monitoring is needed in prospective cohort studies. However, monitoring methods usually have limitations and, over a period of years, some loss to follow-up is inevitable. The OPPERA prospective cohort study of first-onset TMD screened for symptoms using quarterly questionnaires and examined symptomatic participants to definitively ascertain TMD incidence. During the median 2.8-year observation period, 16% of the 3,263 enrollees completed no follow-up questionnaires, others provided incomplete follow-up, and examinations were not conducted for one third of symptomatic episodes. Although screening methods and examinations were found to have excellent reliability and validity, they were not perfect. Loss to follow-up varied according to some putative TMD risk factors, although multiple imputation to correct the problem suggested that bias was minimal. A second method of multiple imputation that evaluated bias associated with omitted and dubious examinations revealed a slight underestimate of incidence and some small biases in hazard ratios used to quantify effects of risk factors. Although “bottom line” statistical conclusions were not affected, multiply-imputed estimates should be considered when evaluating the large number of risk factors under investigation in the OPPERA study. Perspective These findings support the validity of the OPPERA prospective cohort study for the purpose of investigating the etiology of first-onset TMD, providing the foundation for other papers investigating risk factors hypothesized in the OPPERA project. PMID:24275220

  4. Fast response electromagnetic follow-ups from low latency GW triggers

    NASA Astrophysics Data System (ADS)

    Howell, E. J.; Chu, Q.; Rowlinson, A.; Gao, H.; Zhang, B.; Tingay, S. J.; Boër, M.; Wen, L.

    2016-05-01

    We investigate joint low-latency gravitational wave (GW) detection and prompt electromagnetic (EM) follow-up observations of coalescing binary neutron stars (BNSs). Assuming that BNS mergers are associated with short duration gamma ray bursts (SGRBs), we evaluate if rapid EM follow-ups can capture the prompt emission, early engine activity or reveal any potential by-products such as magnetars or fast radio bursts. To examine the expected performance of extreme low-latency search pipelines, we simulate a population of coalescing BNSs and use these to estimate the detectability and localisation efficiency at different times before merger. Using observational SGRB flux data corrected to the range of the advanced GW interferometric detectors, we determine what EM observations could be achieved from low-frequency radio up to high energy γ-ray. We show that while challenging, breakthrough multi-messenger science is possible through low latency pipelines.

  5. Discovery of the nearby long, soft GRB 100316D with an associated supernova

    NASA Astrophysics Data System (ADS)

    Starling, R. L. C.; Wiersema, K.; Levan, A. J.; Sakamoto, T.; Bersier, D.; Goldoni, P.; Oates, S. R.; Rowlinson, A.; Campana, S.; Sollerman, J.; Tanvir, N. R.; Malesani, D.; Fynbo, J. P. U.; Covino, S.; D'Avanzo, P.; O'Brien, P. T.; Page, K. L.; Osborne, J. P.; Vergani, S. D.; Barthelmy, S.; Burrows, D. N.; Cano, Z.; Curran, P. A.; de Pasquale, M.; D'Elia, V.; Evans, P. A.; Flores, H.; Fruchter, A. S.; Garnavich, P.; Gehrels, N.; Gorosabel, J.; Hjorth, J.; Holland, S. T.; van der Horst, A. J.; Hurkett, C. P.; Jakobsson, P.; Kamble, A. P.; Kouveliotou, C.; Kuin, N. P. M.; Kaper, L.; Mazzali, P. A.; Nugent, P. E.; Pian, E.; Stamatikos, M.; Thöne, C. C.; Woosley, S. E.

    2011-03-01

    We report the Swift discovery of the nearby long, soft gamma-ray burst GRB 100316D, and the subsequent unveiling of its low-redshift host galaxy and associated supernova. We derive the redshift of the event to be z= 0.0591 ± 0.0001 and provide accurate astrometry for the gamma-ray burst (GRB) supernova (SN). We study the extremely unusual prompt emission with time-resolved γ-ray to X-ray spectroscopy and find that the spectrum is best modelled with a thermal component in addition to a synchrotron emission component with a low peak energy. The X-ray light curve has a remarkably shallow decay out to at least 800 s. The host is a bright, blue galaxy with a highly disturbed morphology and we use Gemini-South, Very Large Telescope and Hubble Space Telescope observations to measure some of the basic host galaxy properties. We compare and contrast the X-ray emission and host galaxy of GRB 100316D to a subsample of GRB-SNe. GRB 100316D is unlike the majority of GRB-SNe in its X-ray evolution, but resembles rather GRB 060218, and we find that these two events have remarkably similar high energy prompt emission properties. Comparison of the host galaxies of GRB-SNe demonstrates, however, that there is a great diversity in the environments in which GRB-SNe can be found. GRB 100316D is an important addition to the currently sparse sample of spectroscopically confirmed GRB-SNe, from which a better understanding of long GRB progenitors and the GRB-SN connection can be gleaned.

  6. Diagnosis, treatment, and follow-up of borderline ovarian tumors.

    PubMed

    Fischerova, Daniela; Zikan, Michal; Dundr, Pavel; Cibula, David

    2012-01-01

    Borderline ovarian tumors represent a heterogeneous group of noninvasive tumors of uncertain malignant potential with characteristic histology. They occur in younger women, are present at an early stage, and have a favorable prognosis, but symptomatic recurrence and death may be found as long as 20 years after therapy in some patients. The molecular changes in borderline ovarian tumors indicate linkage of this disease to type I ovarian tumors (low-grade ovarian carcinomas). The pathological stage of disease and subclassification of extraovarian disease into invasive and noninvasive implants, together with the presence of postoperative macroscopic residual disease, appear to be the major predictor of recurrence and survival. However, it should be emphasized that the most important negative prognostic factor for recurrence is just the use of conservative surgery, but without any impact on patient survival because most recurrent diseases are of the borderline type-easily curable and with an excellent prognosis. Borderline tumors are difficult masses to correctly preoperatively diagnose using imaging methods because their macroscopic features may overlap with invasive and benign ovarian tumors. Over the past several decades, surgical therapy has shifted from a radical approach to more conservative treatment; however, oncologic safety must always be balanced. Follow-up is essential using routine ultrasound imaging, with special attention paid to the remaining ovary in conservatively treated patients. Current literature on this topic leads to a number of controversies that will be discussed thoroughly in this article, with the aim to provide recommendations for the clinical management of these patients.

  7. Torticollis: a long-term follow-up study.

    PubMed

    Chang, P Y; Tan, C K; Huang, Y F; Sheu, J C; Wang, N L; Yeh, M L; Chen, C C

    1996-01-01

    To achieve better guidelines for the future management of torticollis, this study analyzed surgical and nonsurgical management of 253 torticollis patients who were treated in this hospital from 1971 to 1993. Of those, 37 cases received operation only, 78 cases were operated after failed physical therapy, and 138 cases were treated only at the Rehabilitation Department. If free neck movement was considered to be the primary goal of treatment, most parents were satisfied with the results. However, if facial and skull deformities were the serious sequelae of torticollis, then only less than half of the surgical and nonsurgical groups of patients were graded as normal. Further, 10.9% of physical therapy group and 7% of the surgical patients need further operation to release the fibrotic bundle which limited their neck movement. Therefore, it is suggested that torticollis treatment should include early interventions such as adjusting sleep position, careful planning of physical therapy and/or operation and a long term follow-up period as essential for better management of torticollis.

  8. Cohort Profile: The Manitoba Follow-up Study (MFUS).

    PubMed

    Tate, Robert B; Cuddy, T Edward; Mathewson, Francis A L

    2015-10-01

    The Manitoba Follow-up Study (MFUS) is Canada's longest running study of cardiovascular disease and ageing. The MFUS cohort consists of 3983 men recruited from the Royal Canadian Air Force at the end of World War II. At entry to the study, 1 July 1948, their mean age was 31 years, with 90% between ages 20 and 39 years. All study members were free of clinical evidence of ischaemic heart disease. The protocol of MFUS was to obtain routine medical examinations from these men at regular intervals over time. The research goal of the study was to examine the role that any abnormalities detected on routine electrocardiograms from apparently healthy men might play in the prediction of subsequent diagnoses of cardiovascular disease. Over the course of 65 years, about 35% of the cohort has documented evidence of ischaemic heart disease. The research focus was expanded in 1996 to explore the roles of physical, mental and social functioning in support of healthy and successful ageing. On 1 July 2013, 429 original cohort members were alive with a mean age of 92 years. Collaborative research with others outside the in-house team is welcomed.

  9. Neurological findings at follow-up in neonatal hypoglycaemia.

    PubMed

    Fluge, G

    1975-07-01

    Follow-up examination was carried out in 37 children who had been hypoglycaemic during the neonatal period. Mean age was 3 1/2 years. Five out of 7 children with asymptomatic hypoglycaemia neonatally were completely normal, while minimal brain dysfunction was evident in one, and another child showed pathological EEG. Symptomatic, transient hypoglycaemia seemed to carry a poor prognosis as only one out of 9 individuals was normal. Four patients in this group had convulsions after the neonatal period; two of these had recurrence of hypoglycaemia. One had infantile spasms and was severely mentally retarded with spastic diplegia and epilepsy. One girl was blind due to optic nerve atrophy. Four cases of cerebral palsy were detected in this group. Among 21 cases of secondary hypoglycaemia there were no cases of serious neurological sequelae. It is reasonable to assume that neonatal hypoglycaemia is an important prognostic factor. The deleterious effect on the CNS seems to be related to the duration and severity of the hypoglycaemia.

  10. Intensity of follow-up after pancreatic cancer resection.

    PubMed

    Castellanos, Jason A; Merchant, Nipun B

    2014-03-01

    The prognosis of patients diagnosed with pancreatic adenocarcinoma remains dismal. Of the 15-20 % of patients who are candidates for potentially curative resection, 66-92 % will develop recurrent disease. Although guidelines for surveillance in the postoperative setting exist, they are not evidence based, and there is wide variability of strategies utilized. Current surveillance guidelines as suggested by the National Comprehensive Cancer Network (NCCN) include routine history and physical, measurement of serum cancer-associated antigen 19-9 (CA19-9) levels, and computed tomographic imaging at 3- to 6-month intervals for the first 2 years, and annually thereafter. However, the lack of prospective clinical data examining the efficacy of different surveillance strategies has led to a variability of the intensity of follow-up and a lack of consensus on its necessity and efficacy. Recent therapeutic advances may have the potential to significantly alter survival after recurrence, but a careful consideration of current surveillance strategies should be undertaken to optimize existing approaches in the face of high recurrence and low survival rates.

  11. A long-term follow-up of postpartum thyroiditis.

    PubMed

    Othman, S; Phillips, D I; Parkes, A B; Richards, C J; Harris, B; Fung, H; Darke, C; John, R; Hall, R; Lazarus, J H

    1990-05-01

    To investigate the long-term outcome of postpartum thyroiditis (PPT), 43 patients with PPT and 171 control women were evaluated 3.5 (range 2-4) years postpartum. Ten (23%) PPT patients were hypothyroid compared to none of the controls (P less than 0.001). Factors associated with the development of hypothyroidism were high antimicrosomal antibody titre measured at 16 weeks gestation (P less than 0.01), severity of hypothyroid phase of PPT, multiparity, and a previous history of spontaneous abortion. The presence of microsomal antibody but no PPT in one pregnancy did not prevent the occurrence of PPT in the next pregnancy in two patients and a further five patients had PPT in two successive pregnancies. There was no association between HLA haplotype, family history of thyroid disease, smoking or frequency of oral contraception, and the development of long-term hypothyroidism after PPT. It is concluded that permanent hypothyroidism is an important sequel to PPT and patients with PPT should be followed up appropriately.

  12. Prognosis after myocardial infarction: results of 15 year follow up.

    PubMed Central

    Merrilees, M A; Scott, P J; Norris, R M

    1984-01-01

    A total of 271 out of 757 patients who had suffered a myocardial infarction during 1966-7 were still alive after six years; these patients were subsequently followed up 15 years after the infarction. Two hundred and sixty eight (99%) of the patients alive at six years and 519 (95%) of the 549 originally discharged from hospital were traced. A coronary prognostic index, which had predicted survival both to three years and from three to six years after recovery from the infarct also predicted survival from six to 15 years after recovery. The major factor affecting survival to 15 years was age at the time of the original infarct. Among patients aged under 60 at the time of infarction women fared better than men (p = 0.027). Factors in the coronary prognostic index that were associated with impairment of left ventricular function at the time of infarction and that had predicted mortality to three years and from three to six years also predicted mortality from six to 15 years. These factors were cardiac enlargement, pulmonary venous congestion, and the presence of infarction before the index infarct. The dominant cause of death remained coronary heart disease and its complications. PMID:6229313

  13. Long term follow up after inhalation of foreign bodies.

    PubMed Central

    Davies, H; Gordon, I; Matthew, D J; Helms, P; Kenney, I J; Lutkin, J E; Lenney, W

    1990-01-01

    The long term results of treatment of inhalation of foreign bodies in a district children's hospital and in a tertiary referral centre were reviewed by clinical assessment, chest radiography, and standard four view 81mKr ventilation/99mTc macroaggregated albumin perfusion imaging (V/Q lung scan). The overall incidence in the population served by the district hospital was roughly one in 14,000/year. Of the 12 children reviewed there, three had abnormal chest radiographs and four had abnormal V/Q scans as a result of inhalation of the foreign bodies. Of 21 children treated and reviewed at the referral centre, eight had abnormal chest radiographs, and 14 had abnormal V/Q lung scans. Three factors were assessed for prognostic importance: site of impaction, initial radiographic appearance, and time before removal. A child who had inhaled a foreign body into the left lung and who had collapse/consolidation on the initial chest radiograph was at greatest risk of long term complications. These children merit close follow up. PMID:2378520

  14. Diagnosis, Follow-Up and Treatment Results in Thyroid Ophthalmopathy

    PubMed Central

    Savku, Esra; Gündüz, Kaan

    2015-01-01

    Objectives: To discuss our follow-up and treatment results in thyroid-associated ophthalmopathy (TAO). Ma­te­ri­als and Met­hods: The records of 168 TAO cases who were followed at our clinic between October 1998 and October 2013 were reviewed retrospectively. The severity and activity of the disease were evaluated according to the criteria of the European Group on Graves’ Ophthalmopathy (EUGOGO) and Clinical Activity Score (CAS). Re­sults: Sixty-three men and 105 women participated in the study. The mean age of the patients was 42.3±12.4 years. Smoking habit was noted in 54.2% of the cases. Graves’ disease was the most common (80.4%) thyroid pathology accompanying TAO. TAO was mild in 64.4%, moderate-to-severe in 33.6% and severe in 2% of the eyes. Male gender was found as an independent risk factor for severity of the disease (p=0.040). TAO was in the active phase in 32.6% of the eyes. Older age and high thyroid receptor antibody titer were correlated with disease activity (P=0.031 and P<0.001, respectively). Thirty-four patients (20%) were treated for ocular findings. The most common treatment was systemic steroid therapy (12%); others included orbital decompression (5%), orbital radiotherapy (2%), and topical application of guanethidine (1%). Conclusion: Non-infiltrative phase and mild ocular findings were generally seen in TAO. Therefore, treatment is not recommended for many cases. Systemic steroid therapy is the most commonly used treatment modality in the active phase. However, orbital decompression surgery is necessary in a small number of cases with sight-threatening ocular findings. PMID:27800224

  15. Follow up on the crystal growth experiments of the LDEF

    NASA Technical Reports Server (NTRS)

    Nielsen, K. F.; Lind, M. D.

    1993-01-01

    The results of the 4 solution growth experiments on the LDEF have been published elsewhere. Both the crystals of CaCO3, which were large and well shaped, and the much smaller TTF-TCNQ crystals showed unusual morphological behavior. The follow up on these experiments was begun in 1981, when ESA initiated a 'Concept Definition Study' on a large, 150 kg, Solution Growth Facility (SGF) to be included in the payload of EURECA-1, the European Retrievable Carrier. This carrier was a continuation of the European Spacelab and at that time planned for launch in 1987. The long delay of the LDEF retrieval and of subsequent missions brought about reflections both on the concept of crystal growth in space and on the choice of crystallization materials that had been made for the LDEF. Already before the LDEF retrieval, research on TTF-TCNQ had been stopped, and a planned growth experiment with TTF-TCNQ on the SGF/EURECA had been cancelled. The target of the SGF investigation is now more fundamental in nature. None of the crystals to be grown here are, like TTF-TCNQ, in particular demand by science or industry, and the crystals only serve the purpose of model crystals. The real purpose of the investigation is to study the growth behavior. One of the experiments, the Soret Coefficient Measurement experiment is not growing crystals at all, but has it as its sole purpose to obtain accurate information on thermal diffusion, a process of importance in crystal growth from solution.

  16. Follow-up study among model and pattern makers in a German automobile company. Results of a second follow-up.

    PubMed

    Becker, N; Kuhn, G; Marschall, B

    1997-12-01

    An historical follow-up study of 528 model makers in a German automobile company found an unusual pattern of mortality among these workers that included an increased risk of total cancer and tumors of the stomach, genitourinary organs, and the brain (Becker et al, 1992). Because of small numbers of cases and problems with the validity of causes of death, we carried out a second follow-up using data from the official mortality statistics and extending the observation period by five years. The new results did not confirm the previous observations of an increased risk of total cancer, cancer of the genitourinary organs, and tumors of the brain but confirmed indications of an increased risk of stomach cancer and suggested for the first time that there may be an increased risk of cancer of the intestine. Though the small numbers of cases did not allow statistical confirmation of these findings, they are consistent with the results of other studies recently conducted in the United States and published in this journal.

  17. [Follow up of patients with prostatic cancer after radical prostatectomy: results, late complication, survival rate].

    PubMed

    Romics, I; Bach, D; Würtz, U

    1995-02-19

    The authors performed radical prostatectomy on 35 prostate cancer patients between 1986 and 1991. At the end of 1993 the authors were informed about 25 patients. The mean follow-up was 4.4. years. Two patients have died in tumour related diseases, one in intercurrent diseases. In six patients progression was observed. Five patients had to operated because of anastomosis stricture. One patient was operated because of total incontinence another one uses penis clamp.

  18. H.E.S.S. follow-up of IceCube-160731A

    NASA Astrophysics Data System (ADS)

    de Naurois, Mathieu; H.E.S.S. Collaborarion

    2016-08-01

    The H.E.S.S. instrument was used to carry out follow-up observations of a high energy neutrino detected by IceCube on the 31st July 2016 at 01:55:04 UTC. The IceCube best fit position is Ra = 214.54, Dec = -0.33 with a radius of 0.75 deg at 90% confidence.

  19. Pleomorphic adenoma of the palate in a child: 9-year follow-up.

    PubMed

    de Courten, A; Lombardi, T; Samson, J

    1996-08-01

    Pleomorphic adenoma (PA), the most common of the benign salivary gland tumors, is an extremely rare entity in children before the age of 14 years. Until now, only five cases arising in the palate have been reported in detail. A case of PA of the hard palate in a 10-year-old girl is presented. After a 9-year follow-up period, no recurrence was observed.

  20. Mortality patterns among workers exposed to acrylamide: 1994 follow up

    PubMed Central

    Marsh, G. M.; Lucas, L. J.; Youk, A. O.; Schall, L. C.

    1999-01-01

    OBJECTIVE: To update the mortality experience of a cohort of 8508 workers with potential exposure to acrylamide at three plants in the United States from 1984-94. METHODS: Analyses of standardised mortality ratios (SMR) with national and local rates and relative risk (RR) regression modelling were performed to assess site specific cancer risks by demographic and work history factors, and exposure indicators for acrylamide and muriatic acid. RESULTS: For the 1925-94 study period, excess and deficit overall mortality risks were found for cancer sites of interest: brain and other central nervous system (CNS) (SMR 0.65, 95% confidence interval (95% CI) 0.36 to 1.09), thyroid gland (SMR 2.11, 95% CI 0.44 to 6.17), testis and other male genital organs (SMR 0.28, 95% CI 0.01 to 1.59), and cancer of the respiratory system (SMR 1.10, 95% CI 0.99 to 1.22); however, none was significant or associated with exposure to acrylamide. A previously reported excess mortality risk of cancer of the respiratory system at one plant remained increased among workers with potential exposure to muriatic acid (RR 1.50, 95% CI 0.86 to 2.59), but was only slightly increased among workers exposed or unexposed to acrylamide. In an exploratory exposure-response analysis of rectal, oesophageal, pancreatic, and kidney cancer, we found increased SMRs for some categories of exposure to acrylamide, but little evidence of an exposure-response relation. A significant 2.26-fold risk (95% CI 1.03 to 4.29) was found for pancreatic cancer among workers with cumulative exposure to acrylamide > 0.30 mg/m3.years; however, no consistent exposure-response relations were detected with the exposure measures considered when RR regression models were adjusted for time since first exposure to acrylamide. CONCLUSION: The contribution of 1115 additional deaths and nearly 60,000 person-years over the 11 year follow up period corroborate the original cohort study findings of little evidence for a causal relation between

  1. Intentional replantation of a mandibular molar: case report and 14-year follow-up.

    PubMed

    Herrera, Henry; Leonardo, Mário Roberto; Herrera, Helen; Miralda, Lucas; Bezerra da Silva, Raquel Assed

    2006-10-01

    This case report describes the nonsurgical endodontic treatment and intentional replantation of a mandibular molar and its nearly 14-year follow-up. A 56-year-old woman sought treatment with complaint of discomfort and sensitivity in the mandibular left area. The radiographic examination showed that the mandibular left first molar was endodontically treated, with over-instrumentation of the distal root and unsatisfactory obturation on the mesial root. A large periapical lesion was observed surrounding the roots. In view of the patient's limited interocclusal space and objection to undergo an apical surgery, intentional replantation was suggested as an alternative. The patient returned for clinical and radiographic follow-up at 15 days, 40 days, 6 months, 12 months, and once yearly thereafter. At the last visit, after 14 years, no painful symptomatology was reported, probing depth was no greater than 3 mm, the periradicular area had normal appearance and no evidence of root resorption or periapical lesion.

  2. Free gingival grafting procedure after excisional biopsy, 12-year follow-up.

    PubMed

    Keskiner, Ilker; Alkan, B Arzu; Tasdemir, Zekeriya

    2016-01-01

    The total removal of a lesion via excisional biopsy causes gingival recession, resulting in dentin hypersensitivity and esthetical problems. In this case report, a gingival recession defect resulting from an excisional biopsy was treated with a free gingival grafting procedure performed during the same appointment, and its 12-year follow-up was presented. A 44-year-old female patient was presented to our clinic with a firm, pedunculated, red gingival enlargement located on the labial surface of lower incisors. The exposed root surface, after the excisional biopsy, was covered with a free gingival graft. The lesion was pathologically diagnosed as pyogenic granuloma, and in the early postoperative phase, no recurrence was observed, but partial root coverage was determined. At 6-month follow-up, root coverage resulting from "creeping attachment" was observed, and this situation was maintained throughout the 12-year follow-up period. Repetitious postoperative discomfort and emotional stress for the patient may be avoided with a timesaving single appointment performing excisional biopsy and free gingival graft. Free gingival grafting procedure was used for this purpose not only to cover exposed root surfaces but also to eliminate dentin hypersensitivity and make oral hygiene procedures more effective. PMID:27403067

  3. Free gingival grafting procedure after excisional biopsy, 12-year follow-up

    PubMed Central

    Keskiner, Ilker; Alkan, B. Arzu; Tasdemir, Zekeriya

    2016-01-01

    The total removal of a lesion via excisional biopsy causes gingival recession, resulting in dentin hypersensitivity and esthetical problems. In this case report, a gingival recession defect resulting from an excisional biopsy was treated with a free gingival grafting procedure performed during the same appointment, and its 12-year follow-up was presented. A 44-year-old female patient was presented to our clinic with a firm, pedunculated, red gingival enlargement located on the labial surface of lower incisors. The exposed root surface, after the excisional biopsy, was covered with a free gingival graft. The lesion was pathologically diagnosed as pyogenic granuloma, and in the early postoperative phase, no recurrence was observed, but partial root coverage was determined. At 6-month follow-up, root coverage resulting from “creeping attachment” was observed, and this situation was maintained throughout the 12-year follow-up period. Repetitious postoperative discomfort and emotional stress for the patient may be avoided with a timesaving single appointment performing excisional biopsy and free gingival graft. Free gingival grafting procedure was used for this purpose not only to cover exposed root surfaces but also to eliminate dentin hypersensitivity and make oral hygiene procedures more effective. PMID:27403067

  4. Annealing a Follow-up Program: Improvement of the Dark Energy Figure of Merit for Optical Galaxy Cluster Surveys

    SciTech Connect

    Wu, Hao-Yi; Rozo, Eduardo; Wechsler, Risa H.; /KIPAC, Menlo Park /SLAC /CCAPP, Columbus /KICP, Chicago /KIPAC, Menlo Park /SLAC

    2010-06-02

    The precision of cosmological parameters derived from galaxy cluster surveys is limited by uncertainty in relating observable signals to cluster mass. We demonstrate that a small mass-calibration follow-up program can significantly reduce this uncertainty and improve parameter constraints, particularly when the follow-up targets are judiciously chosen. To this end, we apply a simulated annealing algorithm to maximize the dark energy information at fixed observational cost, and find that optimal follow-up strategies can reduce the observational cost required to achieve a specified precision by up to an order of magnitude. Considering clusters selected from optical imaging in the Dark Energy Survey, we find that approximately 200 low-redshift X-ray clusters or massive Sunyaev-Zel'dovich clusters can improve the dark energy figure of merit by 50%, provided that the follow-up mass measurements involve no systematic error. In practice, the actual improvement depends on (1) the uncertainty in the systematic error in follow-up mass measurements, which needs to be controlled at the 5% level to avoid severe degradation of the results; and (2) the scatter in the optical richness-mass distribution, which needs to be made as tight as possible to improve the efficacy of follow-up observations.

  5. THE AFTERGLOW AND ENVIRONMENT OF THE SHORT GRB 111117A

    SciTech Connect

    Margutti, R.; Berger, E.; Fong, W.; Zauderer, B. A.; Soderberg, A. M.; Milisavljevic, D.; Sanders, N.; Cenko, S. B.; Greiner, J.; Cucchiara, A.

    2012-09-01

    We present multi-wavelength observations of the afterglow of the short GRB 111117A, and follow-up observations of its host galaxy. From rapid optical and radio observations, we place limits of r {approx}> 25.5 mag at {delta}t Almost-Equal-To 0.55 days and F{sub {nu}}(5.8 GHz) {approx}< 18 {mu}Jy at {delta}t Almost-Equal-To 0.50 days, respectively. However, using a Chandra observation at {delta}t Almost-Equal-To 3.0 days we locate the absolute position of the X-ray afterglow to an accuracy of 0.''22 (1{sigma}), a factor of about six times better than the Swift/XRT position. This allows us to robustly identify the host galaxy and to locate the burst at a projected offset of 1.''25 {+-} 0.''20 from the host centroid. Using optical and near-IR observations of the host galaxy we determine a photometric redshift of z = 1.3{sup +0.3}{sub -0.2}, one of the highest for any short gamma-ray burst (GRB), leading to a projected physical offset for the burst of 10.5 {+-} 1.7 kpc, typical of previous short GRBs. At this redshift, the isotropic {gamma}-ray energy is E{sub {gamma},iso} Almost-Equal-To 3.0 Multiplication-Sign 10{sup 51} erg (rest-frame 23-2300 keV) with a peak energy of E{sub pk} Almost-Equal-To 850-2300 keV (rest-frame). In conjunction with the isotropic X-ray energy, GRB 111117A appears to follow our recently reported E{sub x,iso}-E{sub {gamma},iso}-E{sub pk} universal scaling. Using the X-ray data along with the optical and radio non-detections, we find that for a blastwave kinetic energy of E{sub K,iso} Almost-Equal-To E{sub {gamma},iso} erg, the circumburst density is n{sub 0} Almost-Equal-To 3 Multiplication-Sign 10{sup -4} - 1 cm{sup -3} (for a range of {epsilon}{sub B} = 0.001-0.1). Similarly, from the non-detection of a break in the X-ray light curve at {delta}t {approx}< 3 days, we infer a minimum opening angle for the outflow of {theta}{sub j} {approx}> 3-10 Degree-Sign (depending on the circumburst density). We conclude that Chandra observations of short

  6. 20 CFR 664.450 - What are follow-up services for youth?

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... 20 Employees' Benefits 4 2013-04-01 2013-04-01 false What are follow-up services for youth? 664..., and Parameters § 664.450 What are follow-up services for youth? (a) Follow-up services for youth may... in employment after training. (b) All youth participants must receive some form of follow-up...

  7. Swift and GRB's: Unveiling the Relativistic Universe

    NASA Technical Reports Server (NTRS)

    Marshall, Francis E.

    2006-01-01

    We report Swift observations of GRB 051109A, a bright, long burst detected with BAT. A bright afterglow was quickly detected with the X-Ray Telescope and Ultraviolet and Optical Telescope, and observations continued for more than 10 days. The X-ray light is complex with a rapid initial decay followed by a more gradual decay. There is evidence for a jet break with an indicated opening angle of a few degrees. UVOT observations with the V filter are consistent with a power-law day for the first 10 ks. We discuss the observations in light of current models.

  8. A follow up study of vibration induced white finger in compensation claimants

    PubMed Central

    Bovenzi, M; Della, V; Negro, C

    2005-01-01

    Aims: To follow up vibration induced white finger (VWF) in a selected group of 73 vibration exposed workers who claimed unsuccessfully for VWF compensation at a first examination. Methods: The VWF claimants were sent to our unit by the National Insurance Institute. The basic compensatory criteria included a positive history of VWF and abnormal cold response of the digital arteries. Following the first unsuccessful examination, over a mean time period of 4.1 (range 1–11) years the National Insurance Institute requested a second examination for all 73 claimants and a third examination for 29. During the follow up period, all subjects continued to work with vibratory tools. Results: There were 14 new cases who reported white finger during the follow up period. In the new VWF cases, finger blanching attacks became visible after about 3.5 years since the first examination. All incident cases of anamnestic VWF showed an abnormal cold response in the digital arteries and obtained compensation according to the basic compensatory criteria. In the entire sample of VWF claimants, there was a discrepancy between positive history of VWF symptoms at medical interview (55%) and abnormal cold provocation outcomes (19%). Digital arterial hyperresponsiveness to cold was associated with both VWF symptoms and the duration of vibration exposure since the first examination. Over the follow up period, a significant increase in the vasoconstrictor response to cold was observed in the vibration exposed workers with no symptoms of finger whiteness. Abnormal cold response was not associated with either age or smoking habit. Conclusions: Cold test measuring finger systolic blood pressure may be considered a useful laboratory method to confirm objectively VWF symptoms and to disclose abnormal cold induced vasoconstrictor response in vibration exposed workers with a negative history of VWF. Medical interview outcomes should be interpreted with caution in medicolegal situations involving VWF

  9. Lung Tumors Treated With Percutaneous Radiofrequency Ablation: Computed Tomography Imaging Follow-Up

    SciTech Connect

    Palussiere, Jean Marcet, Benjamin; Descat, Edouard; Deschamps, Frederic; Rao, Pramod; Ravaud, Alain; Brouste, Veronique; Baere, Thierry de

    2011-10-15

    Purpose: To describe the morphologic evolution of lung tumors treated with radiofrequency ablation (RFA) by way of computed tomography (CT) images and to investigate patterns of incomplete RFA at the site of ablation. Materials and Methods: One hundred eighty-nine patients with 350 lung tumors treated with RFA underwent CT imaging at 2, 4, 6, and 12 months. CT findings were interpreted separately by two reviewers with consensus. Five different radiologic patterns were predefined: fibrosis, cavitation, nodule, atelectasis, and disappearance. The appearance of the treated area was evaluated at each follow-up CT using the predefined patterns. Results: At 1 year after treatment, the most common evolutions were fibrosis (50.5%) or nodules (44.8%). Differences were noted depending on the initial size of the tumor, with fibrosis occurring more frequently for tumors <2 cm (58.6% vs. 22.9%, P = 1 Multiplication-Sign 10{sup -5}). Cavitation and atelectasis were less frequent patterns (2.4% and 1.4%, respectively, at 1 year). Tumor location (intraparenchymatous, with pleural contact <50% or >50%) was not significantly correlated with follow-up image pattern. Local tumor progressions were observed with each type of evolution. At 1 year, 12 local recurrences were noted: 2 cavitations, which represented 40% of the cavitations noted at 1 year; 2 fibroses (1.9%); 7 nodules (7.4%); and 1 atelectasis (33.3%). Conclusion: After RFA of lung tumors, follow-up CT scans show that the shape of the treatment zone can evolve in five different patterns. None of these patterns, however, can confirm the absence of further local tumor progression at subsequent follow-up.

  10. The effect of ulipristal acetate treatment on symptomatic uterine fibroids within 12-months follow-up

    PubMed Central

    Woźniak, Sławomir; Szkodziak, Piotr; Czuczwar, Piotr; Woźniakowska, Ewa; Paszkowski, Maciej; Milart, Paweł

    2014-01-01

    Aim of the study The purpose of the study was to monitor the effect of ulipristal acetate treatment on symptomatic uterine fibroids within 12-months follow-up. Material and methods Fifty six patients with symptomatic uterine fibroids qualified for surgical treatment were included in the prospective observational study. All patients received preoperative oral UPA treatment for 3 months (1 × 5 mg). Patients that refused surgical treatment after UPA therapy were followed-up for the next 9 months. The volume of the intramural fibroid was estimated by TV-US using and integrated VOCAL 3D imaging program at baseline, after 3 months of UPA treatment and further at 3-months intervals. Results Before UPA mean dominant fibroid volume was estimated to be 216.0 cm3 (38.4-768.2 cm3) and decreased to 117.6 cm3 (12.6-668.0 cm3) after 3 months of UPA therapy. Mean percentage volume reduction was 45.6%. Mean hemoglobin level increased from an initial 10.1 g/dL (6.8-12.9 g/dL) to 12.6 g/dL (10.1-14.8) after 3 months of UPA therapy. At 12 months after initiating UPA treatment mean dominant fibroid volume decreased by 43.9%. In one third of followed-up patients the effect of 3 month UPA therapy persisted for the next 9 months. Conclusions Three month UPA therapy decreases fibroid volume and improves hemoglobin level before planned surgical treatment. In one third of followed-up patients the effect of 3 month UPA therapy persisted for the next 9 months. PMID:26327823

  11. Profile and follow-up of patients with tuberculosis in a priority city in Brazil

    PubMed Central

    Pereira, Jisleny da Cruz; Silva, Marcio Roberto; da Costa, Ronaldo Rodrigues; Guimarães, Mark Drew Crosland; Leite, Isabel Cristina Gonçalves

    2015-01-01

    OBJECTIVE To analyze the cases of tuberculosis and the impact of direct follow-up on the assessment of treatment outcomes. METHODS This open prospective cohort study evaluated 504 cases of tuberculosis reported in the Sistema de Informação de Agravos de Notificação (SINAN – Notifiable Diseases Information System) in Juiz de Fora, MG, Southeastern Brazil, between 2008 and 2009. The incidence of treatment outcomes was compared between a group of patients diagnosed with tuberculosis and directly followed up by monthly consultations during return visits (287) and a patient group for which the information was indirectly collected (217) through the city’s surveillance system. The Chi-square test was used to compare the percentages, with a significance level of 0.05. The relative risk (RR) was used to evaluate the differences in the incidence rate of each type of treatment outcome between the two groups. RESULTS Of the outcomes directly and indirectly evaluated, 18.5% and 3.2% corresponded to treatment default and 3.8% and 0.5% corresponded to treatment failure, respectively. The incidence of treatment default and failure was higher in the group with direct follow-up (p < 0.05) (RR = 5.72, 95%CI 2.65;12.34, and RR = 8.31, 95%CI 1.08;63.92, respectively). CONCLUSIONS A higher incidence of treatment default and failure was observed in the directly followed up group, and most of these cases were neglected by the disease reporting system. Therefore, effective measures are needed to improve the control of tuberculosis and data quality. PMID:25741659

  12. Potential follow-up increases private contributions to public goods.

    PubMed

    Rogers, Todd; Ternovski, John; Yoeli, Erez

    2016-05-10

    People contribute more to public goods when their contributions are made more observable to others. We report an intervention that subtly increases the observability of public goods contributions when people are solicited privately and impersonally (e.g., mail, email, social media). This intervention is tested in a large-scale field experiment (n = 770,946) in which people are encouraged to vote through get-out-the-vote letters. We vary whether the letters include the message, "We may call you after the election to ask about your voting experience." Increasing the perceived observability of whether people vote by including that message increased the impact of the get-out-the-vote letters by more than the entire effect of a typical get-out-the-vote letter. This technique for increasing perceived observability can be replicated whenever public goods solicitations are made in private.

  13. Optical follow-up of ongoing flaring of BL Lacertae

    NASA Astrophysics Data System (ADS)

    Chandra, S.; Ganesh, S.; Baliyan, K. S.; Ahmad, N.; Jain, J. K.; Rajpurohit, G. S.

    2013-11-01

    We report the optical photometry of blazar BL Lacertae and confirm its ongoing flaring activity. This object was reported with flux enhancements in H band observations (ATel #5518, Carrasco et al). Later observations reported by many other groups present an increasing trend in NIR/Optical flux starting from mid October, 2013 (ATel 5550,5558). Historical peak flux was reported by Larionov et al. (ATel:#5597, R~12.34 mag) on 23rd November 2013.

  14. Observational Evidence for a Correlation between Peak Luminosities and Beaming in Gamma-Ray Bursts

    NASA Astrophysics Data System (ADS)

    van Putten, Maurice H. P. M.; Regimbau, Tania

    2003-08-01

    We calculate the unseen-but-true gamma-ray burst (GRB) event rate from a current flux-limited sample of 33 GRBs with individually measured redshifts. We consider a GRB event rate that is proportional to the star formation rate, in view of the GRB-supernovae association in SN 1998bw and GRB 030329. By fitting a lognormal distribution of GRB peak luminosities, we find a ratio 1/fr~=450 for the true-to-observed GRB event rates. This provides an independent derivation of the GRB beaming factor 1/fb~=500 obtained by Frail et al. from sources with standard GRB energies. We discuss applications to GRB 980425.

  15. Swift follow-up of SPIRITS16tn

    NASA Astrophysics Data System (ADS)

    Adams, S. M.; Jencson, J. E.; Kasliwal, M. M.

    2016-08-01

    We report Swift UVOT observations of SPIRITS16tn, a possible supernova in M108 (Jencson et al. ATel #9434). No source is detected in V, B, and U images taken on 2016-08-29.08 UT (14.0 days since SST discovery images) with exposure times of 540, 580, and 540s respectively.

  16. A Follow-up to Pop Culture: The Unpopular Culture.

    ERIC Educational Resources Information Center

    Whitworth, Richard

    1987-01-01

    Suggests an alternative approach for a popular culture course--an exploration of the culture of the students' parents, or "unpopular" culture. Possible activities for a unit include: interviews (on entertainment preferences, for example), observations (dress codes for social gatherings, parental food and drink habits, etc.), or an attic or closet…

  17. Swift follow up of IceCube-160731A

    NASA Astrophysics Data System (ADS)

    Evans, P. A.; Kennea, J. A.; Keivani, A.; Fox, D. B.; Tesic, G.; Cowen, D. F.; Osborne, J. P.; Smith, M. W. E.; Marshall, F. E.

    2016-08-01

    Swift has observed the field of the IceCube HESE event IceCube-160731A, "AMON ICECUBE HESE 128290 6888376" (revision 0), utilising the on-board 19-point tiling pattern to cover a region centred on RA,Dec (J2000) = (215.109, -0.458), with a radius of approximately 0.8 & deg;.

  18. Localization and broadband follow-up of the gravitational-wave transient GW150914

    DOE PAGESBeta

    Abbott, B. P.

    2016-07-20

    A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize themore » follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Furthermore, detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams.« less

  19. Localization and Broadband Follow-up of the Gravitational-wave Transient GW150914

    NASA Astrophysics Data System (ADS)

    Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M. R.; Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya, V. B.; Affeldt, C.; Agathos, M.; Agatsuma, K.; Aggarwal, N.; Aguiar, O. D.; Aiello, L.; Ain, A.; Ajith, P.; Allen, B.; Allocca, A.; Altin, P. A.; Anderson, S. B.; Anderson, W. G.; Arai, K.; Araya, M. C.; Arceneaux, C. C.; Areeda, J. S.; Arnaud, N.; Arun, K. G.; Ascenzi, S.; Ashton, G.; Ast, M.; Aston, S. M.; Astone, P.; Aufmuth, P.; Aulbert, C.; Babak, S.; Bacon, P.; Bader, M. K. M.; Baker, P. T.; Baldaccini, F.; Ballardin, G.; Ballmer, S. W.; Barayoga, J. C.; Barclay, S. E.; Barish, B. C.; Barker, D.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barta, D.; Barthelmy, S.; Bartlett, J.; Bartos, I.; Bassiri, R.; Basti, A.; Batch, J. C.; Baune, C.; Bavigadda, V.; Bazzan, M.; Behnke, B.; Bejger, M.; Bell, A. S.; Bell, C. J.; Berger, B. K.; Bergman, J.; Bergmann, G.; Berry, C. P. L.; Bersanetti, D.; Bertolini, A.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko, I. A.; Billingsley, G.; Birch, J.; Birney, R.; Biscans, S.; Bisht, A.; Bitossi, M.; Biwer, C.; Bizouard, M. A.; Blackburn, J. K.; Blair, C. D.; Blair, D. G.; Blair, R. M.; Bloemen, S.; Bock, O.; Bodiya, T. P.; Boer, M.; Bogaert, G.; Bogan, C.; Bohe, A.; Bojtos, P.; Bond, C.; Bondu, F.; Bonnand, R.; Boom, B. A.; Bork, R.; Boschi, V.; Bose, S.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brau, J. E.; Briant, T.; Brillet, A.; Brinkmann, M.; Brisson, V.; Brockill, P.; Brooks, A. F.; Brown, D. A.; Brown, D. D.; Brown, N. M.; Buchanan, C. C.; Buikema, A.; Bulik, T.; Bulten, H. J.; Buonanno, A.; Buskulic, D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Cahillane, C.; Bustillo, J. C.; Callister, T.; Calloni, E.; Camp, J. B.; Cannon, K. C.; Cao, J.; Capano, C. D.; Capocasa, E.; Carbognani, F.; Caride, S.; Diaz, J. C.; Casentini, C.; Caudill, S.; Cavagliá, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C. B.; Baiardi, L. C.; Cerretani, G.; Cesarini, E.; Chakraborty, R.; Chalermsongsak, T.; Chamberlin, S. J.; Chan, M.; Chao, S.; Charlton, P.; Chassande-Mottin, E.; Chen, H. Y.; Chen, Y.; Cheng, C.; Chincarini, A.; Chiummo, A.; Cho, H. S.; Cho, M.; Chow, J. H.; Christensen, N.; Chu, Q.; Chua, S.; Chung, S.; Ciani, G.; Clara, F.; Clark, J. A.; Cleva, F.; Coccia, E.; Cohadon, P.-F.; Colla, A.; Collette, C. G.; Cominsky, L.; Constancio, M., Jr.; Conte, A.; Conti, L.; Cook, D.; Corbitt, T. R.; Cornish, N.; Corsi, A.; Cortese, S.; Costa, C. A.; Coughlin, M. W.; Coughlin, S. B.; Coulon, J.-P.; Countryman, S. T.; Couvares, P.; Cowan, E. E.; Coward, D. M.; Cowart, M. J.; Coyne, D. C.; Coyne, R.; Craig, K.; Creighton, J. D. E.; Cripe, J.; Crowder, S. G.; Cumming, A.; Cunningham, L.; Cuoco, E.; Dal Canton, T.; Danilishin, S. L.; D'Antonio, S.; Danzmann, K.; Darman, N. S.; Dattilo, V.; Dave, I.; Daveloza, H. P.; Davier, M.; Davies, G. S.; Daw, E. J.; Day, R.; DeBra, D.; Debreczeni, G.; Degallaix, J.; De Laurentis, M.; Deléglise, S.; Del Pozzo, W.; Denker, T.; Dent, T.; Dereli, H.; Dergachev, V.; DeRosa, R. T.; De Rosa, R.; DeSalvo, R.; Dhurandhar, S.; Díaz, M. C.; Di Fiore, L.; Di Giovanni, M.; Di Lieto, A.; Di Pace, S.; Di Palma, I.; Di Virgilio, A.; Dojcinoski, G.; Dolique, V.; Donovan, F.; Dooley, K. L.; Doravari, S.; Douglas, R.; Downes, T. P.; Drago, M.; Drever, R. W. P.; Driggers, J. C.; Du, Z.; Ducrot, M.; Dwyer, S. E.; Edo, T. B.; Edwards, M. C.; Effler, A.; Eggenstein, H.-B.; Ehrens, P.; Eichholz, J.; Eikenberry, S. S.; Engels, W.; Essick, R. C.; Etzel, T.; Evans, M.; Evans, T. M.; Everett, R.; Factourovich, M.; Fafone, V.; Fair, H.; Fairhurst, S.; Fan, X.; Fang, Q.; Farinon, S.; Farr, B.; Farr, W. M.; Favata, M.; Fays, M.; Fehrmann, H.; Fejer, M. M.; Ferrante, I.; Ferreira, E. C.; Ferrini, F.; Fidecaro, F.; Fiori, I.; Fiorucci, D.; Fisher, R. P.; Flaminio, R.; Fletcher, M.; Fournier, J.-D.; Franco, S.; Frasca, S.; Frasconi, F.; Frei, Z.; Freise, A.; Frey, R.; Frey, V.; Fricke, T. T.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Gabbard, H. A. G.; Gair, J. R.; Gammaitoni, L.; Gaonkar, S. G.; Garufi, F.; Gatto, A.; Gaur, G.; Gehrels, N.; Gemme, G.; Gendre, B.; Genin, E.; Gennai, A.; George, J.; Gergely, L.; Germain, V.; Ghosh, A.; Ghosh, S.; Giaime, J. A.; Giardina, K. D.; Giazotto, A.; Gill, K.; Glaefke, A.; Goetz, E.; Goetz, R.; Gondan, L.; González, G.; Castro, J. M. G.; Gopakumar, A.; Gordon, N. A.; Gorodetsky, M. L.; Gossan, S. E.; Gosselin, M.; Gouaty, R.; Graef, C.; Graff, P. B.; Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greco, G.; Green, A. C.; Groot, P.; Grote, H.; Grunewald, S.; Guidi, G. M.; Guo, X.; Gupta, A.; Gupta, M. K.; Gushwa, K. E.; Gustafson, E. K.; Gustafson, R.; Hacker, J. J.; Hall, B. R.; Hall, E. D.; Hammond, G.; Haney, M.; Hanke, M. M.; Hanks, J.; Hanna, C.; Hannam, M. D.; Hanson, J.; Hardwick, T.; Haris, K.; Harms, J.; Harry, G. M.; Harry, I. W.; Hart, M. J.; Hartman, M. T.; Haster, C.-J.; Haughian, K.; Heidmann, A.; Heintze, M. C.; Heitmann, H.; Hello, P.; Hemming, G.; Hendry, M.; Heng, I. S.; Hennig, J.; Heptonstall, A. W.; Heurs, M.; Hild, S.; Hoak, D.; Hodge, K. A.; Hofman, D.; Hollitt, S. E.; Holt, K.; Holz, D. E.; Hopkins, P.; Hosken, D. J.; Hough, J.; Houston, E. A.; Howell, E. J.; Hu, Y. M.; Huang, S.; Huerta, E. A.; Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Idrisy, A.; Indik, N.; Ingram, D. R.; Inta, R.; Isa, H. N.; Isac, J.-M.; Isi, M.; Islas, G.; Isogai, T.; Iyer, B. R.; Izumi, K.; Jacqmin, T.; Jang, H.; Jani, K.; Jaranowski, P.; Jawahar, S.; Jiménez-Forteza, F.; Johnson, W. W.; Jones, D. I.; Jones, R.; Jonker, R. J. G.; Ju, L.; Kalaghatgi, C. V.; Kalogera, V.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Karki, S.; Kasprzack, M.; Katsavounidis, E.; Katzman, W.; Kaufer, S.; Kaur, T.; Kawabe, K.; Kawazoe, F.; Kéfélian, F.; Kehl, M. S.; Keitel, D.; Kelley, D. B.; Kells, W.; Kennedy, R.; Key, J. S.; Khalaidovski, A.; Khalili, F. Y.; Khan, I.; Khan, S.; Khan, Z.; Khazanov, E. A.; Kijbunchoo, N.; Kim, C.; Kim, J.; Kim, K.; Kim, N.; Kim, N.; Kim, Y.-M.; King, E. J.; King, P. J.; Kinzel, D. L.; Kissel, J. S.; Kleybolte, L.; Klimenko, S.; Koehlenbeck, S. M.; Kokeyama, K.; Koley, S.; Kondrashov, V.; Kontos, A.; Korobko, M.; Korth, W. Z.; Kowalska, I.; Kozak, D. B.; Kringel, V.; Królak, A.; Krueger, C.; Kuehn, G.; Kumar, P.; Kuo, L.; Kutynia, A.; Lackey, B. D.; Landry, M.; Lange, J.; Lantz, B.; Lasky, P. D.; Lazzarini, A.; Lazzaro, C.; Leaci, P.; Leavey, S.; Lebigot, E. O.; Lee, C. H.; Lee, H. K.; Lee, H. M.; Lee, K.; Lenon, A.; Leonardi, M.; Leong, J. R.; Leroy, N.; Letendre, N.; Levin, Y.; Levine, B. M.; Li, T. G. F.; Libson, A.; Littenberg, T. B.; Lockerbie, N. A.; Logue, J.; Lombardi, A. L.; Lord, J. E.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lough, J. D.; Lück, H.; Lundgren, A. P.; Luo, J.; Lynch, R.; Ma, Y.; MacDonald, T.; Machenschalk, B.; MacInnis, M.; Macleod, D. M.; Magaña-Sandoval, F.; Magee, R. M.; Mageswaran, M.; Majorana, E.; Maksimovic, I.; Malvezzi, V.; Man, N.; Mandel, I.; Mandic, V.; Mangano, V.; Mansell, G. L.; Manske, M.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markosyan, A. S.; Maros, E.; Martelli, F.; Martellini, L.; Martin, I. W.; Martin, R. M.; Martynov, D. V.; Marx, J. N.; Mason, K.; Masserot, A.; Massinger, T. J.; Masso-Reid, M.; Matichard, F.; Matone, L.; Mavalvala, N.; Mazumder, N.; Mazzolo, G.; McCarthy, R.; McClelland, D. E.; McCormick, S.; McGuire, S. C.; McIntyre, G.; McIver, J.; McManus, D. J.; McWilliams, S. T.; Meacher, D.; Meadors, G. D.; Meidam, J.; Melatos, A.; Mendell, G.; Mendoza-Gandara, D.; Mercer, R. A.; Merilh, E.; Merzougui, M.; Meshkov, S.; Messenger, C.; Messick, C.; Meyers, P. M.; Mezzani, F.; Miao, H.; Michel, C.; Middleton, H.; Mikhailov, E. E.; Milano, L.; Miller, J.; Millhouse, M.; Minenkov, Y.; Ming, J.; Mirshekari, S.; Mishra, C.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Moggi, A.; Mohan, M.; Mohapatra, S. R. P.; Montani, M.; Moore, B. C.; Moore, C. J.; Moraru, D.; Moreno, G.; Morriss, S. R.; Mossavi, K.; Mours, B.; Mow-Lowry, C. M.; Mueller, C. L.; Mueller, G.; Muir, A. W.; Mukherjee, A.; Mukherjee, D.; Mukherjee, S.; Mukund, N.; Mullavey, A.; Munch, J.; Murphy, D. J.; Murray, P. G.; Mytidis, A.; Nardecchia, I.; Naticchioni, L.; Nayak, R. K.; Necula, V.; Nedkova, K.; Nelemans, G.; Neri, M.; Neunzert, A.; Newton, G.; Nguyen, T. T.; Nielsen, A. B.; Nissanke, S.; Nitz, A.; Nocera, F.; Nolting, D.; Normandin, M. E. N.; Nuttall, L. K.; Oberling, J.; Ochsner, E.; O'Dell, J.; Oelker, E.; Ogin, G. H.; Oh, J. J.; Oh, S. H.; Ohme, F.; Oliver, M.; Oppermann, P.; Oram, R. J.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pai, A.; Pai, S. A.; Palamos, J. R.; Palashov, O.; Palliyaguru, N.; Palomba, C.; Pal-Singh, A.; Pan, H.; Pankow, C.; Pannarale, F.; Pant, B. C.; Paoletti, F.; Paoli, A.; Papa, M. A.; Paris, H. R.; Parker, W.; Pascucci, D.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patricelli, B.; Patrick, Z.; Pearlstone, B. L.; Pedraza, M.; Pedurand, R.; Pekowsky, L.; Pele, A.; Penn, S.; Perreca, A.; Phelps, M.; Piccinni, O.; Pichot, M.; Piergiovanni, F.; Pierro, V.; Pillant, G.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Poggiani, R.; Popolizio, P.; Post, A.; Powell, J.; Prasad, J.; Predoi, V.; Premachandra, S. S.; Prestegard, T.; Price, L. R.; Prijatelj, M.; Principe, M.; Privitera, S.; Prodi, G. A.; Prokhorov, L.; Puncken, O.; Punturo, M.; Puppo, P.; Pürrer, M.; Qi, H.; Qin, J.; Quetschke, V.; Quintero, E. A.; Quitzow-James, R.; Raab, F. J.; Rabeling, D. S.; Radkins, H.; Raffai, P.; Raja, S.; Rakhmanov, M.; Rapagnani, P.; Raymond, V.; Razzano, M.; Re, V.; Read, J.; Reed, C. M.; Regimbau, T.; Rei, L.; Reid, S.; Reitze, D. H.; Rew, H.; Reyes, S. D.; Ricci, F.; Riles, K.; Robertson, N. A.; Robie, R.; Robinet, F.; Rocchi, A.; Rolland, L.; Rollins, J. G.; Roma, V. J.; Romano, R.; Romanov, G.; Romie, J. H.; Rosińska, D.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sachdev, S.; Sadecki, T.; Sadeghian, L.; Salconi, L.; Saleem, M.; Salemi, F.; Samajdar, A.; Sammut, L.; Sanchez, E. J.; Sandberg, V.; Sandeen, B.; Sanders, J. R.; Sassolas, B.; Sathyaprakash, B. S.; Saulson, P. R.; Sauter, O.; Savage, R. L.; Sawadsky, A.; Schale, P.; Schilling, R.; Schmidt, J.; Schmidt, P.; Schnabel, R.; Schofield, R. M. S.; Schönbeck, A.; Schreiber, E.; Schuette, D.; Schutz, B. F.; Scott, J.; Scott, S. M.; Sellers, D.; Sentenac, D.; Sequino, V.; Sergeev, A.; Serna, G.; Setyawati, Y.; Sevigny, A.; Shaddock, D. A.; Shah, S.; Shahriar, M. S.; Shaltev, M.; Shao, Z.; Shapiro, B.; Shawhan, P.; Sheperd, A.; Shoemaker, D. H.; Shoemaker, D. M.; Siellez, K.; Siemens, X.; Sigg, D.; Silva, A. D.; Simakov, D.; Singer, A.; Singh, A.; Singh, R.; Singhal, A.; Sintes, A. M.; Slagmolen, B. J. J.; Smith, J. R.; Smith, N. D.; Smith, R. J. E.; Son, E. J.; Sorazu, B.; Sorrentino, F.; Souradeep, T.; Srivastava, A. K.; Staley, A.; Steinke, M.; Steinlechner, J.; Steinlechner, S.; Steinmeyer, D.; Stephens, B. C.; Stone, R.; Strain, K. A.; Straniero, N.; Stratta, G.; Strauss, N. A.; Strigin, S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sun, L.; Sutton, P. J.; Swinkels, B. L.; Szczepańczyk, M. J.; Tacca, M.; Talukder, D.; Tanner, D. B.; Tápai, M.; Tarabrin, S. P.; Taracchini, A.; Taylor, R.; Theeg, T.; Thirugnanasambandam, M. P.; Thomas, E. G.; Thomas, M.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.; Tiwari, S.; Tiwari, V.; Tokmakov, K. V.; Tomlinson, C.; Tonelli, M.; Torres, C. V.; Torrie, C. I.; Töyrä, D.; Travasso, F.; Traylor, G.; Trifirò, D.; Tringali, M. C.; Trozzo, L.; Tse, M.; Turconi, M.; Tuyenbayev, D.; Ugolini, D.; Unnikrishnan, C. S.; Urban, A. L.; Usman, S. A.; Vahlbruch, H.; Vajente, G.; Valdes, G.; van Bakel, N.; van Beuzekom, M.; van den Brand, J. F. J.; Van Den Broeck, C.; Vander-Hyde, D. C.; van der Schaaf, L.; van Heijningen, J. V.; van Veggel, A. A.; Vardaro, M.; Vass, S.; Vasúth, M.; Vaulin, R.; Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Venkateswara, K.; Verkindt, D.; Vetrano, F.; Viceré, A.; Vinciguerra, S.; Vine, D. J.; Vinet, J.-Y.; Vitale, S.; Vo, T.; Vocca, H.; Vorvick, C.; Voss, D.; Vousden, W. D.; Vyatchanin, S. P.; Wade, A. R.; Wade, L. E.; Wade, M.; Walker, M.; Wallace, L.; Walsh, S.; Wang, G.; Wang, H.; Wang, M.; Wang, X.; Wang, Y.; Ward, R. L.; Warner, J.; Was, M.; Weaver, B.; Wei, L.-W.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Welborn, T.; Wen, L.; Weßels, P.; Westphal, T.; Wette, K.; Whelan, J. T.; White, D. J.; Whiting, B. F.; Williams, R. D.; Williamson, A. R.; Willis, J. L.; Willke, B.; Wimmer, M. H.; Winkler, W.; Wipf, C. C.; Wittel, H.; Woan, G.; Worden, J.; Wright, J. L.; Wu, G.; Yablon, J.; Yam, W.; Yamamoto, H.; Yancey, C. C.; Yap, M. J.; Yu, H.; Yvert, M.; Zadrożny, A.; Zangrando, L.; Zanolin, M.; Zendri, J.-P.; Zevin, M.; Zhang, F.; Zhang, L.; Zhang, M.; Zhang, Y.; Zhao, C.; Zhou, M.; Zhou, Z.; Zhu, X. J.; Zucker, M. E.; Zuraw, S. E.; Zweizig, J.; LIGO Scientific Collaboration; Virgo Collaboration; Allison, J.; Bannister, K.; Bell, M. E.; Chatterjee, S.; Chippendale, A. P.; Edwards, P. G.; Harvey-Smith, L.; Heywood, Ian; Hotan, A.; Indermuehle, B.; Marvil, J.; McConnell, D.; Murphy, T.; Popping, A.; Reynolds, J.; Sault, R. J.; Voronkov, M. A.; Whiting, M. T.; Australian Square Kilometer Array Pathfinder (ASKAP) Collaboration; Castro-Tirado, A. J.; Cunniffe, R.; Jelínek, M.; Tello, J. C.; Oates, S. R.; Hu, Y.-D.; Kubánek, P.; Guziy, S.; Castellón, A.; García-Cerezo, A.; Muñoz, V. F.; Pérez del Pulgar, C.; Castillo-Carrión, S.; Castro Cerón, J. M.; Hudec, R.; Caballero-García, M. D.; Páta, P.; Vitek, S.; Adame, J. A.; Konig, S.; Rendón, F.; Mateo Sanguino, T. de J.; Fernández-Muñoz, R.; Yock, P. C.; Rattenbury, N.; Allen, W. H.; Querel, R.; Jeong, S.; Park, I. H.; Bai, J.; Cui, Ch.; Fan, Y.; Wang, Ch.; Hiriart, D.; Lee, W. H.; Claret, A.; Sánchez-Ramírez, R.; Pandey, S. B.; Mediavilla, T.; Sabau-Graziati, L.; BOOTES Collaboration; Abbott, T. M. C.; Abdalla, F. B.; Allam, S.; Annis, J.; Armstrong, R.; Benoit-Lévy, A.; Berger, E.; Bernstein, R. A.; Bertin, E.; Brout, D.; Buckley-Geer, E.; Burke, D. L.; Capozzi, D.; Carretero, J.; Castander, F. J.; Chornock, R.; Cowperthwaite, P. S.; Crocce, M.; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Doctor, Z.; Drlica-Wagner, A.; Drout, M. R.; Eifler, T. F.; Estrada, J.; Evrard, A. E.; Fernandez, E.; Finley, D. A.; Flaugher, B.; Foley, R. J.; Fong, W.-F.; Fosalba, P.; Fox, D. B.; Frieman, J.; Fryer, C. L.; Gaztanaga, E.; Gerdes, D. W.; Goldstein, D. A.; Gruen, D.; Gruendl, R. A.; Gutierrez, G.; Herner, K.; Honscheid, K.; James, D. J.; Johnson, M. D.; Johnson, M. W. G.; Karliner, I.; Kasen, D.; Kent, S.; Kessler, R.; Kim, A. G.; Kind, M. C.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Li, T. S.; Lima, M.; Lin, H.; Maia, M. A. G.; Margutti, R.; Marriner, J.; Martini, P.; Matheson, T.; Melchior, P.; Metzger, B. D.; Miller, C. J.; Miquel, R.; Neilsen, E.; Nichol, R. C.; Nord, B.; Nugent, P.; Ogando, R.; Petravick, D.; Plazas, A. A.; Quataert, E.; Roe, N.; Romer, A. K.; Roodman, A.; Rosell, A. C.; Rykoff, E. S.; Sako, M.; Sanchez, E.; Scarpine, V.; Schindler, R.; Schubnell, M.; Scolnic, D.; Sevilla-Noarbe, I.; Sheldon, E.; Smith, N.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Stebbins, A.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thaler, J.; Thomas, D.; Thomas, R. C.; Tucker, D. L.; Vikram, V.; Walker, A. R.; Wechsler, R. H.; Wester, W.; Yanny, B.; Zhang, Y.; Zuntz, J.; Dark Energy Survey; Dark Energy Camera GW-EM Collaboration; Connaughton, V.; Burns, E.; Goldstein, A.; Briggs, M. S.; Zhang, B.-B.; Hui, C. M.; Jenke, P.; Wilson-Hodge, C. A.; Bhat, P. N.; Bissaldi, E.; Cleveland, W.; Fitzpatrick, G.; Giles, M. M.; Gibby, M. H.; Greiner, J.; von Kienlin, A.; Kippen, R. M.; McBreen, S.; Mailyan, B.; Meegan, C. A.; Paciesas, W. S.; Preece, R. D.; Roberts, O.; Sparke, L.; Stanbro, M.; Toelge, K.; Veres, P.; Yu, H.-F.; Blackburn, L.; Fermi GBM Collaboration; Ackermann, M.; Ajello, M.; Albert, A.; Anderson, B.; Atwood, W. B.; Axelsson, M.; Baldini, L.; Barbiellini, G.; Bastieri, D.; Bellazzini, R.; Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonino, R.; Bottacini, E.; Brandt, T. J.; Bruel, P.; Buson, S.; Caliandro, G. A.; Cameron, R. A.; Caragiulo, M.; Caraveo, P. A.; Cavazzuti, E.; Charles, E.; Chekhtman, A.; Chiang, J.; Chiaro, G.; Ciprini, S.; Cohen-Tanugi, J.; Cominsky, L. R.; Costanza, F.; Cuoco, A.; D'Ammando, F.; de Palma, F.; Desiante, R.; Digel, S. W.; Di Lalla, N.; Di Mauro, M.; Di Venere, L.; Domínguez, A.; Drell, P. S.; Dubois, R.; Favuzzi, C.; Ferrara, E. C.; Franckowiak, A.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Gomez-Vargas, G. A.; Green, D.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Harding, A. K.; Hays, E.; Hewitt, J. W.; Hill, A. B.; Horan, D.; Jogler, T.; Jóhannesson, G.; Johnson, A. S.; Kensei, S.; Kocevski, D.; Kuss, M.; La Mura, G.; Larsson, S.; Latronico, L.; Li, J.; Li, L.; Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Magill, J.; Maldera, S.; Manfreda, A.; Marelli, M.; Mayer, M.; Mazziotta, M. N.; McEnery, J. E.; Meyer, M.; Michelson, P. F.; Mirabal, N.; Mizuno, T.; Moiseev, A. A.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Negro, M.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orienti, M.; Orlando, E.; Ormes, J. F.; Paneque, D.; Perkins, J. S.; Pesce-Rollins, M.; Piron, F.; Pivato, G.; Porter, T. A.; Racusin, J. L.; Rainò, S.; Rando, R.; Razzaque, S.; Reimer, A.; Reimer, O.; Salvetti, D.; Saz Parkinson, P. M.; Sgrò, C.; Simone, D.; Siskind, E. J.; Spada, F.; Spandre, G.; Spinelli, P.; Suson, D. J.; Tajima, H.; Thayer, J. B.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Troja, E.; Uchiyama, Y.; Venters, T. M.; Vianello, G.; Wood, K. S.; Wood, M.; Zhu, S.; Zimmer, S.; Fermi LAT Collaboration; Brocato, E.; Cappellaro, E.; Covino, S.; Grado, A.; Nicastro, L.; Palazzi, E.; Pian, E.; Amati, L.; Antonelli, L. A.; Capaccioli, M.; D'Avanzo, P.; D'Elia, V.; Getman, F.; Giuffrida, G.; Iannicola, G.; Limatola, L.; Lisi, M.; Marinoni, S.; Marrese, P.; Melandri, A.; Piranomonte, S.; Possenti, A.; Pulone, L.; Rossi, A.; Stamerra, A.; Stella, L.; Testa, V.; Tomasella, L.; Yang, S.; GRAvitational Wave Inaf TeAm (GRAWITA); Bazzano, A.; Bozzo, E.; Brandt, S.; Courvoisier, T. J.-L.; Ferrigno, C.; Hanlon, L.; Kuulkers, E.; Laurent, P.; Mereghetti, S.; Roques, J. P.; Savchenko, V.; Ubertini, P.; INTEGRAL Collaboration; Kasliwal, M. M.; Singer, L. P.; Cao, Y.; Duggan, G.; Kulkarni, S. R.; Bhalerao, V.; Miller, A. A.; Barlow, T.; Bellm, E.; Manulis, I.; Rana, J.; Laher, R.; Masci, F.; Surace, J.; Rebbapragada, U.; Cook, D.; Van Sistine, A.; Sesar, B.; Perley, D.; Ferreti, R.; Prince, T.; Kendrick, R.; Horesh, A.; Intermediate Palomar Transient Factory (iPTF) Collaboration; Hurley, K.; Golenetskii, S. V.; Aptekar, R. L.; Frederiks, D. D.; Svinkin, D. S.; Rau, A.; von Kienlin, A.; Zhang, X.; Smith, D. M.; Cline, T.; Krimm, H.; InterPlanetary Network; Abe, F.; Doi, M.; Fujisawa, K.; Kawabata, K. S.; Morokuma, T.; Motohara, K.; Tanaka, M.; Ohta, K.; Yanagisawa, K.; Yoshida, M.; J-GEM Collaboration; Baltay, C.; Rabinowitz, D.; Ellman, N.; Rostami, S.; La Silla–QUEST Survey; Bersier, D. F.; Bode, M. F.; Collins, C. A.; Copperwheat, C. M.; Darnley, M. J.; Galloway, D. K.; Gomboc, A.; Kobayashi, S.; Mazzali, P.; Mundell, C. G.; Piascik, A. S.; Pollacco, Don; Steele, I. A.; Ulaczyk, K.; Liverpool Telescope Collaboration; Broderick, J. W.; Fender, R. P.; Jonker, P. G.; Rowlinson, A.; Stappers, B. W.; Wijers, R. A. M. J.; Low Frequency Array (LOFAR) Collaboration; Lipunov, V.; Gorbovskoy, E.; Tyurina, N.; Kornilov, V.; Balanutsa, P.; Kuznetsov, A.; Buckley, D.; Rebolo, R.; Serra-Ricart, M.; Israelian, G.; Budnev, N. M.; Gress, O.; Ivanov, K.; Poleshuk, V.; Tlatov, A.; Yurkov, V.; MASTER Collaboration; Kawai, N.; Serino, M.; Negoro, H.; Nakahira, S.; Mihara, T.; Tomida, H.; Ueno, S.; Tsunemi, H.; Matsuoka, M.; MAXI Collaboration; Croft, S.; Feng, L.; Franzen, T. M. O.; Gaensler, B. M.; Johnston-Hollitt, M.; Kaplan, D. L.; Morales, M. F.; Tingay, S. J.; Wayth, R. B.; Williams, A.; Murchison Wide-field Array (MWA) Collaboration; Smartt, S. J.; Chambers, K. C.; Smith, K. W.; Huber, M. E.; Young, D. R.; Wright, D. E.; Schultz, A.; Denneau, L.; Flewelling, H.; Magnier, E. A.; Primak, N.; Rest, A.; Sherstyuk, A.; Stalder, B.; Stubbs, C. W.; Tonry, J.; Waters, C.; Willman, M.; Pan-STARRS Collaboration; Olivares E., F.; Campbell, H.; Kotak, R.; Sollerman, J.; Smith, M.; Dennefeld, M.; Anderson, J. P.; Botticella, M. T.; Chen, T.-W.; Della Valle, M.; Elias-Rosa, N.; Fraser, M.; Inserra, C.; Kankare, E.; Kupfer, T.; Harmanen, J.; Galbany, L.; Le Guillou, L.; Lyman, J. D.; Maguire, K.; Mitra, A.; Nicholl, M.; Razza, A.; Terreran, G.; Valenti, S.; Gal-Yam, A.; PESSTO Collaboration; Ćwiek, A.; Ćwiok, M.; Mankiewicz, L.; Opiela, R.; Zaremba, M.; Żarnecki, A. F.; Pi of Sky Collaboration; Onken, C. A.; Scalzo, R. A.; Schmidt, B. P.; Wolf, C.; Yuan, F.; SkyMapper Collaboration; Evans, P. A.; Kennea, J. A.; Burrows, D. N.; Campana, S.; Cenko, S. B.; Giommi, P.; Marshall, F. E.; Nousek, J.; O'Brien, P.; Osborne, J. P.; Palmer, D.; Perri, M.; Siegel, M.; Tagliaferri, G.; Swift Collaboration; Klotz, A.; Turpin, D.; Laugier, R.; TAROT, Zadko, Algerian National Observatory, C2PU Collaboration; Beroiz, M.; Peñuela, T.; Macri, L. M.; Oelkers, R. J.; Lambas, D. G.; Vrech, R.; Cabral, J.; Colazo, C.; Dominguez, M.; Sanchez, B.; Gurovich, S.; Lares, M.; Marshall, J. L.; DePoy, D. L.; Padilla, N.; Pereyra, N. A.; Benacquista, M.; TOROS Collaboration; Tanvir, N. R.; Wiersema, K.; Levan, A. J.; Steeghs, D.; Hjorth, J.; Fynbo, J. P. U.; Malesani, D.; Milvang-Jensen, B.; Watson, D.; Irwin, M.; Fernandez, C. G.; McMahon, R. G.; Banerji, M.; Gonzalez-Solares, E.; Schulze, S.; de Ugarte Postigo, A.; Thoene, C. C.; Cano, Z.; Rosswog, S.; VISTA Collaboration

    2016-07-01

    A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline, and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams.

  20. Collodion baby: a follow-up study of 17 cases.

    PubMed

    Van Gysel, D; Lijnen, R L P; Moekti, S S; de Laat, P C J; Oranje, A P

    2002-09-01

    Seventeen cases of collodion baby are reported. Clinical aspects, complications, treatment, final outcome and family history were studied. We did not observe any clinical features in the collodion baby that could serve as a clue in predicting the final diagnosis. Infections were observed in nine, hypothermia in five and hypernatraemic dehydration in four cases. Skin infection mainly occurred in babies treated with emollients (petrolatum, lanolin and cetomacrogolis cream were used). We therefore recommend treating the collodion baby in a humidified incubator, if necessary with intravenous rehydration, but not to use emollients. The final outcome of these study patients was erythrodermic autosomal recessive lamellar ichthyosis in seven cases (41%), non-erythrodermic autosomal recessive lamellar ichthyosis in three cases (18%), Sjögren-Larsson in one case (6%), epidermolytic hyperkeratosis in one case (6%), acute neonatal variant of Gaucher disease in one case (6%) and normal skin in four cases (24%).

  1. [Twenty years' follow-up study of asbestos workers].

    PubMed

    Morinaga, K; Hara, I; Yasui, I; Yokoyama, K; Sera, Y

    1990-07-01

    This report describes a cohort study conducted on workers who were employed in a factory mainly manufacturing asbestos yarn and cloth and were followed from 1964 to 1981. A total of 208 workers (73 males and 135 females) could be traced and 15 deaths were observed by the end of 1983. Among them, three had lung cancer and its relative risk was 6.8 (p less than 0.05) computed based on the age, sex and year specific death rates of Osaka Prefecture. One case of peritoneal mesothelioma was also found. The period from first asbestos exposure to death of these four cases of asbestos-related malignancies was more than 25 yr. In the analysis of the employees who had more than 1 yr of exposure to asbestos and those who had already been engaged in this factory at the beginning of the observation, the relative risk of lung cancer was 8.1 and 13.6, respectively.

  2. Follow-up of K2 planet candiates with the LCOGT network

    NASA Astrophysics Data System (ADS)

    Dragomir, Diana; Bayliss, Daniel; Colón, Knicole; Cochran, William; Zhou, George; Brown, Timothy; Shporer, Avi; Espinoza, Nestor; Fulton, Benjamin

    2015-12-01

    K2 has proven to be an outstanding successor to the Kepler mission. It has already revealed dozens of new planet candidates, and unlike those found by the primary mission, many of these systems’ host stars are sufficiently bright to allow extensive follow-up observations. This is especially important since each of the K2 observing campaigns are only ~80 days long, leaving the community with the discovery of exciting new systems but often not enough time coverage to enable a thorough characterization of these systems.We are leading a large effort to observe K2 transiting planet candidates with the LCOGT telescope network. LCOGT’s longitudinal coverage, multiple identical telescopes per site and automated queue observing make it an ideal facility for fast, high-precision and multi-color follow-up. Our program focuses on specific aspects of K2 follow-up for which the network is especially powerful: period determination for candidates with fewer than three K2 transits; transit timing variation monitoring to measure planetary masses, orbital parameters and to search for additional planets in multiple systems; and multi-color photometry to vet planet candidates and carry-out preliminary atmospheric spectroscopy.We will present new results for a selection of systems observed so far through this program. These include K2-19, a multi-planet system extremely close to 3:2 resonance and experiencing transit timing variations with amplitudes as large as one hour; EPIC201702477, a long-period planet with only two K2 transits; WASP-47, a system hosting a hot Jupiter and two K2-discovered small planets; and EPIC201637175b, a disintegrating rocky planet.Our program demonstrates that LCOGT is uniquely positioned to be the primary ground-based photometric follow-up resource for K2 exoplanet discoveries, but also for the numerous bright systems that will result from the TESS mission. LCOGT photometry complements ongoing radial velocity and atmospheric spectroscopy efforts to

  3. Patterns of Glaucoma Medication Adherence over Four Years of Follow-Up

    PubMed Central

    Newman-Casey, Paula Anne; Blachley, Taylor; Lee, Paul P.; Heisler, Michele; Farris, Karen B.; Stein, Joshua D.

    2015-01-01

    Purpose To assess longer-term patterns of glaucoma medication adherence and identify whether patterns of adherence established during the first year of medication use persist during three subsequent years of follow-up. Design Retrospective longitudinal cohort analysis. Participants Beneficiaries ≥40 years old enrolled in a U.S. managed care plan for ≥7 years between 2001-2012 newly diagnosed and treated for open-angle glaucoma. Methods For each enrollee, we quantified medication adherence using the medication possession ratio. Group-based trajectory modeling (GBTM) was applied to all enrollees to look for similar patterns of adherence for groups of enrollees. These patterns were described for 1 and 4 years of follow-up and analyses were performed to identify persons who experienced similar adherence patterns at 1 and 4 years and others who had dissimilar patterns. Factors impacting adherence at 1 and 4 years were identified using regression analyses. Main Outcome Measure Patterns of glaucoma medication adherence. Results Of the 1,234 eligible beneficiaries, GBTM identified five distinct glaucoma medication adherence patterns in both the one-year and four-year follow-up periods. These groups were: 1) Never adherent after their index prescription fill (7.5%,15.6% of persons in the one and four-year models, respectively); 2) Persistently very poor adherence (14.9%, 23.4%); 3) Declining adherence (9.5%, 9.1%); 4) Persistently moderate adherence (48.1%, 37.0%); and 5) Persistently good adherence (20.0%, 15.0%). Over 90% of beneficiaries in the 4 groups with the worst and best adherence patterns (Groups 1, 2, 3, 5) maintained their patterns from their first year throughout their 4 years of follow-up while those with Persistently moderate adherence (Group 4) – the largest sized group-were most likely to change groups from 1 to 4 years of follow-up. Persons with the best adherence over 4 years were more likely to be white, older age, earn >$60,000/year, and have more

  4. Control of Blood Pressure and Risk Attenuation: Post Trial Follow-Up of Randomized Groups

    PubMed Central

    Jafar, Tazeen H.; Jehan, Imtiaz; Liang, Feng; Barbier, Sylvaine; Islam, Muhammad; Bux, Rasool; Khan, Aamir Hameed; Nadkarni, Nivedita; Poulter, Neil; Chaturvedi, Nish; Ebrahim, Shah

    2015-01-01

    Background Evidence on long term effectiveness of public health strategies for lowering blood pressure (BP) is scarce. In the Control of Blood Pressure and Risk Attenuation (COBRA) Trial, a 2 x 2 factorial, cluster randomized controlled trial, the combined home health education (HHE) and trained general practitioner (GP) intervention delivered over 2 years was more effective than no intervention (usual care) in lowering systolic BP among adults with hypertension in urban Pakistan. However, it was not clear whether the effect would be sustained after the cessation of intervention. We conducted 7 years follow-up inclusive of 5 years of post intervention period of COBRA trial participants to assess the effectiveness of the interventions on BP during extended follow-up. Methods A total of 1341 individuals 40 years or older with hypertension (systolic BP 140 mm Hg or greater, diastolic BP 90 mm Hg or greater, or already receiving treatment) were followed by trained research staff masked to randomization status. BP was measured thrice with a calibrated automated device (Omron HEM-737 IntelliSense) in the sitting position after 5 minutes of rest. BP measurements were repeated after two weeks. Generalized estimating equations (GEE) were used to analyze the primary outcome of change in systolic BP from baseline to 7- year follow-up. The multivariable model was adjusted for clustering, age at baseline, sex, baseline systolic and diastolic BP, and presence of diabetes. Findings After 7 years of follow-up, systolic BP levels among those randomised to combined HHE plus trained GP intervention were significantly lower (2.1 [4.1–0.1] mm Hg) compared to those randomised to usual care, (P = 0.04). Participants receiving the combined intervention compared to usual care had a greater reduction in LDL-cholesterol (2.7 [4.8 to 0.6] mg/dl. Conclusions The benefit in systolic BP reduction observed in the original cohort assigned to the combined intervention was attenuated but still

  5. The association of clinical follow-up intervals in HIV-infected persons with viral suppression on subsequent viral suppression.

    PubMed

    Buscher, April; Mugavero, Michael; Westfall, Andrew O; Keruly, Jeanne; Moore, Richard; Drainoni, Mari-Lynn; Sullivan, Meg; Wilson, Tracey E; Rodriguez, Allan; Metsch, Lisa; Gardner, Lytt; Marks, Gary; Malitz, Faye; Giordano, Thomas P

    2013-08-01

    The recommendation for the frequency for routine clinical monitoring of persons with well-controlled HIV infection is based on evidence that relies on observed rather than intended follow-up intervals. We sought to determine if the scheduled follow-up interval is associated with subsequent virologic failure. Participants in this 6-clinic retrospective cohort study had an index clinic visit in 2008 and HIV viral load (VL) ≤400 c/mL. Univariate and multivariate tests evaluated if scheduling the next follow-up appointment at 3, 4, or 6 months predicted VL >400 c/mL at 12 months (VF). Among 2171 participants, 66%, 26%, and 8% were scheduled next follow-up visits at 3, 4, and 6 months, respectively. With missing 12-month VL considered VF, 25%, 25%, and 24% of persons scheduled at 3, 4, and 6 months had VF, respectively (p=0.95). Excluding persons with missing 12-month VL, 7.1%, 5.7%, and 4.5% had VF, respectively (p=0.35). Multivariable models yielded nonsignificant odds of VF by scheduled follow-up interval both when missing 12-month VL were considered VF and when persons with missing 12-month VL were excluded. We conclude that clinicians are able to make safe decisions extending follow-up intervals in persons with viral suppression, at least in the short-term.

  6. A real-time fast radio burst: polarization detection and multiwavelength follow-up

    NASA Astrophysics Data System (ADS)

    Petroff, E.; Bailes, M.; Barr, E. D.; Barsdell, B. R.; Bhat, N. D. R.; Bian, F.; Burke-Spolaor, S.; Caleb, M.; Champion, D.; Chandra, P.; Da Costa, G.; Delvaux, C.; Flynn, C.; Gehrels, N.; Greiner, J.; Jameson, A.; Johnston, S.; Kasliwal, M. M.; Keane, E. F.; Keller, S.; Kocz, J.; Kramer, M.; Leloudas, G.; Malesani, D.; Mulchaey, J. S.; Ng, C.; Ofek, E. O.; Perley, D. A.; Possenti, A.; Schmidt, B. P.; Shen, Yue; Stappers, B.; Tisserand, P.; van Straten, W.; Wolf, C.

    2015-02-01

    Fast radio bursts (FRBs) are one of the most tantalizing mysteries of the radio sky; their progenitors and origins remain unknown and until now no rapid multiwavelength follow-up of an FRB has been possible. New instrumentation has decreased the time between observation and discovery from years to seconds, and enables polarimetry to be performed on FRBs for the first time. We have discovered an FRB (FRB 140514) in real-time on 2014 May 14 at 17:14:11.06 UTC at the Parkes radio telescope and triggered follow-up at other wavelengths within hours of the event. FRB 140514 was found with a dispersion measure (DM) of 562.7(6) cm-3 pc, giving an upper limit on source redshift of z ≲ 0.5. FRB 140514 was found to be 21 ± 7 per cent (3σ) circularly polarized on the leading edge with a 1σ upper limit on linear polarization <10 per cent. We conclude that this polarization is intrinsic to the FRB. If there was any intrinsic linear polarization, as might be expected from coherent emission, then it may have been depolarized by Faraday rotation caused by passing through strong magnetic fields and/or high-density environments. FRB 140514 was discovered during a campaign to re-observe known FRB fields, and lies close to a previous discovery, FRB 110220; based on the difference in DMs of these bursts and time-on-sky arguments, we attribute the proximity to sampling bias and conclude that they are distinct objects. Follow-up conducted by 12 telescopes observing from X-ray to radio wavelengths was unable to identify a variable multiwavelength counterpart, allowing us to rule out models in which FRBs originate from nearby (z < 0.3) supernovae and long duration gamma-ray bursts.

  7. Workers exposed to ethylene oxide: a follow up study.

    PubMed Central

    Gardner, M J; Coggon, D; Pannett, B; Harris, E C

    1989-01-01

    A cohort study has been carried out of 2876 men and women with potential exposure to ethylene oxide. Subjects were identified from employment records at four companies that have produced or used ethylene oxide since the 1950s and at eight hospitals which have had ethylene oxide sterilising units since the 1960s. The cohort represents a substantial proportion of the British workforce with a history of occupational exposure to ethylene oxide. Industrial hygiene data were not available before 1977, but since then time weighted average exposures have been less than 5 ppm in almost all jobs and less than 1 ppm in many. Past exposures were probably somewhat higher. In contrast to some previous studies, no clear excess of leukaemia (three deaths observed, 2.09 expected) and no increase in stomach cancer (five deaths observed, 5.95 expected) were found. This discrepancy with earlier reports may be due in part to differences in levels of exposure. Total cancer mortality was similar to that expected from national and local death rates. Some specific cancers showed small excesses but their relevance to ethylene oxide exposure is doubtful. Again, contrary to some earlier reports, no excess of cardiovascular disease was found. This study does not exclude the possibility that ethylene oxide is a human carcinogen but suggests that any risk of cancer from currently permitted occupational exposures is small. PMID:2611160

  8. Following up on the Discovery of Water Vapor at Europa's South Pole with HST

    NASA Astrophysics Data System (ADS)

    Roth, L.; Retherford, K. D.; Saur, J.; Strobel, D. F.; Feldman, P. D.; McGrath, M. A.; Nimmo, F.; Spencer, J. R.; Grava, C.; Bloecker, A.

    2014-12-01

    We will present new Hubble Space Telescope (HST) observations of Europa's UV aurora obtained within two campaigns in 2014 to follow up on the water vapor plume detection. HST aurora images taken in 2012 have revealed coincident signals from atomic hydrogen and oxygen pointing to the existence of transient water vapor plumes near the south pole. The water vapor was detected only during one HST visit in December 2012 when Europa was near apocenter position and was speculated to be correlated with changing tidal stresses along Europa's orbit. In a first follow-up campaign new aurora images were taken by HST early in 2014 with Europa near apocenter, but the initial detection was not confirmed. More HST aurora images will be obtained in the course of a larger Hubble observing campaign starting in November 2014. We will review all HST aurora imaging observations to date and discuss potential sources for varying plume activity and changing detectability by HST. In particular, we will examine various explanations for the non-detections in the early 2014 observations near apocenter.

  9. Optical Studies of Space Debris at GEO: Survey and Follow-up with Two Telescopes

    NASA Technical Reports Server (NTRS)

    Seitzer, P.; Abercomby, K. J.; Rodriquez, H. M.; Barker, E. S.

    2007-01-01

    For 14 nights in March 2007, we used two telescopes at the Cerro Tololo Inter-American Observatory (CTIO) in Chile to study the nature of space debris at Geosynchronous Earth Orbit (GEO). In this project one telescope was dedicated to survey operations, while a second telescope was used for follow-up observations for orbits and colors. The goal was to obtain orbital and photometric information on every faint object found with the survey telescope. Thus we concentrate on objects fainter than R = 15th magnitude.

  10. Sherlock: An Automated Follow-Up Telescope for Wide-Field Transit Searches

    NASA Astrophysics Data System (ADS)

    Kotredes, L.; Charbonneau, D.; O'Donovan, F. T.; Looper, D. L.

    2003-12-01

    The current challenge facing photometric surveys for transiting gas-giant planets is that of confusion with eclipsing binary systems that mimic the photometric signature. A simple way to reject most forms of these false positives is high-precision, rapid-cadence monitoring of the suspected transit at higher angular resolution and in several filters. We are currently building a telescope that will perform higher-angular-resolution, multi-color follow-up observations of candidate systems identified by Sleuth (our wide-field transit survey instrument at Palomar), and its two twin instruments in Tenerife and northern Arizona.

  11. Sherlock: An Automated Follow-Up Telescope for Wide-Field Transit Searches

    NASA Astrophysics Data System (ADS)

    Kotredes, Lewis; Charbonneau, David; Looper, Dagny L.; O'Donovan, Francis T.

    2004-06-01

    The most significant challenge currently facing photometric surveys for transiting gas-giant planets is that of confusion with eclipsing binary systems that mimic the photometric signature. A simple way to reject most forms of these false positives is high-precision, rapid-cadence monitoring of the suspected transit at higher angular resolution and in several filters. We are currently building a system that will perform higher-angular-resolution, multi-color follow-up observations of candidate systems identified by Sleuth (our wide-field transit survey instrument at Palomar), and its two twin system instruments in Tenerife and northern Arizona.

  12. Autonomous global sky monitoring with real-time robotic follow-up

    SciTech Connect

    Vestrand, W Thomas; Davis, H; Wren, J; Wozniak, P; Norman, B; White, R; Bloch, J; Fenimore, E; Hodge, Barry; Jah, Moriba; Rast, Richard

    2008-01-01

    We discuss the development of prototypes for a global grid of advanced 'thinking' sky sentinels and robotic follow-up telescopes that observe the full night sky to provide real-time monitoring of the night sky by autonomously recognizing anomalous behavior, selecting targets for detailed investigation, and making real-time anomaly detection to enable rapid recognition and a swift response to transients as they emerge. This T3 global EO grid avoids the limitations imposed by geography and weather to provide persistent monitoring of the night sky.

  13. Swift-XRT follow-up of 2 unidentified INTEGRAL sources

    NASA Astrophysics Data System (ADS)

    Malizia, A.; Landi, R.; Bassani, L.; Bird, A. Bazzano A. J.; Gehrels, N.; Kennea, J. A.

    2011-04-01

    In this telegram we report the X-ray follow-up observations performed with Swift-XRT of 2 unidentified INTEGRAL sources listed in Bird et al. 2010 (ApJS, 186, 1). IGR J11014-6103. Within the IBIS error circle, XRT detects an X-ray source with coordinates R.A.(J2000) = 11h 01m 46.4s and Dec.(J2000) = -61d 01m 21s and 6 arcsec positional uncertainty. XRT detection is at 7.7 sigma in the 0.3-10 keV band and 4.6 sigma above 3 keV.

  14. Albendazole therapy of hydatid disease: 2-year follow-up of 40 cases.

    PubMed

    el-Mufti, M; Kamag, A; Ibrahim, H; Taktuk, S; Swaisi, I; Zaidan, A; Sameen, A; Shimbish, F; Bouzghaiba, W; Haasi, S

    1993-06-01

    Forty patients with 63 Echinococcus granulosus cysts affecting different sites were treated with albendazole and have been followed up for at least 24 months from completion of therapy. Twenty-one patients (53%) with 37 cysts (59%) showed evidence of healing. The criteria and pattern of healing are outlined. The most serious complication of albendazole therapy was hepatoxic jaundice, which occurred in 5% of patients. Recurrence during the observation period was encountered in 9.5% of patients with a positive response. It is suggested that patients suffering from uncomplicated hydatid disease should be given the benefit of a trial course of albendazole therapy, before surgery is undertaken.

  15. Long-Term Follow-Up and Survivorship.

    PubMed

    Tsirou, Aimilia; Hjorth, Lars

    2016-01-01

    Within this chapter, we begin with the invaluable context of the experience of living after cancer as a young person. Then we move to describe the growing body of data indicating the consequences of cancer in patients diagnosed aged as teenagers and young adults (YAs). We identify that, while the variation in definitions used in the literature hamper firm conclusions, specific patterns of substantial morbidity are observed which are distinct from those seen in younger children. When combined with the epidemiology, the overall burden of late effects of adolescents and YA cancer and its treatment are a substantial public health problem. The progress in parts of Europe and the US in bringing together outcomes into medium-sized data sets, combined with the gaps in the data and remaining uncertainties, mean that the time is right for international epidemiological ascertainment of these adverse effects. There are potential benefits for commencing prospective clinical as well retrospective epidemiological study designs. PMID:27595354

  16. Follow-up of hearing thresholds among forge hammering workers

    SciTech Connect

    Kamal, A.A.; Mikael, R.A.; Faris, R. )

    1989-01-01

    Hearing threshold was reexamined in a group of forge hammering workers investigated 8 years ago with consideration of the age effect and of auditory symptoms. Workers were exposed to impact noise that ranged from 112 to 139 dB(A)--at an irregular rate of 20 to 50 drop/minute--and a continuous background noise that ranged from 90 to 94 dB(A). Similar to what was observed 8 years ago, the present permanent threshold shift (PTS) showed a maximum notch at the frequency of 6 kHz and considerable elevations at the frequencies of 0.25-1 kHz. The age-corrected PTS and the postexposure hearing threshold were significantly higher than the corresponding previous values at the frequencies 0.25, 0.5, 1, and 8 kHz only. The rise was more evident at the low than at the high frequencies. Temporary threshold shift (TTS) values were significantly less than those 8 years ago. Contrary to the previous TTS, the present TTS were higher at low than at high frequencies. Although progression of PTS at the frequencies 0.25 and 0.5 kHz was continuous throughout the observed durations of exposure, progression at higher frequencies occurred essentially in the first 10 to 15 years of exposure. Thereafter, it followed a much slower rate. Tinnitus was significantly associated with difficulty in hearing the human voice and with elevation of PTS at all the tested frequencies, while acoustic after-image was significantly associated with increment of PTS at the frequencies 0.25-2 kHz. No relation between PTS and smoking was found. PTS at low frequencies may provide an indication of progression of hearing damage when the sensitivity at 6 and 4 kHz diminishes after prolonged years of exposure. Tinnitus and acoustic after-image are related to the auditory effect of forge hammering noise.

  17. [Follow-up of children born by ICSI].

    PubMed

    Wittemer, Christiane; Machev, Nadejda; Viville, Stéphane

    2004-03-01

    The debate concerning the health of children conceived by artificial reproduction technology (ART) continues. Among these techniques, intracytoplasmic sperm injection (ICSI) is the subject of most attention. Indeed, several studies have concentrated on the evaluation of risks associated with ICSI. The publication of a few recent articles on the subject is providing an opportunity to reconsider the situation. Generally, women conceiving via ART are older, more often primipar and present increased rates of uterine pathologies compared to women conceiving naturally. Furthermore, ART pregnancies are sources of anxiety resulting in a significant increase rates of caesarean section. ART children present an increased risk of low birth rate often linked to multiple pregnancy, but this is also true for singleton pregnancy. Major studies have not revealed a significantly increased rate of malformations in ICSI children. However, sporadic observations of errors in genomic imprinting or of rare tumors in children conceived by ICSI point to a need for increased vigilance of ICSI practices. Finally, the mental development, the family and social life of ICSI children appears similar to children conceived naturally.

  18. Callosal apraxia: a 34-year follow-up study.

    PubMed

    Falchook, Adam D; Watson, Robert T; Heilman, Kenneth M

    2016-06-01

    Loss of ability of the left upper limb (LUL) to correctly produce spatial and temporal components of skilled purposeful movements was reported 34 years ago in a woman with a callosal infarction. To learn about recovery, we recently reexamined this woman. This woman was tested for ideomotor apraxia by asking her to pantomime to command and to seeing pictures of tools. Whereas she performed normally with her right upper limb, her LUL remained severely apraxic, making many spatial (postural and movement) errors. Initially, she did not reveal loss of finger-hand deftness (limb-kinetic apraxia), and when tested again with the coin rotation task, her left hand performance was normal. Without vision, she could name objects placed in her left hand but not name numbers written in this hand. Since this woman had a callosal lesion, failure to recover cannot be accounted for by left hemisphere inhibition of her right hemisphere. Although failure for her LUL to improve may have been related to not using her LUL for skilled actions, her right hemisphere was able to observe transitive actions, and this failure of her LUL to produce skilled purposeful movements suggests her right hemisphere may have not had the capacity to learn these movement representations. Without vision, her ability to recognize objects with her left hand, but not numbers written on her left palm, suggests graphesthesia may require that her left hand did not have access to movement representations important for programming these numbers when writing.

  19. Callosal apraxia: a 34-year follow-up study.

    PubMed

    Falchook, Adam D; Watson, Robert T; Heilman, Kenneth M

    2016-06-01

    Loss of ability of the left upper limb (LUL) to correctly produce spatial and temporal components of skilled purposeful movements was reported 34 years ago in a woman with a callosal infarction. To learn about recovery, we recently reexamined this woman. This woman was tested for ideomotor apraxia by asking her to pantomime to command and to seeing pictures of tools. Whereas she performed normally with her right upper limb, her LUL remained severely apraxic, making many spatial (postural and movement) errors. Initially, she did not reveal loss of finger-hand deftness (limb-kinetic apraxia), and when tested again with the coin rotation task, her left hand performance was normal. Without vision, she could name objects placed in her left hand but not name numbers written in this hand. Since this woman had a callosal lesion, failure to recover cannot be accounted for by left hemisphere inhibition of her right hemisphere. Although failure for her LUL to improve may have been related to not using her LUL for skilled actions, her right hemisphere was able to observe transitive actions, and this failure of her LUL to produce skilled purposeful movements suggests her right hemisphere may have not had the capacity to learn these movement representations. Without vision, her ability to recognize objects with her left hand, but not numbers written on her left palm, suggests graphesthesia may require that her left hand did not have access to movement representations important for programming these numbers when writing. PMID:26928117

  20. Ground-based follow up of IRAS galaxies

    NASA Technical Reports Server (NTRS)

    Dennefeld, M.; Karoji, H.; Bouchet, P.; Bottinelli, L.; Gouguenheim, L.

    1987-01-01

    Optical, near infrared, radio continuum and HI observations were undertaken of the galaxies identified with IRAS sources in a few fields roughly of the size of a sky survey plate. Results are presented from two fields at galactic latitude +27 and +43 deg over a total area of 100 sq. deg. These regions contained 115 IRAS point sources, out of which 26 were identified with stars and 81 with faint galaxies, 10 of which were difficult to recognize on the Schmidt plates. Spectroscopy was obtained with the ESO telescopes at a resolution of about 10 A. The vast majority of galaxies have low excitation spectra dominated by low ionization lines. The spectra are typical of HII region type galaxies, however of much lower excitation that other starbursts galaxies. The importance of the reddening as determined from the H alpha/H beta ratio is stressed: the visual absorption A sub v ranges from 2 to 6 magnitudes and as a consequence the corrected L sub IR/L sub B ratios are considerably reduced if those reddenings apply to the whole galaxy.

  1. Follow-up of Candidate Companions to Vega

    NASA Astrophysics Data System (ADS)

    Janson, Markus; Quanz, Sascha; Carson, Joseph; Thalmann, Christian; Lafreniere, David; Amara, Adam

    2014-12-01

    Vega hosts one of the most nearby massive debris disks, with a morphology that may be indicative of wide giant planetary companions. Its proximity and relatively young age also make it an attractive target for direct imaging searches for such companions. We therefore observed Vega with Spitzer during cycle 9, which provides the best sensitivity to planets in wide orbits that is available with any existing facility. Three candidates were discovered in the data which are substantially brighter at 4.5 micron than at 3.6 micron, while typical background sources have much smaller brightness differences between these bands. We now propose to follow the system up in a second epoch to test the three candidates for common proper motion with the primary star. If real, physical companions, the candidates have separations of 265-335 AU and masses of 2-3 Mjup according to evolutionary models (regardless of initial entropy conditions), and would therefore constitute the coldest and lowest-mass planets ever imaged outside of the Solar System.

  2. Radio rebrightening of the GRB afterglow by the accompanying supernova

    NASA Astrophysics Data System (ADS)

    Barniol Duran, R.; Giannios, D.

    2015-12-01

    The gamma-ray burst (GRB) jet powers the afterglow emission by shocking the surrounding medium, and radio afterglow can now be routinely observed to almost a year after the explosion. Long-duration GRBs are accompanied by supernovae (SNe) that typically contain much more energy than the GRB jet. Here we consider the fact that the SN blast wave will also produce its own afterglow (supernova remnant emission), which will peak at much later time (since it is non-relativistic), when the SN blast wave transitions from a coasting phase to a decelerating Sedov-Taylor phase. We predict that this component will peak generally a few tens of years after the explosion and it will outshine the GRB powered afterglow well-before its peak emission. In the case of GRB 030329, where the external density is constrained by the ˜10-year coverage of the radio GRB afterglow, the radio emission is predicted to start rising over the next decade and to continue to increase for the following decades up to a level of ˜ mJy. Detection of the SN-powered radio emission will greatly advance our knowledge of particle acceleration in ˜0.1c shocks.

  3. Cognitive evolution in hypertensive patients: a six-year follow-up

    PubMed Central

    Vicario, Augusto; del Sueldo, Mildren A; Zilberman, Judith M; Cerezo, Gustavo H

    2011-01-01

    Background: Several studies have examined the links between hypertension, vascular damage, and cognitive impairment. The functions most commonly involved seem to be those associated with memory and executive function. Aims: 1) to report the cognitive evolution in a cohort of hypertensive patients, 2) to identify the affected domains, and 3) to correlate the results obtained with blood pressure measurements. Materials and Methods: Observational 6-year follow-up cohort study including both males and females aged ≥65 and ≤80 years, and hypertensive patients under treatment. Patients with a history of any of the following conditions were excluded: stroke, transient ischemic attack, diabetes mellitus, atrial fibrillation, cardiac surgery, dementia, or depression. Four neurocognitive evaluations were performed (at baseline and every 2 years). The tests used evaluated memory and executive function domain. Blood pressure was measured on every cognitive evaluation. Results: Sixty patients were followed for 76.4 ± 2.8 months. The average age at baseline was 72.5 ± 4.2 and 77.9 ± 4.6 at 6 years (65% were women). Two patients were lost to follow up (3.3%) and 8 patients died (13.3%).The density incidence for dementia was 0.6% patients per year (pt/y) (n = 3) and for depression was 1.6% pt/y (n = 12). No changes were observed in either memory impairment or the Mini Mental State Examination (MMSE) results (p = ns) during follow-up. A progressive impairment of the executive function was shown regardless of the blood pressure measurements. Conclusion: 1) the incidence of dementia doubled to general population, 2) the initial memory impairment did not change during the evaluation period, 3) cognitive impairment worsened in the areas related to executive function (prefrontal cortex) regardless of the adequacy of anti-hypertensive treatment and blood pressure values. PMID:21603597

  4. Epidemiological Follow-up 15 Years after the Breast Cancer Scandal in Essen.

    PubMed

    Hauth, E A M; Berkemeyer, S; Jaeger, H; Forsting, M; Hoffmann, B; Jöckel, K-H

    2012-06-01

    Purpose: In the years 1993-1996 a number of presumably false-positive breast cancer diagnoses were made by a pathologist in Essen. A follow-up, undertaken 15 years later, investigated how many women had tumour recurrence and/or metastasis or had died from breast cancer. Material and Methods: A total of 151 (68 %) out of 222 women could be traced. One hundred and forty-seven (66.2 %) of the 222 women were alive. The observed survival rate, number of recurrences and/or metastases, and number of deaths from breast cancer were compared with data from the Munich Tumour Registry. The number of breast cancer cases among daughters of the affected women was ascertained. Results: The total observed survival rate at follow-up after 15 years was 93 %, a much higher figure than the survival rate of 45 % given by the Munich Tumour Registry. Recurrence and/or metastasis or death from breast cancer occurred in 9/222 cases (4.1 %). The incidence for these events calculated according to data from the Munich Tumour Registry is 13 %. Two daughters (2.2 %) out of a total of 90 were diagnosed with breast cancer whereas, according to the German Cancer Research Centre, the expected rate would have been between 5 and 10 %. Conclusions: The results of our follow-up after 15 years show that more women survived than expected and that the number of recurrences and/or metastases and deaths due to breast cancer was lower than expected. Fewer daughters of affected women were diagnosed with breast cancer than expected. These results support our suspicion that not all women diagnosed with breast cancer by a pathologist in Essen actually had breast cancer.

  5. Ten-Year Follow-up of Patients with Epidemic Post Infectious Glomerulonephritis

    PubMed Central

    Pinto, Sergio Wyton L.; Mastroianni-Kirsztajn, Gianna; Sesso, Ricardo

    2015-01-01

    Background Scarce information on outcomes of epidemic post infectious glomerulonephritis is available. This is a 10-year follow-up of the patients that developed acute glomerulonephritis in an epidemic outbreak caused by group C Streptococcus zooepidemicus in Brazil in 1998, that were also previously evaluated 2 and 5 years after the acute episode. Methods In this prospective study 60 cases (out of 134 in 1998) were reevaluated after 10 years, as well as community controls matched by gender and age. They underwent clinical and renal function evaluation, including serum creatinine and cystatin C, estimated glomerular filtration rate (eGFR), albuminuria and hematuria. Results Comparisons of clinical and renal function aspects of 60 patients and 48 community controls have not shown significant differences (eGFR <60 ml/min/1.73m2 and/or albuminuria >30mg/g creatinine: 13.8% vs. 12.2%, respectively, p = 0.817) except for a higher frequency of hypertension in the cases (45.0% vs. 20.8%, p = 0.009). Comparing the same patients affected in the acute episode, 2, 5 and 10 years later, it was observed an improvement of median eGFR levels at 2 years and a trend toward subsequent stabilization in these levels, associated with decrease in albuminuria and increased hypertension rates in the last survey. At 10 years it was not observed additional reduction of renal function using serum creatinine, eGFR and cystatin C. Conclusions During the acute episode of epidemic GN a considerable proportion of patients presented hypertension and reduced renal function; after 2 years and particularly at this 10-year follow-up survey there was no worsening of renal function parameters, except for persistent higher frequency of hypertension. Nevertheless, a longer follow up is necessary to confirm that progressive loss of renal function will not occur. PMID:25962068

  6. Multiband photometric follow-up of supernova iPTF13ebh

    NASA Astrophysics Data System (ADS)

    Wyrzykowski, L.; Campbell, H. C.; Koposov, S.; Pawlak, M.; Ulaczyk, K.; Rynkiewicz, A.; Wielgorski, P.; Ilkiewicz, K.; Handzlik, B.; Rybicki, K.; Obuchowicz, W.; Khamitov, I. M.; Esenoglu, H.; Bikmaev, I. F.; Zhuchkov, R. Ya.; Busuttil, R.; Kolb, U.; Burwitz, V.; Rodriguez, J.; Zeilinger, W.; Leonini, S.; Conti, M.; Guerrini, G.; Rosi, P.; Ramirez, L. M. Tinjaca; Damljanovic, G.; Vince, O.; Pavlovic, R.; Cvetkovic, Z.; Stojanovic, M.

    2014-02-01

    We report the results of an extensive photometric follow-up of iPTFebh supernova (ATEL#5580, ATEL#5584) classified as type Ia at z=0.013269, located in NGC 890. The telescopes involved in the follow-up operated in the preparatory mode for the forthcoming Gaia Science Alerts follow-up network.

  7. Multiband photometric follow-up of ASASSN-13aw (SN 2013dr)

    NASA Astrophysics Data System (ADS)

    Wyrzykowski, L.; Campbell, H. C.; Koposov, S.; Ulaczyk, K.; Damljanovic, G.; Vince, O.; Pavlovic, R.; Cvetkovic, Z.; Stojanovic, M.; Kolb, U.; Bochinski, J.; Burwitz, V.; Haswell, C.; Rodriguez, J.; Harding, J.; Busuttil, R.

    2013-08-01

    We report the result of an extensive photometric follow-up of ASASSN-13aw (ATEL#5183) aka SN 2013dr, classified as type Ia supernova (Tomasella et al., CBAT TOCP for PSN J17193026+4742046). The telescopes involved in the follow-up operated in the preparatory mode for the forthcoming Gaia Science Ale$ follow-up network.

  8. 20 CFR 664.450 - What are follow-up services for youth?

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... 20 Employees' Benefits 4 2012-04-01 2012-04-01 false What are follow-up services for youth? 664... (CONTINUED) YOUTH ACTIVITIES UNDER TITLE I OF THE WORKFORCE INVESTMENT ACT Youth Program Design, Elements, and Parameters § 664.450 What are follow-up services for youth? (a) Follow-up services for youth...

  9. 20 CFR 664.450 - What are follow-up services for youth?

    Code of Federal Regulations, 2014 CFR

    2014-04-01

    ... 20 Employees' Benefits 4 2014-04-01 2014-04-01 false What are follow-up services for youth? 664... (CONTINUED) YOUTH ACTIVITIES UNDER TITLE I OF THE WORKFORCE INVESTMENT ACT Youth Program Design, Elements, and Parameters § 664.450 What are follow-up services for youth? (a) Follow-up services for youth...

  10. 20 CFR 672.325 - What timeframes apply for follow-up services?

    Code of Federal Regulations, 2013 CFR

    2013-04-01

    ... 20 Employees' Benefits 4 2013-04-01 2013-04-01 false What timeframes apply for follow-up services? 672.325 Section 672.325 Employees' Benefits EMPLOYMENT AND TRAINING ADMINISTRATION, DEPARTMENT OF... timeframes apply for follow-up services? Follow-up services must be provided to all YouthBuild...

  11. 49 CFR 655.47 - Follow-up testing after returning to duty.

    Code of Federal Regulations, 2011 CFR

    2011-10-01

    ... OPERATIONS Types of Testing § 655.47 Follow-up testing after returning to duty. An employer shall conduct follow-up testing of each employee who returns to duty, as specified in 49 CFR Part 40, subpart O. ... 49 Transportation 7 2011-10-01 2011-10-01 false Follow-up testing after returning to duty....

  12. 49 CFR 655.47 - Follow-up testing after returning to duty.

    Code of Federal Regulations, 2010 CFR

    2010-10-01

    ... OPERATIONS Types of Testing § 655.47 Follow-up testing after returning to duty. An employer shall conduct follow-up testing of each employee who returns to duty, as specified in 49 CFR Part 40, subpart O. ... 49 Transportation 7 2010-10-01 2010-10-01 false Follow-up testing after returning to duty....

  13. 20 CFR 672.325 - What timeframes apply for follow-up services?

    Code of Federal Regulations, 2012 CFR

    2012-04-01

    ... 20 Employees' Benefits 4 2012-04-01 2012-04-01 false What timeframes apply for follow-up services? 672.325 Section 672.325 Employees' Benefits EMPLOYMENT AND TRAINING ADMINISTRATION, DEPARTMENT OF... timeframes apply for follow-up services? Follow-up services must be provided to all YouthBuild...

  14. 49 CFR 655.47 - Follow-up testing after returning to duty.

    Code of Federal Regulations, 2013 CFR

    2013-10-01

    ... OPERATIONS Types of Testing § 655.47 Follow-up testing after returning to duty. An employer shall conduct follow-up testing of each employee who returns to duty, as specified in 49 CFR Part 40, subpart O. ... 49 Transportation 7 2013-10-01 2013-10-01 false Follow-up testing after returning to duty....

  15. 49 CFR 655.47 - Follow-up testing after returning to duty.

    Code of Federal Regulations, 2014 CFR

    2014-10-01

    ... OPERATIONS Types of Testing § 655.47 Follow-up testing after returning to duty. An employer shall conduct follow-up testing of each employee who returns to duty, as specified in 49 CFR Part 40, subpart O. ... 49 Transportation 7 2014-10-01 2014-10-01 false Follow-up testing after returning to duty....

  16. 20 CFR 672.325 - What timeframes apply for follow-up services?

    Code of Federal Regulations, 2014 CFR

    2014-04-01

    ... 20 Employees' Benefits 4 2014-04-01 2014-04-01 false What timeframes apply for follow-up services? 672.325 Section 672.325 Employees' Benefits EMPLOYMENT AND TRAINING ADMINISTRATION, DEPARTMENT OF... timeframes apply for follow-up services? Follow-up services must be provided to all YouthBuild...

  17. 49 CFR 655.47 - Follow-up testing after returning to duty.

    Code of Federal Regulations, 2012 CFR

    2012-10-01

    ... OPERATIONS Types of Testing § 655.47 Follow-up testing after returning to duty. An employer shall conduct follow-up testing of each employee who returns to duty, as specified in 49 CFR Part 40, subpart O. ... 49 Transportation 7 2012-10-01 2012-10-01 false Follow-up testing after returning to duty....

  18. Constraints on Short Gamma-Ray Burst Models with Optical Limits of GRB 050509b

    SciTech Connect

    Hjorth, Jens; Sollerman, J.; Gorosabel, J.; Granot, J.; Klose, S.; Kouveliotou, C.; Melinder, J.; Ramirez-Ruiz, E.; Starling, R.; Thomsen, B.; Andersen, M.I.; Fynbo, J.P.U.; Jensen, B.L.; Vreeswijk, P.M.; Castro-Ceron, J.M.; Jakobsson, P.; Levan, A.; Pedersen, K.; Rhoads, J.E.; Tanvir, N.R.; Watson, D.; /Bohr Inst. /Stockholm U. /IAA, Granada /KIPAC, Menlo Park /TLS, Tautenburg /NASA, Marshall /Princeton, Inst. Advanced Study /Amsterdam U., Astron. Inst. /Aarhus U. /Potsdam, Astrophys. Inst. /European Southern Obs., Chile /Leicester U. /Baltimore, Space Telescope Sci. /Hertfordshire U.

    2005-06-15

    We have obtained deep optical images with the Very Large Telescope at ESO of the first well-localized short-duration gamma-ray burst, GRB 050509b. We observed in the V and R bands at epochs starting at {approx}2 days after the GRB trigger and lasting up to three weeks. We detect no variable objects inside the small Swift/XRT X-ray error circle down to 5{sigma} limiting magnitudes of V = 26.5 and R = 25.2. The X-ray error circle includes a giant elliptical galaxy at z = 0.225, which has been proposed as the likely host of this GRB. Our limits indicate that if the GRB originated at z = 0.225, any supernova-like event accompanying the GRB would have to be over 100 times fainter than normal Type Ia SNe or Type Ic hypernovae, 5 times fainter than the faintest known Ia or Ic SNe, and fainter than the faintest known Type II SNe. Moreover, we use the optical limits to constrain the energetics of the GRB outflow, and conclude that there was very little radioactive material produced during the GRB explosion. These limits strongly constrain progenitor models for this short GRB.

  19. Allostery Mediates Ligand Binding to Grb2 Adaptor in a Mutually Exclusive Manner

    PubMed Central

    McDonald, Caleb B.; El Hokayem, Jimmy; Zafar, Nawal; Balke, Jordan E.; Bhat, Vikas; Mikles, David C.; Deegan, Brian J.; Seldeen, Kenneth L.; Farooq, Amjad

    2012-01-01

    Allostery plays a key role in dictating the stoichiometry and thermodynamics of multi-protein complexes driving a plethora of cellular processes central to health and disease. Herein, using various biophysical tools, we demonstrate that although Sos1 nucleotide exchange factor and Gab1 docking protein recognize two non-overlapping sites within the Grb2 adaptor, allostery promotes the formation of two distinct pools of Grb2-Sos1 and Grb2-Gab1 binary signaling complexes in concert in lieu of a composite Sos1-Grb2-Gab1 ternary complex. Of particular interest is the observation that the binding of Sos1 to the nSH3 domain within Grb2 sterically blocks the binding of Gab1 to the cSH3 domain and vice versa in a mutually exclusive manner. Importantly, the formation of both the Grb2-Sos1 and Grb2-Gab1 binary complexes is governed by a stoichiometry of 2:1, whereby the respective SH3 domains within Grb2 homodimer bind to Sos1 and Gab1 via multivalent interactions. Collectively, our study sheds new light on the role of allostery in mediating cellular signaling machinery. PMID:23334917

  20. Allostery mediates ligand binding to Grb2 adaptor in a mutually exclusive manner.

    PubMed

    McDonald, Caleb B; El Hokayem, Jimmy; Zafar, Nawal; Balke, Jordan E; Bhat, Vikas; Mik