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Start Over Author "John O. Goldsten" Publisher american astronomical society
4 results on '"John O. Goldsten"'

1. A Giant Flare from a Soft Gamma Repeater in the Andromeda Galaxy (M31)

Author

Valentin Pal'shin, S. V. Golenetskii, R. L. Aptekar, A. von Kienlin, D. D. Frederiks, E. P. Mazets, Kevin Hurley, John O. Goldsten, and T. L. Cline

Subjects
Physics, Andromeda Galaxy, Astrophysics (astro-ph), Soft gamma repeater, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, Galaxy, Luminosity, law.invention, Space and Planetary Science, law, Gamma-ray burst, Energy (signal processing), Flare
Abstract

The light curve, energy spectra, energetics, and IPN localization of an exceedingly intense short duration hard spectrum burst, GRB 070201, obtained from Konus-Wind, INTEGRAL (SPI-ACS), and MESSENGER data are presented. The total fluence of the burst and the peak flux are $S = 2.00_{-0.26}^{+0.10} \times 10^{-5}$ erg cm$^{-2}$ and $F_{max} = 1.61_{-0.50}^{+0.29} \times 10^{-3}$ erg cm$^{-2}$ s$^{-1}$. The IPN error box has an area of 446 square arcminutes and covers the peripheral part of the M31 galaxy. Assuming that the source of the burst is indeed in M31 at a distance of 0.78 Mpc, the measured values of the fluence $S$ and maximum flux $F_{max}$ correspond to a total energy of $Q = 1.5 \times 10^{45}$ erg, and a maximum luminosity $L = 1.2 \times 10^{47}$ erg s$^{-1}$. These data are in good agreement with the corresponding characteristics of the previously observed giant flares from other soft gamma repeaters. The evidence for the identification of this event as a giant flare from a soft gamma repeater in the M31 galaxy is presented., Comment: 15 pages, 5 figures, submitted to ApJ

Published
2008
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2. Multiwavelength Studies of the Optically Dark Gamma‐Ray Burst 001025A

Author

D. Smith, K. Hurley, V. D. Pal'shin, Pall Jakobsson, Kristian Pedersen, B. Milvang-Jensen, Jacob I. Trombka, M. Ulanov, Javier Gorosabel, John O. Goldsten, Palle Møller, T. Cline, Johan P. U. Fynbo, T. P. McClanahan, B. L. Jensen, Jens Hjorth, N. Schartel, Lise Christensen, Michael I. Andersen, Darach Watson, and S. Golenetskii

Subjects
Physics, Spectral index, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Extinction (astronomy), FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Plasma, Astrophysics, 01 natural sciences, Afterglow, Wavelength, Space and Planetary Science, 0103 physical sciences, Absorption (electromagnetic radiation), Gamma-ray burst, 010303 astronomy & astrophysics
Abstract

We identify the fading X-ray afterglow of GRB 001025A from XMM-Newton observations obtained 1.9-2.3 days, 2 years, and 2.5 years after the burst. The non-detection of an optical counterpart to an upper limit of R=25.5, 1.20 days after the burst, makes GRB 001025A a ``dark'' burst. Based on the X-ray afterglow spectral properties of GRB 001025A, we argue that some bursts appear optically dark because their afterglow is faint and their cooling frequency is close to the X-ray band. This interpretation is applicable to several of the few other dark bursts where the X-ray spectral index has been measured. The X-ray afterglow flux of GRB 001025A is an order of magnitude lower than for typical long-duration gamma-ray bursts. The spectrum of the X-ray afterglow can be fitted with an absorbed synchrotron emission model, an absorbed thermal plasma model, or a combination thereof. For the latter, an extrapolation to optical wavelengths can be reconciled with the R-band upper limit on the afterglow, without invoking any optical circumburst absorption, provided the cooling frequency is close to the X-ray band. Alternatively, if the X-ray afterglow is due to synchrotron emission only, seven magnitudes of extinction in the observed R-band is required to meet the R-band upper limit, making GRB 001025A much more obscured than bursts with detected optical afterglows. Based on the column density of X-ray absorbing circumburst matter, an SMC gas-to-dust ratio is insufficient to produce this amount of extinction. The X-ray tail of the prompt emission enters a steep temporal decay excluding that the tail of the prompt emission is the onset of the afterglow (abridged)., 32 pages, 8 figures, ApJ in press

Published
2006
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3. INTERPLANETARY NETWORK LOCALIZATIONS OF KONUS SHORT GAMMA-RAY BURSTS

Author

A. B. Sanin, George R. Ricker, Dmitry S. Svinkin, I. Donnarumma, Y. Evangelista, Claudio Labanti, C. Guidorzi, D. D. Frederiks, Robert E. Gold, Yukikatsu Terada, Francesco Lazzarotto, N. Gehrels, Lorenzo Amati, E. Del Monte, F. Rossi, Luigi Pacciani, David M. Smith, R. Starr, Chryssa Kouveliotou, Roland Vanderspek, V. Savchenko, R. M. Kippen, J. L. Atteia, Kazutaka Yamaoka, M. L. Litvak, William V. Boynton, C. Fellows, Luciano Nicastro, Mauro Orlandini, Tadayuki Takahashi, Gerald J. Fishman, G. Di Cocco, Martino Marisaldi, John O. Goldsten, V. Pal'Shin, M. Rapisarda, S. Golenetskii, V. Connaughton, T. P. McClanahan, T. Cline, Charles A. Meegan, M. Feroci, Dmitry Golovin, Paolo Soffitta, Wojtek Hajdas, Jacob I. Trombka, K. Hurley, A. Rau, F. Fuschino, J. Cummings, E. P. Mazets, P. Oleynik, A. S. Kozyrev, S. D. Barthelmy, David Palmer, R. Aptekar, M. Boer, H. A. Krimm, Yasushi Fukazawa, M. Ulanov, F. Frontera, Masanori Ohno, Enrico Montanari, Toshio Murakami, K. Harshman, Enrico Costa, A. von Kienlin, I. G. Mitrofanov, Makoto Tashiro, Y. Hanabata, Michael S. Briggs, Kazuo Makishima, M. Galli, I. Lapshov, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Department of Physics [CUA], Catholic University of America, Max-Planck-Institut für Extraterrestrische Physik (MPE), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Paul Scherrer Institute (PSI), NASA Goddard Space Flight Center (GSFC), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Department of Physical Sciences [Higashi-Hiroshima], Hiroshima University, Institut d'électronique fondamentale (IEF), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Universities Space Research Association (USRA), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Università degli Studi di Ferrara (UniFE), Ecologie des systèmes marins côtiers (Ecosym), Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Université Montpellier 1 (UM1)-Université Montpellier 2 - Sciences et Techniques (UM2)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto di Astrofisica Spaziale, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Terra s.n.c. Servizi al territorio, Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Center for Space Research [Cambridge] (CSR), Massachusetts Institute of Technology (MIT), Galli, M., University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi di Ferrara = University of Ferrara (UniFE), Université Montpellier 1 (UM1)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut Français de Recherche pour l'Exploitation de la Mer (IFREMER)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
catalog, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, Astrophysics, 01 natural sciences, techniques: miscellaneous, catalogs, 0103 physical sciences, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, [PHYS]Physics [physics], Physics, Spacecraft, business.industry, Triangulation (social science), Astronomy and Astrophysics, Space and Planetary Science, Physics::Space Physics, Detection rate, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Gamma-ray burst, business, techniques: miscellaneou
Abstract

著者人数: 74名, Accepted: 2013-07-11, 資料番号: SA1004571000

Published
2013
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4. PTF 10bzf (SN 2010ah): A BROAD-LINE Ic SUPERNOVA DISCOVERED BY THE PALOMAR TRANSIENT FACTORY

Author

Robert Quimby, Valerie Connaughton, Mansi M. Kasliwal, Iair Arcavi, Kevin Hurley, V. Pal'Shin, D. Murray, Eran O. Ofek, Shrinivas R. Kulkarni, Kazutaka Yamaoka, D. A. Howell, Dong Xu, Sagi Ben-Ami, Jay Cummings, Nicholas M. Law, Dale A. Frail, S. B. Cenko, Mark Sullivan, Josh Bloom, William V. Boynton, Paolo A. Mazzali, Avishay Gal-Yam, Dovi Poznanski, Alessandra Corsi, I. G. Mitrofanov, Peter Nugent, Yoav Green, Arne Rau, and John O. Goldsten

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), GRB 980425, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Afterglow, Luminosity, Allen Telescope Array, Supernova, 13. Climate action, Space and Planetary Science, 0103 physical sciences, GRB 030329, Gamma-ray burst, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Line (formation)
Abstract

We present the discovery and follow-up observations of a broad-line type-Ic supernova (SN), PTF 10bzf (SN 2010ah), detected by the Palomar Transient Factory (PTF) on 2010 February 23. The SN distance is \cong 218 Mpc, greater than GRB 980425 / SN 1998bw and GRB 060218 / SN 2006aj, but smaller than the other SNe firmly associated with gamma-ray bursts (GRBs). We conducted a multi-wavelength follow-up campaign with Palomar-48 inch, Palomar 60-inch, Gemini-N, Keck, Wise, Swift, the Allen Telescope Array, CARMA, WSRT, and EVLA. Here we compare the properties of PTF 10bzf with those of SN 1998bw and other broad-line SNe. The optical luminosity and spectral properties of PTF 10bzf suggest that this SN is intermediate, in kinetic energy and amount of 56Ni, between non GRB-associated SNe like 2002ap or 1997ef, and GRB-associated SNe like 1998bw. No X-ray or radio counterpart to PTF 10bzf was detected. X-ray upper-limits allow us to exclude the presence of an underlying X-ray afterglow as luminous as that of other SN-associated GRBs like GRB 030329 or GRB 031203. Early-time radio upper-limits do not show evidence for mildly-relativistic ejecta. Late-time radio upper-limits rule out the presence of an underlying off-axis GRB, with energy and wind density similar to the SN-associated GRB 030329 and GRB 031203. Finally, by performing a search for a GRB in the time window and at the position of PTF 10bzf, we find that no GRB in the IPN catalog could be associated with this SN., Comment: 34 pages, 7 figures, to appear in ApJ; revised version addresses referee's comments; P60 data added; results unchanged

Published
2011
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