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1. Discovery and Confirmation of the Shortest Gamma-Ray Burst from a Collapsar

Author

Tomás Ahumada, Leo P Singer, Shreya Anand, Michael W Coughlin, Mansi M Kasliwal, Geoffrey Ryan, Igor Andreoni, S Bradley Cenko, Christoffer Fremling, Harsh Kumar, Peter T H Pang, Eric Burns, Virginia Cunningham, Simone Dichiara, Tim Dietrich, Dmitry S. Svinkin, Mouza Almualla, Alberto J Castro-Tirado, Kishalay De, Rachel Dunwoody, Pradip Gatkine, Erica Hammerstein, Shabnam Iyyani, Joseph Mangan, Dan Perley, Sonalika Purkayastha, Eric Bellm, Varun Bhalerao, Bryce Bolin, Mattia Bulla, Christopher Cannella, Poonam Chandra, Dmitry A Duev, Dmitry Frederiks, Avishay Gal-Yam, Matthew Graham, Anna Y Q Ho, Kevin Hurley, Viraj Karambelkar, Erik C Kool, S R Kulkarni, Ashish Mahabal, Frank Masci, Sheila McBreen, Shashi B Pandey, Simeon Reusch, Anna Ridnaia, Philippe Rosnet, Benjamin Rusholme, Ana Sagués Carracedo, Roger Smith, Maayane Soumagnac, Robert Stein, Eleonora Troja, Anastasia Tsvetkova, Richard Walters, and Azamat F Valeev

Subjects
Astronomy
Abstract

Gamma-ray bursts (GRBs) are among the brightest and most energetic events in the Universe. The duration and hardness distribution of GRBs has two clusters, now understood to reflect (at least) two different progenitors. Short-hard GRBs (SGRBs; T(sub 90) < 2 s) arise from compact binary mergers, and long-soft GRBs (LGRBs; T(sub 90) > 2 s) have been attributed to the collapse of peculiar massive stars (collapsars). The discovery of SN 1998bw/GRB 980425 marked the first association of an LGRB with a collapsar, and AT 2017gfo/GRB 170817A/GW170817 marked the first association of an SGRB with a binary neutron star merger, which also produced a gravitational wave. Here, we present the discovery of ZTF20abwysqy (AT2020scz), a fast-fading optical transient in the Fermi satellite and the Interplanetary Network localization regions of GRB 200826A; X-ray and radio emission further confirm that this is the afterglow. Follow-up imaging (at rest-frame 16.5 days) reveals excess emission above the afterglow that cannot be explained as an underlying kilonova, but which is consistent with being the supernova. Although the GRB duration is short (rest-frame T90 of 0.65 s), our panchromatic follow-up data confirm a collapsar origin. GRB 200826A is the shortest LGRB found with an associated collapsar; it appears to sit on the brink between a successful and a failed collapsar. Our discovery is consistent with the hypothesis that most collapsars fail to produce ultra-relativistic jets.

Published
2021
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2. SN2020bvc: A Broad-line Type Ic Supernova with a Double-peaked Optical Light Curve and a Luminous X-Ray and Radio Counterpart

Author

Anna Y. Q. Ho, S. R. Kulkarni, Daniel A. Perley, S. Bradley Cenko, Alessandra Corsi, Steve Schulze, Ragnhild Lunnan, Jesper Sollerman, Avishay Gal-Yam, Shreya Anand, Cristina Barbarino, Eric C. Bellm, Rachel J. Bruch, Eric Burns, Kishalay De, Richard Dekany, Alexandre Delacroix, Dmitry A. Duev, Dmitry D. Frederiks, Christoffer Fremling, Daniel A. Goldstein, V. Zach Golkhou, Matthew J. Graham, David Hale, Mansi M. Kasliwal, Thomas Kupfer, Russ R. Laher, Julia Martikainen, Frank J. Masci, James D. Neill, Anna Ridnaia, Ben Rusholme, Volodymyr Savchenko, David L. Shupe, Maayane T. Soumagnac, Nora L. Strotjohann, Dmitry S. Svinkin, Kirsty Taggart, Leonardo Tartaglia, Lin Yan, and Jeffry Zolkower

Subjects
Astronomy, Astrophysics
Abstract

We present optical, radio, and X-ray observations of SN 2020bvc (=ASASSN-20bs, ZTF 20aalxlis), a nearby (z = 0.0252; d = 114Mpc) broad-line (BL) Type Ic supernova (SN) and the first double-peaked Ic-BL discovered without a gamma-ray burst (GRB) trigger. Our observations show that SN 2020bvc shares several properties in common with the Ic-BL SN 2006aj, which was associated with the low-luminosity gamma-ray burst (LLGRB) 060218. First, the 10 GHz radio luminosity (L(radio) ≈ 10^(37) erg/s) is brighter than ordinary core-collapse SNe but fainter than LLGRB SNe such as SN 1998bw (associated with LLGRB 980425). We model our VLA observations (spanning 13–43 days) as synchrotron emission from a mildly relativistic (v ≳ 0.3c) forward shock. Second, with Swift and Chandra, we detect X-ray emission (L(X) ≈ 10^(41) erg/s) that is not naturally explained as inverse Compton emission or part of the same synchrotron spectrum as the radio emission. Third, high-cadence (6 × per night) data from the Zwicky Transient Facility (ZTF) show a double-peaked optical light curve, the first peak from shock cooling of extended low-mass material (mass Me < 10^(-2) Mꙩ at radius Re > 10^(12) cm) and the second peak from the radioactive decay of 56Ni. SN 2020bvc is the first double-peaked Ic-BL SN discovered without a GRB trigger, so it is noteworthy that it shows X-ray and radio emission similar to LLGRB SNe. For four of the five other nearby (z ≲ 0.05) Ic-BL SNe with ZTF high-cadence data, we rule out a first peak like that seen in SN 2006aj and SN 2020bvc, i.e., that lasts ≈1 day and reaches a peak luminosity M ≈ −18. Follow-up X-ray and radio observations of Ic-BL SNe with well-sampled early optical light curves will establish whether double-peaked optical light curves are indeed predictive of LLGRB-like X-ray and radio emission.

Published
2020
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3. The Broad-lined Ic Supernova ZTF18aaqjovh (SN 2018bvw): An Optically Discovered Engine-driven Supernova Candidate with Luminous Radio Emission

Author

Anna Y. Q. Ho, Alessandra Corsi, S. Bradley Cenko, Francesco Taddia, S. R. Kulkarni, Scott Adams, Kishalay De, Richard Dekany, Dmitry D. Frederiks, Christoffer Fremling, V. Zach Golkhou, Matthew J. Graham, Tiara Hung, Thomas Kupfer, Russ R. Laher, Ashish Mahabal, Frank J. Masci, Adam A. Miller, James D. Neill, Daniel Reiley, Reed Riddle, Anna Ridnaia, Benjamin Rusholme, Yashvi Sharma, Jesper Sollerman, Maayane T. Soumagnac, Dmitry S. Svinkin, and David L. Shupe

Subjects
Astrophysics
Abstract

We present ZTF18aaqjovh (SN 2018bvw), a high-velocity ("broad-lined") stripped-envelope (Type Ic) supernova (Ic-BL SN) discovered in the Zwicky Transient Facility one-day cadence survey. ZTF18aaqjovh shares a number of features in common with engine-driven explosions: the photospheric velocity and the shape of the optical light curve are very similar to those of the Type Ic-BL SN 1998bw, which was associated with a low-luminosity gamma-ray burst (LLGRB) and had relativistic ejecta. However, the radio luminosity of ZTF18aaqjovh is almost two orders of magnitude fainter than that of SN 1998bw at the same velocity phase, and the shock velocity is at most mildly relativistic (v = 0.06–0.4c). A search of high-energy catalogs reveals no compelling gamma-ray burst (GRB) counterpart to ZTF18aaqjovh, and the limit on the prompt GRB luminosity of L(γ(ꙩ)iso) ≈ 1.6 x 10^(48) erg/s excludes a classical GRB but not an LLGRB. Altogether, ZTF18aaqjovh represents another transition event between engine-driven SNe associated with GRBs and "ordinary" Ic-BL SNe.

Published
2020
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4. A peculiar hard X-ray counterpart of a Galactic fast radio burst

Author

R. L. Aptekar, S. V. Golenetskii, Dmitry S. Svinkin, A. Tsvetkova, Andrei M. Bykov, A. Ridnaia, Sergei Popov, T. L. Cline, A. Lysenko, M. Ulanov, and D. D. Frederiks

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Fast radio burst, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Magnetar, 01 natural sciences, Coincident, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Event (particle physics), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

Fast radio bursts are bright, millisecond-scale radio flashes of yet unknown physical origin. Recently, their extragalactic nature has been demonstrated and an increasing number of the sources have been found to repeat. Young, highly magnetized, isolated neutron stars - magnetars - have been suggested as the most promising candidates for fast radio burst progenitors owing to their energetics and high X-ray flaring activity. Here we report the detection with the Konus-Wind of a hard X-ray event of April 28, 2020, temporarily coincident with a bright, two-peak radio burst from the Galactic magnetar SGR~1935+2154 with properties remarkably similar to those of fast radio bursts. We show that two peaks of the double-peaked X-ray burst coincide in time with the radio peaks, confirming that the X-ray and radio emission most likely have a common origin. Thus, this is the first simultaneous detection of a fast radio burst from a Galactic magnetar and its high-energy counterpart. The total energy emitted in X-rays in this burst is typical of bright short magnetar bursts, but an unusual hardness of its energy spectrum strongly distinguish the April 28 event among multiple "ordinary" flares detected from SGR~1935+2154 previously. This, and a recent non-detection of radio emission from about one hundred typical soft bursts from SGR 1935+2154 favors the idea that bright, FRB-like magnetar signals are associated with rare, hard-spectrum X-ray bursts, which implied rate ($\sim$ 0.04 yr$^{-1}$ magnetar$^{-1}$) appears consistent with the rate estimate of SGR 1935+2154-like radio bursts (0.007 - 0.04 yr$^{-1}$ magnetar$^{-1}$)., 25 pages, 6 figures, 4 tables

Published
2021

5. X-ray and gamma-ray emission from solar flares

Author

D. Frederiks, Dmitry S. Svinkin, A. Lysenko, A. Ridnaia, A. Tsvetkova, S. Golenetskii, A. Altyntsev, R. Aptekar, M. Ulanov, and Gregory D. Fleishman

Subjects
Physics, Solar flare, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, X-ray, General Physics and Astronomy, Context (language use), Astrophysics, law.invention, Heliophysics, law, Physics::Space Physics, Thermal, Astrophysics::Solar and Stellar Astrophysics, Flare
Abstract

We present a brief review of the contemporary understanding of and topical problems in solar flare physics that can be clarified by methods of X-ray and gamma-ray astronomy. The review focuses on several issues, including the conditions and mechanisms of electron acceleration in solar flares, the flare energy distribution between thermal and nonthermal components, the gamma-ray emission from solar flares and its dynamics, and the spatial structure of X-ray and gamma-ray sources. Discussed in this context are the latest data obtained by the joint Russia–US experiment Konus-Wind, which in 2019 celebrated the 25th anniversary of continuous operation in space.

Published
2020

7. Discovery and confirmation of the shortest gamma-ray burst from a collapsar

Author

Poonam Chandra, Tim Dietrich, Mouza Almualla, Pradip Gatkine, Chris Cannella, Kevin Hurley, Philippe Rosnet, Simeon Reusch, Dmitry S. Svinkin, Frank J. Masci, Igor Andreoni, Erica Hammerstein, Shri Kulkarni, Viraj Karambelkar, Joseph Mangan, Shabnam Iyyani, B. Rusholme, D. D. Frederiks, Maayane T. Soumagnac, Eleonora Troja, Anna Y. Q. Ho, Ana Sagués Carracedo, Shreya Anand, Rachel Dunwoody, Kaushik De, Harsh Kumar, Matthew J. Graham, Richard Walters, Eric Burns, Shashi B. Pandey, Erik C. Kool, P. T.H. Pang, Varun Bhalerao, Bryce Bolin, S. Dichiara, A. J. Castro-Tirado, Geoffrey Ryan, A. F. Valeev, Christoffer Fremling, Tomas Ahumada, Mansi M. Kasliwal, Mattia Bulla, S. Bradley Cenko, Sheila McBreen, Eric C. Bellm, Sonalika Purkayastha, Robert Stein, A. Ridnaia, Dmitry A. Duev, Virginia Cunningham, Ashish Mahabal, Daniel A. Perley, Avishay Gal-Yam, Michael W. Coughlin, A. Tsvetkova, Roger Smith, Leo Singer, Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), National Science Foundation (US), Irish Research Council, Science Foundation Ireland, European Commission, and Ministerio de Economía y Competitividad (España)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, GRB 980425, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Kilonova, Afterglow, NO, Supernova, Neutron star, Stars, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, QC, Fermi Gamma-ray Space Telescope, QB
Abstract

Full list of authors: Ahumada, Tomás; Singer, Leo P.; Anand, Shreya; Coughlin, Michael W.; Kasliwal, Mansi M.; Ryan, Geoffrey; Andreoni, Igor; Cenko, S. Bradley; Fremling, Christoffer; Kumar, Harsh; Pang, Peter T. H.; Burns, Eric; Cunningham, Virginia; Dichiara, Simone; Dietrich, Tim; Svinkin, Dmitry S.; Almualla, Mouza; Castro-Tirado, Alberto J.; De, Kishalay; Dunwoody, Rachel; Gatkine, Pradip; Hammerstein, Erica; Iyyani, Shabnam; Mangan, Joseph; Perley, Dan; Purkayastha, Sonalika; Bellm, Eric; Bhalerao, Varun; Bolin, Bryce; Bulla, Mattia; Cannella, Christopher; Chandra, Poonam; Duev, Dmitry A.; Frederiks, Dmitry; Gal-Yam, Avishay; Graham, Matthew; Ho, Anna Y. Q.; Hurley, Kevin; Karambelkar, Viraj; Kool, Erik C.; Kulkarni, S. R.; Mahabal, Ashish; Masci, Frank; McBreen, Sheila; Pandey, Shashi B.; Reusch, Simeon; Ridnaia, Anna; Rosnet, Philippe; Rusholme, Benjamin; Carracedo, Ana Sagués; Smith, Roger; Soumagnac, Maayane; Stein, Robert; Troja, Eleonora; Tsvetkova, Anastasia; Walters, Richard; Valeev, Azamat F., Gamma-ray bursts (GRBs) are among the brightest and most energetic events in the Universe. The duration and hardness distribution of GRBs has two clusters1, now understood to reflect (at least) two different progenitors2. Short-hard GRBs (SGRBs; T90 < 2 s) arise from compact binary mergers, and long-soft GRBs (LGRBs; T90 > 2 s) have been attributed to the collapse of peculiar massive stars (collapsars)3. The discovery of SN 1998bw/GRB 980425 (ref. 4) marked the first association of an LGRB with a collapsar, and AT 2017gfo (ref. 5)/GRB 170817A/GW170817 (ref. 6) marked the first association of an SGRB with a binary neutron star merger, which also produced a gravitational wave. Here, we present the discovery of ZTF20abwysqy (AT2020scz), a fast-fading optical transient in the Fermi satellite and the Interplanetary Network localization regions of GRB 200826A; X-ray and radio emission further confirm that this is the afterglow. Follow-up imaging (at rest-frame 16.5 days) reveals excess emission above the afterglow that cannot be explained as an underlying kilonova, but which is consistent with being the supernova. Although the GRB duration is short (rest-frame T90 of 0.65 s), our panchromatic follow-up data confirm a collapsar origin. GRB 200826A is the shortest LGRB found with an associated collapsar; it appears to sit on the brink between a successful and a failed collapsar. Our discovery is consistent with the hypothesis that most collapsars fail to produce ultra-relativistic jets. © 2021, The Author(s), under exclusive licence to Springer Nature Limited., This work was supported by the GROWTH (Global Relay of Observatories Watching Transients Happen) project funded by the National Science Foundation under PIRE grant No. 1545949. GROWTH is a collaborative project among California Institute of Technology (USA), University of Maryland College Park (USA), University of Wisconsin Milwaukee (USA), Texas Tech University (USA), San Diego State University (USA), University of Washington (USA), Los Alamos National Laboratory (USA), Tokyo Institute of Technology (Japan), National Central University (Taiwan), Indian Institute of Astrophysics (India), Indian Institute of Technology Bombay (India), Weizmann Institute of Science (Israel), The Oskar Klein Centre at Stockholm University (Sweden), Humboldt University (Germany), Liverpool John Moores University (UK) and University of Sydney (Australia). Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington (UW), Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee and Lawrence Berkeley National Laboratories. Operations are conducted by Caltech Optical Observatories, IPAC and UW. The work is partly based on the observations made with the Gran Telescopio Canarias (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, in the island of La Palma. The material is based on work supported by NASA under award No. 80GSFC17M0002. A.J.C.T. acknowledges all co-Is of the GTC proposal and the financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award to the Instituto de Astrofisica de Andalucia (SEV-2017-0709). The ZTF forced-photometry service was funded under the Heising-Simons Foundation grant No. 12540303 (PI: Graham). S.M. and J.M. acknowledge support from Science Foundation Ireland under grant No. 17/CDA/4723. R.D. acknowledges support from the Irish Research Council (IRC) under grant GOIPG/2019/2033. Analysis was performed on the YORP cluster administered by the Center for Theory and Computation, part of the Department of Astronomy at the University of Maryland. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. These results also made use of Lowell Observatory's Lowell Discovery Telescope (LDT), formerly the Discovery Channel Telescope. Lowell operates the LDT in partnership with Boston University, Northern Arizona University, the University of Maryland and the University of Toledo. Partial support of the LDT was provided by Discovery Communications. LMI was built by Lowell Observatory using funds from the National Science Foundation (AST-1005313). M.W.C. acknowledges support from the National Science Foundation with grant No. PHY-2010970. S.A. gratefully acknowledges support from the GROWTH PIRE grant (1545949). Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. E.C.K. acknowledges support from the G.R.E.A.T research environment and the Wenner-Gren Foundations. P.T.H.P. is supported by the research program of the Netherlands Organization for Scientific Research (NWO). H.K. is an LSSTC Data Science Fellow and thanks the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining grant No. 1829740, the Brinson Foundation and the Moore Foundation; his participation in the program has benefited this work. S.M. and J.M. acknowledge support from Science Foundation Ireland under grant No. 17/CDA/4723. R.D. acknowledges support from the Irish Research Council (IRC) under grant GOIPG/2019/2033. P.C. is a Swarana Jayanti Fellow and acknowledges support from the Department of Science and Technology via award No. DST/SJF/PSA-01/2014-15). We thank the staff of the GMRT who made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. P.C. is a Swarna Jayanti Fellow and thanks the Department of Science & Technology in India. We thank D. Bhattacharya, A. Vibhute and V. Shenoy for help with the CZTI analysis. V.A.F. acknowledges support from the RFBR 18-29-21030.

Published
2021

8. Cosmic gamma-ray bursts and soft gamma-repeaters – observations and modeling of extreme astrophysical phenomena: (100th anniversary of the Ioffe Institute)

Author

D. Frederiks, Dmitry S. Svinkin, Andrei M. Bykov, A. Lysenko, A. Tsvetkova, S. Golenetskii, M. Ulanov, Anna Vladimirovna Kozlova, and R. Aptekar

Subjects
Physics, Stars, Neutron star, COSMIC cancer database, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, General Physics and Astronomy, Cosmic ray, Astrophysics, Astrophysical Phenomena, Gamma-ray burst, Luminosity
Abstract

Cosmic gamma-ray bursts (GRBs) and soft gamma-ray repeaters (SGRs) are the brightest sources of high-energy electromagnetic radiation. For many years, GRB and SGR studies have been among the major basic research areas at the Ioffe Institute. The physical processes that power immense luminosity of the cosmic gamma-ray sources are of utmost interest because they enable exploring physical phenomena in the vicinities of stellar-mass black holes and neutron stars, whose magnetic fields are probably larger than the critical vacuum polarization value, i.e., under conditions inaccessible in terrestrial laboratories. Owing to the high luminosity, GRBs can be detected at distances up to the edge of the visible Universe, and thus enable studying how the first stars emerged and probing the properties of matter along the entire line of sight to the sources. We briefly review the results of modern multi-wavelength studies of cosmic GRBs and SGRs. We discuss the history of the GRBs and SGRs studies, a vibrant area of basic astrophysical research at the Ioffe Institute, their accomplishments and prospects. We describe in detail the results obtained with several generations of KONUS detectors that have been designed and manufactured at the Ioffe Institute. Observational data obtained by space-based instruments are effectively complemented by theoretical modeling of astrophysical processes that exhibit extreme energy release. We also discuss prospects for GRB and SGR studies, including future experiments scheduled at the Ioffe Institute.

Published
2019

9. Identification of a Local Sample of Gamma-Ray Bursts Consistent with a Magnetar Giant Flare Origin

Author

Eric Burns, Matthew G. Baring, R. Aloisi, Adam Goldstein, Dmitry S. Svinkin, M. Negro, A. Tohuvavohu, V. G. Savchenko, Gregory Ashton, Zorawar Wadiasingh, Rachel Hamburg, Michael S. Briggs, C. M. Hui, K. Hurley, Péter Veres, Colleen A. Wilson-Hodge, David L. Kaplan, Oliver J. Roberts, D. Kocevski, Nelson Christensen, A. Ridnaia, Mansi Kasliwal, George Younes, S. B. Cenko, David O. Cook, D. D. Frederiks, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 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, and 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)

Subjects
010504 meteorology & atmospheric sciences, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetar, 01 natural sciences, 0103 physical sciences, Satellite galaxy, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Astronomy and Astrophysics, Galaxy, Neutron star, Supernova, Space and Planetary Science, Gamma-ray burst, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract

Cosmological Gamma-Ray Bursts (GRBs) are known to arise from distinct progenitor channels: short GRBs mostly from neutron star mergers and long GRBs from a rare type of core-collapse supernova (CCSN) called collapsars. Highly magnetized neutron stars called magnetars also generate energetic, short-duration gamma-ray transients called Magnetar Giant Flares (MGFs). Three have been observed from the Milky Way and its satellite galaxies and they have long been suspected to contribute a third class of extragalactic GRBs. We report the unambiguous identification of a distinct population of 4 local ($$99.9% confidence. These properties, the host galaxies, and non-detection in gravitational waves all point to an extragalactic MGF origin. Despite the small sample, the inferred volumetric rates for events above $4\times10^{44}$ erg of $R_{MGF}=3.8_{-3.1}^{+4.0}\times10^5$ Gpc$^{-3}$ yr$^{-1}$ place MGFs as the dominant gamma-ray transient detected from extragalactic sources. As previously suggested, these rates imply that some magnetars produce multiple MGFs, providing a source of repeating GRBs. The rates and host galaxies favor common CCSN as key progenitors of magnetars., Comment: Accepted for publication in ApJL. Updated versions fix typos in the table and updates citations to published versions

Published
2021

10. The Konus-Wind catalog of gamma-ray bursts with known redshifts. II. Waiting mode bursts simultaneously detected by Swift/BAT

Author

Dmitry S. Svinkin, A. Tsvetkova, Kevin Hurley, Thomas L. Cline, M. Ulanov, S. Golenetskii, R. L. Aptekar, A. Ridnaia, D. D. Frederiks, and A. Lysenko

Subjects
Physics, Swift, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Mode (statistics), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Spectral bands, Astrophysics::Cosmology and Extragalactic Astrophysics, Redshift, Luminosity, law.invention, Telescope, Space and Planetary Science, law, Range (statistics), Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, computer, computer.programming_language
Abstract

In the Second part of The Konus-Wind Catalog of Gamma-Ray Bursts with Known Redshifts (first part: Tsvetkova et al. 2017; T17), we present the results of a systematic study of gamma-ray bursts (GRBs) with reliable redshift estimates detected simultaneously by the Konus-Wind (KW) experiment (in the waiting mode) and by the Swift/BAT (BAT) telescope during the period from 2005 January to the end of 2018. By taking advantage of the high sensitivity of BAT and the wide spectral band of KW we were able to constrain the peak spectral energies, the broadband energy fluences, and the peak fluxes for the joint KW-BAT sample of 167 weak, relatively soft GRBs (including four short bursts). Based on the GRB redshifts, which span the range $0.04 \leq z \leq 9.4$, we estimate the rest-frame, isotropic-equivalent energy, and peak luminosity. For 14 GRBs with reasonably constrained jet breaks, we provide the collimation-corrected values of the energetics. This work extends the sample of KW GRBs with known redshifts to 338 GRBs, the largest set of cosmological GRBs studied to date over a broad energy band. With the full KW sample, accounting for the instrumental bias, we explore GRB rest-frame properties, including hardness-intensity correlations, GRB luminosity evolution, luminosity and isotropic-energy functions, and the evolution of the GRB formation rate, which we find to be in general agreement with those reported in T17 and other previous studies., Accepted for publication in ApJ; 41 pages, 5 figures, 7 tables. References in Table 5 fixed compared with the initial submission. See also arXiv:1710.08746 for Part I of the Catalog

Published
2020

11. SN 2020bvc: A Broad-line Type Ic Supernova with a Double-peaked Optical Light Curve and a Luminous X-Ray and Radio Counterpart

Author

Eric Burns, T. Kupfer, Shreya Anand, Cristina Barbarino, David Hale, Avishay Gal-Yam, Shrinivas R. Kulkarni, Steve Schulze, Jesper Sollerman, Julia Martikainen, Kirsty Taggart, Russ R. Laher, Leonardo Tartaglia, Lin Yan, Maayane T. Soumagnac, Frank J. Masci, Mansi M. Kasliwal, Daniel A. Goldstein, Dmitry S. Svinkin, Richard Dekany, V. G. Savchenko, Ben Rusholme, D. D. Frederiks, James D. Neill, Christoffer Fremling, Alessandra Corsi, David L. Shupe, Anna Y. Q. Ho, Rachel Bruch, Eric C. Bellm, Kaushik De, Jeffry Zolkower, A. Ridnaia, Dmitry A. Duev, Ragnhild Lunnan, V. Zach Golkhou, Matthew J. Graham, S. Bradley Cenko, Alexandre Delacroix, Nora L. Strotjohann, Daniel A. Perley, Planetary-system research, and Department of Physics

Subjects
010504 meteorology & atmospheric sciences, Astrophysics, Type Ic supernovae, Surveys, Atomic, 01 natural sciences, 7. Clean energy, Spectral line, Luminosity, Particle and Plasma Physics, 2006AJ, Core-collapse supernovae, 010303 astronomy & astrophysics, QC, QB, astro-ph.HE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), PROGENITORS, X-ray transient sources, BURST, Supernova, Supernovae, Gamma-ray bursts, Astrophysics - High Energy Astrophysical Phenomena, High energy astrophysics, Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Radio transient sources, SHOCK BREAKOUT, TELESCOPE, FOS: Physical sciences, Astronomy & Astrophysics, Type (model theory), GRB-060218, PHYSICS, 0103 physical sciences, Binary star, LOW-RESOLUTION, Nuclear, 0105 earth and related environmental sciences, Molecular, Astronomy and Astrophysics, 115 Astronomy, Space science, Light curve, Transient sources, EVOLUTION, Space and Planetary Science, Variable star, EMISSION, Gamma-ray burst
Abstract

We present optical, radio, and X-ray observations of SN2020bvc (=ASASSN20bs; ZTF20aalxlis), a nearby ($z=0.0252$; $d$=114 Mpc) broad-lined (BL) Type Ic supernova (SN). Our observations show that SN2020bvc shares several properties in common with the Ic-BL SN2006aj, which was associated with the low-luminosity gamma-ray burst (LLGRB) 060218. First, the 10 GHz radio light curve is on the faint end of LLGRB-SNe ($L_\mathrm{radio} \approx 10^{37}$erg/s): we model our VLA observations (spanning 13-43 d) as synchrotron emission from a mildly relativistic ($v \gtrsim 0.3c$) forward shock. Second, with Swift and Chandra we detect X-ray emission ($L_X \approx 10^{41}$erg/s) that is not naturally explained as inverse Compton emission or as part of the same synchrotron spectrum as the radio emission. Third, high-cadence ($6\times$/night) data from the Zwicky Transient Facility (ZTF) shows a double-peaked optical light curve, the first peak from shock-cooling emission from extended low-mass material (mass $M10^{12}$cm) and the second peak from the radioactive decay of Ni-56. SN2020bvc is the first confirmed double-peaked Ic-BL SN discovered without a GRB trigger, and shows X-ray and radio emission similar to LLGRB-SNe: this is consistent with models in which the same mechanism produces both the LLGRB and the shock-cooling emission. For four of the five other nearby ($z\lesssim0.05$) Ic-BL SNe with ZTF high-cadence data, we rule out a first peak like that seen in SN2006aj and SN2020bvc, i.e. that lasts $\approx 1$d and reaches a peak luminosity $M \approx -18$. X-ray and radio follow-up observations of future such events will establish whether double-peaked optical light curves are indeed predictive of LLGRB-like X-ray and radio emission., Accepted to ApJ. 39 pages, 17 figures. Comments welcome

Published
2020

12. A Mildly Relativistic Outflow from the Energetic, Fast-rising Blue Optical Transient CSS161010 in a Dwarf Galaxy

Author

Peter Nugent, Maria R. Drout, Poonam Chandra, Christopher S. Kochanek, Tanmoy Laskar, Michael Bietenholz, S. Valenti, Peter Lundqvist, D. Frederiks, Morgan MacLeod, B. J. Shappee, A. J. Nayana, W. Fong, Damiano Caprioli, Eric R. Coughlin, D. J. Sand, Y. Dong, M. C. Stroh, A. Ridnaia, A. Baldeschi, Kate D. Alexander, Deanne L. Coppejans, C. Guidorzi, B. A. Zauderer, K. H. Hurley, Sheng Yang, C. Frohmaier, Dmitry S. Svinkin, Bing Zhang, Daniel E. Reichart, Dan Milisavljevic, Giacomo Terreran, C. Esquivia, Charlotte Ward, Igor Chilingarian, Raffaella Margutti, Aaron M. Meisner, and Kerry Paterson

Subjects
Accretion, Radio transient sources, 010504 meteorology & atmospheric sciences, Stellar mass, TIDAL DISRUPTION, Astrophysics::High Energy Astrophysical Phenomena, Socio-culturale, FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, CORE-COLLAPSE SUPERNOVAE, 0103 physical sciences, RATES, 010303 astronomy & astrophysics, BLACK-HOLES, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Dwarf galaxy, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, GAMMA-RAY BURSTS, Supernovae, Black holes, X-ray transient sources, RADIO, Star formation, Astronomy and Astrophysics, Galaxy, Black hole, HOST GALAXIES, Stars, Supernova, Space and Planetary Science, STELLAR POPULATION SYNTHESIS, IBC SUPERNOVA, Astrophysics - High Energy Astrophysical Phenomena, EMISSION, Astronomical and Space Sciences
Abstract

We present X-ray and radio observations of the Fast Blue Optical Transient (FBOT) CRTS-CSS161010 J045834-081803 (CSS161010 hereafter) at t=69-531 days. CSS161010 shows luminous X-ray ($L_x\sim5\times 10^{39}\,\rm{erg\,s^{-1}}$) and radio ($L_{\nu}\sim10^{29}\,\rm{erg\,s^{-1}Hz^{-1}}$) emission. The radio emission peaked at ~100 days post transient explosion and rapidly decayed. We interpret these observations in the context of synchrotron emission from an expanding blastwave. CSS161010 launched a mildly relativistic outflow with velocity $\Gamma\beta c\ge0.55c$ at ~100 days. This is faster than the non-relativistic AT2018cow ($\Gamma\beta c\sim0.1c$) and closer to ZTF18abvkwla ($\Gamma\beta c\ge0.3c$ at 63 days). The inferred initial kinetic energy of CSS161010 ($E_k\gtrsim10^{51}$ erg) is comparable to that of long Gamma Ray Bursts (GRBs), but the ejecta mass that is coupled to the mildly relativistic outflow is significantly larger ($\sim0.01-0.1\,\rm{M_{\odot}}$). This is consistent with the lack of observed gamma-rays. The luminous X-rays were produced by a different emission component to the synchrotron radio emission. CSS161010 is located at ~150 Mpc in a dwarf galaxy with stellar mass $M_{*}\sim10^{7}\,\rm{M_{\odot}}$ and specific star formation rate $sSFR\sim 0.3\,\rm{Gyr^{-1}}$. This mass is among the lowest inferred for host-galaxies of explosive transients from massive stars. Our observations of CSS161010 are consistent with an engine-driven aspherical explosion from a rare evolutionary path of a H-rich stellar progenitor, but we cannot rule out a stellar tidal disruption event on a centrally-located intermediate mass black hole. Regardless of the physical mechanism, CSS161010 establishes the existence of a new class of rare (rate $, Comment: Accepted to ApJL

Published
2020

13. Author Correction: Discovery and confirmation of the shortest gamma-ray burst from a collapsar

Author

Anna Y. Q. Ho, Kevin Hurley, Philippe Rosnet, Simeon Reusch, A. J. Castro-Tirado, Harsh Kumar, Viraj Karambelkar, Eleonora Troja, S. R. Kulkarni, Kaushik De, Ashish Mahabal, Igor Andreoni, Leo Singer, Bryce Bolin, Rachel Dunwoody, Christoffer Fremling, A. F. Valeev, Avishay Gal-Yam, Poonam Chandra, S. Dichiara, Roger Smith, Dmitry A. Duev, Chris Cannella, E. C. Kool, S. Bradley Cenko, Richard Walters, Matthew J. Graham, Maayane T. Soumagnac, B. Rusholme, Joseph Mangan, Varun Bhalerao, Eric Burns, Tomas Ahumada, Geoffrey Ryan, Mouza Almualla, A. Tsvetkova, Mansi M. Kasliwal, Shashi B. Pandey, Peter T. H. Pang, Mattia Bulla, Virginia Cunningham, Sheila McBreen, Dmitry S. Svinkin, Eric C. Bellm, Shreya Anand, Sonalika Purkayastha, Pradip Gatkine, Tim Dietrich, Robert Stein, Erica Hammerstein, Frank J. Masci, A. Ridnaia, Shabnam Iyyani, D. D. Frederiks, Michael W. Coughlin, Daniel A. Perley, and Ana Sagués Carracedo

Subjects
Physics, 010504 meteorology & atmospheric sciences, High-energy astronomy, 0103 physical sciences, Astronomy and Astrophysics, Astrophysics, Gamma-ray burst, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences, Time domain astronomy
Published
2021

14. The Sun and heliosphere explorer – the Interhelioprobe mission

Author

Valery V. Dmitrenko, B. Ya. Scherbovsky, I. A. Rubinshtein, A. Remizov, V. M. Grachev, V. V. Bezrukikh, S. I. Svertilov, Z. M. Uteshev, A. F. Iyudin, A. A. Petrukovich, Artem Ulyanov, I. E. Kozhevatov, A. V. Simonov, Oleg Vaisberg, O. V. Dudnik, I. V. Chulkov, A. P. Ryzhenko, V. N. Obridko, E. N. Lavrentiev, Sergey E. Ulin, M. S. Konstantinov, K. S. Gribovskyi, F. Hruška, E. M. Kruglov, V. G. Tyshkevich, J. Šimůnek, Alexander E. Shustov, A. Skalsky, M. I. Verigin, V. M. Sinelnikov, S. E. Andreevskyi, V. S. Dobrovolskyi, V. V. Fomichev, V. P. Lazutkov, V. V. Levedev, E. A. Rudenchik, S. V. Shestov, Yu. A. Trofimov, Yu. Venedictov, A. V. Kochemasov, Ivan Zimovets, Sergey A. Bogachev, V. A. Styazhkin, A. S. Kirichenko, Sergey Kuzin, V. V. Bogomolov, R. A. Kovrazhkin, F. P. Oleinik, Ondrej Santolik, Benoit Lavraud, Marek Siarkowski, A. A. Konovalov, Ivana Kolmasova, Janusz Sylwester, V. A. Dergachev, V. N. Yurov, A. A. Kholodilov, J. Bąkała, O. V. Morozov, R. L. Aptekar, Valentin Pal'shin, D. D. Frederiks, D. V. Petrenko, N. I. Lebedev, M. Hilchenbach, D. V. Skorodumov, H.-U. Auster, M. I. Panasyuk, S. Golenetskii, A Y Shestakov, D A Moiseenko, Vladimir Truhlik, A. S. Tsvetkova, K. Anufreychik, Lev Zelenyi, A. A. Reva, V. N. Stekhanov, V. D. Kuznetsov, Żaneta Szaforz, A.S. Novikov, I. V. Rubtsov, Dmitry S. Svinkin, M. Ulanov, B. V. Marjin, Yu. D. Zhugzhda, V. S. Dokukin, Miroslaw Kowalinski, V. I. Tulupov, A. A. Pertsov, G. Berghofer, R. N. Zhuravlev, V. I. Galkin, G. A. Kotova, M. I. Savchenko, Konstantin F. Vlasik, A. S. Glyanenko, A. I. Repin, Irina V. Chernysheva, E. E. Lupar, A. V. Ivanov, Yu. D. Kotov, V. P. Polyanskyi, V. I. Osedlo, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), 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
010504 meteorology & atmospheric sciences, Computer Science::Digital Libraries, 01 natural sciences, Space exploration, Astrobiology, Interhelioprobe space mission, heliospheric physics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, solar physics, 0105 earth and related environmental sciences, Physics, Energetic neutral atom, Spacecraft, business.industry, Payload, Sun, heliosphere, Astrophysics::Instrumentation and Methods for Astrophysics, Ecliptic, Astronomy, solar-terrestrial relations, Solar physics, Geophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics, business, Heliosphere
Abstract

International audience; The Interhelioprobe mission aims to investigate the inner heliosphere and the Sun from close distances (up to 0.3 AU) and from out of the ecliptic plane (up to 30°). In this paper we present the relevance of the mission and its main scientific objectives, describe the scientific payload, ballistic scenario and orbits of the spacecraft. Possibilities of scientific cooperation with other solar and heliospheric space missions are also mentioned.

Published
2016

15. X-ray and gamma-ray emission of solar flares

Author

A. Tsvetkova, S. Golenetskii, M. Ulanov, Dmitry S. Svinkin, Gregory D. Fleishman, A. Ridnaia, D. Frederiks, R. Aptekar, A. Altyntsev, and A. Lysenko

Subjects
Materials science, Solar flare, Gamma ray, X-ray, General Physics and Astronomy, Astrophysics
Published
2019

17. The Broad-lined Ic Supernova ZTF18aaqjovh (SN 2018bvw): An Optically-discovered Engine-driven Supernova Candidate with Luminous Radio Emission

Author

Matthew J. Graham, Alessandra Corsi, Adam A. Miller, S. Bradley Cenko, Russ R. Laher, Ashish Mahabal, David L. Shupe, Jesper Sollerman, D. D. Frederiks, Maayane T. Soumagnac, Anna Y. Q. Ho, Richard Dekany, Shrinivas R. Kulkarni, Ben Rusholme, Scott M. Adams, Christoffer Fremling, Yashvi Sharma, Thomas Kupfer, A. Ridnaia, Francesco Taddia, Kaushik De, Reed Riddle, V. Zach Golkhou, Daniel J. Reiley, Frank J. Masci, Tiara Hung, Dmitry S. Svinkin, and James D. Neill

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Luminosity, Supernova, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Ejecta, Gamma-ray burst, 010303 astronomy & astrophysics, Event (particle physics), Order of magnitude, 0105 earth and related environmental sciences
Abstract

We present ZTF18aaqjovh (SN 2018bvw), a high-velocity ("broad-lined") stripped-envelope (Type Ic) supernova (Ic-BL SN) discovered in the Zwicky Transient Facility one-day cadence survey. ZTF18aaqjovh shares a number of features in common with engine-driven explosions: the photospheric velocity and the shape of the optical light curve are very similar to that of the Type Ic-BL SN 1998bw, which was associated with a low-luminosity gamma-ray burst (LLGRB) and had relativistic ejecta. However, the radio luminosity of ZTF18aaqjovh is almost two orders of magnitude fainter than that of SN 1998bw at the same velocity phase, and the shock velocity is at most mildly relativistic (v=0.06-0.4c). A search of high-energy catalogs reveals no compelling GRB counterpart to ZTF18aaqjovh, and the limit on the prompt GRB luminosity of $L_{\gamma,\mathrm{iso}} \approx 1.6 \times 10^{48}$ erg/sec excludes a classical GRB but not an LLGRB. Altogether, ZTF18aaqjovh represents another transition event between engine-driven SNe associated with GRBs and "ordinary" Ic-BL SNe., Comment: 18 pages, 8 figures. Accepted to the Astrophysical Journal on 2 March 2020. Revised from proofs on 4 Apr 2020

Published
2019
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18. The first observation of an intermediate flare from SGR 1935+2154

Author

D. D. Frederiks, I. G. Mitrofanov, A. Tsvetkova, Dmitry Golovin, Dmitry S. Svinkin, V. Pal'Shin, G. L. Israel, Kevin Hurley, Xiao-Ling Zhang, John O. Goldsten, and A. Kozlova

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Bremsstrahlung, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Power law, Spectral line, law.invention, Space and Planetary Science, law, 0103 physical sciences, Black-body radiation, Astrophysics - High Energy Astrophysical Phenomena, Interplanetary spaceflight, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Flare
Abstract

We report on the bright burst detected by four Interplanetary network (IPN) spacecraft on 2015 April 12. The IPN localization of the source is consistent with the position of the recently discovered soft gamma-repeater SGR 1935+2154. From the Konus-Wind (KW) observation, we derive temporal and spectral parameters of the emission, and the burst energetics. The rather long duration of the burst ($\sim$1.7 s) and the large measured energy fluence ($\sim2.5\times10^{-5}$ erg cm$^{-2}$) put it in the class of rare "intermediate" SGR flares, and this is the first one observed from SGR 1935+2154. A search for quasi-periodic oscillations in the KW light curve yields no statistically significant signal. Of four spectral models tested, optically thin thermal bremsstrahlung and a single blackbody (BB) function can be rejected on statistical grounds; two more complex models, a cutoff power law (CPL) and a sum of two BB functions (2BB), fit the burst spectra well and neither of them may be ruled out by the KW observation. The CPL and 2BB model parameters we report for this bright flare are typical of SGRs; they are also consistent with those obtained from observations of much weaker and shorter SGR 1935+2154 bursts with other instruments. From the distribution of double blackbody spectral fit parameters we estimate the SGR 1935+2154 distance to be $, Comment: 7 pages, 6 figures, accepted for publication in MNRAS

Published
2016

19. AGILE and Konus-Wind Observations of GRB 190114C: The Remarkable Prompt and Early Afterglow Phases

Author

R. Aptekar, Francesco Lucarelli, V. Vittorini, F. Paoletti, Dmitry S. Svinkin, M. Feroci, C. Pittori, I. Donnarumma, Y. Evangelista, M. Romani, D. Frederiks, P. A. Caraveo, F. Fuschino, P. W. Cattaneo, A. Tsvetkova, F. Lazzarotto, G. Piano, Martino Marisaldi, N. Parmiggiani, A. Morselli, F. Longo, M. Pilia, M. Cardillo, C. Casentini, E. Costa, Arnaud Ferrari, M. Tavani, A. Ursi, M. Galli, F. Verrecchia, A. Giuliani, G. Barbiellini, Claudio Labanti, A. Trois, L. A. Antonelli, A. W. Chen, A. Argan, Andrea Bulgarelli, S. Vercellone, Ursi, A., Tavani, M., Frederiks, D. D., Romani, M., Verrecchia, F., Marisaldi, M., Aptekar, R. L., Antonelli, L. A., Argan, A., Bulgarelli, A., Barbiellini, G., Caraveo, P., Cardillo, M., Casentini, C., Cattaneo, P. W., Chen, A., Costa, E., Donnarumma, I., Evangelista, Y., Feroci, M., Ferrari, A., Fuschino, F., Galli, M., Giuliani, A., Labanti, C., Lazzarotto, F., Longo, F., Lucarelli, F., Morselli, A., Paoletti, F., Parmiggiani, N., Piano, G., Pilia, M., Pittori, C., Svinkin, D. S., Trois, A., Tsvetkova, A. E., Vercellone, S., and Vittorini, V.

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Flux, Astrophysics, 01 natural sciences, Gamma-ray transient sources, 0103 physical sciences, Radiative transfer, Gamma-ray transient sources (1853), Adiabatic process, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Gamma-ray astronomy, Gamma-ray astronomy (628), Astronomy and Astrophysics, Spectral component, Afterglow, Space and Planetary Science, Gamma-ray bursts (629), Gamma-ray bursts, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract

GRB 190114C represents a breakthrough for the physics of gamma-ray bursts (GRBs), being the first GRB with delayed emission above 300 GeV, as reported by MAGIC. We present in this paper the sub-MeV/MeV data of the prompt and early afterglow emissions of GRB 190114C, as detected by AGILE and Konus-Wind, in the 20 keV-100 MeV energy range. The first stages of the burst exhibit multiple emission components, associated with an interesting spectral evolution. The first 2 s of the prompt emission can be described by a single "Band-like" spectral component. The successive 4 s show the presence of an additional high-energy spectral component, which quickly evolves into a "hard-flat" component of the νFν spectrum, extending up to 10-100 MeV and likely produced by inverse Compton radiation, whose onset and evolution are clearly shown in our data. After this phase, the νFν spectrum evolves into a "V shape," showing the persistence and spectral hardening of the additional high-energy component in substantial agreement with Fermi and Swift results. We also analyze the first ∼200 s of the early afterglow that show a reflaring episode near T0 + 15 s. We identify a new, so-far-unnoticed flux temporal break near T0 + 100 s, which is detected in hard X-rays by both Konus-Wind and INTEGRAL/SPI-ACS. We find this break incompatible with the commonly assumed adiabatic evolution of a fireball in a constant-density medium. We interpret this break as a consequence of radiative evolution of the early afterglow from a fireball expanding in a wind-like circumburst medium.

Published
2020

20. An embedded X-ray source shines through the aspherical AT2018cow: revealing the inner workings of the most luminous fast-evolving optical transients

Author

Maria R. Drout, A. Kozlova, Indrek Vurm, Enrico Bozzo, D. Frederiks, Wen-fai Fong, R. Cartier, Brian D. Metzger, Sandro Mereghetti, Brian W. Grefenstette, Giacomo Terreran, P. Laurent, Edo Berger, Nathaniel Roth, James F. Steiner, C. Guidorzi, Lorenzo Ducci, P. K. Blanchard, Carlo Ferrigno, Tanmoy Laskar, Michael Bietenholz, P. Ubertini, Kate D. Alexander, Kerry Paterson, G. Migliori, Ryan Chornock, Dan Milisavljevic, D. Gotz, D. Brethauer, A. Hajela, E. Kuulkers, Kevin Hurley, Tarraneh Eftekhari, Matt Nicholl, Eric R. Coughlin, Ben Margalit, Dmitry S. Svinkin, Igor Chilingarian, V. G. Savchenko, John Banovetz, Raffaella Margutti, Norbert Bartel, Daniel J. Patnaude, Deanne L. Coppejans, Andrew MacFadyen, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and Margutti, R. and Metzger, B.~D. and Chornock, R. and Vurm, I. and Roth, N. and Grefenstette, B.~W. and Savchenko, V. and Cartier, R. and Steiner, J.~F. and Terreran, G. and Margalit, B. and Migliori, G. and Milisavljevic, D. and Alexander, K.~D. and Bietenholz, M. and Blanchard, P.~K. and Bozzo, E. and Brethauer, D. and Chilingarian, I.~V. and Coppejans, D.~L. and Ducci, L. and Ferrigno, C. and Fong, W. and G

Subjects
(AT 2018cow), 010504 meteorology & atmospheric sciences, Socio-culturale, FOS: Physical sciences, Astrophysics, Compact star, Magnetar, X-rays: general, 01 natural sciences, 7. Clean energy, Spectral line, Luminosity, accretion, 0103 physical sciences, Blue supergiant, accretion, accretion disks, stars: black holes, supernovae: individual: AT 2018cow, X-rays: general, 010303 astronomy & astrophysics, supernovae: individual, 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Photosphere, supernovae: individual (AT 2018cow), accretion disks, Astronomy and Astrophysics, accretion, accretion disks, stars: black holes, Supernova, Stars, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

We present the first extensive radio to gamma-ray observations of a fast-rising blue optical transient (FBOT), AT2018cow, over its first ~100 days. AT2018cow rose over a few days to a peak luminosity $L_{pk}\sim4\times 10^{44}$ erg/s exceeding those of superluminous supernovae (SNe), before declining as $\propto t^{-2}$. Initial spectra at $\lesssim 15$ days were mostly featureless and indicated large expansion velocities v~0.1c and temperatures reaching 30000 K. Later spectra revealed a persistent optically-thick photosphere and the emergence of H and He emission features with v~sim 4000 km/s with no evidence for ejecta cooling. Our broad-band monitoring revealed a hard X-ray spectral component at $E\ge 10$ keV, in addition to luminous and highly variable soft X-rays, with properties unprecedented among astronomical transients. An abrupt change in the X-ray decay rate and variability appears to accompany the change in optical spectral properties. AT2018cow showed bright radio emission consistent with the interaction of a blastwave with $v_{sh}$~0.1c with a dense environment ($\dot M\sim10^{-3}-10^{-4}\,M_{\odot}yr^{-1}$ for $v_w=1000$ km\s). While these properties exclude Ni-powered transients, our multi-wavelength analysis instead indicates that AT2018cow harbored a "central engine", either a compact object (magnetar or black hole) or an embedded internal shock produced by interaction with a compact, dense circumstellar medium. The engine released $\sim10^{50}-10^{51.5}$ erg over $\sim10^3-10^5$ s and resides within low-mass fast-moving material with equatorial-polar density asymmetry ($M_{ej,fast}\lesssim0.3\,\rm{M_{\odot}}$). Successful SNe from low-mass H-rich stars (like electron-capture SNe) or failed explosions from blue supergiants satisfy these constraints. Intermediate-mass black-holes are disfavored by the large environmental density probed by the radio observations., Comment: 26 pages + tables. Submitted

Published
2018
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21. GRB171205A/SN2017iuk: A local low-luminosity gamma-ray burst

Author

A. Tsvetkova, Antonino D'Ai, A. Tohuvavohu, Dmitry S. Svinkin, M. de Pasquale, Valerio D'Elia, P. T. O'Brien, S. W. K. Emery, J. P. Osborne, A. Melandri, S. R. Oates, Peter J. Brown, D. D. Frederiks, Sergio Campana, David N. Burrows, S. B. Cenko, R. L. C. Starling, M. H. Siegel, A. Y. Lien, A. A. Breeveld, G. Tagliaferri, K. L. Page, ITA, USA, GBR, and TUR

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Light curve, 01 natural sciences, Universe, Redshift, Galaxy, Luminosity, Supernova, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, Gamma-ray burst, 010303 astronomy & astrophysics, media_common
Abstract

Gamma-ray bursts (GRBs) occurring in the local Universe constitute an interesting sub-class of the GRB family, since their luminosity is on average lower than that of their cosmological analogs. We aim to contribute to the study of local bursts by reporting the case of GRB 171205A. This source was discovered by Swift Burst Alert Telescope (BAT) on 2017, December 5 and soon associated with a low redshift host galaxy (z=0.037), and an emerging SN (SN 2017iuk). We analyzed the full Swift, dataset, comprising the UV-Optical Telescope (UVOT), X-ray Telescope (XRT) and BAT data. In addition, we employed the Konus-Wind high energy data as a valuable extension at gamma-ray energies. The photometric SN signature is clearly visible in the UVOT u, b and v filters. The maximum emission is reached at ~ 13 (rest frame) days, and the whole bump resembles that of SN 2006aj, but lower in magnitude and with a shift in time of +2 d. A prebump in the v-band is also clearly visible, and this is the first time that such a feature is not observed achromatically in GRB-SNe. Its physical origin cannot be easily explained. The X-ray spectrum shows an intrinsic Hydrogen column density N_H,int = 7.4(+4.1 -3.6) X 10^20 / cm^2$, which is at the low end of the N_H,int, even considering just low redshift GRBs. The spectrum also features a thermal component, which is quite common in GRBs associated with SNe, but whose origin is still a matter of debate. Finally, the isotropic energy in the gamma-ray band, E_iso = 2.18(+0.63 -0.50) X 10^49 erg, is lower than those of cosmological GRBs. Combining this value with the peak energy in the same band, E_p=125(+141 -37) keV, implies that GRB 171205A is an outlier of the Amati relation, as are some other low redshift GRBs, and its emission mechanism should be different from that of canonical, farther away GRBs., Comment: 13 pages, 10 figures, A&A in press

Published
2018
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22. Transition from fireball to Poynting-flux-dominated outflow in the three-episode GRB 160625B

Author

Ronan Cunniffe, Sergey Bondar, Bing Zhang, R. Inasaridze, S. R. Oates, J. C. Tello, Lijing Shao, R. Aptekar, P.-H. T. Tam, A. Cwiek, Rumyantsev, P. Ferrero, Sokolov, A. Perkov, E. Klunko, O. Burhonov, A. J. Castro-Tirado, Lech Mankiewicz, Shashi B. Pandey, E. Katkova, R. Sanchez-Ramirez, R. Opiela, A. Castellon, Sergey Karpov, He Gao, Martin Jelínek, S. Jeong, Zi-Gao Dai, Qing-Wen Tang, Bin-Bin Zhang, Fu-Wen Zhang, Gregory Beskin, Ignacio de Gregorio Monsalvo, E. Ivanov, P. Minaev, Alexei Pozanenko, N. Orekhova, A. Kusakin, Sasyuk, Anton Biryukov, D. D. Frederiks, A. S. Moskvitin, Aleksander Filip Żarnecki, A. K. Zadrożny, M. D. Caballero-Garcia, T. A. Fatkhullin, S. R. Oats, Dmitry S. Svinkin, Xue-Feng Wu, Aleksander Filip Zarnecki, E. Mazaeva, A. F. Valeev, Il Han Park, A. Volnova, Y. D. Hu, X.-Y. Wang, Ministerio de Economía y Competitividad (España), European Commission, National Aeronautics and Space Administration (US), National Natural Science Foundation of China, China Scholarship Council, Russian Foundation for Basic Research, Russian Science Foundation, Leverhulme Trust, Government of South Korea, and Kazakh Government

Subjects
Physics, Brightness, Jet (fluid), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Synchrotron radiation, Astronomy, Flux, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spectral component, 01 natural sciences, Stars, Luminosity, High-energy astrophysics, 0103 physical sciences, Ejecta, Gamma-ray burst, 010303 astronomy & astrophysics
Abstract

The ejecta composition is an open question in gamma-ray burst (GRB) physics . Some GRBs possess a quasi-thermal spectral component in the time-resolved spectral analysis , suggesting a hot fireball origin. Others show a featureless non-thermal spectrum known as the Band function , consistent with a synchrotron radiation origin and suggesting that the jet is Poynting-flux dominated at the central engine and probably in the emission region as well . There are also bursts showing a sub-dominant thermal component and a dominant synchrotron component , suggesting a probable hybrid jet composition . Here, we report an extraordinarily bright GRB 160625B, simultaneously observed in gamma-ray and optical wavelengths, whose prompt emission consists of three isolated episodes separated by long quiescent intervals, with the durations of each sub-burst being approximately 0.8 s, 35 s and 212 s, respectively. Its high brightness (with isotropic peak luminosity L ≈ 4 × 10 erg s) allows us to conduct detailed time-resolved spectral analysis in each episode, from precursor to main burst and to extended emission. The spectral properties of the first two sub-bursts are distinctly different, allowing us to observe the transition from thermal to non-thermal radiation between well-separated emission episodes within a single GRB. Such a transition is a clear indication of the change of jet composition from a fireball to a Poynting-flux-dominated jet., B.-B.Z. thanks Y.-Z. Fan, Y.-Z. Wang, H. Wang, K. D. Alexander and D. Lazzati for helpful discussions. We are grateful to K. Hurley, I. Mitrofanov, A. Sanin, M. Litvak and W. Boynton for the use of Mars Odyssey data in the triangulation. We acknowledge the use of the public data from the Swift and Fermi data archives. B.-B. Z. and A.J. C.-T. acknowledge support from the Spanish Ministry Projects AYA2012-39727-C03-01 and AYA2015-71718-R. Part of this work made use of B.-B.Z.'s personal Interactive Data Language (IDL) code library ZBBIDL and personal Python library ZBBPY. The computation resources used in this work are owned by Scientist Support LLC. B.Z. acknowledges NASA NNX14AF85G and NNX15AK85G for support. Z. G. D. acknowledges the National Natural Science Foundation of China(NSFC) (grant 11573014). Y.-D. H. acknowledges support by China Scholarships Council (grant 201406660015). Mini-MegaTORTORA belongs to Kazan Federal University, and the work is performed according to the Russian Government Program of Competitive Growth of Kazan Federal University. A. P., E.M., P. M. and A.V. are grateful to the Russian Foundation for Basic Research (grant 17-02-01388) for partial support. A. P. and S.B.P. acknowledge joint BRICS (Brazil, Russia, India, China and South Africa) grant RFBR 17-52-80139 and 388-ProFChEAP for partial support. R. I. is grateful to grant RUSTAVELI FR/379/6300/ 14 for partial support. Observations on Mini-MegaTORTORA are supported by the Russian Science Foundation (grant 14-50-00043). A.V.F. and A. M. thank the Russian Science Foundation (grant 14-50-00043). L.M. and A.F.Z. acknowledge support from INTA-CEDEA ESAt personnel hosting the Pi of the Sky facility at the BOOTES-1 station. H. G. and X.-Y.W. acknowledge NSFC (grants 11603003 and 11625312, respectively). Z. G. D., X.-F. W., B.Z., X.-Y. W.,L.S. and F.-W.Z. are also supported by the 973 program (grant 2014CB845800). F.-W.Z. is also supported in part by the NSFC (grants U1331101 and 11163003), the Guangxi Natural Science Foundation (grant 2013GXNSFAA019002) and the project of outstanding young teachers' training in higher education institutions of Guangxi. L.S. acknowledges support by the NSFC (grant 11103083) and the Joint NSFC-ISF Research Program (grant 11361140349). S.O. acknowledges the support of the Leverhulme Trust. S.J. acknowledges support from Korea Basic Science Research Program through NRF-2014R1A6A3A03057484 and NRF-2015R1D1A4A01020961, and I. H. P. through NRF-2015R1A2A1A01006870 and NRF-2015R1A2A1A15055344. R. A., D. F. and D. S. acknowledge support from RSF (grant 17-12-01378). A. K. acknowledges the Science and Education Ministry of Kazakhstan (grant 0075/GF4).

Published
2018

23. Analysis of hard X- and gamma-rays and microwave emissions during the flare of July 18, 2002

Author

D. D. Frederiks, Valentin Pal'shin, S. A. Kuznetsov, Dmitry S. Svinkin, R. L. Aptekar, A. E. Tsvetkova, S. V. Golenetsky, Yu. E. Charikov, M. Ulanov, Victor F. Melnikov, Z. Ya. Sokolova, A. N. Shabalin, and I. V. Kudryavtsev

Subjects
Physics, Spectral index, Solar flare, Spectrometer, Astrophysics::High Energy Astrophysical Phenomena, Flux, Energy flux, Astrophysics, law.invention, Geophysics, Space and Planetary Science, law, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Microwave, Radio wave, Flare
Abstract

The Nobeyama Radioheliograph observation results and data from the KONUS-Wind spectrometer mounted at the Wind and RHESSI satellites on several solar flares are jointly analyzed. The analysis results for data on the flare of July 18, 2002 are described. The hard X-rays were measured in the 18 keV-15 MeV range (KONUS-Wind), and spectroheliograph measurements were carried out in the radio range at frequencies of 17 and 34 GHz. Spatial distributions of the radio brightness were calculated for the flare of July 18, 2002; they show the presence of two sources at the footpoints and one source at the top of the supposed flaring loop. The energy spectra of hard X-rays, energy flux, and the total number of accelerated electrons were found from the KONUS spectrometer data. The number of accelerated X-ray emitted electrons was estimated as N ≥ 1036, and the maximum X-ray energy flux was estimated as ∼5 × 10−6 erg cm−2 s−1. The spectrum index varies in time from −4.6 to −3.6, i.e., the soft-hard-harder trend is implemented. The spectral index of the radio waves is α ≈ −0.3 at the flare start, attains the value α ≈ −0.5 at the flux maximum, and even change the sign further. The accelerated electron transport model in the flare loop plasma is suggested for interpretation of relationships between parameters of the radio emission and hard X-rays.

Published
2014

24. The Konus-Wind catalog of gamma-ray bursts with known redshifts. I. Bursts detected in the triggered mode

Author

Philipp Oleynik, Thomas L. Cline, A. Lysenko, V. D. Pal'shin, S. Golenetskii, D. D. Frederiks, Dmitry S. Svinkin, Kevin Hurley, M. Ulanov, A. Tsvetkova, and R. Aptekar

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Jet (fluid), 010308 nuclear & particles physics, media_common.quotation_subject, Horizon, Astrophysics::High Energy Astrophysical Phenomena, Mode (statistics), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Universe, Redshift, Luminosity, Space and Planetary Science, 0103 physical sciences, Range (statistics), Formation rate, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Energy (signal processing), media_common
Abstract

In this catalog, we present the results of a systematic study of gamma-ray bursts (GRBs) with reliable redshift estimates detected in the triggered mode of the Konus-Wind (KW) experiment during the period from 1997 February to 2016 June. The sample consists of 150 GRBs (including twelve short/hard bursts) and represents the largest set of cosmological GRBs studied to date over a broad energy band. From the temporal and spectral analyses of the sample, we provide the burst durations, the spectral lags, the results of spectral fits with two model functions, the total energy fluences, and the peak energy fluxes. Based on the GRB redshifts, which span the range 0.1, Accepted for publication in ApJ; 65 pages, 15 figures, 8 tables

Published
2017

25. iPTF16asu: A Luminous, Rapidly-Evolving, and High-Velocity Supernova

Author

Gary Doran, N. Blagorodnova, Frank J. Masci, D. A. Perley, P. E. Nugent, S. B. Cenko, Giorgos Leloudas, Adam Rubin, Jesper Sollerman, P. R. Wozniak, Ragnhild Lunnan, K. Hurley, M. M. Kasliwal, F. Taddia, D. Frederiks, Alessandra Corsi, V. Savchenko, Y. Cao, S. R. Kulkarni, Emir Karamehmetoglu, Andreas Ritter, Dmitry S. Svinkin, David O. Cook, Christoffer Fremling, P. M. Vreeswijk, and L. Whitesides

Subjects
Absolute magnitude, High velocity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, general [gamma-ray burst], Astronomy & Astrophysics, Magnetar, Atomic, Physical Chemistry, 7. Clean energy, 01 natural sciences, Spectral line, Particle and Plasma Physics, individual [supernovae], 0103 physical sciences, magnetars [stars], Astrophysics::Solar and Stellar Astrophysics, Nuclear, 010303 astronomy & astrophysics, Very Energetic, QC, Astrophysics::Galaxy Astrophysics, QB, astro-ph.HE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Molecular, Astronomy and Astrophysics, shock waves, Light curve, Supernova, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Energy source, general [supernovae], Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

Wide-field surveys are discovering a growing number of rare transients whose physical origin is not yet well understood. Here, we present optical and UV data and analysis of iPTF16asu, a luminous, rapidly-evolving, high velocity, stripped-envelope supernova. With a rest-frame rise-time of just 4 days and a peak absolute magnitude of $M_{\rm g}=-20.4$ mag, the light curve of iPTF16asu is faster and more luminous than previous rapid transients. The spectra of iPTF16asu show a featureless, blue continuum near peak that develops into a Type Ic-BL spectrum on the decline. We show that while the late-time light curve could plausibly be powered by $^{56}$Ni decay, the early emission requires a different energy source. Non-detections in the X-ray and radio strongly constrain any associated gamma-ray burst to be low-luminosity. We suggest that the early emission may have been powered by either a rapidly spinning-down magnetar, or by shock breakout in an extended envelope of a very energetic explosion. In either scenario a central engine is required, making iPTF16asu an intriguing transition object between superluminous supernovae, Type Ic-BL supernovae, and low-energy gamma-ray bursts., Comment: ApJ in press; matches published version. Minor changes following referee's comments; conclusions unchanged

Published
2017
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26. GRB 051008: a long, spectrally hard dust-obscured GRB in a Lyman-break galaxy at z ≈ 2.8★

Author

A. Pozanenko, O. A. Burkhonov, Dmitry S. Svinkin, P. Yu. Minaev, M. Ulanov, B. Stecklum, Javier Gorosabel, D. D. Frederiks, A. de Ugarte Postigo, V. V. Biryukov, Vasilij Rumyantsev, A. J. Castro-Tirado, S. Golenetskii, D. A. Kann, P. Ferrero, A. Tsvetkova, A. Volnova, Daniel A. Perley, V. M. Loznikov, and S. Klose

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, Extinction (astronomy), FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, Afterglow, Space and Planetary Science, QD, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Formation rate, Gamma-ray burst, Lyman-break galaxy, QC, Astrophysics::Galaxy Astrophysics, QB
Abstract

We present observations of the dark Gamma-Ray Burst GRB 051008 provided by Swift/BAT, Swift/XRT, Konus-WIND, INTEGRAL/SPI-ACS in the high-energy domain and the Shajn, Swift/UVOT, Tautenburg, NOT, Gemini and Keck I telescopes in the optical and near-infrared bands. The burst was detected only in gamma- and X-rays and neither a prompt optical nor a radio afterglow were detected down to deep limits. We identified the host galaxy of the burst, which is a typical Lyman-break Galaxy (LBG) with R-magnitude of 24.06 +/- 0.10. A redshift of the galaxy of z = 2.77 (-0.20,+0.15) is measured photometrically due to the presence of a clear, strong Lyman-break feature. The host galaxy is a small starburst galaxy with moderate intrinsic extinction (A_V = 0.3 mag) and has a SFR of ~ 60 M_Sun / yr typical for LBGs. It is one of the few cases where a GRB host has been found to be a classical Lyman-break galaxy. Using the redshift we estimate the isotropic-equivalent radiated energy of the burst to be E_iso = (1.15 +/- 0.20) x 10^54 erg. We also provide evidence in favour of the hypothesis that the darkness of GRB 051008 is due to local absorption resulting from a dense circumburst medium., 15 pages, 8 figures Accepted to MNRAS

Published
2014

27. A search for transient events in Konus-Wind data

Author

A. Kozlova, Dmitry S. Svinkin, D. Frederiks, M. Ulanov, A. Lysenko, and A. Tsvetkova

Subjects
Physics, History, Transient (oscillation), Mechanics, Computer Science Applications, Education
Abstract

We present the search for and classification of hard X-ray and soft γ-ray transient events in the archive of continuous (waiting-mode) Konus-Wind observations. We found ∼ 26 000 transient events; among them, ∼ 12 000 are solar flares (∼ 10 times as much as observed in triggered mode); and ∼ 5 000 are gamma-ray bursts (GRBs) or soft gamma repeaters (SGRs) confirmed by other space missions (∼ 2 times as much as detected in triggered mode). The remaining ∼ 9 000 events include Galactic transients, unconfirmed GRBs and possible solar flares. We discuss the application of developed techniques for GRBs accompanied by supernovae, high-energy neutrinos and sources of gravitational waves.

Published
2019

28. Gamma-Ray Emission from the Impulsive Phase of the 2017 September 6 X9.3 Flare

Author

Gregory D. Fleishman, A. Lysenko, D. D. Frederiks, Sergey Anfinogentov, and Dmitry S. Svinkin

Subjects
Physics, 010504 meteorology & atmospheric sciences, Solar flare, Phase (waves), Gamma ray, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, law.invention, Space and Planetary Science, law, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Flare
Published
2019

29. A Search for Gravitationally Lensed Gamma-Ray Bursts in the Data of the Interplanetary Network and Konus-Wind

Author

M. L. Litvak, William V. Boynton, A. B. Sanin, A. Lysenko, Dmitry S. Svinkin, A. A. Kokomov, Kevin Hurley, A. Kozlova, Dmitry Golovin, M. Ulanov, R. Aptekar, T. L. Cline, I. G. Mitrofanov, A. Tsvetkova, K. Harshman, S. Golenetskii, A. von Kienlin, D. D. Frederiks, Arne Rau, C. Fellows, R. D. Starr, and Xiao-Ling Zhang

Subjects
Physics, 010504 meteorology & atmospheric sciences, Space and Planetary Science, 0103 physical sciences, Astronomy, Astronomy and Astrophysics, Interplanetary spaceflight, Gamma-ray burst, 010303 astronomy & astrophysics, 01 natural sciences, 0105 earth and related environmental sciences
Abstract

NASA's 2014 Astrophysics Data Analysis Program [NNX15AE60G]; RFBR [18-02-00062]; Federal Agency for Scientific Organizations "Exploration" [AAAA-A18-118012290370-6]

Published
2019

30. The Interplanetary Network

Author

Xiao-Ling Zhang, M. L. Litvak, J. Cummings, Charles A. Meegan, A. B. Sanin, E. P. Mazets, Dmitry S. Svinkin, Marco Feroci, D. D. Frederiks, Toshio Murakami, David Palmer, K. Harshman, E. Del Monte, Michael S. Briggs, A. von Kienlin, R. L. Aptekar, Yukikatsu Terada, Kazuo Makishima, Valerie Connaughton, Masanori Ohno, Martino Marisaldi, David M. Smith, Y. Hanabata, John O. Goldsten, S. Golenetskii, Neil Gehrels, Yasushi Fukazawa, Tadayuki Takahashi, T. L. Cline, I. G. Mitrofanov, Makoto Tashiro, Kevin Hurley, Wojtek Hajdas, Arne Rau, William V. Boynton, R. Starr, C. Fellows, Scott Barthelmy, Kazutaka Yamaoka, Dmitry Golovin, Hans A. Krimm, and Valentin Pal'shin

Subjects
Physics, Space and Planetary Science, business.industry, General Engineering, Astronomy and Astrophysics, Current (fluid), Aerospace engineering, Interplanetary spaceflight, business
Abstract

We describe the current, 9-spacecraft Interplanetary Network (IPN). The IPN detects about 325 gamma-ray bursts per year, of which about 100 are not localized by any other missions. We give some examples of how the data, which are public, can be utilized.

Published
2013

31. Studies of cosmic gamma-ray bursts and soft gamma repeaters in the Russian-American Konus-Wind experiment

Author

T. L. Cline, Dmitry S. Svinkin, D. D. Frederiks, S. Golenetskii, M. Ulanov, A. E. Tsvetkova, E. P. Mazets, R. L. Aptekar, and F. P. Oleinik

Subjects
Physics, COSMIC cancer database, Physics and Astronomy (miscellaneous), Spacecraft, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Soft gamma repeater, Astronomy, Celestial sphere, Astrophysics, symbols.namesake, Van Allen radiation belt, Physics::Space Physics, symbols, business, Gamma-ray burst, Noise (radio)
Abstract

The studies of the cosmic gamma-ray bursts and soft gamma repeaters that have been performed in the Russian-American Konus-Wind experiment during the last several years have been summarized. The experiment has been continuously performed using the Konus Russian scientific instrument on the Wind American spacecraft since 1994 under the optimal interplanetary space conditions in the absence of noise caused by the Earth’s radiation belts and the shadowing of detectors. Two high-sensitivity detectors have constantly observed the entire celestial sphere and recorded detailed time and spectral characteristics of bursts in a wide range of energies (20 keV–15 MeV). The Konus-Wind data have been widely used in the present-day multiwave studies of gamma-ray bursts.

Published
2012

32. Investigation of Primordial Black Hole Bursts using Interplanetary Network Gamma-ray Bursts

Author

Kazutaka Yamaoka, T. N. Ukwatta, John O. Goldsten, A. S. Kozyrev, R. L. Aptekar, Valerie Connaughton, Kevin Hurley, Hans A. Krimm, Jane H. MacGibbon, Neil Gehrels, William V. Boynton, Valentin Pal'shin, D. D. Frederiks, A. von Kienlin, Dmitry S. Svinkin, N. Ohmori, Marco Feroci, C. Guidorzi, Filippo Frontera, T. L. Cline, J. M. McTiernan, Arne Rau, Masanori Ohno, S. V. Golenetskii, and Xiao-Ling Zhang

Subjects
Physics, Novel technique, High Energy Astrophysical Phenomena (astro-ph.HE), gamma-ray bursts: general, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Evaporation rate, black hole physics, primordial black holes, FOS: Physical sciences, Astronomy and Astrophysics, Primordial black hole, Astrophysics, 01 natural sciences, NO, primordial black holes, black hole physics, gamma-ray bursts: general, Space and Planetary Science, 0103 physical sciences, Gamma-ray burst, Interplanetary spaceflight, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Short duration, Phenomenology (particle physics)
Abstract

The detection of a gamma-ray burst (GRB) in the solar neighborhood would have very important implications for GRB phenomenology. The leading theories for cosmological GRBs would not be able to explain such events. The final bursts of evaporating Primordial Black Holes (PBHs), however, would be a natural explanation for local GRBs. We present a novel technique that can constrain the distance to gamma-ray bursts using detections from widely separated, non-imaging spacecraft. This method can determine the actual distance to the burst if it is local. We applied this method to constrain distances to a sample of 36 short duration GRBs detected by the Interplanetary Network (IPN) that show observational properties that are expected from PBH evaporations. These bursts have minimum possible distances in the 10^13-10^18 cm (7-10^5 AU) range, consistent with the expected PBH energetics and with a possible origin in the solar neighborhood, although none of the bursts can be unambiguously demonstrated to be local. Assuming these bursts are real PBH events, we estimate lower limits on the PBH burst evaporation rate in the solar neighborhood., Accepted to the Astrophysical Journal (9 Figures, 3 Tables)

Published
2015

33. Publisher Correction: Transition from fireball to Poynting-flux-dominated outflow in the three-episode GRB 160625B

Author

Ronan Cunniffe, S. Jeong, P.-H. T. Tam, E. Katkova, E. Klunko, O. Burhonov, E. Mazaeva, Lijing Shao, R. Sanchez-Ramirez, Qing-Wen Tang, Bin-Bin Zhang, R. Inasaridze, Il Han Park, A. Castellon, Anton Biryukov, E. Ivanov, P. Minaev, Aleksander Filip Żarnecki, A. F. Valeev, A. J. Castro-Tirado, S. R. Oates, T. A. Fatkhullin, Zi-Gao Dai, A. K. Zadrożny, D. D. Frederiks, Bing Zhang, A. Volnova, V. Sasyuk, M. D. Caballero-Garcia, A. Kusakin, Vasilij Rumyantsev, Xue-Feng Wu, A. S. Moskvitin, He Gao, R. Opiela, R. Aptekar, Sergey Bondar, A. Perkov, Shashi B. Pandey, Fu-Wen Zhang, Y. D. Hu, Gregory Beskin, J. C. Tello, A. Cwiek, Sergey Karpov, V. V. Sokolov, F. K. Peng, N. Orekhova, Dmitry S. Svinkin, Lech Mankiewicz, Alexei Pozanenko, Martin Jelínek, P. Ferrero, and X.-Y. Wang

Subjects
Physics, Poynting vector, Flux, Astronomy and Astrophysics, Outflow, Astrophysics, Gamma-ray burst
Abstract

In the version of this Letter originally published, the letter i was mistakenly omitted from the surname of the author R. Sanchez-Ramirez. This has now been corrected.

Published
2018

34. Discovery of a new soft gamma repeater: SGR J0418 + 5729

Author

Michael S. Briggs, Christopher R. Gelino, Ersin Gogus, E. P. Mazets, P. Oleynik, Scott Barthelmy, David Palmer, Dmitry S. Svinkin, S. V. Golenetskii, Valerie Connaughton, Colleen A. Wilson-Hodge, D. D. Frederiks, Dawn M. Gelino, Hans A. Krimm, Jay Cummings, Charles A. Meegan, Enrico Ramirez-Ruiz, Paul M. Woods, Mark H. Finger, A. J. van der Horst, Yuki Kaneko, Valentin Pal'shin, Anna L. Watts, Stefanie Wachter, M. van der Klis, Chryssa Kouveliotou, Jonathan Granot, Julie McEnery, Neil Gehrels, A. von Kienlin, Kevin Hurley, M. Ulanov, Asaf Pe'er, R. L. Aptekar, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Swift Gamma-Ray Burst Mission, Astrophysics::High Energy Astrophysical Phenomena, Population, Soft gamma repeater, Perseus Arm, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Magnetar, Galaxy, Spitzer Space Telescope, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, education, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

On 2009 June 5, the Gamma-ray Burst Monitor (GBM) onboard the Fermi Gamma-ray Space Telescope triggered on two short, and relatively dim bursts with spectral properties similar to Soft Gamma Repeater (SGR) bursts. Independent localizations of the bursts by triangulation with the Konus-RF and with the Swift satellite, confirmed their origin from the same, previously unknown, source. The subsequent discovery of X-ray pulsations with the Rossi X-ray Timing Explorer (RXTE), confirmed the magnetar nature of the new source, SGR J0418+5729. We describe here the Fermi/GBM observations, the discovery and the localization of this new SGR, and our infrared and Chandra X-ray observations. We also present a detailed temporal and spectral study of the two GBM bursts. SGR J0418+5729 is the second source discovered in the same region of the sky in the last year, the other one being SGR J0501+4516. Both sources lie in the direction of the galactic anti-center and presumably at the nearby distance of ~2 kpc (assuming they reside in the Perseus arm of our galaxy). The near-threshold GBM detection of bursts from SGR J0418+5729 suggests that there may be more such dim SGRs throughout our galaxy, possibly exceeding the population of bright SGRs. Finally, using sample statistics, we conclude that the implications of the new SGR discovery on the number of observable active magnetars in our galaxy at any given time is, 6 pages, 3 figures, 2 tables; accepted for publication in ApJL on 2010 January 8

Published
2010

35. THE NEEDLE IN THE 100 deg2 HAYSTACK: UNCOVERING AFTERGLOWS OF FERMI GRBs WITH THE PALOMAR TRANSIENT FACTORY

Author

Dmitry S. Svinkin, Mansi M. Kasliwal, Arne Rau, A. de Ugarte Postigo, David Alexander Kann, Umaa Rebbapragada, Leo Singer, Iair Arcavi, Antonino Cucchiara, Brian D. Bue, Yi Cao, Alan J. Weinstein, Shri Kulkarni, Yuji Urata, Rob Fender, G. C. Anupama, Alessandra Corsi, Daniel A. Perley, Peter Nugent, Adam Goldstein, G. E. Anderson, Derek B. Fox, Assaf Horesh, S. Bradley Cenko, Varun Bhalerao, Chryssa Kouveliotou, Tim D. Staley, Neil Gehrels, Joel Johansson, Javier Gorosabel, Christina C. Thöne, Valerie Connaughton, Frank J. Masci, Kuiyun Huang, and Kevin Hurley

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, observational [methods], FOS: Physical sciences, Context (language use), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Atomic, Particle and Plasma Physics, surveys, Nuclear, Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, Astrophysics::Galaxy Astrophysics, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, Molecular, Astronomy and Astrophysics, LIGO, Redshift, Galaxy, Neutron star, Supernova, gravitational waves, Space and Planetary Science, individual [gamma-ray burst], astro-ph.CO, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, general [supernovae], Astronomical and Space Sciences, Fermi Gamma-ray Space Telescope, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM, Physical Chemistry (incl. Structural)
Abstract

The Fermi Gamma-ray Space Telescope has greatly expanded the number and energy window of observations of gamma-ray bursts (GRBs). However, the coarse localizations of tens to a hundred square degrees provided by the Fermi GRB Monitor instrument have posed a formidable obstacle to locating the bursts' host galaxies, measuring their redshifts, and tracking their panchromatic afterglows. We have built a target-of-opportunity mode for the intermediate Palomar Transient Factory in order to perform targeted searches for Fermi afterglows. Here, we present the results of one year of this program: 8 afterglow discoveries out of 35 searches. Two of the bursts with detected afterglows (GRBs 130702A and 140606B) were at low redshift (z=0.145 and 0.384 respectively) and had spectroscopically confirmed broad-line Type Ic supernovae. We present our broadband follow-up including spectroscopy as well as X-ray, UV, optical, millimeter, and radio observations. We study possible selection effects in the context of the total Fermi and Swift GRB samples. We identify one new outlier on the Amati relation. We find that two bursts are consistent with a mildly relativistic shock breaking out from the progenitor star, rather than the ultra-relativistic internal shock mechanism that powers standard cosmological bursts. Finally, in the context of the Zwicky Transient Facility, we discuss how we will continue to expand this effort to find optical counterparts of binary neutron star mergers that may soon be detected by Advanced LIGO and Virgo., 22 pages, 13 figures, 6 tables, 1 online figure set, 3 machine readable tables

Published
2015

36. A search for giant flares from soft gamma-repeaters in nearby galaxies in the Konus-Wind short burst sample

Author

Dmitry S. Svinkin, D. D. Frederiks, S. Golenetskii, R. Aptekar, and Kevin Hurley

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gamma ray, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Magnetar, Energy budget, Galaxy, law.invention, Supernova, Space and Planetary Science, law, Interplanetary spaceflight, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, Flare
Abstract

The knowledge of the rate of soft gamma-ray repeater (SGR) giant flares is important for understanding the giant flare mechanism and the SGR energy budget in the framework of the magnetar model. We estimate the upper limit to the rate using the results of an extensive search for extragalactic soft gamma-repeater giant flares (GFs) among 140 short gamma-ray bursts detected between 1994 and 2010 by Konus-Wind using InterPlanetary Network (IPN) localizations and temporal parameters. We show that Konus-Wind and the IPN are capable of detecting GFs with energies of 2.3x10^46 erg (which is the energy of the GF from SGR 1806-20 assuming a distance of 15 kpc) at distances of up to about 30 Mpc and GFs with energies of, 6 pages, 3 figures. Accepted for publication in MNRAS

Published
2014

37. Konus-Wind and Helicon-Coronas-F Observations of Solar Flares

Author

Yu. E. Charikov, V. Pal'shin, R. L. Aptekar, D. D. Frederiks, M. Ulanov, Z. Ya. Sokolova, S. V. Golenetskii, A. A. Kokomov, A. Tsvetkova, and Dmitry S. Svinkin

Subjects
Physics, Geophysics, Helicon, Astrophysics - Solar and Stellar Astrophysics, Solar flare, Space and Planetary Science, FOS: Physical sciences, Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Results of solar flare observations obtained in the Konus-Wind experiment from November, 1994 to December, 2013 and in the Helicon Coronas-F experiment during its operation from 2001 to 2005, are presented. For the periods indicated Konus-Wind detected in the trigger mode 834 solar flares, and Helicon-Coronas-F detected more than 300 solar flares. A description of the instruments and data processing techniques are given. As an example, the analysis of the spectral evolution of the flares SOL2012-11-08T02:19 (M 1.7) and SOL2002-03-10T01:34 (C5.1) is made with the Konus-Wind data and the flare SOL2003-10-26T06:11 (X1.2) is analyzed in the 2.223 MeV deuterium line with the Helicon-Coronas-F data., Comment: Published version. A list of the Konus-Wind solar flare triggers and figures of their time profiles are available at http://www.ioffe.ru/LEA/Solar/

Published
2014
Full Text
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38. Search for Gravitational Waves Associated with gamma-ray Bursts Detected by the Interplanetary Network

Author

Robert Stone, A. Di Virgilio, A. R. Williamson, R. P. Croce, Namjun Kim, Xing-Jiang Zhu, S. T. Countryman, V. Necula, I. Santiago-Prieto, Hee-Suk Cho, Heinz-Bernd Eggenstein, A. K. Poteomkin, Tania Regimbau, Chiara M. F. Mingarelli, V. V. Frolov, Riccardo Bassiri, J. B. Kanner, Oscar Reula, F. Carbognani, M. M. Hanke, W. Ortega, H. Fehrmann, S. B. Anderson, C. Maglione, Ruslan Vaulin, E. O. Lebigot, E. Katsavounidis, Ludovico Carbone, P. Couvares, Benno Willke, Jean-Luc Atteia, E. Maros, Stanislav Babak, M. Constancio, Duncan A. Brown, Hans A. Krimm, David B. Tanner, F. Jiménez-Forteza, H. Radkins, Christian Gräf, S. Walsh, Alessandra Buonanno, M. R. Smith, N. Letendre, Jeonghoon Ha, S. P. Vyachanin, T. P. Downes, E. Dominguez, F. Brückner, M. Edwards, B. J. J. Slagmolen, D. Fazi, M. Brinkmann, T. Etzel, H. P. Daveloza, H. Dereli, K. Siellez, N. Mangini, P. Thomas, Benjamin William Allen, Karsten Danzmann, C. Aulbert, R. Cavalieri, M. Pedraza, Stefaan Franco, Maria Alessandra Papa, F. Cavalier, G. Vedovato, D. B. Kozak, C. Vorvick, T. Williams, David Coward, L. Bonelli, C. S. Unnikrishnan, S. H. Huttner, Piotr Jaranowski, Florent Robinet, M. Colombini, Roy Williams, C. J. Guido, Jonathan F. Stebbins, A. Basti, R. Bonnand, Collin Capano, D. Hoske, G. Kang, Karoline Wiesner, Sourav Ghosh, Imre Bartos, A. Rocchi, G. Endroczi, Andrew Melatos, M. Lorenzini, A. Masserot, M. J. Lubinski, M. Punturo, Shane L. Larson, Leopoldo Milano, Slawomir Gras, G. Mazzolo, D. S. Rabeling, M. Factourovich, Ryan DeRosa, Valerie Connaughton, B. M. Levine, V. Quetschke, Bangalore Suryanarayana Sathyaprakash, E. Black, J.-P. Coulon, Martin M. Fejer, J. R. Smith, R. Bork, Z. Frei, S. M. Scott, G. Mendell, S. G. Gaonkar, Mark Hannam, C. Buy, Maik Frede, A. Di Lieto, D. B. Kelley, Jordan Camp, Zhihui Du, C. Osthelder, M. Ducrot, D. O. Bridges, Rebecca Fisher, Prayush Kumar, K. E. Gushwa, G. P. Newton, M. Fyffe, Gabriela Gonzalez, D. Feldbaum, F. Cleva, T. B. Edo, V. D. Pal'Shin, M. A. Bizouard, V. Sequino, J. Betzwieser, Antoine Heidmann, C. C. Yancey, Haixing Miao, S. L. Danilishin, I. Kowalska, Rocco Romano, Markus A. Wimmer, John D. Scott, P. Leaci, A. Colla, Rajesh Kumar, Vladimir B. Braginsky, H. Vahlbruch, G. Bogaert, M. Shaltev, Rosa Poggiani, O. Bock, P. J. Sutton, C. C. Wipf, Alex B. Nielsen, J. H. Romie, J.-D. Fournier, Philip F. Hopkins, A. Mytidis, M. Born, K. Mailand, D. L. Kinzel, R. A. Mercer, W. G. Anderson, G. Cella, Peter Fritschel, Denis Martynov, Howard Pan, Aaron Buikema, R. Mittleman, István Rácz, K. L. Dooley, K. Riles, J. Y. Vinet, F. Frasconi, H. Overmier, Giacomo Ciani, A. Mullavey, D. Nolting, G. Manca, M. Weinert, S. J. Chamberlin, M. Vasúth, L. Cunningham, C. R. Ramet, R. Flaminio, S. Farinon, Lisa Barsotti, E. J. King, I. Fiori, M. Agathos, S. R. Morriss, N. A. Robertson, Q. Chu, B. P. Abbott, E. K. Gustafson, D. E. Clark, Kipp Cannon, M. Steinke, A. Staley, Nelson Christensen, L. Pinard, I. M. Pinto, F. Fidecaro, G. M. Guidi, M. J. Cowart, K. Loew, P. Raffai, R. Douglas, F. J. Raab, M. Pickenpack, J. Hanks, A. Pele, Sanichiro Yoshida, E. Lopez, D. Sellers, A. Kumar, Kevin M. Ryan, A. Moggi, H. J. Bulten, Nergis Mavalvala, M. Boer, Matthew Evans, Yukikatsu Terada, R. S. Ottens, Jerome Degallaix, R. J. G. Jonker, J. Meidam, David Jonathan Hofman, D. Hammer, A. von Kienlin, P. J. Lee, S. Vass, R. Vincent-Finley, Jesper Munch, M. Pichot, Federico Ferrini, Enrico Calloni, G. Traylor, Thomas Corbitt, W. Z. Korth, C. A. Costa, R. Inta, S. Klimenko, A. F. Brooks, Fabrice Matichard, Fumiko Kawazoe, Bala R. Iyer, Riccardo Sturani, L. R. Cominsky, C. Palomba, S. Privitera, S. S. Y. Chua, Roman Schnabel, J. E. Brau, A. A. van Veggel, L. Martinelli, B. Moe, Odylio D. Aguiar, I. W. Martin, B. C. Barish, M. S. Shahriar, S. Mitra, Scott Koranda, E. Saracco, C. Tomlinson, László Gondán, W. Kells, G. Vajente, Kevin Hurley, Graham Woan, H. Augustus, S. Ast, C. M. Reed, W. D. Vousden, C. I. Torrie, R. Gustafson, M. P. Thirugnanasambandam, D. Schuette, D. D. Frederiks, Katrin Dahl, Soma Mukherjee, Drew Keppel, C. Belczynski, Alberto Vecchio, M. A. Barton, Stuart Reid, G. Rajalakshmi, L. Matone, C-H. Lee, D. Barker, Efim A. Khazanov, G. Ballardin, Moritz Mehmet, M. Phelps, M. Branchesi, S. Kim, L. Prokhorov, H. R. Paris, Will M. Farr, J. Dickson, D. Hoak, D. Sentenac, C. L. Mueller, Patrick Brady, Peter Kalmus, Sebastien Biscans, S. Kaufer, Sascha Husa, N. Straniero, Rainer Weiss, D. R. Ingram, David Palmer, Nancy Aggarwal, Tobias Westphal, R. Aptekar, J. C. Batch, Jan Harms, A. S. Sengupta, J. Eichholz, Tobias Eberle, Meng Wang, D.B. DeBra, F. Ricci, R. W. P. Drever, W. W. Johnson, John A. Clark, Ben Farr, I. Yakushin, Jacob Scheuer, Viswanath Bavigadda, Christophe Collette, Ho-Gyu Lee, R. J. S. Greenhalgh, Gavin Davies, M. C. Araya, T. Prestegard, Bernard F. Schutz, Kip S. Thorne, T. Chalermsongsak, Alessandro Bertolini, P. Puppo, David Jones, D. Bersanetti, J. V. van Heijningen, K. A. Hodge, S. Sankar, P. G. Murray, D. Passuello, Thanh Vinh Nguyen, David Blair, S. Roddy, Eric Thrane, T. Kaur, L. Sammut, Tristan Briant, F. Clara, S. Recchia, A. Idrisy, Kevin M. McLin, V. Dolique, C. Baune, D. Ugolini, Sung-Po Chao, J. R. Leong, Fabien Kéfélian, J. H. Hough, C. Lazzaro, B. Hughey, E. C. Ferreira, Anton B. Ivanov, J. Bauchrowitz, M. Razzano, R. M. Magee, Patricia Schmidt, V. Brisson, Marilyne Andersen, S. Raja, S. E. Strigin, Marco Cavaglia, M. Lormand, C. Michel, A. Nitz, M. Tonelli, Larry R. Price, Sarah Caudill, R. De Rosa, Hyun Lee, N. Gehrels, T. Vo, J. Slutsky, R. Quitzow-James, R. Day, Jeffery Kline, Xuan Wang, J. S. Areeda, I. Leonor, V. Loriette, J. D. Lough, D. J. Stops, M. Prijatelj, Douglas R. Cook, R. Coyne, K. A. Thorne, C. Bradaschia, Li Ju, Daniel A. Shaddock, Michele Zanolin, T. Dal Canton, T. J. Massinger, R. Passaquieti, M. Huynh, V. Kalogera, J. Hanson, M. Damjanic, P. Oppermann, Marco Aurelio Diaz, Samaya Nissanke, Michele Vallisneri, M. Leonardi, R. Goetz, C. Bogan, E. Macdonald, G. A. Prodi, I. Nardecchia, F. Ohme, Martino Marisaldi, Laura Cadonati, F. Martelli, Carlos Cepeda, Ik Siong Heng, S. Steplewski, Evan Ochsner, Francesco Salemi, A. J. Weinstein, D. Buskulic, S. E. Zuraw, C. Padilla, Robert J. McCarthy, E. Cuoco, M. Kasprzack, Charlotte Bond, Alessandra Corsi, R. DeSalvo, S. A. Usman, G. D. Hammond, O. V. Palashov, F. Piergiovanni, Linqing Wen, C. Messenger, David Tshilumba, Tarun Souradeep, V. P. Mitrofanov, N. A. Gordon, P. J. Veitch, E. A. Huerta, G. M. Keiser, A. M. Sintes, Lee Samuel Finn, H. Tuennermann, Guido Mueller, Gijs Nelemans, Chandra Kant Mishra, M. V. van der Sluys, S. Golenetskii, Jinhyoung Lee, E. D. Hall, A. L. Stuver, S. Grunewald, J. Zweizig, S. E. Gossan, M. Davier, O. Puncken, S. Meshkov, Seog Oh, D. Moraru, A. W. Heptonstall, Vivien Raymond, Peter R. Saulson, B. Sassolas, E. J. Daw, F. Travasso, Michał Bejger, P. Astone, F. Marion, W. Del Pozzo, N. Leroy, Trevor Sidery, H. Heitmann, Rana X. Adhikari, Chad Hanna, R. Abbott, G. Tellez, K. Williams, C. Wilkinson, Andrew Lundgren, B. Machenschalk, F. Donovan, S. Caride, M. Landry, Lindy Blackburn, V. Kondrashov, L. Di Fiore, D. Amariutei, K. Holt, Andreas Freise, Vincenzo Pierro, Jessica McIver, Chunglee Kim, Paul D. Lasky, Gianpietro Cagnoli, S. D'Antonio, Sebastian Steinlechner, L. Kuo, H. Yamamoto, A. Effler, Paolo Addesso, K. D. Giardina, I. Di Palma, A. Cumming, A. Alemic, Y. Minenkov, F. Garufi, R. Burman, David Murphy, D. Lodhia, E. Genin, Joshua Yablon, G. May, M. Barsuglia, S. Chung, A. Conte, V. Sandberg, Ping Koy Lam, G. Debreczeni, Alexander Khalaidovski, F. Nocera, D. J. White, C. Zhao, H. Wittel, Kenneth G. Libbrecht, Chris Pankow, B. Mours, M. E. Normandin, Joshua L. Willis, J. Prasad, F. Vetrano, R. L. Savage, A. S. Bell, S. E. Dwyer, David Keitel, Matthew Pitkin, A. Perreca, G. Gemme, Elizabeth Harstad, A. K. Zadrożny, V. Boschi, E. Schreiber, P. T. Baker, A. Grant, J. Aasi, Jade Powell, V. Mangano, Sunil Susmithan, A. Chiummo, Matthew Heintze, L. Zhang, A. L. Lombardi, B. Lantz, Steven Bloemen, Philip Graff, Jonathan R. Gair, T. Isogai, C. J. Bell, N. A. Lockerbie, M. van Beuzekom, F. Y. Khalili, N. Mazumder, G. McIntyre, Leo Singer, M. Drago, Guenakh Mitselmakher, W. O. Hamilton, T. M. C. Abbott, M. Wade, M. J. Hart, A. M. Gretarsson, L. Naticchioni, Salvatore Vitale, K. Haris, Luca Gammaitoni, David H. Reitze, J. C. Driggers, Tyson Littenberg, Nicolás Wolovick, A. Allocca, Michael Thomas, Walter Winkler, Thomas Dent, Vladimir Dergachev, A. S. Markosyan, Yi-Ming Hu, Suvadeep Bose, J. D. E. Creighton, L. K. Nuttall, K. Mason, Matthew Abernathy, Harald Lück, Z. Márka, G. Valdes, B. C. Stephens, J. P. Zendri, James Whelan, P. Ajith, A. M. Sergeev, M. Granata, A. L. Urban, Huan Yang, Kasem Mossavi, Pierre-François Cohadon, J. K. Blackburn, E. Chassande-Mottin, Badri Krishnan, Sweta Shah, H. Kaufer, Koji Arai, G. Islas, Sheila Rowan, Sanjeev Dhurandhar, M. Cho, M. Pürrer, T. T. Fricke, S. C. McGuire, A. Giazotto, R. M. S. Schofield, A. R. Wade, G. Kuehn, C. M. Mow-Lowry, J. Logue, M. Was, Xin Chen, R. M. Martin, Christopher M. Biwer, S. Frasca, P. Shawhan, I. Ferrante, Ilya Mandel, Todd Adams, H. Vocca, Benjamin J. Owen, J. F. J. van den Brand, B. F. Whiting, Eugeniy E. Mikhailov, Xavier Siemens, Stephen S. Eikenberry, Máté Nagy, I. Maksimovic, J. Marque, P. Charlton, R. L. Ward, G. Hemming, C. Van Den Broeck, M. Tacca, Martin Hendry, K. V. Tokmakov, A. Viceré, D. Simakov, Yi Chen, I. A. Bilenko, C. Affeldt, S. M. Koehlenbeck, Martin Hewitson, S. Doravari, E. Goetz, Junwei Cao, David J. Ottaway, Igor Neri, S. Penn, Gleb Romanov, Stephen Fairhurst, A. C. Lin, G. L. Mansell, P. Fulda, V. Dattilo, Edwin J. Son, Archana Pai, Tjonnie G. F. Li, F. Paoletti, R. Taylor, Stefan Hild, Y. Ma, Eric Howell, S. Leavey, M. Schilman, Adam A. Libson, Jon M. Miller, A. Brillet, G. Billingsley, Matthew West, L. Bosi, Travis Horrom, P. Ruggi, M. Jacobson, M. G. Beker, Dmitry S. Svinkin, T. P. Bodiya, Qi Fang, Robinjeet Singh, Richard O'Shaughnessy, B. Barr, Malik Rakhmanov, M. Yvert, J. Worden, Peter Wessels, J. Tao, Kieran Craig, L. Williams, A. Rüdiger, A. Le Roux, A. Gennai, Curt Cutler, V. Lockett, William Yam, L. Wallace, J. Poeld, A. Królak, R. Frey, Mark S. Meyer, Duncan Meacher, V. Predoi, R. Riesen, Roland Schilling, J. O'Dell, T. Dayanga, P. J. King, B. Shapiro, Virginio Sannibale, David E. McClelland, Xi-Long Fan, A. G. Wiseman, Y. Ji, S. P. Tarabrin, Samuel Deléglise, Benjamin Canuel, J. C. Barayoga, D. C. Coyne, K. Grover, K. Izumi, P. M. Meyers, Paul J. Groot, John Veitch, M. MacInnis, P. Rapagnani, C. C. Arceneaux, J. Karlen, T. Huynh-Dinh, J. S. Kissel, Marc Favata, L. E. Wade, Roger Jones, D. D. Brown, S. S. Premachandra, K. Kawabe, S. M. Aston, Michael W. Coughlin, M. Mageswaran, V. Malvezzi, Timothy MacDonald, Giuseppe Castaldi, E. Rhoades, Carl-Johan Haster, N. Morgado, L. Rolland, Fabrizio Barone, M. Mohan, N. Man, H. J. Jang, K. Haughian, Nam-Gyu Kim, D. Talukder, C. V. Torres, I. W. Harry, T. L. Cline, R. Gouaty, Fausto Acernese, C. Gray, M. Mantovani, Vaibhav Tiwari, S. Omar, H. Zhu, David H. Shoemaker, D. Verkindt, Albert Lazzarini, M. T. Hartman, V. Kringel, S. Goßler, Tomasz Bulik, Richard J. Oram, François Bondu, K. Kokeyama, N. D. Smith-Lefebvre, J. Calderón Bustillo, J. Birch, D. J. Hosken, E. Coccia, K. E. Ramirez, M. E. Zucker, B. A. Weaver, J. G. Rollins, L.-W. Wei, Michael L. Gorodetsky, Simon Stevenson, E. A. Quintero, Joseph Gleason, Hartmut Grote, V. Fafone, Farhan Feroz, T. Denker, G. Losurdo, Kendall Ackley, R. K. Nayak, F. Magaña-Sandoval, Neil J. Cornish, Peter Aufmuth, Jiayi Qin, A. Singer, J. N. Marx, R. Chakraborty, B. E. Aylott, C. Celerier, V. Re, Bruce Gendre, Saps Buchman, J. H. Clayton, Vuk Mandic, Th. S. Bauer, M. Neri, J. A. Giaime, S. G. Crowder, Satya Mohapatra, Yu-Ning Wu, Y. M. Kim, J. R. Sanders, E. Cesarini, F. Mezzani, S. Márka, Kenneth A. Strain, Fabio Marchesoni, P. Hello, Kyungmin Kim, B. O'Reilly, Eric Oelker, Yi Pan, Jong H. Chow, A. Pasqualetti, M. Tse, D. M. Macleod, M. Barbet, M. Meinders, B. L. Swinkels, Timothy A Welborn, Grant David Meadors, W. Katzman, Ettore Majorana, P. Ehrens, J. B. Lewis, Z. Shao, M. Bitossi, G. Bergmann, K. Wette, John J. Oh, Timothy Evans, Rory Smith, C. Adams, D. Sigg, S. W. Ballmer, P. Campsie, Michelle E. Walker, G. Moreno, D. Rosińska, Fan Zhang, D. Nanda Kumar, Ruth A. Anderson, Jessica Steinlechner, M. Heurs, Reed Essick, S. Kandhasamy, B. Sorazu, A. Kutynia, Andrea Chincarini, T. Z. Summerscales, B. Behnke, G. M. Harry, K. Venkateswara, Yuri Levin, (Astro)-Particles Physics, APC - Cosmologie, 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)-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), Université Paris sciences et lettres (PSL), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE 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), Institut de Physique de Rennes (IPR), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire des matériaux avancés (LMA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), 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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), 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)-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 Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-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), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Aasi, J., Abbott, B. P., Abbott, R., Abbott, T., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Affeldt, C., Agathos, M., Aggarwal, N., Aguiar, O. D., Ajith, P., Alemic, A., Allen, B., Allocca, A., Amariutei, D., Andersen, M., Anderson, R. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C., Areeda, J. S., Ast, S., Aston, S. M., Astone, P., Aufmuth, P., Augustus, H., Aulbert, C., Aylott, B. E., Babak, S., Baker, P. T., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barbet, M., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bauchrowitz, J., Bauer, T. h. S., Baune, C., Bavigadda, V., Behnke, B., Bejger, M., Beker, M. G., Belczynski, C., Bell, A. S., Bell, C., Bergmann, G., Bersanetti, D., Bertolini, A., Betzwieser, J., Bilenko, I. A., Billingsley, G., Birch, J., Biscans, S., Bitossi, M., Biwer, C., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bond, C., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Boschi, V., Sukanta, Bose, Bosi, L., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Brooks, A. F., Brown, D. A., Brown, D. D., Brckner, F., Buchman, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Burman, R., Buskulic, D., Buy, C., Cadonati, L., Cagnoli, G., Caldern Bustillo, J., Calloni, Enrico, Camp, J. B., Campsie, P., Cannon, K. C., Canuel, B., Cao, J., Capano, C. D., Carbognani, F., Carbone, L., Caride, S., Castaldi, G., Caudill, S., Cavagli, M., Cavalier, F., Cavalieri, R., Celerier, C., Cella, G., Cepeda, C., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chao, S., Charlton, P., Chassande Mottin, E., Chen, X., Chen, Y., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S. S. Y., Chung, S., Ciani, G., Clara, F., Clark, D. E., Clark, J. A., Clayton, J. H., Cleva, F., Coccia, E., Cohadon, P. F., Colla, A., Collette, C., Colombini, M., Cominsky, L., Constancio, M., Conte, A., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Costa, C. A., Coughlin, M. W., Coulon, J. P., Countryman, S., Couvares, P., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Croce, R. P., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Cutler, C., Dahl, K., Dal Canton, T., Damjanic, M., Danilishin, S. L., Dantonio, S., Danzmann, K., Dattilo, V., Daveloza, H., Davier, M., Davies, G. S., Daw, E. J., Day, R., Dayanga, T., Debra, D., Debreczeni, G., Degallaix, J., Delglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DE ROSA, Rosario, Derosa, R. T., Desalvo, R., Dhurandhar, S., Daz, M., Dickson, J., Di Fiore, L., Di Lieto, A., Di Palma, I., Di Virgilio, A., Dolique, V., Dominguez, E., 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., Eberle, T., Edo, T., Edwards, M., Effler, A., Eggenstein, H. B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Endrczi, G., Essick, R., Etzel, T., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fazi, D., Fehrmann, H., Fejer, M. M., Feldbaum, D., Feroz, F., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finn, L. S., Fiori, I., Fisher, R. P., Flaminio, R., Fournier, J. D., Franco, S., Frasca, S., Frasconi, F., Frede, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gair, J. R., Gammaitoni, L., Gaonkar, S., Garufi, Fabio, Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gleason, J., Goetz, E., Goetz, R., Gondan, L., Gonzlez, G., Gordon, N., Gorodetsky, M. L., Gossan, S., Goler, S., Gouaty, R., Grf, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Groot, P., Grote, H., Grover, K., Grunewald, S., Guidi, G. M., Guido, C. J., Gushwa, K., Gustafson, E. K., Gustafson, R., Ha, J., Hall, E. D., Hamilton, W., Hammer, D., Hammond, G., Hanke, M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hart, M., Hartman, M. T., Haster, C. J., Haughian, K., Heidmann, A., Heintze, M., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Heptonstall, A. W., Heurs, M., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Holt, K., Hopkins, P., Horrom, T., Hoske, D., Hosken, D. J., Hough, J., Howell, E. J., Hu, Y., Huerta, E., Hughey, B., Husa, S., Huttner, S. H., Huynh, M., Huynh Dinh, T., Idrisy, A., Ingram, D. R., Inta, R., Islas, G., Isogai, T., Ivanov, A., Iyer, B. R., Izumi, K., Jacobson, M., Jang, H., Jaranowski, P., Ji, Y., Jimnez Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Haris, K., Kalmus, P., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karlen, J., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, H., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kflian, F., Keiser, G. M., Keitel, D., Kelley, D. B., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, C., Kim, K., Kim, N. G., Kim, N., Kim, S., Kim, Y. M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kline, J., Koehlenbeck, S., Kokeyama, K., Kondrashov, V., Koranda, S., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnan, B., Krlak, A., Kuehn, G., Kumar, A., Nanda Kumar, D., Kumar, P., Kumar, R., Kuo, L., Kutynia, A., Lam, P. K., Landry, M., Lantz, B., Larson, S., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, J., Lee, P. J., Leonardi, M., Leong, J. R., Leonor, I., Le Roux, A., Leroy, N., Letendre, N., Levin, Y., Levine, B., Lewis, J., T. G. F., Li, Libbrecht, K., Libson, A., Lin, A. C., Littenberg, T. B., Lockerbie, N. A., Lockett, V., Lodhia, D., Loew, K., Logue, J., Lombardi, A. L., Lopez, E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J., Lubinski, M. J., Lck, H., Lundgren, A. P., Ma, Y., Macdonald, E. P., Macdonald, T., Machenschalk, B., Macinnis, M., Macleod, D. M., Magaa Sandoval, F., Magee, R., Mageswaran, M., Maglione, C., Mailand, K., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Manca, G. M., Mandel, I., Mandic, V., Mangano, V., Mangini, N. M., Mansell, G., Mantovani, M., Marchesoni, F., Marion, F., Mrka, S., Mrka, Z., Markosyan, A., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Martinelli, L., Martynov, D., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Matichard, F., Matone, L., Mavalvala, N., May, G., Mazumder, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mcguire, S. C., Mcintyre, G., Mciver, J., Mclin, K., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Meinders, M., Melatos, A., Mendell, G., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Mikhailov, E. E., Milano, Leopoldo, Miller, J., Minenkov, Y., Mingarelli, C. M. F., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moe, B., Moggi, A., Mohan, M., Mohapatra, S. R. P., Moraru, D., Moreno, G., Morgado, N., Morriss, S. R., Mossavi, K., Mours, B., Mow Lowry, C. M., Mueller, C. L., Mueller, G., Mukherjee, S., Mullavey, A., Munch, J., Murphy, D., Murray, P. G., Mytidis, A., Nagy, M. F., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nelemans, G., Neri, I., Neri, M., Newton, G., Nguyen, T., Nielsen, A. B., Nissanke, S., Nitz, A. H., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Ochsner, E., Odell, J., Oelker, E., J. J., Oh, S. H., Oh, Ohme, F., Omar, S., Oppermann, P., Oram, R., Oreilly, B., Ortega, W., Oshaughnessy, R., Osthelder, C., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Padilla, C., Pai, A., Palashov, O., Palomba, C., Pan, H., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Paris, H., Pasqualetti, A., Passaquieti, R., Passuello, D., Pedraza, M., Pele, A., Penn, S., Perreca, A., Phelps, M., Pichot, M., Pickenpack, M., Piergiovanni, F., Pierro, V., Pinard, L., Pinto, I. M., Pitkin, M., Poeld, J., Poggiani, R., Poteomkin, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S., Prestegard, T., Price, L. R., Prijatelj, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Prrer, M., Qin, J., Quetschke, V., Quintero, E., Quitzow James, R., Raab, F. J., Rabeling, D. S., Rcz, I., Radkins, H., Raffai, P., Raja, S., Rajalakshmi, G., Rakhmanov, M., Ramet, C., Ramirez, K., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Recchia, S., Reed, C. M., Regimbau, T., Reid, S., Reitze, D. H., Reula, O., Rhoades, E., Ricci, F., Riesen, R., Riles, K., Robertson, N. A., Robinet, F., Rocchi, A., Roddy, S. B., Rolland, L., Rollins, J. G., Romano, R., Romanov, G., Romie, J. H., Rosiska, D., Rowan, S., Rdiger, A., Ruggi, P., Ryan, K., Salemi, F., Sammut, L., Sandberg, V., Sanders, J. R., Sankar, S., Sannibale, V., Santiago Prieto, I., Saracco, E., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Savage, R., Scheuer, J., Schilling, R., Schilman, M., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shah, S., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sidery, T. L., Siellez, K., Siemens, X., Sigg, D., Simakov, D., Singer, A., Singer, L., Singh, R., Sintes, A. M., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, R. J. E., Smith Lefebvre, N. D., Son, E. J., Sorazu, B., Souradeep, T., Staley, A., Stebbins, J., Steinke, M., Steinlechner, J., Steinlechner, S., Stephens, B. C., Steplewski, S., Stevenson, S., Stone, R., Stops, D., Strain, K. A., Straniero, N., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Susmithan, S., Sutton, P. J., Swinkels, B., Tacca, M., Talukder, D., Tanner, D. B., Tao, J., Tarabrin, S. P., Taylor, R., Tellez, G., Thirugnanasambandam, M. P., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Travasso, F., Traylor, G., Tse, M., Tshilumba, D., Tuennermann, H., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Vallisneri, M., van Beuzekom, M., van den Brand, J. F. J., Van Den Broeck, C., van der Sluys, M. V., van Heijningen, J., van Veggel, A. A., Vass, S., Vasth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Vicer, A., Vincent Finley, R., Vinet, J. Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vousden, W. D., Vyachanin, S. P., Wade, A. R., Wade, L., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, M., Wang, X., Ward, R. L., Was, M., Weaver, B., Wei, L. W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Wiesner, K., Wilkinson, C., Williams, K., Williams, L., Williams, R., Williams, T. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M., Winkler, W., Wipf, C. C., Wiseman, A. G., Wittel, H., Woan, G., Wolovick, N., Worden, J., Wu, Y., Yablon, J., Yakushin, I., Yam, W., Yamamoto, H., Yancey, C. C., Yang, H., Yoshida, S., Yvert, M., Zadrony, A., Zanolin, M., Zendri, J. P., Fan, Zhang, Zhang, L., Zhao, C., Zhu, H., Zhu, X. J., Zucker, M. E., Zuraw, S., Zweizig, J., Aptekar, R. L., Atteia, J. L., Cline, T., Connaughton, V., Frederiks, D. D., Golenetskii, S. V., Hurley, K., Krimm, H. A., Marisaldi, M., Palshin, V. D., Palmer, D., Svinkin, D. S., Terada, Y., von Kienlin, A., Pinto, Innocenzo, Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ) -AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique de Rennes ( IPR ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ) -Université de Rennes ( UNIV-RENNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire des matériaux avancés ( LMA ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Annecy de Physique des Particules ( LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), APC - Gravitation ( APC-Gravitation ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, ESPCI ParisTech, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), LIGO, California Institute of Technology, Louisiana State University, Università di Salerno, INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo, University of Florida, LIGO Livingston Observatory, Cardiff University, University of Sannio at Benevento, Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik, Nikhef, LIGO, Massachusetts Institute of Technology, Instituto Nacional de Pesquisas Espaciais, International Centre for Theoretical Sciences, Tata Institute of Fundamental Research, Syracuse University, University of Wisconsin-Milwaukee, Leibniz Universität Hannover, Università di Siena, INFN, Sezione di Pisa, Stanford University, University of Mississippi, California State University Fullerton, INFN, Sezione di Roma, University of Birmingham, Montana State University, European Gravitational Observatory (EGO), LIGO Hanford Observatory, SUPA, University of Glasgow, APC, AstroParticule et Cosmologie, Université Paris Diderot, Observatoire de Paris, Columbia University, Università di Pisa, CAMK-PAN, Astronomical Observatory Warsaw University, Università Degli Studi di Genova, INFN, Sezione di Genova, Faculty of Physics, Lomonosov Moscow State University, LAL, Université Paris-Sud, IN2P3/CNRS, NASA/Goddard Space Flight Center, University of Western Australia, Université Nice-Sophia-Antipolis, CNRS, Observatoire de la Côte d'Azur, Institut de Physique de Rennes, CNRS, Université de Rennes 1, Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université de Savoie, CNRS/IN2P3, Washington State University, Inter-University Centre for Astronomy and Astrophysics, INFN, Sezione di Perugia, Yukawa Institute for Theoretical Physics, Kyoto University, Università Degli Studi di Urbino Carlo Bo, INFN, Sezione di Firenze, University of Oregon, Laboratoire Kastler Brossel, UPMC, Université Pierre et Marie Curie, VU University Amsterdam, University of Maryland, University of Massachusetts Amherst, Laboratoire des Matériaux Avancés (LMA), IN2P3/CNRS, Université de Lyon, Universitat de les Illes Balears, Università di Napoli 'Federico II', Complesso Universitario di Monte S. Angelo, Canadian Institute for Theoretical Astrophysics, University of Toronto, Tsinghua University, University of Michigan, INFN, Sezione di Roma Tor Vergata, National Tsing Hua University, Charles Sturt University, Caltech-CaRT, Pusan National University, Australian National University, Carleton College, Università di Roma Tor Vergata, INFN, Gran Sasso Science Institute, Università di Roma 'La Sapienza', University of Brussels, Sonoma State University, George Washington University, University of Cambridge, University of Minnesota, University of Texas at Brownsville, University of Sheffield, Wigner RCP, RMKI, Argentinian Gravitational Wave Group, Università di Trento, INFN, Gruppo Collegato di Trento, Northwestern University, Montclair State University, Pennsylvania State University, MTA Eötvös University, Lendulet A. R. G., Università di Perugia, Rutherford Appleton Laboratory, HSIC, Embry-Riddle Aeronautical University, Seoul National University, Perimeter Institute for Theoretical Physics, American University, College of William and Mary, University of Adelaide, Raman Research Institute, Korea Institute of Science and Technology Information, Białystok University, University of Southampton, IISER-TVM, CET Campus, Institute of Applied Physics, Hanyang University, NCBJ, IM-PAN, Institute for Plasma Research, University of Melbourne, INFN, Sezione di Padova, Monash University, SUPA, University of Strathclyde, Louisiana Tech University, ESPCI, CNRS, Università di Camerino, Dipartimento di Fisica, Southern University and AandM College, IISER-Kolkata, National Institute for Mathematical Sciences, Hobart and William Smith Colleges, RRCAT, Tata Institute for Fundamental Research, SUPA, University of the West of Scotland, Institute of Astronomy, Indian Institute of Technology, Universidade Estadual Paulista (UNESP), Andrews University, Trinity University, University of Washington, Rochester Institute of Technology, Southeastern Louisiana University, Abilene Christian University, Ioffe Physical-Technical Institute, Université de Toulouse, UPS-OMP, IRAP, CNRS, IRAP, CSPAR, University of Alabama in Huntsville, University of California-Berkeley, Space Sciences Lab, Center for Research and Exploration in Space Science and Technology (CRESST), NASA Goddard Space Flight Center, Universities Space Research Association, INAF-IASF Bologna, Saint Petersburg State Polytechnical University, Los Alamos National Laboratory, Graduate School of Science and Engineering, Saitama University, Max-Planck-Institut für Extraterrestrische Physik, INFN, Sezione di Napoli, The LIGO Scientific Collaboration, and The Virgo Collaboration

Subjects
Gamma ray burst, Astronomy, Interplanetary network, General Physics and Astronomy, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Pacs number: 04.80.Nn, Pacs number: 07.05.Kf, gravitational wave, 010303 astronomy & astrophysics, QC, QB, LIGO Scientific Collaboration, REPEATER, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, ORIGIN, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational waves, GRB, Interferometers, SDG 10 - Reduced Inequalities, 3. Good health, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, GIANT FLARE, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Population, REDSHIFT, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational waves, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Physics and Astronomy (all), Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Binary star, education, SHORT-DURATION, UNUSUAL SUPERNOVA, 010308 nuclear & particles physics, Gravitational wave, 5TH, [ PHYS.ASTR.HE ] Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Redshift, LIGO, Neutron star, [ SDU.ASTR.HE ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma-ray burst, GRB 051103
Abstract

We present the results of a search for gravitational waves associated with 223 gamma-ray bursts (GRBs) detected by the InterPlanetary Network (IPN) in 2005-2010 during LIGO's fifth and sixth science runs and Virgo's first, second and third science runs. The IPN satellites provide accurate times of the bursts and sky localizations that vary significantly from degree scale to hundreds of square degrees. We search for both a well-modeled binary coalescence signal, the favored progenitor model for short GRBs, and for generic, unmodeled gravitational wave bursts. Both searches use the event time and sky localization to improve the gravitational-wave search sensitivity as compared to corresponding all-time, all-sky searches. We find no evidence of a gravitational-wave signal associated with any of the IPN GRBs in the sample, nor do we find evidence for a population of weak gravitational-wave signals associated with the GRBs. For all IPN-detected GRBs, for which a sufficient duration of quality gravitational-wave data is available, we place lower bounds on the distance to the source in accordance with an optimistic assumption of gravitational-wave emission energy of $10^{-2}M_{\odot}c^2$ at 150 Hz, and find a median of 13 Mpc. For the 27 short-hard GRBs we place 90% confidence exclusion distances to two source models: a binary neutron star coalescence, with a median distance of 12Mpc, or the coalescence of a neutron star and black hole, with a median distance of 22 Mpc. Finally, we combine this search with previously published results to provide a population statement for GRB searches in first-generation LIGO and Virgo gravitational-wave detectors, and a resulting examination of prospects for the advanced gravitational-wave detectors., 15 pages, 8 figures, 2 tables; for the science summary, see http://www.ligo.org/science/Publication-IPNS56VSR123grb/index.php

Published
2014

39. A Missing-Link in the Supernova-GRB Connection: The Case of SN 2012ap

Author

R. L. Aptekar, V. Savchenko, Masanori Ohno, Andrew MacFadyen, Dmitry S. Svinkin, John O. Goldsten, Maxim Litvak, D. D. Frederiks, Alak Ray, Kazutaka Yamaoka, Mario Hamuy, C. Fellows, I. G. Mitrofanov, David Palmer, Claes Fransson, Giuliano Pignata, Miriam I. Krauss, Andreas Brunthaler, Valerie Connaughton, Kevin Hurley, Jason A. Dittmann, Naveen Yadav, Makoto Tashiro, Yukikatsu Terada, Toshio Murakami, K. Harshman, S. V. Golenetskii, A. von Kienlin, Alicia M. Soderberg, Dan Milisavljevic, H. A. Krimm, Emily M. Levesque, Laura Chomiuk, William V. Boynton, Michael Bietenholz, Scott Barthelmy, Tadayuki Takahashi, T. L. Cline, Sayan Chakraborti, J. R. Cummings, D. Golovin, H. L. Enos, Yasushi Fukazawa, Arne Rau, Michael S. Briggs, Atish Kamble, Paolo A. Mazzali, X. Zhang, Anton Sanin, Elena Pian, Neil Gehrels, Raffaella Margutti, and Norbert Bartel

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), GRB 980425, supernovae: individual (SN 2012ap), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, shock waves, Astrophysics::Cosmology and Extragalactic Astrophysics, radiation mechanisms: non-thermal, Baryon, Supernova, Space and Planetary Science, techniques: interferometric, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Ejecta, Astrophysics::Galaxy Astrophysics, QB, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

著者人数: 53名, Accepted: 2015-04-05, 資料番号: SA1150078000

Published
2014
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40. GRB 091024 and the nature of ultra-long gamma-ray bursts

Author

Nial R. Tanvir, D. Bersier, Peter Milne, A. V. Filippenko, Dieter H. Hartmann, R. Harrison, A. Gomboc, Iain A. Steele, Edo Berger, Raffaella Margutti, S. B. Cenko, Carole Mundell, P. T. O'Brien, Andrew J. Levan, Zach Cano, N. Clay, Weidong Li, Antonino Cucchiara, Adria C. Updike, S. V. Golenetskii, A. Melandri, G. Grant Williams, Drejc Kopač, Valentin Pal'shin, J. Japelj, Dmitry S. Svinkin, Fabio Virgili, Derek B. Fox, Arne Henden, Ryan Chornock, C. Guidorzi, Shiho Kobayashi, and C. J. Mottram

Subjects
Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, gamma-ray burst: individual GRB 091024A, Population, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 0103 physical sciences, QD, education, 010303 astronomy & astrophysics, QC, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Light curve, Redshift, Afterglow, Space and Planetary Science, Optical emission spectroscopy, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract

We present a broadband study of gamma-ray burst (GRB) 091024A within the context of other ultra-long-duration GRBs. An unusually long burst detected by Konus-Wind, Swift, and Fermi, GRB 091024A has prompt emission episodes covering ~1300 s, accompanied by bright and highly structured optical emission captured by various rapid-response facilities, including the 2-m autonomous robotic Faulkes North and Liverpool Telescopes, KAIT, S-LOTIS, and SRO. We also observed the burst with 8- and 10-m class telescopes and determine the redshift to be z = 1.0924 \pm 0.0004. We find no correlation between the optical and gamma-ray peaks and interpret the optical light curve as being of external origin, caused by the reverse and forward shock of a highly magnetized jet (R_B ~ 100-200). Low-level emission is detected throughout the near-background quiescent period between the first two emission episodes of the Konus-Wind data, suggesting continued central-engine activity; we discuss the implications of this ongoing emission and its impact on the afterglow evolution and predictions. We summarize the varied sample of historical GRBs with exceptionally long durations in gamma-rays (>~ 1000 s) and discuss the likelihood of these events being from a separate population; we suggest ultra-long GRBs represent the tail of the duration distribution of the long GRB population., Updated abstract, acknowledgements. Accepted for publication in ApJ; 21 pages, 10 figures, 6 tables

Published
2013

41. First intermediate flare from SGR 1935+2154

Author

G. L. Israel, A. Kozlova, D. Frederiks, and Dmitry S. Svinkin

Subjects
Physics, History, Spectrometer, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Cosmic ray, Astrophysics, Light curve, Electromagnetic radiation, Spectral line, Computer Science Applications, Education, law.invention, law, Physics::Space Physics, Black-body radiation, Interplanetary spaceflight, Flare
Abstract

The first intermediate flare from newly discovered SGR 1935+2154 was detected and localized by four Interplanetary network (IPN) spacecraft on 2015 April 12. Among the observing instruments, only Konus- Wind gamma-ray burst spectrometer (KW) was able to measure high-resolution light curves and multi-channel energy spectra of the flare. We report on the results of temporal and spectral analyses of the KW data, the flare energetics, a search for Quasi-Periodic Oscillations in the light curve, and, finally, discuss the source distance estimate based on the distribution of double blackbody spectral fit parameters

Published
2016

42. THE INTERPLANETARY NETWORK RESPONSE TO LIGO GW150914

Author

Kevin Hurley, D. Frederiks, S. Golenetskii, Dmitry Golovin, N. Gehrels, Valerie Connaughton, A. B. Sanin, Arne Rau, A. von Kienlin, Dmitry S. Svinkin, M. L. Litvak, T. L. Cline, I. G. Mitrofanov, Xiao-Ling Zhang, R. Aptekar, William V. Boynton, A. S. Kozyrev, and Charles A. Meegan

Subjects
Physics, Gravitational wave, Conjunction (astronomy), Event (relativity), Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics, 01 natural sciences, LIGO, Space and Planetary Science, 0103 physical sciences, Transient (oscillation), 010306 general physics, Gamma-ray burst, Interplanetary spaceflight, 010303 astronomy & astrophysics
Abstract

We have performed a blind search for a gamma-ray transient of arbitrary duration and energy spectrum around the time of the LIGO gravitational-wave event GW150914 with the six-spacecraft interplanetary network (IPN). Four gamma-ray bursts were detected between 30 hr prior to the event and 6.1 hr after it, but none could convincingly be associated with GW150914. No other transients were detected down to limiting 15–150 keV fluences of roughly 5 ×10−8–5 × 10−7 erg cm−2. We discuss the search strategies and temporal coverage of the IPN on the day of the event and compare the spatial coverage to the region where GW150914 originated. We also report the negative result of a targeted search for the Fermi-GBM event reported in conjunction with GW150914.

Published
2016

43. THE SECOND KONUS- WIND CATALOG OF SHORT GAMMA-RAY BURSTS

Author

P. Oleynik, D. D. Frederiks, A. Tsvetkova, V. D. Pal'shin, S. Golenetskii, R. L. Aptekar, Kevin Hurley, M. Ulanov, T. L. Cline, and Dmitry S. Svinkin

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Context (language use), Astrophysics, Spectral component, 01 natural sciences, Spectral line, Space and Planetary Science, 0103 physical sciences, Emission spectrum, Total energy, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, 010303 astronomy & astrophysics, Energy (signal processing)
Abstract

In this catalog, we present the results of a systematic study of 295 short gamma-ray bursts (GRBs) detected by Konus-Wind (KW) from 1994 to 2010. From the temporal and spectral analyses of the sample, we provide the burst durations, the spectral lags, the results of spectral fits with three model functions, the total energy fluences and the peak energy fluxes of the bursts. We discuss evidence found for an additional power-law spectral component and the presence of extended emission in a fraction of the KW short GRBs. Finally, we consider the results obtained in the context of the Type I (merger-origin) / Type II (collapsar-origin) classifications., Comment: Accepted to the Astrophysical Journal Supplement Series (7 Figures, 8 Tables)

Published
2016

44. Constraining the energy budget of GRB 080721

Author

P. T. O'Brien, Cedric Ledoux, K. L. Page, Valentin Pal'shin, Johan P. U. Fynbo, Sung-Chul Yoon, J. P. Osborne, Evert Rol, Dmitry S. Svinkin, R. L. C. Starling, Pall Jakobsson, A. de Ugarte Postigo, Ian D. Howarth, Klaas Wiersema, T. Oosting, C. Guidorzi, Andrew J. Levan, A. J. van der Horst, Nial R. Tanvir, P. A. Curran, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Physics, Jet (fluid), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, 02 engineering and technology, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 021001 nanoscience & nanotechnology, Light curve, Energy budget, Magnetar, 01 natural sciences, Afterglow, Space and Planetary Science, Homogeneous, 0103 physical sciences, gamma-rays: bursts, Total energy, 0210 nano-technology, Gamma-ray burst, 010303 astronomy & astrophysics
Abstract

We follow the bright, highly energetic afterglow of Swift-discovered GRB 080721 at z=2.591 out to 36 days or 3e6 s since the trigger in the optical and X-ray bands. We do not detect a break in the late-time light curve inferring a limit on the opening angle of theta_j >= 7.3 deg and setting tight constraints on the total energy budget of the burst of E_gamma >= 9.9e51 erg within the fireball model. To obey the fireball model closure relations the GRB jet must be expanding into a homogeneous surrounding medium and likely lies behind a significant column of dust. The energy constraint we derive can be used as observational input for models of the progenitors of long gamma-ray bursts: we discuss how such high collimation-corrected energies could be accommodated with certain parameters of the standard massive star core-collapse models. We can, however, most probably rule out a magnetar progenitor for this GRB which would require 100% efficiency to reach the observed total energy., 11 pages, 6 figures (3 colour), accepted for publication in MNRAS following minor revision of Sections 4.2 and 5

Published
2009

45. THE ULTRALUMINOUS GRB 110918A

Author

Xiao-Ling Zhang, R. L. Aptekar, S. V. Golenetskii, K. Harshman, Valentin Pal'shin, A. von Kienlin, Kevin Hurley, D. D. Frederiks, Dmitry S. Svinkin, M. Ulanov, Hans A. Krimm, A. A. Kokomov, Maxim Litvak, I. G. Mitrofanov, R. Starr, E. P. Mazets, C. Pagani, V. Mangano, Michael H. Siegel, William V. Boynton, S. R. Oates, T. L. Cline, B. Sbarufatti, David N. Burrows, A. Tsvetkova, Anton Sanin, D. Golovin, H. L. Enos, P. Oleynik, Arne Rau, J. Goldstein, and C. Fellows

Subjects
Physics, Jet (fluid), Astrophysics::High Energy Astrophysical Phenomena, Horizon, media_common.quotation_subject, Energy flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Universe, Afterglow, Luminosity, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Astrophysics::Galaxy Astrophysics, Energy (signal processing), media_common
Abstract

GRB 110918A is the brightest long GRB detected by Konus-WIND during its 19 years of continuous observations and the most luminous GRB ever observed since the beginning of the cosmological era in 1997. We report on the final IPN 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 moderare $E_{peak}$ 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 $E_{iso}=(2.1\pm0.1)\times10^{54}$ erg. The record-breaking energy flux observed at the peak of the short, bright, hard initial pulse results in an unprecedented isotropic-equivalent luminosity $L_{iso}=(4.7\pm0.2)\times10^{54}$erg s$^{-1}$. A tail of the soft gamma-ray emission was detected with temporal and spectral behavior typical of that predicted by the synchrotron forward-shock model. Swift/XRT and Swift/UVOT 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 ISM-like circumburst environment implied. We conclude that, among 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 deg 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 $z\sim7.5$ for Konus-WIND, and $z\sim12$ for Swift/BAT, which stresses the importance of GRBs as probes of the early Universe., Comment: 22 pages, 20 figures, accepted for publication in ApJ

Published
2013

46. 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

47. GROND coverage of the main peak of Gamma-Ray Burst 130925A

Author

M. Tanga, John F. Graham, Dmitry S. Svinkin, J. Bolmer, J. Elliott, Hoi-Fung Yu, David Alexander Kann, V. Sudilovsky, Xiao-Ling Zhang, Sylvio Klose, A. Nicuesa Guelbenzu, Thomas Krühler, Karla Varela, Andrei M. Beloborodov, Patricia Schady, H. van Eerten, Arne Rau, R. L. Aptekar, P. N. Bhat, A. von Kienlin, Kevin Hurley, M. Ulanov, S. V. Golenetskii, Jochen Greiner, S. Schmidl, and D. D. Frederiks

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Detector, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, law.invention, Telescope, Decay time, Amplitude, Space and Planetary Science, law, Astrophysics::Solar and Stellar Astrophysics, Optical emission spectroscopy, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Astrophysics::Galaxy Astrophysics, Flare
Abstract

Prompt or early optical emission in gamma-ray bursts is notoriously difficult to measure, and observations of the dozen cases show a large variety of properties. Yet, such early emission promises to help us achieve a better understanding of the GRB emission process(es). We performed dedicated observations of the ultra-long duration (T90 about 7000 s) GRB 130925A in the optical/near-infrared with the 7-channel "Gamma-Ray Burst Optical and Near-infrared Detector" (GROND) at the 2.2m MPG/ESO telescope. We detect an optical/NIR flare with an amplitude of nearly 2 mag which is delayed with respect to the keV--MeV prompt emission by about 300--400 s. The decay time of this flare is shorter than the duration of the flare (500 s) or its delay. While we cannot offer a straightforward explanation, we discuss the implications of the flare properties and suggest ways toward understanding it., Comment: 9 pages, 9 figures, accepted for publ. in A&A

48. The Koala: A Fast Blue Optical Transient with Luminous Radio Emission from a Starburst Dwarf Galaxy at z=0.27

Author

D. D. Frederiks, Mansi M. Kasliwal, Kevin B. Burdge, Igor Andreoni, Daniel A. Perley, Matthew J. Graham, Assaf Horesh, Shrinivas R. Kulkarni, Christoffer Fremling, Adam A. Miller, Dmitry S. Svinkin, D. Dong, David L. Shupe, Poonam Chandra, Eric C. Bellm, Anna Y. Q. Ho, Michael W. Coughlin, Kaushik De, V. Zach Golkhou, Maayane T. Soumagnac, George Helou, Russ R. Laher, David Hale, Michael Feeney, Richard Dekany, Ben Rusholme, Michael Porter, Frank J. Masci, and A. Ridnaia

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Spectral line, Luminosity, Stars, Supernova, Space and Planetary Science, 0103 physical sciences, Binary star, Variable star, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QC, 0105 earth and related environmental sciences, QB
Abstract

We present ZTF18abvkwla (the "Koala"), a fast blue optical transient discovered in the Zwicky Transient Facility (ZTF) One-Day Cadence (1DC) Survey. ZTF18abvkwla has a number of features in common with the groundbreaking transient AT2018cow: blue colors at peak ($g-r\approx-0.5$ mag), a short rise time from half-max of under two days, a decay time to half-max of only three days, a high optical luminosity ($M_{g,\mathrm{peak}}\approx-20.6$mag), a hot ($\gtrsim 40,000$K) featureless spectrum at peak light, and a luminous radio counterpart. At late times ($\Delta t>80$d) the radio luminosity of ZTF18abvkwla ($\nu L_\nu \gtrsim 10^{40}$erg/s at 10 GHz, observer-frame) is most similar to that of long-duration gamma-ray bursts (GRBs). The host galaxy is a dwarf starburst galaxy ($M\approx5\times10^{8}M_\odot$, $\mathrm{SFR}\approx7 M_\odot$/yr) that is moderately metal-enriched ($\log\mathrm{[O/H]} \approx 8.5$), similar to the hosts of GRBs and superluminous supernovae. As in AT2018cow, the radio and optical emission in ZTF18abvkwla likely arise from two separate components: the radio from fast-moving ejecta ($\Gamma \beta c >0.38c$) and the optical from shock-interaction with confined dense material ($, Comment: 27 pages, 11 figures. Resubmitted to ApJ on 13 April following comments by referee. Comments welcome!

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