Interplanetary Network Localizations of Konus Short Gamma-Ray Bursts

INTERPLANETARY NETWORK LOCALIZATIONS OF KONUS SHORT GAMMA-RAY BURSTS The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Pal’shin, V. D., K. Hurley, D. S. Svinkin, R. L. Aptekar, S. V. Golenetskii, D. D. Frederiks, E. P. Mazets, et al. “INTERPLANETARY NETWORK LOCALIZATIONS OF KONUS SHORT GAMMA-RAY BURSTS.” The Astrophysical Journal Supplement Series 207, no. 2 (August 1, 2013): 38. © The American Astronomical Society As Published http://dx.doi.org/10.1088/0067-0049/207/2/38 Publisher IOP Publishing Version Final published version Citable link http://hdl.handle.net/1721.1/93742 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astrophysical Journal Supplement Series, 207:38 (14pp), 2013 August doi:10.1088/0067-0049/207/2/38 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INTERPLANETARY NETWORK LOCALIZATIONS OF KONUS SHORT GAMMA-RAY BURSTS V. D. Pal’shin1, K. Hurley2,D.S.Svinkin1, R. L. Aptekar1, S. V. Golenetskii1, D. D. Frederiks1, E. P. Mazets 1,31, P. P. Oleynik1, M. V. Ulanov1,T.Cline3,32, I. G. Mitrofanov4, D. V. Golovin4, A. S. Kozyrev4, M. L. Litvak4, A. B. Sanin4, W. Boynton5, C. Fellows5,K.Harshman5, J. Trombka3, T. McClanahan3, R. Starr3, J. Goldsten6, R. Gold6,A.Rau7, A. von Kienlin7, V. Savchenko8,D.M.Smith9, W. Hajdas10, S. D. Barthelmy3, J. Cummings11,12, N. Gehrels3,H.Krimm11,13, D. Palmer14, K. Yamaoka15, M. Ohno16, Y. Fukazawa16, Y. Hanabata16, T. Takahashi15, M. Tashiro17, Y. Terada17, T. Murakami18, K. Makishima19, M. S. Briggs20, R. M. Kippen14, C. Kouveliotou21, C. Meegan22, G. Fishman21, V. Connaughton20,M.Boer¨ 23, C. Guidorzi24, F. Frontera24,25, E. Montanari24,26,F.Rossi24, M. Feroci27, L. Amati25, L. Nicastro25, M. Orlandini25,E.DelMonte27, E. Costa27, I. Donnarumma27, Y. Evangelista27, I. Lapshov27, F. Lazzarotto27, L. Pacciani27, M. Rapisarda27, P. Soffitta27, G. Di Cocco25,F.Fuschino25, M. Galli28, C. Labanti25, M. Marisaldi25, J.-L. Atteia29, R. Vanderspek30, and G. Ricker30 1 Ioffe Physical Technical Institute, St. Petersburg, 194021, Russia; [email protected] 2 Space Sciences Laboratory, University of California, 7 Gauss Way, Berkeley, CA 94720-7450, USA 3 NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 4 Space Research Institute, 84/32, Profsoyuznaya, Moscow 117997, Russia 5 Department of Planetary Sciences, University of Arizona, Tucson, AZ 85721, USA 6 Applied Physics Laboratory, Johns Hopkins University, Laurel, MD 20723, USA 7 Max-Planck-Institut fur¨ extraterrestrische Physik, Giessenbachstrasse, Postfach 1312, D-85748 Garching, Germany 8 Fran¸cois Arago Centre, APC, Universite´ Paris Diderot, CNRS/IN2P3, CEA/Irfu, Observatoire de Paris, Sorbonne Paris Cite,´ 10 rue Alice Domon et Leonie´ Duquet, F-75205 Paris Cedex 13, France 9 Physics Department and Santa Cruz Institute for Particle Physics, University of California, Santa Cruz, Santa Cruz, CA 95064, USA 10 Paul Scherrer Institute, CH-5232 Villigen PSI, Switzerland 11 UMBC/CRESST/NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 12 UMBC Physics Department, 1000 Hilltop Circle, Baltimore, MD 21250, USA 13 Universities Space Research Association, 10211 Wincopin Circle, Suite 500, Columbia, MD 20144, USA 14 Los Alamos National Laboratory, Los Alamos, NM 87545, USA 15 Institute of Space and Astronautical Science (ISAS/JAXA), 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5210, Japan 16 Department of Physics, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526, Japan 17 Department of Physics, Saitama University, 255 Shimo-Okubo, Sakura-ku, Saitama-shi, Saitama 338-8570, Japan 18 Department of Physics, Kanazawa University, Kadoma-cho, Kanazawa, Ishikawa 920-1192, Japan 19 Department of Physics, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan 20 CSPAR and Physics Department, University of Alabama in Huntsville, Huntsville, AL 35899, USA 21 Space Science Office, VP62, NASA Marshall Space Flight Center, Huntsville, AL 35812, USA 22 Universities Space Research Association, 320 Sparkman drive, Huntsville, AL 35805, USA 23 Observatoire de Haute Provence (CNRS), F-04870 Saint Michel l’Observatoire, France 24 Physics Department, University of Ferrara, Via Saragat 1, I-44100 Ferrara, Italy 25 INAF/Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, I-40129 Bologna, Italy 26 Istituto IS Calvi, I-41034 Finale Emilia (MO), Italy 27 INAF–Istituto di Astrofisica Spaziale e Fisica Cosmica, via Fosso del Cavaliere, I-00133 Rome, Italy 28 ENEA-Bologna, Via Martiri Montesole 4, I-40129 Bologna, Italy 29 Universite´ de Toulouse; UPS-OMP; CNRS; IRAP; 14 Avenue Edouard Belin, F-31400 Toulouse, France 30 Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 70 Vassar Street, Cambridge, MA 02139, USA Received 2013 June 25; accepted 2013 July 11; published 2013 August 2 ABSTRACT Between the launch of the Global Geospace Science Wind spacecraft in 1994 November and the end of 2010, the Konus-Wind experiment detected 296 short-duration gamma-ray bursts (including 23 bursts which can be classified as short bursts with extended emission). During this period, the Interplanetary Network (IPN) consisted of up to 11 spacecraft, and using triangulation, the localizations of 271 bursts were obtained. We present the most comprehensive IPN localization data on these events. The short burst detection rate, ∼18 yr−1, exceeds that of many individual experiments. Key words: catalogs – gamma-ray burst: general – techniques: miscellaneous Online-only material: color figures, machine-readable tables 1. INTRODUCTION as short-duration GRBs or short bursts with extended emission (EE). The classification was made based on the duration distri- Between 1994 November and 2010 December, the Konus bution of an unbiased sample of 1168 Konus-Wind GRBs. The gamma-ray spectrometer on board the Global Geospace Sci- instrument trigger criteria cause undersampling of faint short ence Wind spacecraft detected 1989 cosmic gamma-ray bursts bursts relative to faint long bursts, so this subsample of fairly (GRBs) in the triggered mode, 296 of which were classified bright (in terms of peak count rate in Konus-Wind’s trigger energy band) bursts has been chosen for the purpose of classifi- 31 Deceased. cation. Taking into account other characteristics of these short- 32 Emeritus. duration bursts such as hardness ratio and spectral lag shows that 1 The Astrophysical Journal Supplement Series, 207:38 (14pp), 2013 August Pal’shin et al. about 16% of them can be in fact Type II (collapsar-origin), or at spacecraft (s/c). In a companion paper, we present the durations, least their classification as Type I (merger-origin) is questionable energy spectra, peak fluxes, and fluences of these bursts. (see Zhang et al. 2009 for more information on the Type I/II classification scheme). Nevertheless we consider here all 296 2. OBSERVATIONS Konus-Wind short-duration and possible short-duration with EE For each Konus short GRB, a search was initiated in the bursts (hereafter we refer to them simply as Konus short bursts). data of the IPN spacecraft. For the near-Earth spacecraft and Full details of the Konus-Wind GRB classification are given in INTEGRAL, the search window was centered on the Konus- D. S. Svinkin et al. (2013, in preparation). Wind trigger time, and its duration was somewhat greater than Every short burst detected by Konus was searched for the Wind distance from Earth. For the spacecraft at interplanetary in the data of the spacecraft comprising the Interplanetary ∼ distances, the search window was twice the light-travel time to Network (IPN). We found that 271 ( 92%) of the Konus- the spacecraft if the event arrival direction was unknown, which Wind short GRBs were observed by at least one other IPN was the case for most events. If the arrival direction was known, spacecraft, enabling their localizations to be constrained by even coarsely, the search window was defined by calculating triangulation. the expected arrival time at the spacecraft, and searching in a The IPN contained between 3 and 11 spacecraft during this window around it. period. They were, in addition to Konus-Wind, Ulysses (the The mission timelines and the number of Konus-Wind short solar X-ray/cosmic gamma-ray burst instrument, GRB), in he- GRBs observed by each mission/instrument are shown in liocentric orbit at distances between 670 and 3180 lt-s from Figure 1. In this study, the largest number of bursts detected by an Earth (Hurley et al. 1992); the Near-Earth Asteroid Rendezvous IPN instrument, after Konus, was 139, detected by INTEGRAL (NEAR) mission (the remote sensing X-ray/Gamma-Ray Spec- (SPI-ACS). trometer, XGRS; Trombka et al. 1999), at distances up to Table 1 lists the 271 Konus-Wind short GRBs observed by 1300 lt-s from Earth; Mars Odyssey (the Gamma-Ray Spectrom- the IPN. The first column gives the burst designation, “GR- eter (GRS) that includes two detectors with GRB detection ca- BYYYYMMDD_Tsssss”, where YYYYMMDD is the burst pabilities, the gamma sensor head (GSH), and the High Energy date, and sssss is the Konus-Wind trigger time (s UT) trun- Neutron Detector (HEND); Boynton et al. 2004; Hurley et al. cated to integer seconds (Note that, due to Wind’s large distance 2006), launched in 2001 April and in orbit around Mars starting from Earth, this trigger time can differ by up to 6.1 s from the in 2001 October, up to 1250 lt-s from Earth (Saunders et al. Earth-crossing time; see below). The next two columns give 2004); the Mercury Surface, Space Environment, Geochemistry, the burst date and Konus-Wind trigger time in the standard date and Ranging (MESSENGER) mission (the Gamma-Ray and and time formats.

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