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The Interstellar Medium in the Environment of the Supernova-less Long-duration GRB 111005A

Leśniewska, Aleksandra and Michałowski, M. J. and Kamphuis, P. and Dziadura, K. and Baes, M. and Castro Cerón, J. M. and Gentile, G. and Hjorth, J. and Hunt, L. K. and Jespersen, C. K. and Koprowski, M. P. and Le Floc'h, E. and Miraghaei, H. and Nicuesa Guelbenzu, A. and Oszkiewicz, D. and Palazzi, E. and Polińska, M. and Rasmussen, J. and Schady, P. and Watson, D. (2022) The Interstellar Medium in the Environment of the Supernova-less Long-duration GRB 111005A. Astrophysical Journal Supplement Series, 259 (2). Art. No. 67. ISSN 0067-0049. doi:10.3847/1538-4365/ac5022.

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Long (>2 s) gamma-ray bursts (GRBs) are associated with explosions of massive stars, although in three instances, supernovae (SNe) have not been detected, despite deep observations. With new H i line and archival optical integral-field spectroscopy data, we characterize the interstellar medium (ISM) of the host galaxy of one of these events, GRB 111005A, in order to shed light on the unclear nature of these peculiar objects. We found that the atomic gas, radio continuum, and rotational patterns are in general very smooth throughout the galaxy, which does not indicate a recent gas inflow or outflow. There is also no gas concentration around the GRB position. The ISM in this galaxy differs from that in hosts of other GRBs and SNe, which may suggest that the progenitor of GRB 111005A was not an explosion of a very massive star (e.g., a compact object merger). However, there are subtle irregularities of the GRB 111005A host (most at a 2σ level), which may point to a weak gas inflow or interaction. Because in the SE part of the host there is 15% more atomic gas and half the molecular gas than in the NW part, the molecular gas fraction is low. In the SE part there is also a region with a very high Hα equivalent width. There is more continuum 1.4 GHz emission to the SE and an S-shaped warp in the UV. Finally, there is also a low-metallicity region 3.″5 (1 kpc) from the GRB position. Two galaxies within 300 kpc or a past merger can be responsible for these irregularities.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Leśniewska, Aleksandra0000-0001-8723-3533
Michałowski, M. J.0000-0001-9033-4140
Kamphuis, P.0000-0002-5425-6074
Dziadura, K.0000-0001-7562-9661
Baes, M.0000-0002-3930-2757
Hjorth, J.0000-0002-4571-2306
Hunt, L. K.0000-0001-9162-2371
Jespersen, C. K.0000-0002-8896-6496
Koprowski, M. P.0000-0001-5785-1154
Miraghaei, H.0000-0003-1829-9402
Nicuesa Guelbenzu, A.0000-0002-6856-9813
Oszkiewicz, D.0000-0002-5356-6433
Palazzi, E.0000-0002-8691-7666
Polińska, M.0000-0003-4473-3372
Schady, P.0000-0002-1214-770X
Watson, D.0000-0002-4465-8264
Additional Information:© 2022. The Author(s). Published by the American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2020 March 27; revised 2022 January 25; accepted 2022 January 28; published 2022 April 13. We wish to thank the referee for the detailed comments, which helped us to clarify our conclusions. A.L. and M.J.M. acknowledge the support of the National Science Centre, Poland through the SONATA BIS grant 2018/30/E/ST9/00208. This research was funded in whole or in part by National Science Centre, Poland (grant Nos. 2021/41/N/ST9/02662 and 2020/39/D/ST9/03078). For the purpose of open access, the author has applied a CC-BY public copyright licence to any author accepted manuscript (AAM) version arising from this submission. M.J.M. acknowledges the Fulbright Senior Award from the Polish-U.S. Fulbright Commission. P.K. is supported by the BMBF project 05A17PC2 for D-MeerKAT. J.H. was supported by a VILLUM FONDEN Investigator grant (project number 16599). L.K.H. acknowledges funding from the INAF PRIN-SKA program The Cosmic Dawn Center is funded by the DNRF. M.P.K. acknowledges support from the First TEAM grant of the Foundation for Polish Science No. POIR.04.04.00-00-5D21/18-00. This article has been supported by the Polish National Agency for Academic Exchange under grant No. PPI/APM/2018/1/00036/U/001. We thank the staff of the GMRT who have made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. This research has made use of SAOImage DS9, developed by Smithsonian Astrophysical Observatory (Joye & Mandel 2003); the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; and NASA's Astrophysics Data System Bibliographic Services. We acknowledge the use of Starlink software which is currently supported by the East Asian Observatory. We acknowledge the usage of the HyperLeda database (
Funding AgencyGrant Number
National Science Centre (Poland)2018/30/E/ST9/00208
National Science Centre (Poland)2021/41/N/ST9/02662
National Science Centre (Poland)2020/39/D/ST9/03078
Polish-U.S. Fulbright CommissionUNSPECIFIED
Bundesministerium für Bildung und Forschung (BMBF)05A17PC2
Villum Foundation16599
Istituto Nazionale di Astrofisica (INAF)
Danish National Research FoundationUNSPECIFIED
Foundation for Polish SciencePOIR.04.04.00-00-5D21/18-00
Polish National Agency for Academic ExchangePPI/APM/2018/1/00036/U/001
Subject Keywords:Supernovae; Interstellar atomic gas; H I line emission; Spiral galaxies; Galaxy kinematics; Star formation; Gamma-ray bursts
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Supernovae (1668); Interstellar atomic gas (833); H I line emission (690); Spiral galaxies (1560); Galaxy kinematics (602); Star formation (1569); Gamma-ray bursts (629)
Record Number:CaltechAUTHORS:20220414-26611000
Persistent URL:
Official Citation:Aleksandra Leśniewska et al 2022 ApJS 259 67
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:114312
Deposited By: George Porter
Deposited On:18 Apr 2022 22:39
Last Modified:18 Apr 2022 22:39

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