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Evidence for dust destruction from the early-time colour change of GRB 120119A

Morgan, Adam N. and Perley, Daniel A. and Cenko, S. Bradley and Bloom, Joshua S. and Cucchiara, Antonino and Richards, Joseph W. and Filippenko, Alexei V. and Haislip, Joshua B. and LaCluyze, Aaron and Corsi, Alessandra and Melandri, Andrea and Cobb, Bethany E. and Gomboc, Andreja and Horesh, Assaf and James, Berian and Li, Weidong and Mundell, Carole G. and Reichart, Daniel E. and Steele, Iain (2014) Evidence for dust destruction from the early-time colour change of GRB 120119A. Monthly Notices of the Royal Astronomical Society, 440 (2). pp. 1810-1823. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20140530-145017040

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Abstract

We present broad-band observations and analysis of Swift gamma-ray burst (GRB) 120119A. Our early-time afterglow detections began under 15 s after the burst in the host frame (redshift z = 1.73), and they yield constraints on the burst energetics and local environment. Late-time afterglow observations of the burst show evidence for a moderate column of dust (A_V ≈ 1.1 mag) similar to, but statistically distinct from, dust seen along Small Magellanic Cloud sightlines. Deep late-time observations reveal a dusty, rapidly star-forming host galaxy. Most notably, our early-time observations exhibit a significant red-to-blue colour change in the first ∼200 s after the trigger at levels heretofore unseen in GRB afterglows. This colour change, which is coincident with the final phases of the prompt emission, is a hallmark prediction of the photodestruction of dust in GRB afterglows. We test whether dust-destruction signatures are significantly distinct from other sources of colour change, namely a change in the intrinsic spectral index β. We find that a time-varying power-law spectrum alone cannot adequately describe the observed colour change, and allowing for dust destruction (via a time-varying A_V) significantly improves the fit. While not definitively ruling out other possibilities, this event provides the best support yet for the direct detection of dust destruction in the local environment of a GRB.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1305.1928arXivArticle
http://dx.doi.org/10.1093/mnras/stu344DOIArticle
http://mnras.oxfordjournals.org/content/440/2/1810.abstractPublisherArticle
http://mnras.oxfordjournals.org/content/440/2/1810/suppl/DC1Related ItemData Supplement
ORCID:
AuthorORCID
Perley, Daniel A.0000-0001-8472-1996
Cenko, S. Bradley0000-0003-1673-970X
Filippenko, Alexei V.0000-0003-3460-0103
Corsi, Alessandra0000-0001-8104-3536
Steele, Iain0000-0001-8397-5759
Additional Information:© 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. First published online: March 27, 2014. Accepted 2014 February 19. Received 2014 January 31; in original form 2013 May 8. PAIRITEL is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, a camera loan from the University of Virginia, and continued support of the SAO and UC Berkeley. The PAIRITEL project is further supported by NASA/Swift Guest Investigator grants NNX10AI21G and NNX12AD73G. We utilized observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the NSF (USA), the Science and Technology Facilities Council (UK), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministèrio da Ciência, Tecnologia e Inovação (Brazil), and Ministerio de Ciencia, Tecnología e Innovaciόn Productiva (Argentina). The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia and Jim Katzman Foundation, and the TABASGO Foundation. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We wish to extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. We are grateful to the staffs at the Gemini, Keck, and Lick Observatories for their assistance. This publication has made use of data obtained from the Swift interface of the High-Energy Astrophysics Archive (HEASARC), provided by NASA’s Goddard Space Flight Center.We sincerely thank the Swift team for the rapid public dissemination, calibration, and analysis of the Swift data. We also thank Scott Barthelmy for his invaluable efforts in creating and maintaining the GCN system. We thank the anonymous referee for useful comments on this paper. We also thank Alex Kann for providing helpful suggestions to the text. CGM acknowledges support from the Royal Society. AVF’s group at UC Berkeley has received generous financial assistance from Gary and Cynthia Bengier, the Christopher R. Redlich Fund, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, NSF grant AST-1211916, and NASA/Swift grants NNX10AI21G and NNX12AD73G. AG acknowledges funding from the Slovenian Research Agency and from the Centre of Excellence for Space Science and Technologies SPACE-SI, an operation partly financed by the European Union, the European Regional Development Fund, and the Republic of Slovenia. Support for this work was provided by NASA to DAP through Hubble Fellowship grant HST-HF-51296.01-A awarded by the Space Telescope Science Institute, which is operated for NASA by AURA, Inc., under contract NAS 5-26555. We dedicate this paper to the memory of Weidong Li, who developed the software for KAIT automatic follow-up observations of GRBs; we deeply miss his friendship and collaboration, which were tragically taken away from us much too early.
Funders:
Funding AgencyGrant Number
Harvard University Milton FundUNSPECIFIED
NASANNX10AI21G
NASANNX12AD73G
Science and Technology Facilities Council (UK)UNSPECIFIED
Sun Microsystems, Inc.UNSPECIFIED
Hewlett-Packard CompanyUNSPECIFIED
AutoScope CorporationUNSPECIFIED
Lick ObservatoryUNSPECIFIED
University of CaliforniaUNSPECIFIED
Sylvia and Jim Katzman FoundationUNSPECIFIED
TABASGO FoundationUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Royal SocietyUNSPECIFIED
Gary and Cynthia BengierUNSPECIFIED
Christopher R. Redlich FundUNSPECIFIED
Richard and Rhoda Goldman FundUNSPECIFIED
NSFAST-1211916
Slovenian Research AgencyUNSPECIFIED
Centre of Excellence for Space Science and Technologies SPACE-SIUNSPECIFIED
European UnionUNSPECIFIED
European Regional Development FundUNSPECIFIED
NASA Hubble FellowshipHST-HF-51296.01-A
NASANAS 5-26555
Subject Keywords: gamma-ray burst: individual: GRB 120119A dust, extinction
Record Number:CaltechAUTHORS:20140530-145017040
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140530-145017040
Official Citation:Adam N. Morgan, Daniel A. Perley, S. Bradley Cenko, Joshua S. Bloom, Antonino Cucchiara, Joseph W. Richards, Alexei V. Filippenko, Joshua B. Haislip, Aaron LaCluyze, Alessandra Corsi, Andrea Melandri, Bethany E. Cobb, Andreja Gomboc, Assaf Horesh, Berian James, Weidong Li, Carole G. Mundell, Daniel E. Reichart, and Iain Steele Evidence for dust destruction from the early-time colour change of GRB 120119A MNRAS (May 11, 2014) Vol. 440 1810-1823 first published online March 27, 2014 doi:10.1093/mnras/stu344
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:46018
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:30 May 2014 22:51
Last Modified:27 Oct 2017 22:21

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