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Discovery of GRB 020405 and Its Late Red Bump

Price, P. A. and Kulkarni, S. R. and Berger, E. and Fox, D. W. and Bloom, J. S. and Djorgovski, S. G. and Frail, D. A. and Galama, T. J. and Harrison, F. A. and McCarthy, P. and Reichart, D. E. and Sari, R. and Yost, S. A. and Jerjen, H. and Flint, K. and Phillips, A. and Warren, B. E. and Axelrod, T. S. and Chevalier, R. A. and Holtzman, J. and Kimble, R. A. and Schmidt, B. P. and Wheeler, J. C. and Frontera, F. and Costa, E. and Piro, L. and Hurley, K. and Cline, T. and Guidorzi, C. and Montanari, E. and Mazets, E. and Golenetskii, S. and Mitrofanov, I. and Anfimov, D. and Kozyrev, A. and Litvak, M. and Sanin, A. and Boynton, W. and Fellows, C. and Harshman, K. and Shinohara, C. and Gal-Yam, A. and Ofek, E. and Lipkin, Y. (2003) Discovery of GRB 020405 and Its Late Red Bump. Astrophysical Journal, 589 (2). pp. 838-843. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20190924-080104925

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Abstract

We present the discovery of GRB 020405 made with the Interplanetary Network (IPN). With a duration of 60 s, the burst appears to be a typical long-duration event. We observed the 75 arcmin2 IPN error region with the Mount Stromlo Observatory's 50 inch robotic telescope and discovered a transient source that subsequently decayed and was also associated with a variable radio source. We identify this source as the afterglow of GRB 020405. Subsequent observations by other groups found varying polarized flux and established a redshift of 0.690 to the host galaxy. Motivated by the low redshift, we triggered observations with WFPC2 on board the Hubble Space Telescope (HST). Modeling the early ground-based data with a jet model, we find a clear red excess over the decaying optical light curves that is present between day 10 and day 141 (the last HST epoch). This bump has the spectral and temporal features expected of an underlying supernova (SN). In particular, the red color of the putative SN is similar to that of the SN associated with GRB 011121 at late time. Restricting the sample of GRBs to those with z < 0.7, a total of five bursts, red bumps at late times are found in GRB 970228, GRB 011121, and GRB 020405. It is possible that the simplest idea, namely, that all long-duration γ-ray bursts have underlying SNe with a modest dispersion in their properties (especially peak luminosity), is sufficient to explain the nondetections.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1086/374730DOIArticle
https://arxiv.org/abs/astro-ph/0208008arXivDiscussion Paper
ORCID:
AuthorORCID
Kulkarni, S. R.0000-0001-5390-8563
Berger, E.0000-0002-9392-9681
Fox, D. W.0000-0002-3714-672X
Bloom, J. S.0000-0002-7777-216X
Djorgovski, S. G.0000-0002-0603-3087
Harrison, F. A.0000-0003-2992-8024
Reichart, D. E.0000-0002-5060-3673
Sari, R.0000-0002-1084-3656
Schmidt, B. P.0000-0001-6589-1287
Guidorzi, C.0000-0001-6869-0835
Gal-Yam, A.0000-0002-3653-5598
Ofek, E.0000-0002-6786-8774
Additional Information:© 2003 The American Astronomical Society. Received 2002 July 31; accepted 2003 February 7. B. P. S. and P. A. P. thank the ARC for supporting Australian GRB research. GRB research at Caltech (S. R. K., S. G. D., F. A. H., R. S.) is supported by grants from NSF and NASA.K. H. is grateful for Ulysses and IPN support under JPL contract 958056 and NASA grant NAG5-11451. Support for Proposal HST-GO-09180.01-A was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. We thank M. Pettini, N. Reddy, and C. Steidel for undertaking observations at Keck under the auspices of the Caltech ToO program. Finally, we thank the staff of MSO, SSO, Wise, LCO, Keck, and the STScI for their assistance.
Group:TAPIR, Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
Australian Research CouncilUNSPECIFIED
NSFUNSPECIFIED
NASANAG5-11451
JPL958056
NASAHST-GO-09180.01-A
NASANAS5-26555
Subject Keywords:gamma rays: bursts
Issue or Number:2
Record Number:CaltechAUTHORS:20190924-080104925
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20190924-080104925
Official Citation:P. A. Price et al 2003 ApJ 589 838
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:98819
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:24 Sep 2019 16:12
Last Modified:06 Nov 2020 19:38

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