CaltechAUTHORS
Published June 1, 2003 | Version Submitted + Published
Journal Article Open

Discovery of GRB 020405 and Its Late Red Bump

Creators

  • 1. ROR icon Mount Stromlo Observatory
  • 2. ROR icon California Institute of Technology
  • 3. ROR icon National Radio Astronomy Observatory
  • 4. ROR icon Carnegie Observatories
  • 5. ROR icon University of California, Santa Cruz
  • 6. ROR icon UNSW Sydney
  • 7. ROR icon University of Virginia
  • 8. ROR icon New Mexico State University
  • 9. ROR icon Goddard Space Flight Center
  • 10. ROR icon The University of Texas at Austin
  • 11. ROR icon National Research Council
  • 12. ROR icon University of Ferrara
  • 13. ROR icon University of California, Berkeley
  • 14. ROR icon Ioffe Institute
  • 15. ROR icon Space Research Institute
  • 16. ROR icon Tel Aviv University

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.

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.

Attached Files

Published - Price_2003_ApJ_589_838.pdf

Submitted - 0208008.pdf

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0208008.pdf

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Additional details

Identifiers

Eprint ID
98819
Resolver ID
CaltechAUTHORS:20190924-080104925

Related works

Describes
https://arxiv.org/abs/astro-ph/0208008 (URL)

Funding

Australian Research Council
NSF
NASA
NAG5-11451
JPL
958056
NASA
HST-GO-09180.01-A
NASA
NAS5-26555

Dates

Created
2019-09-24
Created from EPrint's datestamp field
Updated
2021-11-16
Created from EPrint's last_modified field

Caltech Custom Metadata

Caltech groups
TAPIR, Space Radiation Laboratory, Division of Geological and Planetary Sciences (GPS)