The late afterglow and host galaxy of GRB 990712

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dc.contributor.authorHjorth, J
dc.contributor.authorHolland, S
dc.contributor.authorCourbin, F
dc.contributor.authorDar, A
dc.contributor.authorOlsen, LF
dc.contributor.authorScodeggio, M
dc.date.accessioned2025-01-21T01:31:23Z
dc.date.available2025-01-21T01:31:23Z
dc.date.issued2000
dc.description.abstractWe present deep Hubble Space Telescope (HST) imaging, as well as ground-based imaging and spectroscopy, of the optical afterglow associated with the long-duration gamma-ray burst GRB 990712 and its host galaxy. The data were obtained 48-123 days after the burst occurred. The magnitudes of the host (R = 21.9, V = 22.5) and optical afterglow (R = 25.4, V= 25.8, 47.7 days after the burst) favor a scenario in which the optical light follows a pure power-law decay with an index of alpha similar to -1.0. We find no evidence for a contribution from a supernova like SN 1998bw. This suggests that either there are multiple classes of long-duration gamma-ray bursts or that the peak luminosity of the supernova was more than 1.5 mag fainter than SN 1998bw. The HST images and EFOSC2 spectra indicate that the gamma-ray burst was located in a bright, extended feature (possibly a star-forming region) 1.4 kpe from the nucleus of a 0.2L*(B) galaxy at z = 0.434, possibly a Seyfert 2 galaxy. The late-time afterglow and host galaxy of GRB 990712 bear some resemblance to those of GRB 970508.
dc.fuente.origenWOS
dc.identifier.eissn1538-4357
dc.identifier.issn0004-637X
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/97052
dc.identifier.wosidWOS:000087429500008
dc.issue.numero2
dc.language.isoen
dc.pagina.finalL150
dc.pagina.inicioL147
dc.revistaAstrophysical journal
dc.rightsacceso restringido
dc.subjectcosmology : observations
dc.subjectgalaxies : active
dc.subjectgalaxies : distances and redshifts galaxies : starburst
dc.subjectgamma rays : bursts
dc.titleThe late afterglow and host galaxy of GRB 990712
dc.typeartículo
dc.volumen534
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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