Optical Observations of γ-Ray Burst Afterglows

Pian, E.

doi:10.1007/3-540-45863-8_17

Cited by 2 publications

(2 citation statements)

References 182 publications

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“…However, based on the light-curve and the SN hypothesis, the presumed redshift is z ∼1 (see Bloom et al 1999c). Bloom et al (1999c) reported that no galaxy was found at the position of the optical transient down to a 3-σ limiting magnitude a Since the GRB position pierces through the Large Magellanic Cloud (Djorgovski et al 1999d), we have added 0.13 mag extinction to the Galactic extinction quoted in Pian (2001). This assumes an average extinction through the LMC of E(B − V ) = 0.05 (Dutra et al 2001).…”

Section: Grb 980326mentioning

confidence: 99%

“…-Column 2 gives the de-reddened host magnitude as referenced in Pian (2001), Djorgovski et al (2001) and . Column 3 gives the estimated extinction in the direction of the GRB host galaxy Pian (2001). Column 4 gives the estimated probability that the assigned host is a chance superposition and not physically related to the GRB (following §6.6.1).…”

Section: Grb 980326mentioning

confidence: 99%

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Toward an Understanding of the Progenitors of Gamma‐Ray Bursts

Bloom¹

2003

PUBL ASTRON SOC PAC

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The various possibilities for the origin ("progenitors") of gamma-ray bursts (GRBs) manifest in differing observable properties. Through deep spectroscopic and high-resolution imaging observations of some GRB hosts, I demonstrate that well-localized long-duration GRBs are connected with otherwise normal star-forming galaxies at moderate redshifts of order unity. Using high-mass binary stellar population synthesis models, I quantify the expected spatial extent around galaxies of coalescing neutron stars, one of the leading contenders for GRB progenitors. I then test this scenario by examining the offset distribution of GRBs about their apparent hosts making extensive use of ground-based optical data from Keck and Palomar and space-based imaging from the Hubble Space Telescope. The offset distribution appears to be inconsistent with the coalescing neutron star binary hypothesis (and, similarly, blackhole-neutron star coalescences); instead, the distribution is statistically consistent with a population of progenitors that closely traces the ultraviolet light of galaxies. This is naturally explained by bursts which originate from the collapse of massive stars ("collapsars"). This claim is further supported by the unambiguous detections of intermediate-time (approximately three weeks after the bursts) emission "bumps" which appear substantially more red than the afterglows themselves. I claim that these bumps could originate from supernovae that occur at approximately the same time as the associated GRB; if true, GRB 980326 and GRB 011121 provide strong observational evidence connecting cosmological GRBs to high-redshift supernovae and implicate massive stars as the progenitors of at least some long-duration GRBs. Regardless of the true physical origin of these bumps, it appears that all viable alternative models of these bumps (such as dust scattering of the afterglow light) require a substantial amount of circumburst matter that is distributed as a wind-stratified medium; this too, implicates massive stars. Also suggested herein are some future observations which could further solidify or refute the supernova claim. In addition to the observational and modeling work, I also constructed the Jacobs Camera (JCAM), a dual-beam optical camera for the Palomar 200-inch Telescope designed to follow-up rapid GRB localizations. viii

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Section: Grb 980326mentioning

confidence: 99%

Section: Grb 980326mentioning

confidence: 99%

Toward an Understanding of the Progenitors of Gamma‐Ray Bursts

Bloom¹

2003

PUBL ASTRON SOC PAC

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The First Two Host Galaxies of X‐Ray Flashes: XRF 011030 and XRF 020427

Bloom¹,

Fox²,

Dokkum³

et al. 2003

ApJ

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Given the paucity of empirical constraints, the nature of the newly recognized phenomena called X-ray flashes (XRFs) has been an open question. However, with the recent detections of radio and X-ray afterglow it is finally possible to study the large-and small-scale environments of XRFs. We present Chandra, Hubble Space Telescope (HST), and Keck observations of the fields of XRFs 011030 and 020427. Astrometric comparisons of the X-ray transient positions and the HST images reveal the XRFs to be associated with faint blue galaxies. Photometric evidence of these putative hosts suggests that these two XRFs originated from redshifts less than z $ 3:5, and thus cannot be due to GRBs at very high redshifts. In both host-burst offsets and host properties, these XRFs could have been drawn from distributions similar to those measured of gamma-ray bursts (GRBs). We conclude with a discussion of the implications of this XRF-GRB host connection for the possible progenitors of XRFs.

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Optical Observations of γ-Ray Burst Afterglows

Cited by 2 publications

References 182 publications

Toward an Understanding of the Progenitors of Gamma‐Ray Bursts

Toward an Understanding of the Progenitors of Gamma‐Ray Bursts

The First Two Host Galaxies of X‐Ray Flashes: XRF 011030 and XRF 020427

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