Signatures of Extragalactic Dust in Pre-Swift GRB Afterglows

By D. A. Kann, S. Klose, A. Zeh. 2005

193 citations recorded by the source corpus.

We present the results of a systematic analysis of gamma-ray burst afterglow spectral energy distributions (SEDs) in the optical/near-infrared bands. Our input list includes the entire world sample of afterglows observed in the pre-Swift era by the end of 2004 that have sufficient publicly available data. We apply various dust extinction models to fit the observed SEDs (Milky Way, Large Magellanic Cloud, and Small Magellanic Cloud) and derive the corresponding intrinsic extinction in the GRB host galaxies and the intrinsic spectral slopes of the afterglows. We then use these results to explore the parameter space of the power-law index of the electron distribution function and to derive the absolute magnitudes of the unextinguished afterglows.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3146c1b8996e4ef8f316004ddb08c81ea37e9d07

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In Astronomy and Astrophysics

1. Bing Zhang
2. E. Berger
3. E. Liang
4. Pawan Kumar
5. B. Metzger
6. E. Nakar
7. Xuefeng Wu
8. N. Smith

Citations in the corpus

• THE FIRST POSITIVE DETECTION OF MOLECULAR GAS IN A GRB HOST GALAXY (2009, background): “These characteristics are distinguished from the extinction laws commonly inferred for GRB sightlines which generally have SMC-like or “grey” extinction curves and lack evidence for a 2175 Å bump (e.g., Kann et al. 2006; Butler et al. 2006; Watson et al. 2006; Perley et al. 2008).”
• The 2175 Å Dust Feature in a Gamma-Ray Burst Afterglow at Redshift 2.45 (2008, background): “However, most previous bursts show only a moderate or low reddening (Galama &Wijers 2001; Kann et al. 2006, 2008), contrary to the observed high column densities of heavy elements and strongdepletion of refractory elements (Savaglio&Fall 2004).”
• AFTERGLOW OBSERVATIONS OF FERMI LARGE AREA TELESCOPE GAMMA-RAY BURSTS AND THE EMERGING CLASS OF HYPER-ENERGETIC EVENTS (2010, unknown): “28 We have assumed an SMC-like extinction curve for all events here (Pei 1992; Kann et al. 2006).”
• The SEDs and host galaxies of the dustiest GRB afterglows (2011, methodology): “In other words, an NH,X column even as large as 1022 cm−2 does not necessarily imply a significant visual extinction (see also, e.g., Galama & Wijers 2001; Kann et al. 2006; Schady et al. 2007).”
• A RADIO-SELECTED SAMPLE OF GAMMA-RAY BURST AFTERGLOWS (2011, background): “Optical catalogs have derived mean dust-extinction laws of GRB host galaxies (Kann et al. 2006; Starling et al. 2007), and have lead to claims of clustering of the optical afterglow luminosities (Liang & Zhang 2006; Kann et al. 2006; Nardini et al. 2006).”
• Swift Observations of GRB 070110: An Extraordinary X-Ray Afterglow Powered by the Central Engine (2007, background): “Discrepancies between optical and X-ray extinctions in GRBs environments were first found by Galama &Wijers (2001) and then confirmed by following studies on large GRBs samples (e.g. Kann et al. 2006; Starling et al. 2006; Tagliaferri et al. 2007).”
• The Observer's Guide to the Gamma-Ray Burst-Supernova Connection (2016, background): “different sight-lines through the Milky Way (MW) [20, 21], and extinction local to the event itself [22, 23, 24, 25, 26], in a given filter needs to be modelled and quantified.”
• THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. II. TYPE I GRB VERSUS TYPE II GRB OPTICAL AFTERGLOWS (2008, background): “The revised XRT position (Troja et al. 2006b) lies close to a bright, early type galaxy which was first suggested as a possible host by Kann et al. (2006b), a position put forth in more detail by Bloom et al. (2007a), who find a redshift of z = 0.287 and note the similarity to GRB 050509B and GRB…”
• A POPULATION OF MASSIVE, LUMINOUS GALAXIES HOSTING HEAVILY DUST-OBSCURED GAMMA-RAY BURSTS: IMPLICATIONS FOR THE USE OF GRBs AS TRACERS OF COSMIC STAR FORMATION (2013, methodology): “We select this threshold on the basis of the fact that that very few optically bright GRBs exceed it (Kann et al. 2006, 2010; Schady et al. 2007, 2010)19, yet events of higher AV do represent a significant contribution to the overall GRB rate (∼ 15%; Figure 1).”
• OBSERVATIONS OF THE NAKED-EYE GRB 080319B: IMPLICATIONS OF NATURE'S BRIGHTEST EXPLOSION (2008, background): “The small amount of extinction inferred is also typical (e.g., Kann et al. 2006).”
• Gamma-Ray Bursts in the Swift Era (2007, background): “Among the optically bright GRBs, it is intriguing to discover that there are two sub-classes, namely optically luminous and optically dim categories (Liang & Zhang 2006a; Nardini et al. 2006; Kann et al. 2006).”
• Gamma-ray burst afterglows (2006, background): “Among the optically bright GRBs, it is intriguing to discover that there are two sub-categories, namely optically luminous and optically dim (Liang & Zhang 2006; Nardini et al. 2006; Kann et al. 2006).”
• THE HOST GALAXIES OF SWIFT DARK GAMMA-RAY BURSTS: OBSERVATIONAL CONSTRAINTS ON HIGHLY OBSCURED AND VERY HIGH REDSHIFT GRBs (2009, background): “For most bursts in the full P60 sample, there is little extinction: the median AV is about 0.5, within the range of values typically seen in previous studies of optically well-studied bursts (e.g., Kann et al. 2006).”
• A new method for estimating the bolometric properties of Ibc supernovae (2013, unknown): “…et al. (2010), (3) Sahu et al. (2000), (4) Christensen et al. (2004), (5) Björnsson et al. (2001), (6) Hjorth et al. (2000), (7) Zeh et al. (2004), (8) Kann et al. (2006), (9) Küpcü Yoldaş et al. (2007), (10) Garnavich et al. (2003), (11) Bersier et al. (2003), (12) Price et al. (2003), (13)…”
• GRB 080913 AT REDSHIFT 6.7 (2008, methodology): “Using β = 1.1 we shift the light curve to z = 1 following Kann et al. (2006).”