GRB 070306: A Highly Extinguished Afterglow

Jaunsen, A. O.; Rol, E.; Watson, Derrick G.; Malesani, D.; Fynbo, J. P. U.; Milvang-Jensen, B.; Hjorth, J.; Vreeswijk, P. M.; Ovaldsen, J. E.; Wiersema, K.; Tanvir, N. R.; Gorosabel, J.; Levan, A. J.; Schirmer, M.; Castro-Tirado, A. J.

doi:10.1086/588602

Cited by 76 publications

(75 citation statements)

References 49 publications

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“…Optical and near-infrared measurements of the afterglows of GRBs 070306, 070802, 080605, 080607, 080805, and 090926B or results thereof are taken from Jaunsen et al (2008), Krühler et al (2008), Perley et al (2011b), Greiner et al (2011), andZafar et al (2011), respectively. GROND observations of the afterglows of GRB 081109 and GRB 100621A are not presented elsewhere and are briefly described in the following.…”

Section: Afterglowsmentioning

confidence: 99%

“…In addition to the public VLT imaging data (FORS R, ISAAC J s HK s ), the host of GRB 070306 was observed with GROND (g r i z JHK s simultaneously), and its SED (Fig. 8) was complemented with published u and I-band data (Jaunsen et al 2008). The host is bright (r = 23.1 mag), mildly red 7 with (R − K) AB ∼ 1.5 mag, and shows evidence of a Balmer/4000 Å break.…”

Section: The Host Of Grb 070306mentioning

confidence: 99%

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The SEDs and host galaxies of the dustiest GRB afterglows

Krühler

Greiner

Schady

et al. 2011

A&A

176

273

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Context. The afterglows and host galaxies of long gamma-ray bursts (GRBs) offer unique opportunities to study star-forming galaxies in the high-z Universe. Until recently, however, the information inferred from GRB follow-up observations was mostly limited to optically bright afterglows, biasing all demographic studies against sight-lines that contain large amounts of dust. Aims. Here we present afterglow and host observations for a sample of bursts that are exemplary of previously missed ones because of high visual extinction (A GRB V 1 mag) along the sight-line. This facilitates an investigation of the properties, geometry, and location of the absorbing dust of these poorly-explored host galaxies, and a comparison to hosts from optically-selected samples. Methods. This work is based on GROND optical/NIR and Swift/XRT X-ray observations of the afterglows, and multi-color imaging for eight GRB hosts. The afterglow and galaxy spectral energy distributions yield detailed insight into physical properties such as the dust and metal content along the GRB sight-line and galaxy-integrated characteristics such as the host's stellar mass, luminosity, color-excess, and star-formation rate. Results. For the eight afterglows considered in this study, we report for the first time the redshift of GRB 081109 (z = 0.9787±0.0005), and the visual extinction towards GRBs 081109 (A GRB V = 3.4 +0.4 −0.3 mag) and 100621A (A GRB V = 3.8 ± 0.2 mag), which are among the largest ever derived for GRB afterglows. Combined with non-extinguished GRBs, there is a strong anti-correlation between the afterglow's metal-to-dust ratio and visual extinction. The hosts of the dustiest afterglows are diverse in their properties, but on average redder ( (R − K) AB ∼ 1.6 mag), more luminous ( L ∼ 0.9 L * ), and massive ( log M * [M ] ∼ 9.8) than the hosts of optically-bright events. Hence, we probe a different galaxy population, suggesting that previous host samples miss most of the massive and metal-rich members. This also indicates that the dust along the sight-line is often related to host properties, and thus probably located in the diffuse ISM or interstellar clouds and not in the immediate GRB environment. Some of the hosts in our sample, are blue, young, or of low stellar mass illustrating that even apparently non-extinguished galaxies possess very dusty sight-lines owing to a patchy dust distribution. Conclusions. The afterglows and host galaxies of the dustiest GRBs provide evidence of a complex dust geometry in star-forming galaxies. In addition, they establish a population of luminous, massive, and correspondingly chemically evolved GRB hosts. This suggests that GRBs trace the global star-formation rate better than studies based on optically selected host samples indicate, and that the previously claimed deficiency of high-mass hosts was at least partially a selection effect.

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Section: Afterglowsmentioning

confidence: 99%

Section: The Host Of Grb 070306mentioning

confidence: 99%

The SEDs and host galaxies of the dustiest GRB afterglows

Krühler

Greiner

Schady

et al. 2011

A&A

176

273

View full text Add to dashboard Cite

show abstract

“…On the other hand, GRB 070306 and GRB 100621A were heavily extinguished GRBs (A V ∼ 5.5 and A V ∼ 3.8 respectively), but both had very blue host galaxies, with R − K colours comparable to the host galaxies of relatively unextinguished GRBs (Jaunsen et al 2008;Krühler et al 2011), indicative of a very clumpy distribution of dust. In a sample of six highly extinguished GRBs, Perley et al (2009) also found evidence for a patchy dust distribution.…”

Section: Variation In Grb Host Extinction Lawsmentioning

confidence: 99%

The dust extinction curves of gamma-ray burst host galaxies

Schady¹,

Dwelly²,

Page³

et al. 2011

A&A

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The composition and amount of interstellar dust within gamma-ray burst (GRB) host galaxies is of key importance when addressing selection effects in the GRB redshift distribution, and when studying the properties of their host galaxies. As well as the implications for GRB research, probing the dust within the high-z hosts of GRBs also contributes to our understanding of the conditions of the interstellar medium and star-formation in the distant Universe. Nevertheless, the physical properties of dust within GRB host galaxies continues to be a highly contended issue. In this paper we explore the mean extinction properties of dust within the host galaxies of a sample of 17 GRBs with total host galaxy visual extinction A V < 1 ( A V = 0.4), covering a redshift range z = 0.7−3.1. We find the average host extinction curve to have an ultraviolet slope comparable to that of the LMC, but with little evidence of a 2175 Å dust extinction feature as observed along Milky Way and LMC sightlines. We cannot at present rule out the presence of a 2175 Å feature, and both the standard SMC and LMC extinction curves also provide good fits to our data. However, we can reject an extinction curve that has a UV slope as flat as the mean Milky Way extinction curve, whilst also having a 2175 Å feature as prominent as seen in the mean Milky Way extinction curve. This is in contrast to the clear detection of a 2175 Å bump and the flatter extinction curves of some more heavily extinguished GRBs (A V > 1), which may be indicative of there being a dependence between dust abundance and the wavelength dependence of dust extinction, as has been previously speculated.

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“…Nevertheless, a few extremely red and luminous GRB hosts have been found ( Levan et al 2006;Berger et al 2007). So far there are few examples of GRB sight lines with very large dust columns (for recent examples see Rol et al 2007;Jaunsen et al 2008;Tanvir et al 2008). The near-, mid-, and far-IR properties of GRB host galaxies have been studied by a number of groups (e.g., Chary et al 2002;Le Floc'h et al 2003Berger et al 2003;Tanvir et al 2004;Priddey et al 2006;Castro Cerón et al 2007).…”

Section: How Biased Are the Qso-dla And Grb-dla Samples?mentioning

confidence: 99%

Reconciling the Metallicity Distributions of Gamma‐Ray Burst, Damped Lyα, and Lyman Break Galaxies atz≈ 3

Fynbo¹,

Prochaska²,

Sommer–Larsen³

et al. 2008

Astrophysical Journal

167

219

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We test the hypothesis that the host galaxies of long-duration gamma-ray bursts (GRBs) as well as quasar-selected damped Ly ( DLA) systems are drawn from the population of UV-selected star-forming, high-z galaxies (generally referred to as Lyman break galaxies). Specifically, we compare the metallicity distributions of the GRB and DLA populations against simple models where these galaxies are drawn randomly from the distribution of star-forming galaxies according to their star formation rate and H i cross section, respectively. We find that it is possible to match both observational distributions assuming very simple and constrained relations between luminosity, metallicity, and H i sizes. The simple model can be tested by observing the luminosity distribution of GRB host galaxies and by measuring the luminosity and impact parameters of DLA-selected galaxies as a function of metallicity. Our results support the expectation that GRB and DLA samples, in contrast with magnitude-limited surveys, provide an almost complete census of z % 3 star-forming galaxies that are not heavily obscured.

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GRB 070306: A Highly Extinguished Afterglow

Cited by 76 publications

References 49 publications

The SEDs and host galaxies of the dustiest GRB afterglows

The SEDs and host galaxies of the dustiest GRB afterglows

The dust extinction curves of gamma-ray burst host galaxies

Reconciling the Metallicity Distributions of Gamma‐Ray Burst, Damped Lyα, and Lyman Break Galaxies atz≈ 3

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