Prompt Observations of the Early-Time Optical Afterglow of GRB 060607a

Nysewander, M.; Reichart, D.; Crain, J. A.; Foster, Antonina; Haislip, J.; Ivarsen, K.; Lacluyzé, A.; Trotter, A.

doi:10.1088/0004-637x/693/2/1417

Cited by 36 publications

(49 citation statements)

References 44 publications

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“…On the other hand, the color evolution of the afterglow of GRB 061126 (Perley et al 2008c) goes from redder to bluer, similar to the case of the very well sampled early afterglow of GRB 080319B Racusin et al 2008;Woźniak et al 2009). Several other afterglows show no early color changes at all, e.g., those of GRB 060418 and GRB 060607A (Molinari et al 2007;Nysewander et al 2009b) and GRB 061007 (Mundell et al 2007b;Schady et al 2007b).…”

Section: The Luminosity Distribution At Early Times: Diversity and CLmentioning

confidence: 99%

“…The flat, blue SED and the redshift close to z = 1 imply a minimal dRc shift, though, and it would be R C ≈ 14 at 43 s in the rest frame. (Roming et al 2006) or a late afterglow onset (e.g., Molinari et al 2007;Nysewander et al 2009b). In some cases (e.g., GRB 060729, Grupe et al 2007), there are also indications that significant long-term energy injection similar to what may cause the shallow decay/plateau phase of the "canonical" X-ray afterglow Zhang et al 2006;Panaitescu et al 2006a) occurs, although in most cases the plateau phase in X-rays and the following break to a "classical" afterglow decay are not mirrored in the optical (Panaitescu et al 2006b).…”

Section: The Luminosity Distribution At Early Times: Diversity and CLmentioning

confidence: 99%

“…We constructed the light curve and the SED with data from the following sources: Covino et al (2010), Cenko et al (2009b), Fynbo et al (2009), Nysewander et al (2006b, as well as a single data point published here. The light curve is adequately fit with a single power law: m k = 22.66 ± 0.03 mag and α = 1.08 ± 0.007 (for our fits, we use host-subtracted data).…”

Section: B2 Details On the Swift-era Golden Samplementioning

confidence: 99%

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THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

Канн

Klose

Zhang

et al. 2010

ApJ

289

356

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15131514 KANN ET AL.Vol. 720 ABSTRACT We have gathered optical photometry data from the literature on a large sample of Swift-era gamma-ray burst (GRB) afterglows including GRBs up to 2009 September, for a total of 76 GRBs, and present an additional three pre-Swift GRBs not included in an earlier sample. Furthermore, we publish 840 additional new photometry data points on a total of 42 GRB afterglows, including large data sets for GRBs 050319, 050408, 050802, 050820A, 050922C, 060418, 080413A, and 080810. We analyzed the light curves of all GRBs in the sample and derived spectral energy distributions for the sample with the best data quality, allowing us to estimate the host-galaxy extinction. We transformed the afterglow light curves into an extinction-corrected z = 1 system and compared their luminosities with a sample of pre-Swift afterglows. The results of a former study, which showed that GRB afterglows clustered and exhibited a bimodal distribution in luminosity space, are weakened by the larger sample. We found that the luminosity distribution of the two afterglow samples (Swift-era and pre-Swift) is very similar, and that a subsample for which we were not able to estimate the extinction, which is fainter than the main sample, can be explained by assuming a moderate amount of line-of-sight host extinction. We derived bolometric isotropic energies for all GRBs in our sample, and found only a tentative correlation between the prompt energy release and the optical afterglow luminosity at 1 day after the GRB in the z = 1 system. A comparative study of the optical luminosities of GRB afterglows with echelle spectra (which show a high number of foreground absorbing systems) and those without, reveals no indication that the former are statistically significantly more luminous. Furthermore, we propose the existence of an upper ceiling on afterglow luminosities and study the luminosity distribution at early times, which was not accessible before the advent of the Swift satellite. Most GRBs feature afterglows that are dominated by the forward shock from early times on. Finally, we present the first indications of a class of long GRBs, which form a bridge between the typical highluminosity, high-redshift events and nearby low-luminosity events (which are also associated with spectroscopic supernovae) in terms of energetics and observed redshift distribution, indicating a continuous distribution overall.

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Section: The Luminosity Distribution At Early Times: Diversity and CLmentioning

confidence: 99%

Section: The Luminosity Distribution At Early Times: Diversity and CLmentioning

confidence: 99%

Section: B2 Details On the Swift-era Golden Samplementioning

confidence: 99%

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THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

Канн

Klose

Zhang

et al. 2010

ApJ

289

356

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“…Vreeswijk et al (2008a). (1) Huang et al (2007); (2) Kamble et al (2007); (3) Woźniak et al (2005); (4) Cobb & Bailyn (2005); (5) Rosenberg & Garnavich (2005); (6) Flasher et al (2005); (7) Yanagisawa et al (2005); (8) Homewood et al (2005); (9) Mirabal et al (2005); (10) Pandey et al (2006); (11) Macomb et al (2005); (12) Cenko et al (2006b); (13) Durig & Price (2005); (14) Jakobsson et al (2005b); (15) Andreev & Pozanenko (2005); (16) Henych et al (2005); (17) Piranomonte et al (2005); (18) D'Elia et al (2005); (19) Alatalo et al (2006); (20) Curran et al (2007); (21) Stanek et al (2007); (22) Woźniak et al (2006); (23) Molinari et al (2007); (24) Nysewander et al (2006); (25) …”

Section: Xrt Datamentioning

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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“…Some light curves show small, achromatic bumps overlying the smooth power law decay (e.g., A&A 523, A70 (2010) GRB 050502A, Guidorzi et al 2005; GRB 061007, Mundell et al 2007;GRBs 090323 and 090328, McBreen et al 2010), early bumps with chromatic evolution (e.g., GRB 061126, Perley et al 2008a;GRB 071003, Perley et al 2008b), "steps" due to energy injection episodes (e.g., GRB 070125, Updike et al 2008; GRB 071010A, Covino et al 2008;GRB 080913, Greiner et al 2009b, GRB 090926A, Rau et al 2010;Cenko et al 2010;Swenson et al 2010) or powerful late-time rebrightenings of up to several magnitudes (e.g., GRB 050721, Antonelli et al 2006; GRB 060206, Woźniak et al 2006;Monfardini et al 2006;Stanek et al 2007; GRB 070311, Guidorzi et al 2007; GRB 071003, Perley et al 2008b). The early time domain, which can now be routinely accessed by rapid follow-up in the Swift era, has yielded more types of variability, like rising afterglows (e.g., GRB 060418, Molinari et al 2007;GRB 060605, Ferrero et al 2009; GRB 060607A, Nysewander et al 2009, Molinari et al 2007GRB 081008, Yuan et al 2010; see Oates et al 2009;Rykoff et al 2009, for further examples) and short-term variability directly linked to the prompt emission (e.g., GRB 041219A, Vestrand et al 2005;Blake et al 2005; GRB 050820A, Vestrand et al 2006; GRB 080319B, Racusin et al 2008; GRB 080129, Greiner et al 2009a). In all these cases, dense photometric follow-up during the periods of variability was needed to characterize the phenomena involved.…”

Section: Introductionmentioning

confidence: 99%

Photometry and spectroscopy of GRB 060526: a detailed study of the afterglow and host galaxy of az = 3.2 gamma-ray burst

Thöne

Канн²,

Jóhannesson

et al. 2010

A&A

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Aims. With this paper we want to investigate the highly variable afterglow light curve and environment of gamma-ray burst (GRB) 060526 at z = 3.221. Methods. We present one of the largest photometric datasets ever obtained for a GRB afterglow, consisting of multi-color photometric data from the ultraviolet to the near infrared. The data set contains 412 data points in total to which we add additional data from the literature. Furthermore, we present low-resolution high signal-to-noise spectra of the afterglow. The afterglow light curve is modeled with both an analytical model using broken power law fits and with a broad-band numerical model which includes energy injections. The absorption lines detected in the spectra are used to derive column densities using a multi-ion single-component curve-of-growth analysis from which we derive the metallicity of the host of GRB 060526. Results. The temporal behaviour of the afterglow follows a double broken power law with breaks at t = 0.090 ± 0.005 and t = 2.401 ± 0.061 days. It shows deviations from the smooth set of power laws that can be modeled by additional energy injections from the central engine, although some significant microvariability remains. The broadband spectral-energy distribution of the afterglow shows no significant extinction along the line of sight. The metallicity derived from S ii and Fe ii of [S/H] = -0.57 ± 0.25 and [Fe/H] = -1.09 ± 0.24 is relatively high for a galaxy at that redshift but comparable to the metallicity of other GRB hosts at similar redshifts. At the position of the afterglow, no host is detected to F775W(AB) = 28.5 mag with the HST, implying an absolute magnitude of the host M(1500 Å) > -18.3 mag which is fainter than most long-duration hosts, although the GRB may be associated with a faint galaxy at a distance of 11 kpc.

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Prompt Observations of the Early-Time Optical Afterglow of GRB 060607a

Cited by 36 publications

References 44 publications

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

THE AFTERGLOWS OFSWIFT-ERA GAMMA-RAY BURSTS. I. COMPARING PRE-SWIFTANDSWIFT-ERA LONG/SOFT (TYPE II) GRB OPTICAL AFTERGLOWS

The dust extinction curves of gamma-ray burst host galaxies

Photometry and spectroscopy of GRB 060526: a detailed study of the afterglow and host galaxy of az = 3.2 gamma-ray burst

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