RAPTOR Observations of the Early Optical Afterglow from GRB 050319

Woźniak, P. R.; Vestrand, W. T.; Wren, J.; White, Robert R.; Evans, S. M.; Casperson, D.

doi:10.1086/431975

Cited by 41 publications

(59 citation statements)

References 23 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…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

View full text Add to dashboard Cite

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.

show abstract

Section: Xrt Datamentioning

confidence: 99%

The dust extinction curves of gamma-ray burst host galaxies

Schady¹,

Dwelly²,

Page³

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…A particular cautionary tale is GRB 050319. The original analysis of early optical data showed a shallow light curve break, when using the BAT trigger time Woźniak et al (2005). Further analysis of BAT slew data demonstrated that the main GRB event was in fact 137 s prior to the original BAT trigger time (Chincarini et al 2005).…”

Section: Estimating γmentioning

confidence: 99%

“…However, the cessation of early energy injection would be expected to produce an achromatic light curve break, which is not generally observed (e.g., Panaitescu et al 2006;Fan & Piran 2006), although interpretation of X-ray breaks is not always straightforward (Racusin et al 2009). Observations of individual bursts (e.g., Akerlof et al 1999;Smith et al 2003;Rykoff et al 2004Rykoff et al , 2006bWoźniak et al 2005;Quimby et al 2006;Vestrand et al 2006;Romano et al 2006;Molinari et al 2007;Schady et al 2007) have been interpreted in the context of various models. It is clear that for most early afterglows the "closure relationships" (e.g., Granot & Sari 2002), which compare the spectral index of the synchrotron emission to the temporal decay Vol.…”

Section: Introductionmentioning

confidence: 99%

LOOKING INTO THE FIREBALL: ROTSE-III ANDSWIFTOBSERVATIONS OF EARLY GAMMA-RAY BURST AFTERGLOWS

Rykoff

Aharonian

Akerlof

et al. 2009

ApJ

Self Cite

104

122

View full text Add to dashboard Cite

We report on a complete set of early optical afterglows of gamma-ray bursts (GRBs) obtained with the Robotic Optical Transient Search Experiment (ROTSE-III) telescope network from 2005 March through 2007 June. This set is comprised of 12 afterglows with early optical and Swift/X-Ray Telescope observations, with a median ROTSE-III response time of 45 s after the start of γ -ray emission (8 s after the GCN notice time). These afterglows span 4 orders of magnitude in optical luminosity, and the contemporaneous X-ray detections allow multi-wavelength spectral analysis. Excluding X-ray flares, the broadband synchrotron spectra show that the optical and X-ray emission originate in a common region, consistent with predictions of the external forward shock in the fireball model. However, the fireball model is inadequate to predict the temporal decay indices of the early afterglows, even after accounting for possible long-duration continuous energy injection. We find that the optical afterglow is a clean tracer of the forward shock, and we use the peak time of the forward shock to estimate the initial bulk Lorentz factor of the GRB outflow, and find 100 Γ 0 1000, consistent with expectations.

show abstract

“…Data for GRB 021004 are from Fox et al (2003a) and GCNCs 1564GCNCs , 1566GCNCs , 1570GCNCs , 1573GCNCs , 1576GCNCs , 1577GCNCs , 1578GCNCs , 1580GCNCs , 1581GCNCs , 1582GCNCs , 1584GCNCs , 1587GCNCs , 1591GCNCs , 1594GCNCs , 1606GCNCs , 1614GCNCs , 1615GCNCs , 1628. Data for GRB 050319 are from Woźniak et al (2005) and GCNCs …”

Section: Early Optical Grb Afterglowsmentioning

confidence: 99%

Early re-brightening of the afterglow of GRB 050525a

Klotz

Boër

Atteia

et al. 2005

A&A

View full text Add to dashboard Cite

Abstract. We present time resolved optical data acquired by the TAROT automated observatory on the afterglow of GRB 050525a from 6 to 136 min after the GRB. We find evidence for a rapid re-brightening of 0.65 mag of the afterglow at ∼33 min after the GRB. The decay slope α is 1.14 ± 0.07 in the first part and is 1.23 ± 0.27 after the re-brightening event.The afterglow of GRB 050525a is the third known afterglow that exhibits a re-brightening event beginning at 0.01-0.02 day in the rest time frame.

show abstract

RAPTOR Observations of the Early Optical Afterglow from GRB 050319

Cited by 41 publications

References 23 publications

The dust extinction curves of gamma-ray burst host galaxies

The dust extinction curves of gamma-ray burst host galaxies

LOOKING INTO THE FIREBALL: ROTSE-III ANDSWIFTOBSERVATIONS OF EARLY GAMMA-RAY BURST AFTERGLOWS

Early re-brightening of the afterglow of GRB 050525a

Contact Info

Product

Resources

About