High‐Resolution Grating Spectroscopy of Gamma‐Ray Bursts 030328 and 041006 with<i>Chandra</i>LETGS

Butler, Nathaniel R.; Ricker, G.; Ford, P. G.; Vanderspek, R.; Marshall, Herman L.; Jernigan, J. G.; Garmire, G. P.; Lamb, D. Q.

doi:10.1086/431644

Cited by 11 publications

(25 citation statements)

References 40 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…3.5). Moreover, if we consider a fireball model consisting of a fixed-angle jet-collimated expansion in a homogeneous medium (Mészáros & Rees 1999), we obtain α is consistent with the X-ray temporal slope as determined by Butler et al (2005), as the Chandra observation starts after the optical jet break time.…”

Section: Discussionsupporting

confidence: 79%

“…The solid line towards the bottom of the figure represents the 1σ Poisson error spectrum. As also suggested from the X-ray spectral fitting (Butler et al 2005), weak absorption is associated with this GRB environment; thus, we do not expect dust in the neutral gas to obscure significantly the optical afterglow. From the Fe ii column density, we estimate A V < 0.1 mag (Savaglio et al 2003;Savaglio & Fall 2004).…”

Section: Spectroscopysupporting

confidence: 74%

“…Multicolor imaging and analysis of the host galaxy was reported by Gorosabel et al (2005). Chandra observations, starting about 15 h after the GRB, revealed a new, fading X-ray source at a position consistent with that of the optical transient, identified with the X-ray afterglow (Butler et al 2005). Its temporal decrease followed a powerlaw with index α X = 1.5 ± 0.1, and its 0.5-5 keV spectrum was well fitted by an absorbed power-law of photon index Γ X = 2.0 ± 0.2.…”

Section: Introductionmentioning

confidence: 83%

See 2 more Smart Citations

Physics of the GRB 030328 afterglow and its environment

Maiorano

Masetti

Palazzi

et al. 2006

A&A

View full text Add to dashboard Cite

Aims. To investigate the physical nature of the afterglow emission. We report on the photometric, spectroscopic and polarimetric observations of the optical afterglow of Gamma-Ray Burst (GRB) 030328 detected by HETE-2. Methods. Photometric, spectroscopic and polarimetric monitoring of the optical afterglow. Results. Photometry, collected at 7 different telescopes, shows that a smoothly broken powerlaw decay, with indices α 1 = 0.76 ± 0.03, α 2 = 1.50 ± 0.07 and a break at t b = 0.48 ± 0.03 days after the GRB, provides the best fit of the optical afterglow decline. This shape is interpreted as due to collimated emission, for which we determine a jet opening angle θ jet ∼ 3.• 2. An achromatic bump starting around ∼0.2 d after the GRB is possibly marginally detected in the optical light curves. Optical spectroscopy shows the presence of two rest-frame ultraviolet metal absorption systems at z = 1.5216 ± 0.0006 and at z = 1.295 ± 0.001, the former likely associated with the GRB host galaxy. Analysis of the absorption lines at z = 1.5216 suggests that the host of this GRB may be a Damped Lyman-α Absorber. The optical V-band afterglow appears polarized, with P = (2.4 ± 0.6)% and θ = 170• ± 7• , suggesting an asymmetric blastwave expansion. An X-ray-to-optical spectral flux distribution of the GRB 030328 afterglow was obtained at 0.78 days after the GRB and fitted using a broken powerlaw, with an optical spectral slope β opt = 0.47 ± 0.15, and an X-ray slope β X = 1.0 ± 0.2. Conclusions. The discussion of the results in the context of the "fireball model" shows that the preferred scenario for this afterglow is collimated structured jet with fixed opening angle in a homogeneous medium. Observatory (Australia), the 1m Sampurnanand telescope at the ARIES observatory (India), and the 1 m NOFS telescope of USNO in Flagstaff (USA).

show abstract

Section: Discussionsupporting

confidence: 79%

Section: Spectroscopysupporting

confidence: 74%

Section: Introductionmentioning

confidence: 83%

See 1 more Smart Citation

Physics of the GRB 030328 afterglow and its environment

Maiorano

Masetti

Palazzi

et al. 2006

A&A

View full text Add to dashboard Cite

show abstract

“…Thus, we adopt z ¼ 0:35. Fynbo et al (2004) find tentative evidence for a low redshift (although the host galaxy would be very faint), and Butler et al (2005a) find a preferred z ¼ 0:4 from the Amati relation (Amati et al 2002). In both cases, the SED is fit well by a power law with an additional small amount of source frame extinction.…”

Section: The Fitting Proceduresmentioning

confidence: 99%

Signatures of Extragalactic Dust in Pre‐SwiftGRB Afterglows

Канн

Klose

Zeh

2006

ApJ

304

553

View full text Add to dashboard Cite

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 preSwift 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.

show abstract

“…About ∼1 hour after the GRB, its optical afterglow has been detected by the 40-inch Siding Spring Observatory (SSO) telescope (Peterson & Price 2003). A study of the X-ray afterglow of GRB 030328 was performed by Butler et al (2005) using Chandra data.…”

Section: Introductionmentioning

confidence: 99%

The broadband afterglow of GRB 030328

Maiorano¹,

Masetti²,

Palazzi³

et al. 2006

AIP Conference Proceedings

View full text Add to dashboard Cite

We here report on the photometric, spectroscopic and polarimetric monitoring of the optical afterglow of the Gamma-Ray Burst (GRB) 030328 detected by HETE-2. We found that a smoothly broken power-law decay provides the best fit of the optical light curves, with indices alpha_1 = 0.76 +/- 0.03, alpha_2 = 1.50 +/- 0.07, and a break at t_b = 0.48 +/- 0.03 d after the GRB. Polarization is detected in the optical V-band, with P = (2.4 +/- 0.6)% and theta = (170 +/- 7) deg. Optical spectroscopy shows the presence of two absorption systems at z = 1.5216 +/- 0.0006 and at z = 1.295 +/- 0.001, the former likely associated with the GRB host galaxy. The X-ray-to-optical spectral flux distribution obtained 0.78 days after the GRB was best fitted using a broken power-law, with spectral slopes beta_opt = 0.47 +/- 0.15 and beta_X = 1.0 +/- 0.2. The discussion of these results in the context of the "fireball model" shows that the preferred scenario is a fixed opening angle collimated expansion in a homogeneous medium.Comment: To appear in the proceedings of the 16th Annual October Astrophysics Conference in Maryland, "Gamma Ray Bursts in the Swift Era", Washington DC., November 29-December 2, 2005, 4 pages, 3 figure

show abstract

High‐Resolution Grating Spectroscopy of Gamma‐Ray Bursts 030328 and 041006 withChandraLETGS

Cited by 11 publications

References 40 publications

Physics of the GRB 030328 afterglow and its environment

Physics of the GRB 030328 afterglow and its environment

Signatures of Extragalactic Dust in Pre‐SwiftGRB Afterglows

The broadband afterglow of GRB 030328

Contact Info

Product

Resources

About