Physics of the GRB 030328 afterglow and its environment

Maiorano, E.; Masetti, N.; Palazzi, E.; Savaglio, S.; Rol, E.; Vreeswijk, P. M.; Pian, E.; Price, P. A.; Peterson, Bruce A.; Jelínek, M.; Amati, L.; Andersen, M. I.; Castro-Tirado, A. J.; Cerón, J. M. Castro; Postigo, A. de Ugarte; Frontera, F.; Fruchter, A. S.; Fynbo, J. P. U.; Gorosabel, J.; Henden, A. A.; Hjorth, J.; Jensen, B. L.; Klose, S.; Kouveliotou, C.; Møller, P.; Ofek, E. O.; Rhoads, James E.; Tanvir, N. R.; Wijers, R. A. M. J.; Heuvel, E. P. J. van den

doi:10.1051/0004-6361:20054728

Cited by 21 publications

(4 citation statements)

References 56 publications

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“…We constructed the SED (I C R C VBU) of GRB 030328 at z ≈ 1.52 (Martini et al 2003) with data from Maiorano et al (2006). From the Fe ii column density derived from the VLT optical spectrum of its afterglow, Maiorano et al (2006) Kann et al (2006) fitted the afterglow SED with a SMC-type extinction of A V ≈ 0.05 ± 0.15 mag. The Drude approach derives A V ≈ 0.20 ± 0.06 mag with an extinction curve just like that of the MW but with the 2175 Å bump removed (see Figure 5).…”

Section: Resultsmentioning

confidence: 99%

Probing Extragalactic Dust Through Nearby Gamma-Ray Burst Afterglows

Liang

2010

ApJ

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The quantities and wavelength dependencies of the dust extinction along the lines of sight toward 33 nearby gammaray bursts (GRBs) with redshifts z < 2 are derived from fitting their afterglow spectral energy distributions. Unlike previous studies which often assume a specific extinction law like that of the Milky Way (MW) and the Large and Small Magellanic Clouds (LMC/SMC), our approach-we call it the "Drude" approach-is more flexible in determining the true wavelength dependence of the extinction (while the shape of the extinction curve inferred from that relying on a priori assumption of a template extinction law is, of course, fixed). The extinction curves deduced from the Drude approach display a wide diversity of shapes, ranging from relatively flat curves to curves which are featureless and steeply rise toward the far-ultraviolet, and from curves just like that of the MW, LMC, and SMC to curves resembling that of the MW and LMC but lacking the 2175 Å bump. The visual extinction A V derived from the Drude approach is generally larger by a factor of ∼2-5 than that inferred by assuming a SMC-type template extinction law. Consistent with previous studies, the extinction-togas ratio is mostly smaller than that of the MW, and does not seem to correlate with the shape of the extinction curve. It is shown that the standard silicate-graphite interstellar grain model closely reproduces the extinction curves of all 33 GRBs host galaxies. For these 33 bursts at z < 2, we find no evidence for the evolution of the dust extinction, dust sizes, and relative abundances of silicate to graphite on redshifts.

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Section: Resultsmentioning

confidence: 99%

Probing Extragalactic Dust Through Nearby Gamma-Ray Burst Afterglows

Liang

2010

ApJ

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“…At least in a couple of cases a homogeneous jet geometry could be formally ruled out: i.e. for GRB 020813 (Lazzati et al 2004) and for GRB 030328 (Maiorano et al 2006).…”

Section: Discussionmentioning

confidence: 99%

The complex light curve of the afterglow of GRB071010A

Covino

D’Avanzo

Klotz

et al. 2008

Monthly Notices of the Royal Astronomical Society

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We present and discuss the results of an extensive observational campaign devoted to GRB071010A, a long-duration gamma-ray burst detected by the Swift satellite. This event was followed for almost a month in the optical/near-infrared (NIR) with various telescopes starting from about 2min after the high-energy event. Swift XRT observations started only later at about 0.4d. The light-curve evolution allows us to single out an initial rising phase with a maximum at about 7min, possibly the afterglow onset in the context of the standard fireball model, which is then followed by a smooth decay interrupted by a sharp rebrightening at about 0.6d. The rebrightening was visible in both the optical/NIR and X-rays and can be interpreted as an episode of discrete energy injection, although various alternatives are possible. A steepening of the afterglow light curve is recorded at about 1d. The entire evolution of the optical/NIR afterglow is consistent with being achromatic. This could be one of the few identified GRB afterglows with an achromatic break in the X-ray through the optical/NIR bands. Polarimetry was also obtained at about 1d, just after the rebrightening and almost coincident with the steepening. This provided a fairly tight upper limit of 0.9 per cent for the polarized-flux fraction

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“…Linear polarization at the level of a few percent has been detected in the optical or NIR afterglow of about a dozen GRBs [22,[269][270][271][272][273][274][275][276][277][278][279]. Higher levels of polarization (10% Π 30%) have been measured mostly in the very early afterglow, likely being dominated by reverse shock emission, as discussed above (see, however, [280]).…”

Section: Afterglow Emissionmentioning

confidence: 99%