2015A&A...579A..74J


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST02:48:49

2015A&A...579A..74J - Astronomy and Astrophysics, volume 579A, 74-74 (2015/7-1)

Spectrophotometric analysis of gamma-ray burst afterglow extinction curves with X-Shooter.

JAPELJ J., COVINO S., GOMBOC A., VERGANI S.D., GOLDONI P., SELSING J., CANO Z., D'ELIA V., FLORES H., FYNBO J.P.U., HAMMER F., HJORTH J., JAKOBSSON P., KAPER L., KOPAC D., KRUEHLER T., MELANDRI A., PIRANOMONTE S., SANCHEZ-RAMIREZ R., TAGLIAFERRI G., TANVIR N.R., DE UGARTE POSTIGO A., WATSON D. and WIJERS R.A.M.J.

Abstract (from CDS):

We use gamma-ray burst (GRB) afterglow spectra observed with the VLT/X-Shooter spectrograph to measure rest-frame extinction in GRB lines-of-sight by modelling the broadband near-infrared (NIR) to X-ray afterglow spectral energy distributions (SEDs). Our sample consists of nine Swift GRBs, of which eight belong to the long-duration and one to the short-duration class. Dust is modelled using the average extinction curves of the Milky Way and the two Magellanic Clouds. We derive the rest-frame extinction of the entire sample, which fall in the range 0≲AV≲1.2. Moreover, the SMC extinction curve is the preferred extinction curve template for the majority of our sample, a result that is in agreement with those commonly observed in GRB lines of sights. In one analysed case (GRB120119A), the common extinction curve templates fail to reproduce the observed extinction. To illustrate the advantage of using the high-quality, X-Shooter afterglow SEDs over the photometric SEDs, we repeat the modelling using the broadband SEDs with the NIR-to-UV photometric measurements instead of the spectra. The main result is that the spectroscopic data, thanks to a combination of excellent resolution and coverage of the blue part of the SED, are more successful in constraining extinction curves and therefore dust properties in GRB hosts with respect to photometric measurements. In all cases but one the extinction curve of one template is preferred over the others. We show that the modelled values of the extinction AV and the spectral slope, obtained through spectroscopic and photometric SED analysis, can differ significantly for individual events, though no apparent trend in the differences is observed. Finally we stress that, regardless of the resolution of the optical-to-NIR data, the SED modelling gives reliable results only when the fit is performed on a SED covering a broader spectral region (in our case extending to X-rays).

Abstract Copyright:

Journal keyword(s): gamma-ray burst: general - dust, extinction

Simbad objects: 16

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Number of rows : 16

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9440 1
2 GRB 100814A gB 01 29 53.61 -17 59 43.6           ~ 149 0
3 GRB 100901A gB 01 49 03.56 +22 45 30.6           ~ 125 0
4 SN 2009nz SN* 02 26 19.87 -18 57 08.6           ~ 226 1
5 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 5665 1
6 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14826 1
7 GRB 120119A gB 08 00 06.940 -09 04 53.83           ~ 116 0
8 GRB 100219A gB 10 16 48.46 -12 34 00.2           ~ 90 0
9 GRB 130603B gB 11 28 48.16 +17 04 18.2           ~ 265 0
10 SN 2013cq SN* 11 32 32.84 +27 41 56.2           SNIc 378 1
11 GRB 130606A gB 16 37 35.12 +29 47 46.4           ~ 114 0
12 GRB 080210 gB 16 45 04.03 +13 49 36.3           ~ 92 0
13 GRB 100418A gB 17 05 26.96 +11 27 41.9           ~ 142 0
14 GRB 120815A gB 18 15 54.40 -52 07 29.0           ~ 65 0
15 GRB 140506A gB 18 27 06.04 -55 38 08.7           ~ 51 0
16 NAME Local Group GrG ~ ~           ~ 6970 0

    Equat.    Gal    SGal    Ecl

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2020.07.04-02:48:49

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