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|Title:||Spectrophotometric analysis of gamma-ray burst afterglow extinction curves with X-Shooter||Authors:||Japelj, J.
Vergani, S. D.
Fynbo, J. P. U.
Tanvir, N. R.
de Ugarte Postigo, A.
Wijers, R. A. M. J.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||579||First Page:||A74||Abstract:||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 ≲ A<SUB>V</SUB> ≲ 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 (GRB 120119A), 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 themodelled values of the extinction A<SUB>V</SUB> 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). <P />Based on observations collected at the European Southern Observatory, Paranal, Chile, under programs 084.A-0260(B), 085.A-0009(B), 088.A-0051(B), 089.A-0067(B) and 091.C-0934(C). Appendix A is available in electronic form at http://www.aanda.org/10.1051/0004-6361/201525665/olm||Acknowledgments:||A.d.U.P. acknowledges support from a Ramón y Cajal fellowship. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester.||URI:||http://hdl.handle.net/20.500.12386/23682||URL:||https://www.aanda.org/articles/aa/abs/2015/07/aa25665-15/aa25665-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201525665||Bibcode ADS:||2015A&A...579A..74J||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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