English   español  
Please use this identifier to cite or link to this item: http://hdl.handle.net/10261/167372
logo share SHARE logo core CORE   Add this article to your Mendeley library MendeleyBASE

Visualizar otros formatos: MARC | Dublin Core | RDF | ORE | MODS | METS | DIDL | DATACITE
Exportar a otros formatos:


Colour variations in the GRB 120327A afterglow

AuthorsMelandri, A.; Covino, S.; Zaninoni, E.; Campana, S.; Bolmer, J.; Cobb, B.E.; Gorosabel, Javier ; Kim, J.W.; Kuin, P.; Kuroda, D.; Malesani, D.; Mundell, C.G.; Nappo, F.; Sbarufatti, B.; Smith, R.J.; Steele, I.A.; Topinka, M.; Trotter, A.S.; Virgili, F.J.; Bernardini, M.G.; D'Avanzo, P.; D'Elia, V.; Fugazza, D.; Ghirlanda, G.; Gomboc, A.; Greiner, J.; Guidorzi, C.; Haislip, J.B.; Hanayama, H.; Hanlon, L.; Im, M.; Ivarsen, K.M.; Japelj, J.; Jelínek, M.; Kawai, N.; Kobayashi, S.; Kopac, D.; Lacluyzé, A.P.; Martin-Carrillo, A.; Murphy, D.; Reichart, D.E.; Salvaterra, R.; Salafia, O.S.; Tagliaferri, G.; Vergani, S.D.
KeywordsDust, extinction
Gamma-ray burst: individual: GRB 120327A
Issue Date2017
PublisherEDP Sciences
CitationAstronomy and Astrophysics 607: A29 (2017)
AbstractAims. We present a comprehensive temporal and spectral analysis of the long Swift GRB 120327A afterglow data to investigate possible causes of the observed early-time colour variations. Methods. We collected data from various instruments and telescopes in X-ray, ultraviolet, optical, and near-infrared bands, and determined the shapes of the afterglow early-time light curves. We studied the overall temporal behaviour and the spectral energy distributions from early to late times. Results. The ultraviolet, optical, and near-infrared light curves can be modelled with a single power-law component between 200 and 2 × 10 s after the burst event. The X-ray light curve shows a canonical steep-shallow-steep behaviour that is typical of long gamma-ray bursts. At early times a colour variation is observed in the ultraviolet/optical bands, while at very late times a hint of a re-brightening is visible. The observed early-time colour change can be explained as a variation in the intrinsic optical spectral index, rather than an evolution of the optical extinction.© 2017 ESO.
Identifiersdoi: 10.1051/0004-6361/201731759
issn: 1432-0746
Appears in Collections:(IAA) Artículos
Files in This Item:
File Description SizeFormat 
IAA_2017_aa31759-17.pdf1,63 MBAdobe PDFThumbnail
Show full item record
Review this work

WARNING: Items in Digital.CSIC are protected by copyright, with all rights reserved, unless otherwise indicated.