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Titolo:
GRB010222: Afterglow emission from a rapidly decelerating shock
Autore:
Masetti, N; Palazzi, E; Pian, E; Mannucci, F; Antonelli, LA; Di Paola, A; Saracco, P; Savaglio, S; Amati, L; Bartolini, C; Bernabei, S; Bettoni, D; Covino, S; Cristiani, S; Desidera, S; Alighieri, SD; Falomo, R; Frontera, F; Ghinassi, F; Guarnieri, A; Magazzu, A; Maiolino, R; Mignoli, M; Nicastro, L; Pedani, M; Piccioni, A; Poggianti, BM; Testa, V; Valentini, G; Zacchei, A;
Indirizzi:
CNR, Ist Tecnol & Studio Radiaz Extraterr, I-40129 Bologna, Italy CNR Bologna Italy I-40129 tudio Radiaz Extraterr, I-40129 Bologna, Italy Osserv Astron Trieste, I-34131 Trieste, Italy Osserv Astron Trieste Trieste Italy I-34131 este, I-34131 Trieste, Italy CNR, Ctr Astron Infrarossa & Studio Mezzo Interstellar, I-50125 Florence, Italy CNR Florence Italy I-50125 o Mezzo Interstellar, I-50125 Florence, Italy Osserv Astron Roma, I-00040 Monteporzio Catone, Italy Osserv Astron Roma Monteporzio Catone Italy I-00040 porzio Catone, Italy Osserv Astron Brera, I-23807 Merate, Italy Osserv Astron Brera Merate Italy I-23807 on Brera, I-23807 Merate, Italy Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy Univ Bologna Bologna Italy I-40127 imento Astron, I-40127 Bologna, Italy Osservatorio Astron Bologna, I-40127 Bologna, Italy Osservatorio Astron Bologna Bologna Italy I-40127 I-40127 Bologna, Italy Inst Astrofis Canarias, Tenerife 38200, Spain Inst Astrofis Canarias Tenerife Spain 38200 arias, Tenerife 38200, Spain Osserv Astron Padova, I-35122 Padua, Italy Osserv Astron Padova Padua Italy I-35122 on Padova, I-35122 Padua, Italy Univ Padua, Dipartimento Astron, I-35122 Padua, Italy Univ Padua Padua Italy I-35122 Dipartimento Astron, I-35122 Padua, Italy Osservatorio Astron Asiago, I-36012 Asiago, Italy Osservatorio Astron Asiago Asiago Italy I-36012 o, I-36012 Asiago, Italy Osserv Astrofis Arcetri, I-50125 Florence, Italy Osserv Astrofis Arcetri Florence Italy I-50125 , I-50125 Florence, Italy Univ Ferrara, Dipartimento Fis, I-44100 Ferrara, Italy Univ Ferrara Ferrara Italy I-44100 artimento Fis, I-44100 Ferrara, Italy Telescopio Nazl Galileo, Roque Muchachos Astron Observ, Santa Cruz De La Palma 38700, Spain Telescopio Nazl Galileo Santa Cruz De La Palma Spain 38700 38700, Spain Osservatorio Astron Collurania Teramo, I-64100 Teramo, Italy Osservatorio Astron Collurania Teramo Teramo Italy I-64100 Teramo, Italy CNR, Ist Fis Cosm & Applicaz Informat, I-90146 Palermo, Italy CNR Palermo Italy I-90146 sm & Applicaz Informat, I-90146 Palermo, Italy
Titolo Testata:
ASTRONOMY & ASTROPHYSICS
fascicolo: 2, volume: 374, anno: 2001,
pagine: 382 - 393
SICI:
1432-0746(200108)374:2<382:GAEFAR>2.0.ZU;2-W
Fonte:
ISI
Lingua:
ENG
Soggetto:
GAMMA-RAY BURST; OPTICAL AFTERGLOW; LIGHT CURVES; FOLLOW-UP; GRB-990510; VARIABILITY; PHOTOMETRY; EXTINCTION; DISCOVERY; REDSHIFTS;
Keywords:
gamma rays : bursts; radiation mechanisms : non-thermal; line : identification; cosmology : observations;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
73
Recensione:
Indirizzi per estratti:
Indirizzo: Masetti, N CNR, Ist Tecnol & Studio Radiaz Extraterr, Via Gobetti 101, I-40129 Bologna, Italy CNR Via Gobetti 101 Bologna Italy I-40129 40129 Bologna, Italy
Citazione:
N. Masetti et al., "GRB010222: Afterglow emission from a rapidly decelerating shock", ASTRON ASTR, 374(2), 2001, pp. 382-393

Abstract

The GRB010222 optical and near-infrared (NIR) afterglow was monitored at the TNG and other Italian telescopes starting similar to 1 day after the high-energy prompt event. The BVR light curves, which are the best sampled, are continuously steepening and can be described by two power laws, f(t) proportional to t(-alpha), of indices alpha (1) similar to 0.7 and alpha (2) similar to 1.3 before and after a break occurring at about 0.5 days after theGRB start time, respectively. This model accounts well also for the flux in the U, I and J bands, which are less well monitored. The temporal break appears to be achromatic. The two K-band points are not consistent with the above behaviour, and rather suggest a constant trend. A low-resolution optical spectrum has also been taken with TNG. In the optical spectrum we foundthree absorption systems at different redshifts (0.927, 1.155 and 1.475), the highest of which represents a lower limit to, and probably coincides with, the redshift of the GRB. The broad-band optical spectral energy distributions do not appear to vary with time, consistently with the achromatic behaviour of the light curves. We compare our measurements with different afterglow evolution scenarios and we find that they favor a transition from relativistic to non-relativistic conditions in the shock propagation.

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Documento generato il 18/11/17 alle ore 03:39:21