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Titolo:
The fading optical counterpart of GRB 970228, 6 months and 1 year later
Autore:
Fruchter, AS; Pian, E; Thorsett, SE; Bergeron, LE; Gonzalez, RA; Metzger, M; Goudfrooij, P; Sahu, KC; Ferguson, H; Livio, M; Mutchler, M; Petro, L; Frontera, F; Galama, T; Groot, P; Hook, R; Kouveliotou, C; Macchetto, D; van Paradijs, J; Palazzi, E; Pedersen, H; Sparks, W; Tavani, M;
Indirizzi:
Space Telescope Sci Inst, Baltimore, MD 21218 USA Space Telescope Sci Inst Baltimore MD USA 21218 , Baltimore, MD 21218 USA CNR, Ist Tecnol & Studio Radiaz Extraterr, I-40129 Bologna, Italy CNR Bologna Italy I-40129 tudio Radiaz Extraterr, I-40129 Bologna, Italy Princeton Univ, Joseph Henry Labs, Princeton, NJ 08544 USA Princeton UnivPrinceton NJ USA 08544 Henry Labs, Princeton, NJ 08544 USA Princeton Univ, Dept Phys, Princeton, NJ 08544 USA Princeton Univ Princeton NJ USA 08544 Dept Phys, Princeton, NJ 08544 USA CALTECH, Dept Astron, Pasadena, CA 91125 USA CALTECH Pasadena CA USA 91125 ALTECH, Dept Astron, Pasadena, CA 91125 USA EuropeaneSpace Agcy, Dept Space Sci, Div Astrophys, F-75738 Paris 15, Franc European Space Agcy Paris France 15 v Astrophys, F-75738 Paris 15, Franc Univ Ferrara, Dipartmento Fis, I-44100 Ferrara, Italy Univ Ferrara Ferrara Italy I-44100 partmento Fis, I-44100 Ferrara, Italy Univndssterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherla Univ Amsterdam Amsterdam Netherlands NL-1098 SJ 8 SJ Amsterdam, Netherla Space Telescope European Coordinating Facil, D-85748 Garching, Germany Space Telescope European Coordinating Facil Garching Germany D-85748 any NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA NASA Huntsville AL USA 35812 l Space Flight Ctr, Huntsville, AL 35812 USA Copenhagen Univ Observ, DK-2100 Copenhagen A, Denmark Copenhagen Univ Observ Copenhagen Denmark A K-2100 Copenhagen A, Denmark Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA Columbia Univ New York NY USA 10027 Astrophys Lab, New York, NY 10027 USA CNR, Ist Fis Cosm & Tecnol Relat, I-20133 Milan, Italy CNR Milan Italy I-20133 st Fis Cosm & Tecnol Relat, I-20133 Milan, Italy
Titolo Testata:
ASTROPHYSICAL JOURNAL
fascicolo: 2, volume: 516, anno: 1999,
parte:, 1
pagine: 683 - 692
SICI:
0004-637X(19990510)516:2<683:TFOCOG>2.0.ZU;2-1
Fonte:
ISI
Lingua:
ENG
Soggetto:
GAMMA-RAY BURST; HUBBLE-SPACE-TELESCOPE; HIGH-REDSHIFT GALAXIES; INTERSTELLAR NA I; DEEP FIELD; CA-II; EMISSION; SPECTRA; LINES; STARS;
Keywords:
gamma rays : bursts; infrared : galaxies;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
68
Recensione:
Indirizzi per estratti:
Indirizzo: Fruchter, AS Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA Space Telescope Sci Inst 3700 San Martin Dr Baltimore MD USA 21218
Citazione:
A.S. Fruchter et al., "The fading optical counterpart of GRB 970228, 6 months and 1 year later", ASTROPHYS J, 516(2), 1999, pp. 683-692

Abstract

We report on observations of the fading optical counterpart of the gamma-ray burst GRB 970228, made with the Hubble Space Telescope (HST) and the Keck I telescope. The gamma-ray burst (GRB) was observed approximately 6 months after outburst, on 1997 September 4, using the HST/STIS CCD, and approximately 1 year after outburst, on 1998 February 24, using HST/NICMOS, and on 1998 April 4 using the NIRC on Keck. The unresolved counterpart is detectedby STIS at V = 28.0 +/- 0.25, consistent with a continued power-law decline with exponent -1.10 +/- 0.05. The counterpart is located within, but nearthe edge of, a faint extended source with diameter similar to 0." 8 and integrated magnitude V = 25.8 +/- 0.25. A reanalysis of HST and New Technology Telescope observations performed shortly after the burst shows no evidence of proper motion of the point source or fading of the extended emission. Although the optical transient is not detected in the NICMOS images (H greater than or equal to 25.3), the extended source is visible and has a total magnitude H = 23.3 +/- 0.1. The Keck observations find K = 22.8 +/- 0.3. Comparison with observations obtained shortly after outburst suggests that the nebular luminosity has also been stable in the infrared. We find that several distinct and independent means of deriving the foreground extinction in the direction of GRB 970228 all agree with A(V) = 0.75 +/- 0.2. After adjusting for this Galactic extinction, we find that the size of the observed extended emission is consistent with that of galaxies of comparable magnitude found in the Hubble Deep Field (HDF) and other deep HST images. Only 2% of the sky is covered by galaxies of similar or greater surface brightness. We therefore conclude that the extended source observed about GRB 970228 is almost certainly its host galaxy. Additionally, we find that independent of assumed redshift, the host is significantly bluer than typical nearby blue dwarf irregulars. With the caveat that the presently available infrared observations of the HDF are only fully complete to a limit about one-half magnitude brighter than the host, we find that the extinction-corrected V-H and V-K colors of the host are as blue as any galaxy of comparable or brighter magnitude in the HDF. Taken in concert with recent observations of GRB 970508, GRB 971214, and GRB 980703 our work suggests that all four GRBs with spectroscopic identification or deep multicolor broadband imaging of the host lie in rapidly star-forming galaxies.

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Documento generato il 26/09/17 alle ore 09:12:35