Astronomy and Astrophysics, volume 404, 465-481 (2003/6-3)
Optical and near-infrared observations of the GRB 020405 afterglow.
MASETTI N., PALAZZI E., PIAN E., SIMONCELLI A., HUNT L.K., MAIORANO E., LEVAN A., CHRISTENSEN L., ROL E., SAVAGLIO S., FALOMO R., CASTRO-TIRADO A.J., HJORTH J., DELSANTI A., PANNELLA M., MOHAN V., PANDEY S.B., SAGAR R., AMATI L., BURUD I., CASTRO CERON J.M., FRONTERA F., FRUCHTER A.S., FYNBO J.P.U., GOROSABEL J., KAPER L., KLOSE S., KOUVELIOTOU C., NICASTRO L., PEDERSEN H., RHOADS J., SALAMANCA I., TANVIR N., VREESWIJK P.M., WIJERS R.A.M.J. and VAN DEN HEUVEL E.P.J.
Abstract (from CDS):
We report on photometric, spectroscopic and polarimetric monitoring of the optical and near-infrared (NIR) afterglow of GRB020405. Ground-based optical observations, performed with 8 different telescopes, started about 1-day after the high-energy prompt event and spanned a period of ∼10-days; the addition of archival HST data extended the coverage up to ∼150-days after the GRB. We report the first detection of the afterglow in NIR bands. The detection of Balmer and oxygen emission lines in the optical spectrum of the host galaxy indicates that the GRB is located at redshift z=0.691. Fe ii and Mg ii absorption systems are detected at z=0.691 and at z=0.472 in the afterglow optical spectrum. The latter system is likely caused by absorbing clouds in the galaxy complex located ∼2" southwest of the GRB020405 host. Hence, for the first time, the galaxy responsible for an intervening absorption line system in the spectrum of a GRB afterglow is spectroscopically identified. Optical and NIR photometry of the afterglow indicates that, between 1 and 10-days after the GRB, the decay in all bands is consistent with a single power law of index α=1.54±0.06. The late-epoch VLT J-band and HST optical points lie above the extrapolation of this power law, so that a plateau (or ``bump") is apparent in the VRIJ light curves at 10-20days after the GRB. The light curves at epochs later than day ∼20 after the GRB are consistent with a power-law decay with index α'=1.85±0.15. While other authors have proposed to reproduce the bump with the template of the supernova (SN) 1998bw, considered the prototypical ``hypernova'', we suggest that it can also be modeled with a SN having the same temporal profile as the other proposed hypernova SN2002ap, but 1.3mag brighter at peak, and located at the GRB redshift. Alternatively, a shock re-energization may be responsible for the rebrightening. A single polarimetric R-band measurement shows that the afterglow is polarized, with P = 1.5±0.4% and polarization angle θ= 172°±8°. Broad-band optical-NIR spectral flux distributions show, in the first days after the GRB, a change of slope across the J band which we interpret as due to the presence of the electron cooling frequency νc. The analysis of the multiwavelength spectrum within the standard fireball model suggests that a population of relativistic electrons with index p∼2.7 produces the optical-NIR emission via synchrotron radiation in an adiabatically expanding blastwave, with negligible host galaxy extinction, and the X-rays via Inverse Compton scattering off lower-frequency afterglow photons.
gamma rays: bursts - radiation mechanisms: non-thermal - line: identification - cosmology: observations
Fig.1, Table 2: [MPP2003] Star N (Nos 1-6), [MPP2003] Star A (Nos A-B). Fig.6: [MPP2003] Galaxy N (Nos 1-2). Text: [MPP2003] GRB 020405 abs N.NNNN N=2.
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