Bibcode
Melandri, A.; Pian, E.; Ferrero, P.; D'Elia, V.; Walker, E. S.; Ghirlanda, G.; Covino, S.; Amati, L.; D'Avanzo, P.; Mazzali, P. A.; Della Valle, M.; Guidorzi, C.; Antonelli, L. A.; Bernardini, M. G.; Bersier, D.; Bufano, F.; Campana, S.; Castro-Tirado, A. J.; Chincarini, G.; Deng, J.; Filippenko, A. V.; Fugazza, D.; Ghisellini, G.; Kouveliotou, C.; Maeda, K.; Marconi, G.; Masetti, N.; Nomoto, K.; Palazzi, E.; Patat, F.; Piranomonte, S.; Salvaterra, R.; Saviane, I.; Starling, R. L. C.; Tagliaferri, G.; Tanaka, M.; Vergani, S. D.
Referencia bibliográfica
Astronomy and Astrophysics, Volume 547, id.A82, 7 pp.
Fecha de publicación:
11
2012
Revista
Número de citas
63
Número de citas referidas
54
Descripción
Aims: The association of Type Ic supernovae (SNe) with
long-duration gamma-ray bursts (GRBs) is well established. We endeavor,
through accurate ground-based observational campaigns, to characterize
these SNe at increasingly high redshifts. Methods: We obtained a
series of optical photometric and spectroscopic observations of the Type
Ic SN 2012bz associated with the Swift long-duration GRB 120422A
(redshift z = 0.283) using the 3.6-m TNG and the 8.2-m VLT telescopes
during the time interval between 4 and 36 days after the burst.
Results: The peak times of the light curves of SN 2012bz in various
optical filters differ, with the B-band and i'-band light curves
reaching maximum at 9 ± 4 and 23 ± 3 rest-frame days,
respectively. The bolometric light curve has been derived from
individual bands photometric measurements, but no correction for the
unknown contribution in the near-infrared (probably around 10-15%) has
been applied. Therefore, the present light curve should be considered as
a lower limit to the actual UV-optical-IR bolometric light curve. This
pseudo-bolometric curve reaches its maximum (Mbol = -18.56
± 0.06) at 13 ± 1 rest-frame days; it is similar in shape
and luminosity to the bolometric light curves of the SNe associated with
z < 0.2 GRBs and more luminous than those of SNe associated with
X-ray flashes (XRFs). A comparison with the model generated for the
bolometric light curve of SN 2003dh suggests that SN 2012bz produced
only about 15% less 56Ni than SN 2003dh, about 0.35
M&sun;. Similarly the VLT spectra of SN 2012bz, after
correction for Galactic extinction and for the contribution of the host
galaxy, suggest comparable explosion parameters with those observed in
SN 2003dh (EK ~ 3.5 × 1052 erg,
Mej ~ 7 M&sun;) and a similar progenitor mass
(~25-40 M&sun;). GRB 120422A is consistent with the
Epeak - Eiso and the EX,iso -
Eγ,iso - Epeak relations. GRB 120422A / SN
2012bz shows the GRB-SN connection at the highest redshift so far
accurately monitored both photometrically and spectroscopically.
Based on observations made with the Italian 3.6-m Telescopio Nazionale
Galileo (TNG), operated on the island of La Palma by the
Fundación Galileo Galilei of the INAF (Instituto Nazionale di
Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of
the Instituto de Astrofísica de Canarias under program A25TAC_11,
and with the ESO 8.2-m Very Large Telescope (VLT) at Paranal Observatory
under program 089.D-0033(A).
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Ismael
Pérez Fournon