IAFE   05512
INSTITUTO DE ASTRONOMIA Y FISICA DEL ESPACIO
Unidad Ejecutora - UE
artículos
Título:
The Highly Energetic Expansion of SN 2010bh Associated with GRB 100316D
Autor/es:
MIRABEL IF Y 92 MÁSY OTROS
Revista:
ASTROPHYSICAL JOURNAL
Editorial:
IOP PUBLISHING LTD
Referencias:
Lugar: Londres; Año: 2012 vol. 753 p. 67 - 79
ISSN:
0004-637X
Resumen:
We present the spectroscopic and photometric evolution of the nearby (z
= 0.059) spectroscopically confirmed Type Ic supernova, SN 2010bh,
associated with the soft, long-duration gamma-ray burst (X-ray flash)
GRB 100316D. Intensive follow-up observations of SN 2010bh were
performed at the ESO Very Large Telescope (VLT) using the X-shooter and
FORS2 instruments. Thanks to the detailed temporal coverage and the
extended wavelength range (3000-24800 Å), we obtained an
unprecedentedly rich spectral sequence among the hypernovae, making SN
2010bh one of the best studied representatives of this SN class. We find
that SN 2010bh has a more rapid rise to maximum brightness (8.0 ±
1.0 rest-frame days) and a fainter absolute peak luminosity (L
bol ≈ 3 × 1042 erg s-1) than
previously observed SN events associated with GRBs. Our estimate of the
ejected 56Ni mass is 0.12 ± 0.02 M sun.
From the broad spectral features, we measure expansion velocities up to
47,000 km s-1, higher than those of SNe 1998bw (GRB 980425)
and 2006aj (GRB 060218). Helium absorption lines He I λ5876 and
He I 1.083 μm, blueshifted by ~20,000-30,000 km s-1 and
~28,000-38,000 km s-1, respectively, may be present in the
optical spectra. However, the lack of coverage of the He I 2.058 μm
line prevents us from confirming such identifications. The nebular
spectrum, taken at ~186 days after the explosion, shows a broad but
faint [O I] emission at 6340 Å. The light curve shape and
photospheric expansion velocities of SN 2010bh suggest that we witnessed
a highly energetic explosion with a small ejected mass (E k
≈ 1052 erg and M ej ≈ 3 M sun).
The observed properties of SN 2010bh further extend the heterogeneity of
the class of GRB SNe.