期刊
ASTROPHYSICAL JOURNAL
卷 832, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.3847/0004-637X/832/2/108
关键词
gamma-ray burst: general; gamma-ray burst: individual (GRB-980425, GRB-030329, GRB-060218, GRB-100316D, GRB-120422A, GRB-130427A, GRB-130702A, GRB130215A); supernovae: general; supernovae: individual (SN-1994I, SN-2004aw, SN-2007gr, SN-1998bw, SN-2003dh, SN-2006aj, SN-2009bb, SN-2010bh, SN-2012ap, SN-2012bz, SN-2013cq, SN-2013dx, SN-2013ez)
资金
- NSF CAREER award [AST-1352405]
- NSF award [AST-1413260]
- NYU/CCPP James Arthur Graduate Award
- NYU/CCPP James Arthur Postdoctoral Fellowship
- Direct For Mathematical & Physical Scien
- Division Of Astronomical Sciences [1352405] Funding Source: National Science Foundation
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1413260] Funding Source: National Science Foundation
We present the first systematic investigation of spectral properties of 17 Type Ic Supernovae (SNe Ic), 10 broad-lined SNe Ic (SNe Ic-bl) without observed gamma-ray bursts (GRBs), and 11 SNe Ic-bl with GRBs (SN-GRBs) as a function of time in order to probe their explosion conditions and progenitors. Using a number of novel methods, we analyze a total of 407 spectra, which were drawn from published spectra of individual SNe as well as from the densely time-sampled spectra of Modjaz et al (2014). In order to quantify the diversity of the SN spectra as a function of SN subtype, we construct average spectra of SNe Ic, SNe Ic-bl without GRBs,. and SNe Ic-bl with GRBs. We find that SN. 1994I is not a typical SN Ic, contrasting the general view, while the spectra of SN. 1998bw/GRB. 980425 are representative of mean spectra of SNe Ic-bl. We measure the ejecta absorption and width velocities using a new method described here and find that SNe Ic-bl with GRBs, on average, have quantifiably higher absorption velocities, as well as broader line widths than SNe without observed GRBs. In addition, we search for correlations between SN-GRB spectral properties and the energies of their accompanying GRBs. Finally, we show that the absence of clear He lines in optical spectra of SNe Ic-bl, and in particular of SN-GRBs, is not due to them being too smeared-out due to the high velocities present in the ejecta. This implies that the progenitor stars of SN-GRBs are probably free of the He-layer, in addition to being H-free, which puts strong constraints on the stellar evolutionary paths needed to produce such SN-GRB progenitors at the observed low metallicities.
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