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Late-Time Spectral Observations of the Strongly Interacting Type Ia Supernova PTF11kx | | Jeffrey M. Silverman
; Peter E. Nugent
; Avishay Gal-Yam
; Mark Sullivan
; D. Andrew Howell
; Alexei V. Filippenko
; Yen-Chen Pan
; S. Bradley Cenko
; Isobel M. Hook
; | | Date: |
28 Mar 2013 | | Abstract: | PTF11kx was a Type Ia supernova (SN Ia) that showed time-variable absorption
features, including saturated Ca II H&K lines that weakened and eventually went
into emission. H{alpha} was in emission, and its strength gradually increased,
implying that the SN was undergoing significant interaction with its
circumstellar medium (CSM). Many of these features were blueshifted slightly
and showed a P-Cygni profile, likely indicating that the CSM was directly
related to, and probably previously ejected by, the progenitor system itself.
These and other observations led Dilday et al. (2012) to conclude that PTF11kx
came from a symbiotic nova progenitor like RS Oph. In this work we extend the
spectral coverage of PTF11kx to 124-680 rest-frame days past maximum
brightness. These spectra of PTF11kx are dominated by H{alpha} emission (with
widths of ~2000 km/s), strong Ca II emission features (~10,000 km/s wide), and
a blue "quasi-continuum" due to many overlapping narrow lines of Fe II.
Emission from oxygen, He I, and Balmer lines higher than H{alpha} is weak or
completely absent at all epochs, leading to large observed H{alpha}/H{eta}
intensity ratios. The broader (~2000 km/s) H{alpha} emission appears to
increase in strength with time for ~1 yr, but it subsequently decreases
significantly along with the Ca II emission. Our latest spectrum also indicates
the possibility of newly formed dust in the system as evidenced by a slight
decrease in the red wing of H{alpha}. During the same epochs, multiple narrow
emission features from the CSM temporally vary in strength. The weakening of
the H{alpha} and Ca II emission at late times is possible evidence that the SN
ejecta have overtaken the majority of the CSM and agrees with models of other
strongly interacting SNe Ia. The varying narrow emission features, on the other
hand, may indicate that the CSM is clumpy or consists of multiple thin shells. | | Source: | arXiv, 1303.7234 | | Services: | Forum | Review | PDF | Favorites | |
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