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Metallicity from Type II Supernovae from the (i)PTF | | F. Taddia
; P. Moquist
; J. Sollerman
; A. Rubin
; G. Leloudas
; A. Gal-Yam
; I. Arcavi
; Y. Cao
; A. V. Filippenko
; M. L. Graham
; P. A. Mazzali
; P. E. Nugent
; Y.-C. Pan
; J. M. Silverman
; D. Xu
; O. Yaron
; | | Date: |
2 Feb 2016 | | Abstract: | Type IIP supernovae (SNe IIP) have recently been proposed as metallicity
($Z$) probes. The spectral models of Dessart et al. (2014) showed that the
pseudo-equivalent width of Fe II $lambda$5018 (pEW$_{5018}$) during the
plateau phase depends on the primordial $Z$, but there was a paucity of SNe IIP
exhibiting pEW$_{5018}$ compatible with $Z < 0.4 {
m Z}_{odot}$. This lack
might be due to some physical property of the SN II population, or to the fact
that those SNe were discovered in luminous, metal-rich targeted galaxies. Here
we use SN II observations from the untargeted (intermediate) Palomar Transient
Factory [(i)PTF] survey, aiming to investigate the pEW$_{5018}$ distribution of
this SN population and in particular to look for the presence of SNe II at
lower $Z$. We perform pEW$_{5018}$ measurements on the spectra of a sample of
39 (i)PTF SNe II, selected to have well-constrained explosion epochs and
light-curve properties (Rubin et al. 2015). Based on the comparison with the
pEW$_{5018}$ spectral models we subgrouped our SNe into four $Z$ bins, from $Z
approx 0.1$ $Z_{odot}$ up to $Z approx 2$ $Z_{odot}$. We also independently
investigated the $Z$ of the hosts by using their absolute magnitudes and
colors, and in a few cases with strong-line diagnostics from spectra. We
searched for possible correlations between SN observables such as their peak
magnitudes and the $Z$ inferred from pEW$_{5018}$. We found 11 events with
pEW$_{5018}$ sufficiently small to indicate $Z approx 0.1$ $Z_{odot}$. The
trend of pEW$_{5018}$ with $Z$ matches the $Z$ estimates obtained from the
host-galaxy photometry, although the significance of the correlation is weak.
We also found that SNe with brighter peak magnitudes have smaller pEW$_{5018}$
and occur at lower $Z$. | | Source: | arXiv, 1602.1433 | | Services: | Forum | Review | PDF | Favorites | |
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