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arXiv 1602.01433astro-ph.HEastro-ph.CO
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（i）PTF中II型超新星的金属丰度

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. P… 展开作者

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

备注：
Replaced to match the accepted version
发表信息：
A&A 587, L7 (2016)
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摘要：

IIP型超新星（SNe IIP）最近被提议作为金属丰度（$Z$）探针。Dessart等人（2014）的光谱模型表明，在平台期期间Fe II $λ$ 5018（pEW $_{5018}$）的伪等效宽度取决于原始$Z$，但缺乏表现出与$Z < 0.4$ ${\rm Z}_{\odot}$相容的pEW $_{5018}$的SNe IIP。这种缺乏可能是由于SN II人口的某些物理特性，或者是因为这些SNe已经在明亮的富含金属的目标星系中被发现。在这里，我们使用来自非靶向（中间）帕洛玛瞬态工厂[（i）PTF]调查的SN II观测，旨在研究该SN群体的pEW $_{5018}$分布，特别是在较低的$Z$下寻找SNe II的存在。我们执行pEW $_{5018}$测量的光谱样品的39（i）PTF SNe II，选择具有良好的约束爆炸时期和光变曲线属性。基于与pEW $_{5018}$光谱模型的比较，我们将我们的SNe分成从$Z \approx 0.1$ $Z_{\odot}$到$Z \approx 2$ $Z_{\odot}$的四个$Z$箱。我们还独立地调查了主机的$Z$，通过使用它们的绝对大小和颜色，在少数情况下，使用强线诊断光谱。我们搜索SN观测值之间可能的相关性，例如它们的峰值幅度和从pEW $_{5018}$推断的$Z$。我们发现了11例pEW $_{5018}$事件，这些事件小到足以表明$Z \approx 0.1$ $Z_{\odot}$。pEW $_{5018}$与$Z$的趋势与从宿主星系测光获得的$Z$估计值相匹配，尽管相关性的显著性较弱。我们还发现，具有较亮峰值幅度的SNe具有较小的pEW $_{5018}$，并且发生在较低的$Z$。

英文摘要：

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 $λ$5018 (pEW$_{5018}$) during the plateau phase depends on the primordial $Z$, but there was a paucity of SNe IIP exhibiting pEW$_{5018}$ that were compatible with $Z < 0.4$ ${\rm Z}_{\odot}$. This lack might be due to some physical property of the SN II population or to the fact that those SNe have been 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. 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, using 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$_{5018}$ that were small enough 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 $Z$.

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