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Metallicity from Type II supernovae from the (i)PTF

Taddia, F and Moquist, P and Sollerman, J and Rubin, A and Leloudas, G and Gal-Yam, A and Arcavi, I and Cao, Y and Filippenko, AV and Graham, ML and Mazzali, PA and Nugent, PE and Pan, YC and Silverman, JM and Xu, D and Yaron, O (2016) Metallicity from Type II supernovae from the (i)PTF. Astronomy and Astrophysics, 587. ISSN 0004-6361

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Abstract

Type IIP supernovae (SNe IIP) have recently been proposed as metallicity (Z) probes. The spectral models of Dessart et al. (2014, MNRAS, 440, 1856) showed that the pseudo-equivalent width of Fe ii λ5018 (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 Z ⊙ . 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 ≈ 0.1 Z ⊙ up to Z ≈ 2 Z ⊙ . 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 ≈ 0.1 Z ⊙ . 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. © ESO, 2016.

Item Type: Article
Uncontrolled Keywords: 0201 Astronomical And Space Sciences
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Q Science > QD Chemistry
Divisions: Astrophysics Research Institute
Publisher: EDP Sciences
Date Deposited: 18 Oct 2017 11:16
Last Modified: 18 Oct 2017 11:16
DOI or Identification number: 10.1051/0004-6361/201527983
URI: http://researchonline.ljmu.ac.uk/id/eprint/7377

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