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Metallicity from Type II supernovae from the (i)PTF
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
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Number of Authors: 16
2016 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 587, L7Article in journal (Refereed) Published
Abstract [en]

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 lambda 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 Z(circle dot). 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 pEW5018 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 approximate to 0.1 Z(circle dot) up to Z approximate to 2 Z(circle dot). 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 approximate to 0.1 Z(circle dot). 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.

Place, publisher, year, edition, pages
2016. Vol. 587, L7
Keyword [en]
supernovae: general, Galaxy: abundances
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:su:diva-130111DOI: 10.1051/0004-6361/201527983ISI: 000371589800010OAI: oai:DiVA.org:su-130111DiVA: diva2:926752
Available from: 2016-05-09 Created: 2016-05-09 Last updated: 2016-05-09Bibliographically approved

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Taddia, FrancescoSollerman, Jesper
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Department of AstronomyThe Oskar Klein Centre for Cosmo Particle Physics (OKC)
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