Metallicity from Type II supernovae from the (i)PTF

Taddia, F.; Moquist, P.; Sollerman, J.; Rubin, A.; Leloudas, G.; Gal‐Yam, A.; Arcavi, I.; Cao, Y.; Filippenko, A. V.; Graham, M. L.; Mazzali, P. A.; Nugent, P.; Pan, Y.-C.; Silverman, J. M.; Xu, D.; Yaron, O.

doi:10.1051/0004-6361/201527983

Cited by 25 publications

(32 citation statements)

References 24 publications

(38 reference statements)

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“…Our pEW results clearly support previous findings from Dessart et al (2014); Anderson et al (2016); Taddia et al (2016); Gutiérrez et al (2018). Our SNe are in faint galaxies (absolute M r > −17), which are expected to be of low metallicity.…”

Section: Metallicitysupporting

confidence: 93%

Bright Type IIP Supernovae in Low-metallicity Galaxies

Scott

Nicholl

Blanchard

et al. 2019

ApJL

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We present measurements of the pseudo-equivalent width of the Fe II λ5018 absorption feature in the spectra of 12 Type IIP supernovae (SNe II) in low luminosity (M > −17) dwarf host galaxies. The Fe II λ5018 line has been suggested to be a useful diagnostic of the metallicity of the SN progenitor stars. The events in our sample were discovered photometrically by the Pan-STARRS Survey for Transients (PSST), and classified spectroscopically by us. Comparing our sample to 24 literature SNe II, we find that those in low luminosity hosts have significantly weaker Fe II features, with a probability of 10 −4 that the two samples are drawn from the same distribution. Since lowmass galaxies are expected to contain a lower fraction of metals, our findings are consistent with a metallicity dependence for Fe II λ5018, and therefore support the use of this line as a metallicity probe, in agreement with a number of recent works. In addition, we find that the SNe in faint (lowmetallicity) hosts may be more luminous on average than those in the literature sample, suggesting possible physical differences between Type IIP SNe at low and high metallicity. However, accurate determinations of host galaxy extinction will be needed to quantify such an effect.

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Section: Metallicitysupporting

confidence: 93%

Bright Type IIP Supernovae in Low-metallicity Galaxies

Scott

Nicholl

Blanchard

et al. 2019

ApJL

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“…Nugent et al (2006) proposed to use the Hβ λ4861 absorption line, which is stronger than the weaker Fe II absorption line but also present in the early spectrum. The original correlation between the Hβ λ4861 and the Fe II velocities found by Nugent et al (2006) was revisited recently by Poznanski et al (2010) and Takáts & Vinkó (2012). Using 28 spectra over 5 of 40 days after the explosion, Poznanski et al (2010) v H .…”

Section: Photospheric Expansion Velocitiesmentioning

confidence: 97%

“…From an observational point of view, Anderson et al (2016) and Taddia et al (2016), using SNeII from the CSP-I and the intermediate Palomar Transient Factory (iPTF), respectively, showed that the equivalent width of the Fe II (EW Fe ) and the absolute magnitude at maximum peak are correlated in the sense that SNeII with smaller EW Fe tend to be brighter.…”

Section: Sensitivity To Progenitor Metallicity?mentioning

confidence: 99%

A Type II Supernova Hubble Diagram from the CSP-I, SDSS-II, and SNLS Surveys*

Jaeger

González–Gaitán

Hamuy

et al. 2017

ApJ

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The coming era of large photometric wide-field surveys will increase the detection rate of supernovae by orders of magnitude. Such numbers will restrict spectroscopic follow-up in the vast majority of cases, and hence new methods based solely on photometric data must be developed. Here, we construct a complete Hubble diagram of Type II supernovae (SNe II) combining data from three different samples: the Carnegie Supernova Project-I, the Sloan Digital Sky Survey II SN, and the Supernova Legacy Survey. Applying the Photometric Color Method (PCM) to 73 SNe II with a redshift range of 0.01-0.5 and with no spectral information, we derive an intrinsic dispersion of 0.35 mag. A comparison with the Standard Candle Method (SCM) using 61 SNeII is also performed and an intrinsic dispersion in the Hubble diagram of 0.27 mag, i.e., 13% in distance uncertainties, is derived. Due to the lack of good statistics at higher redshifts for both methods, only weak constraints on the cosmological parameters are obtained. However, assuming a flat universe and using the PCM, we derive the universe's matter density: W = -+ 0.32 m 0.21 0.30 providing a new independent evidence for dark energy at the level of two sigma.

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“…In a sample by Taddia et al (2016), the strength of the Fe II λ5018 feature was used to determine the metallicity according to the method of Dessart et al (2014). In Fig.…”

Section: Spectral Propertiesmentioning

confidence: 99%

On the Origin of SN 2016hil—A Type II Supernova in the Remote Outskirts of an Elliptical Host

Irani

Schulze

Gal‐Yam

et al. 2019

ApJ

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Type II supernovae (SNe) stem from the core collapse of massive (> 8 M ) stars. Owing to their short lifespan, we expect a very low rate of such events in elliptical host galaxies, where the starformation rate is low, and which mostly consist of an old stellar population. SN 2016hil (iPTF16hil) is a Type II supernova located in the extreme outskirts of an elliptical galaxy at redshift z = 0.0608 (projected distance 27.2 kpc). It was detected near peak brightness (M r ≈ −17 mag) 9 days after the last nondetection. SN 2016hil has some potentially peculiar properties: while presenting a characteristic spectrum, the event was unusually short lived and declined by ∼ 1.5 mag in < 40 days, following an apparently double-peaked light curve. Its spectra suggest a low metallicity (Z < 0.4 Z ). We place a tentative upper limit on the mass of a potential faint host at log(M/M ) = 7.27 +0.43 −0.24 using deep Keck optical imaging. In light of this, we discuss the possibility of the progenitor forming locally, and other more exotic formation scenarios such as a merger or common-envelope evolution causing a time-delayed explosion. Further observations of the explosion site in the ultraviolet are needed in order to distinguish between the cases. Regardless of the origin of the transient, observing a population of such seemingly hostless Type II SNe could have many uses, including an estimate the number of faint galaxies in a given volume, and tests of the prediction of a time-delayed population of core-collapse SNe in locations otherwise unfavorable for the detection of such events.

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Metallicity from Type II supernovae from the (i)PTF

Cited by 25 publications

References 24 publications

Bright Type IIP Supernovae in Low-metallicity Galaxies

Bright Type IIP Supernovae in Low-metallicity Galaxies

A Type II Supernova Hubble Diagram from the CSP-I, SDSS-II, and SNLS Surveys*

On the Origin of SN 2016hil—A Type II Supernova in the Remote Outskirts of an Elliptical Host

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