SIMBAD references

2018ApJ...854...24K - Astrophys. J., 854, 24-24 (2018/February-2)

Environmental dependence of Type Ia supernova luminosities from a sample without a local-global difference in host star formation.

KIM Y.-L., SMITH M., SULLIVAN M. and LEE Y.-W.

Abstract (from CDS):

It is established that there is a dependence of the luminosity of type Ia supernovae (SNe Ia) on environment: SNe Ia in young, star-forming, metal-poor stellar populations appear fainter after light-curve shape corrections than those in older, passive, metal-rich environments. This is accounted for in cosmological studies using a global property of the SN host galaxy, typically the host galaxy stellar mass. However, recent low-redshift studies suggest that this effect manifests itself most strongly when using the local star formation rate (SFR) at the SN location, rather than the global SFR or the stellar mass of the host galaxy. At high-redshift, such local SFRs are difficult to determine; here, we show that an equivalent local correction can be made by restricting the SN Ia sample in globally star-forming host galaxies to a low-mass host galaxy subset (<=1010 M). Comparing this sample of SNe Ia (in locally star-forming environments) to those in locally passive host galaxies, we find that SNe Ia in locally star-forming environments are 0.081 ± 0.018 mag fainter (4.5σ), consistent with the result reported by Rigault et al., but our conclusion is based on a sample ∼5 times larger over a wider redshift range. This is a larger difference than when splitting the SN Ia sample based on global host galaxy SFR or host galaxy stellar mass. This method can be used in ongoing and future high-redshift SN surveys, where local SN Ia environments are difficult to determine.

Abstract Copyright: © 2018. The American Astronomical Society. All rights reserved.

Journal keyword(s): cosmology: observations - distance scale - supernovae: general

VizieR on-line data: <Available at CDS (J/ApJ/854/24): table2.dat table3.dat>

Simbad objects: 699

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2020.10.28-07:16:04

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