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Elemental gas-phase abundances of intermediate redshift type Ia supernova star-forming host galaxies

AutorMoreno-Raya, M.E.; Galbany, L.; López-Sánchez, R.; Mollá, M.; González-Gaitán, S.; Vílchez Medina, José Manuel ; Carnero, A.
Palabras clavelTechniques: spectroscopic
Supernovae: genera
Galaxies: abundances
Methods: data analysis
ISM: abundances
HII regions
Fecha de publicación2018
EditorOxford University Press
CitaciónMonthly Notices of the Royal Astronomical Society 476(1): 307- 322 (2018)
ResumenThe maximum luminosity of type Ia supernovae (SNe Ia) depends on the oxygen abundance of the regions of the host galaxies, where they explode. This metallicity dependence reduces the dispersion in the Hubble diagram (HD) when included with the traditional two-parameter calibration of SN Ia light-curve parameters and absolute magnitude. In this work, we use empirical calibrations to carefully estimate the oxygen abundance of galaxies hosting SNe Ia from the SDSS-II/SN (Sloan Digital Sky Survey-II Supernova) survey at intermediate redshift by measuring their emission-line intensities. We also derive electronic temperature with the direct method for a small fraction of objects for consistency. We find a trend of decreasing oxygen abundance with increasing redshift for the most massive galaxies. Moreover, we study the dependence of the HD residuals (HR) with galaxy oxygen abundance obtaining a correlation in line with those found in other works. In particular, the HR versus oxygen abundance shows a slope of -0.186± 0.123 mag dex (1.52σ) in good agreement with theoretical expectations. This implies smaller distance modulii after corrections for SNe Ia in metal-rich galaxies. Based on our previous results on local SNe Ia, we propose this dependence to be due to the lower luminosity of the SNe Ia produced in more metal-rich environments.© 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
Identificadoresdoi: 10.1093/mnras/sty185
issn: 1365-2966
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