Nearby supernova host galaxies from the CALIFA survey: II. Supernova environmental metallicity

• Autores: Galbany, Lluís; Stanishev, V.; Mourão, A. M.; Rodrigues, M.; Flores, H.; Walcher, C. J.; Sánchez, S. F.; García Benito, Rubén; Mast, Damian; Badenes, C.; González Delgado, R. M.; Kehrig, C.; Lyubenova, M.; Marino, R. A.; Mollá, M.; Meidt, S.; Pérez, E.; van de Ven, G.; Vílchez, J. M.
• Año de publicación: 2016
• Idioma: inglés
• Tipo de recurso: artículo
• Materia: GALAXIES: ABUNDANCES; GALAXIES: GENERAL; SUPERNOVAE: GENERAL
• Institución: Consejo Nacional de Investigaciones Científicas y Técnicas

The metallicity of a supernova progenitor, together with its mass, is one of the main parameters that can rule the progenitor's fate. We present the second study of nearby supernova (SN) host galaxies (0.005 10 dex) by targeted searches. We neither found evidence that the metallicity at the SN location differs from the average metallicity at the galactocentric distance of the SNe. By extending our SN sample with published metallicities at the SN location, we are able to study the metallicity distributions for all SN subtypes split into SN discovered in targeted and untargeted searches. We confirm a bias toward higher host masses and metallicities in the targeted searches. By combining data from targeted and untargeted searches, we found a sequence from higher to lower local metallicity: SN Ia, Ic, and II show the highest metallicity, which is significantly higher than those of SN Ib, IIb, and Ic-BL. Our results support the scenario according to which SN Ib result from binary progenitors. Additionally, at least part of the SN Ic are the result of single massive stars that were stripped of their outer layers by metallicity-driven winds. We studied several proxies of the local metallicity that are frequently used in the literature and found that the total host metallicity allows estimating the metallicity at the SN location with an accuracy better than 0.08 dex and very small bias. In addition, weak AGNs that cannot be seen in the total spectrum may weakly bias (by 0.04 dex) the metallicity estimate that is derived from the galaxy-integrated spectrum.
Fil: Galbany, Lluís. Universidad de Chile; Chile. Millennium Institute of Astrophysics; Chile
Fil: Stanishev, V.. Universidade Nova de Lisboa; Portugal
Fil: Mourão, A. M.. Universidade Nova de Lisboa; Portugal
Fil: Rodrigues, M.. European Southern Observatory; Chile. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Flores, H.. Centre National de la Recherche Scientifique. Observatoire de Paris; Francia
Fil: Walcher, C. J.. Gobierno de la República Federal de Alemania. Max Planck Institut für Astrophysik; Alemania
Fil: Sánchez, S. F.. Universidad Nacional Autonoma de Mexico. Instituto de Astronomia; México
Fil: García Benito, Rubén. Instituto de Astrofísica de Andalucía; España
Fil: Mast, Damian. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - Córdoba; Argentina. Centro Brasileiro de Pesquisas Físicas; Brasil
Fil: Badenes, C.. University of Pittsburgh at Johnstown; Estados Unidos
Fil: González Delgado, R. M.. Instituto de Astrofísica de Andalucía; España
Fil: Kehrig, C.. Instituto de Astrofísica de Andalucía; España
Fil: Lyubenova, M.. University of Groningen; Países Bajos
Fil: Marino, R. A.. Eidgenossische Technische Hochschule zurich (eth Zurich); . Universidad Complutense de Madrid; España
Fil: Mollá, M.. Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas; España
Fil: Meidt, S.. Max-Planck-Institut für Astronomie; Alemania
Fil: Pérez, E.. Instituto de Astrofsica de Andalucía; España
Fil: van de Ven, G.. Max-Planck-Institut für Astronomie; Alemania
Fil: Vílchez, J. M.. Instituto de Astrofsica de Andalucía; España