Nearby supernova host galaxies from the CALIFA Survey

I. Sample, data analysis, and correlation to star-forming regions^⋆

¹ CENTRA – Centro Multidisciplinar de Astrofísica, Instituto Superior Técnico, Av. Rovisco Pais 1, 1049-001 Lisbon, Portugal
² Millennium Institute of Astrophysics, Universidad de Chile, Casilla 36-D, Santiago, Chile
³ Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
⁴ European Southern Observatory, Alonso de Cordova 3107 Casilla 19001 – Vitacura-Santiago, Chile
⁵ GEPI, Observatoire de Paris, UMR 8111, CNRS, Université Paris Diderot, 5 place Jules Janssen, 92190 Meudon, France
⁶ Instituto de Astrofśica de Andalucía (CSIC), Glorieta de la Astronomía s/n, Aptdo. 3004, 18080- Granada, Spain
⁷ Instituto de Cosmologia, Relatividade e Astrofísica – ICRA, Centro Brasileiro de Pesquisas Físicas, Rua Dr. Xavier Sigaud 150, CEP 22290-180, Rio de Janeiro, RJ, Brazil
⁸ Instituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, Mexico, D.F
⁹ Department of Physics and Astronomy, University of Pittsburgh, Allen Hall, 3941 O’Hara St, Pittsburgh, PA 15260, USA
¹⁰ Instituto de Astrofísica de Canarias (IAC), 38205 La Laguna, Tenerife, Spain
¹¹ Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain
¹² Sydney Institute for Astronomy, School of Physics A28, University of Sydney, NSW 2006, Australia
¹³ Centro de Astrofísica and Faculdade de Ciencias, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal
¹⁴ Max-Planck-Institut für Astronomie, Konigstuhl 17, 69117 Heidelberg, Germany
¹⁵ Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia
¹⁶ Department of Physics and Astronomy, Macquarie University, NSW 2109, Australia
¹⁷ School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, KY16 9SS, UK (SUPA)
¹⁸ CEI Campus Moncloa, UCM-UPM, Departamento de Astrofísica y CC. de la Atmósfera, Facultad de CC. Físicas, Universidad Complutense de Madrid, Avda. Complutense s/n, 28040 Madrid, Spain
¹⁹ Departamento de Investigación Básica, CIEMAT, Avda. Complutense 40, 28040 Madrid, Spain
²⁰ Centro de Estudios de la Física del Cosmos de Aragón, 44001 Teruel, Spain
²¹ Visiting Scientist: Departamento de Física Teorica, Facultad de Ciencias, Universidad de Zaragoza, Spain
²² Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis E. Erro 1, 72840 Tonantzintla, Puebla, Mexico

Received: 30 July 2014
Accepted: 4 September 2014

Abstract

We use optical integral field spectroscopy (IFS) of nearby supernova (SN) host galaxies (0.005 <z< 0.03) provided by the Calar Alto Legacy Integral Field Area (CALIFA) Survey with the goal of finding correlations in the environmental parameters at the location of different SN types. In this first study of a series we focus on the properties related with star formation (SF). We recover the sequence in association of different SN types to the star-forming regions by using several indicators of the ongoing and recent SF related to both the ionized gas and the stellar populations. While the total ongoing SF is on average the same for the three SN types, SNe Ibc/IIb tend to occur closer to star-forming regions and in higher SF density locations than SNe II and SNe Ia; the latter shows the weakest correlation. SNe Ia host galaxies have masses that are on average ~0.3−0.8 dex higher than those of the core collapse (CC) SNe hosts because the SNe Ia hosts contain alarger fraction of old stellar populations. Using the recent SN Ia delay-time distribution and the SFHs of the galaxies, we show that the SN Ia hosts in our sample are expected to produce twice as many SNe Ia as the CC SN hosts. Since both types occur in hosts with a similar SF rate and hence similar CC SN rate, this can explain the mass difference between the SN Ia and CC SN hosts, and reinforces the finding that at least part of the SNe Ia originate from very old progenitors. By comparing the mean SFH of the eight least massive galaxies with that of the massive SF SN Ia hosts, we find that the low-mass galaxies formed their stars during a longer time (0.65%, 24.46%, and 74.89% in the intervals 0–0.42 Gyr, 0.42–2.4 Gyr, and >2.4 Gyr, respectively) than the massive SN Ia hosts (0.04%, 2.01%, and 97.95% in these intervals). We estimate that the low-mass galaxies produce ten times fewer SNe Ia and three times fewer CC SNe than the high-mass group. Therefore the ratio between the number of CC SNe and SNe Ia is expected to increase with decreasing galaxy mass. CC SNe tend to explode at positions with younger stellar populations than the galaxy average, but the galaxy properties at SNe Ia locations are one average the same as the global galaxy properties.