Nearby supernova host galaxies from the CALIFA Survey



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Galbany, L. and Stanishev, V. and Mourão, A. M. and Rodrigues, M. and Flores, H. and García Benito, R. and Mast, D. and Mendoza, M. A. and Sánchez, S. F. and Badenes, C. and Barrera Ballesteros, J. and Bland-Hawthorn, J. and Falcón Barroso, J. and García Lorenzo, B. and Gomes, J. M. and González Delgado, R. M. and Kehrig, C. and Lyubenova, M. and López Sánchez, A. R. and Lorenzo Cáceres, A. de and Marino, Raffaella Anna and Meidt, S. and Mollá, M. and Papaderos, P. and Pérez Torres, M. A. and Rosales Ortega, F. F. and van de Ven, G. (2014) Nearby supernova host galaxies from the CALIFA Survey. Astronomy & Astrophysics, 572 . ISSN 0004-6361

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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 similar to 0.3-0.8 dex higher than those of the core collapse (CC) SNe hosts because the SNe Ia hosts contain a larger 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.

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© ESO 2014. We acknowledge the anonymous referee for her/his helpful comments and suggestions. This work was partly funded by Fundaçao para a Ciencia e a Tecnologia (FCT, Portugal) with the research grant PTDC/CTE-AST/112582/2009. V.S. acknowledges financial support from Fundaçao para a Ciencia e a Tecnologia (FCT) under program Ciencia 2008. Support for L.G. is partially provided by FCT, by CONICYT through FONDECYT grant 3140566, and from the Ministry of Economy, Development, and Tourism's Millennium Science Initiative through grant IC12009, awarded to The Millennium Institute of Astrophysics (MAS). L.G. thanks Damian Mast, Luzma Montoya, Ana Guijarro and Chandreyee Sengupta for the IFS observations of CALIFA galaxies at Calar Alto Observatory. J.B.-B. and B.G.-L. acknowledge the support from the Plan Nacional de I+D+i (PNAYA) funding programme (AYA2012-39408-C02-02) of the Spanish Ministry of Economy and Competitiveness (MINECO). J.F.-B. acknowledges support from the Ramón y Cajal Program, grants AYA2010-21322-C03-02 from the Spanish Ministry of Economy and Competitiveness (MINECO). J.F.-B. also acknowledges support from the FP7 Marie Curie Actions of the European Commission, via the Initial Training Network DAGAL under REA grant agreement number 289313. J.M.G. acknowledges support from the FCT through the Fellowship SFRH/BPD/66958/2009 and the research grant PTDC/FIS-AST/3214/2012. R.G.D. and R.G.B. acknowledge support from the Spanish Ministerio de Economía y Competitividad, through projects AYA2010-15081. R.A.M. is funded by the Spanish program of International Campus of Excellence Moncloa (CEI). This study makes use of the data provided by the Calar Alto Legacy Integral Field Area (CALIFA) survey ( CALIFA is the first legacy survey being performed at Calar Alto. The CALIFA collaboration would like to thank the IAA-CSIC and MPIA-MPG as major partners of the observatory, and CAHA itself, for the unique access to telescope time and support in manpower and infrastructures. The CALIFA collaboration also thanks also the CAHA staff for the dedication to this project. Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut fur Astronomie and the Instituto de Astrofísica de Andalucía (CSIC). The STARLIGHT project is supported by the Brazilian agencies CNPq, CAPES and FAPESP and by the France-Brazil CAPES/Cofecub program. This research has made use of the Asiago Supernova Catalog, the SIMBAD database, operated at CDS, Strasbourg, France, the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration, IAU Circulars presented by the Central Bureau for Astronomical Telegrams, and data products from SDSS and SDSS-II surveys.

Uncontrolled Keywords:Core-collapse supernovae; Integral field spectroscopy; Digital sky survey; Delay-time distribution; Star-forming galaxies: Potsdam multiaperture spectrophotometer; Mass-metallicity relation; Giant branch stars; Wolf-rayet stars; H-alpha emission
Subjects:Sciences > Physics > Astrophysics
Sciences > Physics > Astronomy
Sciences > Physics > Atmospheric physics
ID Code:28488
Deposited On:02 Mar 2015 12:42
Last Modified:10 Dec 2018 15:05

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