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|Title:||Supernova rates from the SUDARE VST-OmegaCAM search. I. Rates per unit volume||Authors:||CAPPELLARO, Enrico
BOTTICELLA, MARIA TERESA
De Cicco, D.
DELLA VALLE, Massimo
NAPOLITANO, NICOLA ROSARIO
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||584||First Page:||1||Abstract:||<BR /> Aims: We describe the observing strategy, data reduction tools, and early results of a supernova (SN) search project, named SUDARE, conducted with the ESO VST telescope, which is aimed at measuring the rate of the different types of SNe in the redshift range 0.2 < z < 0.8. <BR /> Methods: The search was performed in two of the best studied extragalactic fields, CDFS and COSMOS, for which a wealth of ancillary data are available in the literature or in public archives. We developed a pipeline for the data reduction and rapid identification of transients. As a result of the frequent monitoring of the two selected fields, we obtained light curve and colour information for the transients sources that were used to select and classify SNe by means of an especially developed tool. To accurately characterise the surveyed stellar population, we exploit public data and our own observations to measure the galaxy photometric redshifts and rest frame colours. <BR /> Results: We obtained a final sample of 117 SNe, most of which are SN Ia (57%) with the remaining ones being core collapse events, of which 44% are type II, 22% type IIn and 34% type Ib/c. To link the transients, we built a catalogue of ~1.3 × 10<SUP>5</SUP> galaxies in the redshift range 0 < z ≤ 1, with a limiting magnitude K<SUB>AB</SUB> = 23.5 mag. We measured the SN rate per unit volume for SN Ia and core collapse SNe in different bins of redshifts. The values are consistent with other measurements from the literature. <BR /> Conclusions: The dispersion of the rate measurements for SNe-Ia is comparable to the scatter of the theoretical tracks for single degenerate (SD) and double degenerate (DD) binary systems models, therefore it is not possible to disentangle among the two different progenitor scenarios. However, among the three tested models (SD and the two flavours of DD that either have a steep DDC or a wide DDW delay time distribution), the SD appears to give a better fit across the whole redshift range, whereas the DDC better matches the steep rise up to redshift ~1.2. The DDW instead appears to be less favoured. Unlike recent claims, the core collapse SN rate is fully consistent with the prediction that is based on recent estimates of star formation history and standard progenitor mass range. <P />Based on observations made with ESO telescopes at the Paranal Observatory under programme ID 088.D-4006, 088.D-4007, 089.D-0244, 089.D-0248, 090.D-0078, 090.D-0079, 088.D-4013, 089.D-0250, 090.D-0081.Appendix A is available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201526712/olm">http://www.aanda.org||Acknowledgments:||We thank the referee, Steve Rodney, for useful comments and suggestions. We also thank G. Brammer for helping with galaxy photometric redshifts. We acknowledge the support of grant ASI n.I/023/12/0 “Attivitá relative alla fase B2/C per la missione Euclid”, MIUR PRIN 2010-2011, “The dark Universe and the cosmic evolution of baryons: from current surveys to Euclid” and PRIN-INAF “Galaxy Evolution With The VLT Survey Telescope (VST)” (PI A. Grado). G.P. acknowledge the support of Proyecto Regular FONDECYT 1140352 and of the Ministry of Economy, Development, and Tourism’s Millennium Science Initiative through grant IC 12009, awarded to The Millennium Institute of Astrophysics, MAS. M.V. acknowledges support from the Square Kilometre Array South Africa project, the South African National Research Foundation and Department of Science and Technology (DST/CON 0134/2014), the European Commission Research Executive Agency (FP7-SPACE-2013-1 GA 607254) and the Italian Ministry for Foreign Affairs and International Cooperation (PGR GA ZA14GR02).||URI:||http://hdl.handle.net/20.500.12386/23581||URL:||https://www.aanda.org/articles/aa/abs/2015/12/aa26712-15/aa26712-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201526712||Bibcode ADS:||2015A&A...584A..62C||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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