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dc.creatorTaddia, F.en_US
dc.creatorSollerman, J.en_US
dc.creatorLeloudas, G.en_US
dc.creatorStritzinger, M. D.en_US
dc.creatorValenti, S.en_US
dc.creatorGalbany, L.en_US
dc.creatorKessler, R.en_US
dc.creatorSchneider, D. P.en_US
dc.creatorWheeler, J. C.en_US
dc.date.accessioned2016-04-22T19:49:02Z
dc.date.available2016-04-22T19:49:02Z
dc.date.issued2015-02en
dc.identifierdoi:10.15781/T2MN6G
dc.identifier.citationTaddia, Francesco, Jesper Sollerman, G. Leloudas, M. D. Stritzinger, S. Valenti, L. Galbany, R. Kessler, D. P. Schneider, and J. C. Wheeler. >Early-time light curves of Type Ib/c supernovae from the SDSS-II Supernova Survey.> Astronomy & Astrophysics, Vol. 574 (Feb., 2015): A60.en_US
dc.identifier.issn0004-6361en_US
dc.identifier.urihttp://hdl.handle.net/2152/34574
dc.description.abstractContext. Type Ib/c supernovae (SNe Ib/c) have been investigated in several single-object studies; however, there is still a paucity of works concerning larger, homogeneous samples of these hydrogen-poor transients, in particular regarding the premaximum phase of their light curves. Aims. In this paper we present and analyze the early-time optical light curves (LCs, ugriz) of 20 SNe Ib/c from the Sloan Digital Sky Survey (SDSS) SN survey II, aiming to study their observational and physical properties, as well as to derive their progenitor parameters. Methods. High-cadence, multiband LCs are fitted with a functional model and the best-fit parameters are compared among the SN types. Bolometric LCs (BLCs) are constructed for the entire sample. We also computed the black-body (BB) temperature (T-BB) and photospheric radius (R-ph) evolution for each SN via BB fits on the spectral energy distributions. In addition, the bolometric properties are compared to both hydrodynamical and analytical model expectations. Results. Complementing our sample with literature data, we find that SNe Ic and Ic-BL (broad-line) have shorter rise times than those of SNe Ib and IIb. The decline rate parameter, Delta m(15), is similar among the different subtypes. SNe Ic appear brighter and bluer than SNe Ib, but this difference vanishes if we consider host galaxy extinction corrections based on colors. Templates for SN Ib/c LCs are presented. Our SNe have typical T-BB of similar to 10000 K at the peak and R-ph of similar to 10(15) cm. Analysis of the BLCs of SNe Ib and Ic gives typical ejecta masses M-ej approximate to 3.6-5.7 M-circle dot, energies E-K approximate to 1.5-1.7x10(51) erg, and M(Ni-56) approximate to 0.3 M-circle dot. Higher values for E-K and M(Ni-56) are estimated for SNe Ic-BL (M-ej approximate to 5.4 M-circle dot, E-K 10.7x10(51) erg, M(Ni-56) approximate to 1.1 M-circle dot). For the majority of SNe Ic and Ic-BL, we can put strong limits (<2-4 days) on the duration of the expected early-time plateau. Less stringent limits can be placed on the duration of the plateau for the sample of SNe Ib. In the single case of SN Ib 20061c, a >5.9 days plateau seems to be detected. The rising part of the BLCs is reproduced by power laws with index <2. For two events (SN 2005hm and SN 2007qx), we find signatures of a possible shock break-out cooling tail. Conclusions. Based on the limits for the plateau length and on the slow rise of the BLCs, we find that in most of our SNe Ic and Ic-BL the Ni-56 is mixed out to the outer layers, suggesting that SN Ic progenitors are de facto helium poor. The derived progenitor parameters (Ni-56, E-K, M-ej) are consistent with previous works.en_US
dc.description.sponsorshipSwedish Research Councilen_US
dc.description.sponsorshipInstrument Center for Danish Astrophysics (IDA)en_US
dc.description.sponsorshipDanish Agency for Science and Technology and Innovationen_US
dc.description.sponsorshipMinistry of Economy, Development, and Tourism's Millennium Science Initiative IC12009en_US
dc.description.sponsorshipCONICYT through FONDECYT 3140566en_US
dc.description.sponsorshipDanish National Research Foundationen_US
dc.description.sponsorshipAlfred P. Sloan Foundationen_US
dc.description.sponsorshipNational Science Foundationen_US
dc.description.sponsorshipUS Department of Energyen_US
dc.description.sponsorshipNational Aeronautics and Space Administrationen_US
dc.description.sponsorshipJapanese Monbukagakushoen_US
dc.description.sponsorshipMax Planck Societyen_US
dc.description.sponsorshipHigher Education Funding Council for Englanden_US
dc.description.sponsorshipAmerican Museum of Natural Historyen_US
dc.description.sponsorshipAstrophysical Institute Potsdamen_US
dc.description.sponsorshipUniversity of Baselen_US
dc.description.sponsorshipCambridge Universityen_US
dc.description.sponsorshipCase Western Reserve Universityen_US
dc.description.sponsorshipUniversity of Chicagoen_US
dc.description.sponsorshipDrexel Universityen_US
dc.description.sponsorshipFermilaben_US
dc.description.sponsorshipInstitute for Advanced Studyen_US
dc.description.sponsorshipJapan Participation Groupen_US
dc.description.sponsorshipJohns Hopkins Universityen_US
dc.description.sponsorshipJoint Institute for Nuclear Astrophysicsen_US
dc.description.sponsorshipKavli Institute for Particle Astrophysics and Cosmologyen_US
dc.description.sponsorshipKorean Scientist Groupen_US
dc.description.sponsorshipChinese Academy of Sciences (LAMOST)en_US
dc.description.sponsorshipLos Alamos National Laboratoryen_US
dc.description.sponsorshipMax-Planck-Institute for Astronomy (MPIA)en_US
dc.description.sponsorshipMax-Planck-Institute for Astrophysics (MPA)en_US
dc.description.sponsorshipNew Mexico State Universityen_US
dc.description.sponsorshipOhio State Universityen_US
dc.description.sponsorshipUniversity of Pittsburghen_US
dc.description.sponsorshipUniversity of Portsmouthen_US
dc.description.sponsorshipPrinceton Universityen_US
dc.description.sponsorshipUnited States Naval Observatoryen_US
dc.description.sponsorshipUniversity of Washingtonen_US
dc.language.isoEnglishen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectsupernovae: generalen_US
dc.subjectdigital sky surveyen_US
dc.subjectcore-collapse supernovaeen_US
dc.subjectgamma-ray bursten_US
dc.subjectabsolute-magnitude distributionsen_US
dc.subjectia supernovaeen_US
dc.subjectshock breakouten_US
dc.subjecticen_US
dc.subjectsupernovaen_US
dc.subjectx-rayen_US
dc.subjectsupergiant progenitoren_US
dc.subjectbinary progenitoren_US
dc.subjectastronomy & astrophysicsen_US
dc.titleEarly-Time Light Curves Of Type Ib/c Supernovae From The SDSS-II Supernova Surveyen_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.doi10.1051/0004-6361/201423915en_US
dc.contributor.utaustinauthorWheeler, J. C.en_US
dc.relation.ispartofserialAstronomy & Astrophysicsen_US


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