1. SN 2012fr: Ultraviolet, Optical, and Near-Infrared Light Curves of a Type Ia Supernova Observed Within a Day of Explosion
- Author
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David Rabinowitz, C. Baltay, Wendy L. Freedman, Peter Nugent, Richard Scalzo, M. Childress, Damien Turpin, Peter Hoeflich, Christopher Cain, Nicholas B. Suntzeff, Nidia Morrell, Emma S. Walker, S. Castellon, Brian P. Schmidt, E. Conseil, Carlos Contreras, Alain Klotz, Maximilian Stritzinger, Gastón Folatelli, Brad E. Tucker, Christopher R. Burns, Eric Hsiao, Peter J. Brown, Kevin Krisciunas, C. Corco, Benjamin J. Shappee, S. Parker, Anthony L. Piro, J. Serón, S. E. Persson, Mario Hamuy, Mark M. Phillips, C. Gonzalez, Abdo Campillay, E. Baron, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie ( IRAP ), and Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS )
- Subjects
Infrared ,DELAY-TIME DISTRIBUTION ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Ciencias Físicas ,CHEMICAL EVOLUTION ,Astrophysics ,medicine.disease_cause ,01 natural sciences ,Atomic ,Physical Chemistry ,purl.org/becyt/ford/1 [https] ,Particle and Plasma Physics ,010303 astronomy & astrophysics ,Ultraviolet radiation ,Physics ,astro-ph.HE ,High Energy Astrophysical Phenomena (astro-ph.HE) ,supernovae: individual (SN 2012fr) ,Visible radiation ,Supernova ,IMPROVED DISTANCES ,Astrophysics - High Energy Astrophysical Phenomena ,Astronomical and Space Sciences ,CIENCIAS NATURALES Y EXACTAS ,Physical Chemistry (incl. Structural) ,INDIVIDUAL (SN 2012FR) [SUPERNOVAE] ,MAXIMUM BRIGHTNESS ,FOS: Physical sciences ,Astronomy & Astrophysics ,NEBULAR-PHASE SPECTRA ,GENERAL [SUPERNOVAE] ,supernovae: general ,ABUNDANCE RATIOS ,individual [supernovae] ,0103 physical sciences ,medicine ,Nuclear ,WHITE-DWARFS ,supernovae: individual ,Near infrared light ,010308 nuclear & particles physics ,STANDARD STARS ,Molecular ,Astronomy and Astrophysics ,purl.org/becyt/ford/1.3 [https] ,Astronomía ,Space and Planetary Science ,DIGITAL SKY SURVEY ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Near infrared radiation ,Ultraviolet ,HUBBLE CONSTANT - Abstract
We present detailed ultraviolet, optical, and near-infrared light curves of the Type Ia supernova (SN) 2012fr, which exploded in the Fornax cluster member NGC 1365. These precise high-cadence light curves provide a dense coverage of the flux evolution from −12 to +140 days with respect to the epoch of B-band maximum (tBmax). Supplementary imaging at the earliest epochs reveals an initial slow and nearly linear rise in luminosity with a duration of ∼2.5 days, followed by a faster rising phase that is well reproduced by an explosion model with a moderate amount of 56Ni mixing in the ejecta. From our analysis of the light curves, we conclude that: (i) the explosion occurred 1800 Å) luminosity was 16.5 ± 0.6 days, (iii) the supernova suffered little or no host-galaxy dust reddening, (iv) the peak luminosity in both the optical and near-infrared was consistent with the bright end of normal Type Ia diversity, and (v) 0.60 ± 0.15 M⊙ of 56Ni was synthesized in the explosion. Despite its normal luminosity, SN 2012fr displayed unusually prevalent high-velocity Ca II and Si II absorption features, and a nearly constant photospheric velocity of the Si II λ6355 line at ∼12,000 km s-1 that began ∼5 days before tBmax. We also highlight some of the other peculiarities in the early phase photometry and the spectral evolution. SN 2012fr also adds to a growing number of Type Ia supernovae that are hosted by galaxies with direct Cepheid distance measurements., Facultad de Ciencias Astronómicas y Geofísicas, Instituto de Astrofísica de La Plata
- Published
- 2018
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