PERSISTENT C II ABSORPTION IN THE NORMAL TYPE Ia SUPERNOVA 2002fk

We present well-sampled UBVRIJHK photometry of SN 2002fk starting 12 days before maximum light through 122 days after peak brightness, along with a series of 15 optical spectra from -4 to +95 days since maximum. Our observations show the presence of C II lines in the early-time spectra of SN 2002fk,...

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Bibliographic Details
Published in:The Astrophysical journal 2014-07, Vol.789 (1), p.1-22
Main Authors: Cartier, Regis, HAMUY, MARIO, Pignata, Giuliano, ster, Francisco, Zelaya, Paula, FOLATELLI, GASTON, Phillips, Mark M, Morrell, Nidia, Krisciunas, Kevin, SUNTZEFF, NICHOLAS B
Format: Article
Language:English
Subjects:
ABSORPTION
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
AUGMENTATION
BRIGHTNESS
Cepheid variables
COSMOLOGY
DISTANCE
EXPLOSIONS
GALAXIES
Ignition
PHOTOMETRY
SPECTRA
SUPERNOVAE
Supernovas
VELOCITY
Viewing
VISIBLE RADIATION
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Summary:We present well-sampled UBVRIJHK photometry of SN 2002fk starting 12 days before maximum light through 122 days after peak brightness, along with a series of 15 optical spectra from -4 to +95 days since maximum. Our observations show the presence of C II lines in the early-time spectra of SN 2002fk, expanding at 11,000 km super(s-1) and persisting until 8 days past maximum light with a velocity of ~9000 km s super(-1). SN 2002fk is characterized by a small velocity gradient of [upsilon] sub(Si II) = 26 km s super(-1) day super(-1), possibly caused by an off-center explosion with the ignition region oriented toward the observer. The connection between the viewing angle of an off-center explosion and the presence of C II in the early-time spectrum suggests that the observation of C II could be also due to a viewing angle effect. Adopting the Cepheid distance to NGC 1309 we provide the first H sub(0) value based on nearinfrared (near-IR) measurements of a Type Ia supernova (SN) between 63.0 + or - 0.8 (+ or - 3.4 systematic) and 66.7 + or - 1.0 (+ or - 3.5 systematic) km s super(-1) Mpc super(-1), depending on the absolutemagnitude/decline rate relationship adopted. It appears that the near-IR yields somewhat lower (6%-9%) H sub(0) values than the optical. It is essential to further examine this issue by (1) expanding the sample of high-quality near-IR light curves of SNe in the Hubble flow, and (2) increasing the number of nearby SNe with near-IR SN light curves and precise Cepheid distances, which affords the promise to deliver a more precise determination of H sub(0).
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/789/1/89