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Publication Details
AFRICAN RESEARCH NEXUS
SHINING A SPOTLIGHT ON AFRICAN RESEARCH
earth and planetary sciences
SN 2006oz: Rise of a super-luminous supernova observed by the SDSS-II SN Survey
Astronomy and Astrophysics, Volume 541, Article A129, Year 2012
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Description
Context. A new class of super-luminous transients has recently been identified. These objects reach absolute luminosities of Mu < -21, lack hydrogen in their spectra, and are exclusively discovered by non-targeted surveys because they are associated with very faint galaxies. Aims. We aim to contribute to a better understanding of these objects by studying SN 2006oz, a newly-recognized member of this class. Methods. We present multi-color light curves of SN 2006oz from the SDSS-II SN Survey that cover its rise time, as well as an optical spectrum that shows that the explosion occurred at z ∼ 0.376. We fitted black-body functions to estimate the temperature and radius evolution of the photosphere and used the parametrized code SYNOW to model the spectrum. We constructed a bolometric light curve and compared it with explosion models. In addition, we conducted a deep search for the host galaxy with the 10 m GTC telescope. Results. The very early light curves show a dip in the g- and r-bands and a possible initial cooling phase in the u-band before rising to maximum light. The bolometric light curve shows a precursor plateau with a duration of 6-10 days in the rest-frame. A lower limit of Mu < - 21.5 can be placed on the absolute peak luminosity of the SN, while the rise time is constrained to be at least 29 days. During our observations, the emitting sphere doubled its radius to ∼2 × 1015 cm, while the temperature remained hot at ∼15 000 K. As for other similar SNe, the spectrum is best modeled with elements including O II and Mg II, while we tentatively suggest that Fe III might be present. The host galaxy is detected in gri with 25.74 ± 0.19, 24.43 ± 0.06, and 24.14 ± 0.12, respectively. It is a faint dwarf galaxy with Mg = -16.9. Conclusions. We suggest that the precursor plateau might be related to a recombination wave in a circumstellar medium (CSM) and discuss whether this is a common property of all similar explosions. The subsequent rise can be equally well described by input from a magnetar or by ejecta-CSM interaction, but the models are not well constrained owing to the lack of post-maximum observations, and CSM interaction has difficulties accounting for the precursor plateau self-consistently. Radioactive decay is less likely to be the mechanism that powers the luminosity. The host is a moderately young and star-forming, but not a starburst, galaxy. © 2012 ESO.
Authors & Co-Authors
Leloudas, Giorgos
Denmark, Copenhagen
Niels Bohr Institutet
Sweden, Stockholm
Stockholms Universitet
Chatzopoulos, Emmanouil
United States, Austin
The University of Texas at Austin
Dilday, Benjamin
United States, Santa Barbara
Las Cumbres Observatory Global Telescope Network, Inc
United States, Santa Barbara
University of California, Santa Barbara
Gorosabel, Javier
Spain, Granada
Instituto de Astrofísica de Andalucía - Csic
Vinkó, József
United States, Austin
The University of Texas at Austin
Hungary, Szeged
Szegedi Tudományegyetem Szte
Gallazzi, Anna R.
Denmark, Copenhagen
Niels Bohr Institutet
Wheeler, J. Craig
United States, Austin
The University of Texas at Austin
Bassett, Bruce A.C.C.
South Africa, Muizenberg
African Institute for Mathematical Sciences
South Africa, Cape Town
South African Astronomical Observatory
South Africa, Cape Town
University of Cape Town
Fischer, John A.
United States, Philadelphia
University of Pennsylvania
Frieman, Joshua A.
United States, Chicago
The University of Chicago
United States, Chicago
The Kavli Institute for Cosmological Physics
United States, Batavia
Fermi National Accelerator Laboratory
Fynbo, Johan Peter Uldall
Denmark, Copenhagen
Niels Bohr Institutet
Goobar, Ariel M.
Sweden, Stockholm
Stockholms Universitet
Jelínek, Martin
Spain, Granada
Instituto de Astrofísica de Andalucía - Csic
Malesani, Daniele B.
Denmark, Copenhagen
Niels Bohr Institutet
Nichol, Robert C.
United Kingdom, Portsmouth
University of Portsmouth
Nordin, Jakob
United States, Berkeley
Space Sciences Laboratory
United States, Berkeley
Lawrence Berkeley National Laboratory
Östman, Linda
Spain, Cerdanyola Del Valles
Universitat Autònoma de Barcelona
Sako, Masao
United States, Philadelphia
University of Pennsylvania
P. Schneider, Donald P.
United States, University Park
Pennsylvania State University
Smith, Matthew W.L.
South Africa, Muizenberg
African Institute for Mathematical Sciences
South Africa, Cape Town
University of Cape Town
Sollerman, Jesper
Sweden, Stockholm
Stockholms Universitet
Stritzinger, Maximilian D.
Sweden, Stockholm
Stockholms Universitet
Denmark, Aarhus
Aarhus Universitet
Thöne, Christina C.
Spain, Granada
Instituto de Astrofísica de Andalucía - Csic
de Ugarte Postigo, Antonio
Denmark, Copenhagen
Niels Bohr Institutet
Spain, Granada
Instituto de Astrofísica de Andalucía - Csic
Statistics
Citations: 115
Authors: 24
Affiliations: 20
Identifiers
Doi:
10.1051/0004-6361/201118498
ISSN:
00046361
e-ISSN:
14320746
Study Design
Cross Sectional Study
Study Approach
Quantitative