Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21543030m&link_type=abstract
American Astronomical Society, AAS Meeting #215, #430.30; Bulletin of the American Astronomical Society, Vol. 42, p.361
Astronomy and Astrophysics
Astronomy
Scientific paper
We present an extensive set of data that cover UV through NIR spectroscopy and photometry of the unusual Type Ia supernova 2009dc. The data are well sampled from -13d to +90d with respect to the time of Bmax. SN 2009dc was very luminous across all measured pass bands (MV < -21 mag without extinction) and exceptionally blue at early phases. The light curves were slow to rise and slow to decline. The decline parameter Δm15(B) is about 0.65. The Doppler velocities of explosion products were very slow (7,000-9,000 km/s) in early data and both light and intermediate mass elements appear to occupy the same line-forming regions. SN 2009dc exhibited the strongest and most persistent spectral signature from carbon yet observed in a SN Ia with CII lines from both 6580 and 7234 Angstroms detected in the earliest spectral data and continuing through one week past maximum light. CI however is not detected in multiple NIR spectra. Spectral analysis is conducted with SYNOW.
We discuss the exceptional characteristics of the SN 2009dc data and explore possible implications for a super-Chandrasekhar mass progenitor as has been suggested for SNe 2003fg and 2006gz. Such an event may result from the double-degenerate merger of two white dwarf stars.
Light curve data is presented for the UBVRIJHK bands, spectral coverage extends from 2,000-25,000 Angstroms at several epochs, and near daily optical spectra are presented from two weeks before to five weeks after maximum light. The data include moderate and high resolution spectra of the intersteller NaI and CaII lines. Data were obtained using Swift, FWLO, APO, MMT, HET, MAGE, PAIRITEL, and the IRTF.
Brown Patrick
Challis Peter
Foley Ryan
Garnavich Peter
Howie Marion G.
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