THE SDSS-II SUPERNOVA SURVEY: PARAMETERIZING THE TYPE Ia SUPERNOVA RATE AS A FUNCTION OF HOST GALAXY PROPERTIES
- Department of Physics, University of Western Cape, Bellville 7530, Cape Town (South Africa)
- Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX (United Kingdom)
- Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117 (United States)
- Center for Particle Astrophysics, Fermilab, P.O. Box 500, Batavia, IL 60510 (United States)
- Department of Astronomy and Astrophysics, University of Chicago, 5640 S. Ellis Ave, Chicago, IL 60637 (United States)
- African Institute for Mathematical Sciences, 6-8 Melrose Road, Muizenberg 7945 (South Africa)
- Department of Physics and Astronomy, Wayne State University, Detroit, MI 48201 (United States)
- Department of Physics, University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556 (United States)
- Department of Physics and Astronomy, Rutgers, State University of New Jersey, 136 Frelinghuysen Road, Piscataway, NJ 08854 (United States)
- Astrophysics, Cosmology and Gravity Centre (ACGC), Department of Mathematics and Applied Mathematics, University of Cape Town, Rondebosch 7701 (South Africa)
- Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA 19104 (United States)
- Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802 (United States)
- Oskar Klein Centre, Department of Astronomy, AlbaNova, Stockholm University, SE-106 91 Stockholm (Sweden)
Using data from the Sloan Digital Sky Supernova Survey-II (SDSS-II SN Survey), we measure the rate of Type Ia supernovae (SNe Ia) as a function of galaxy properties at intermediate redshift. A sample of 342 SNe Ia with 0.05 < z < 0.25 is constructed. Using broadband photometry and redshifts, we use the PEGASE.2 spectral energy distributions to estimate host galaxy stellar masses and recent star formation rates (SFRs). We find that the rate of SNe Ia per unit stellar mass is significantly higher (by a factor of {approx}30) in highly star-forming galaxies compared to passive galaxies. When parameterizing the SN Ia rate (SNR{sub Ia}) based on host galaxy properties, we find that the rate of SNe Ia in passive galaxies is not linearly proportional to the stellar mass; instead an SNR{sub Ia}{proportional_to}M{sup 0.68} is favored. However, such a parameterization does not describe the observed SNR{sub Ia} in star-forming galaxies. The SNR{sub Ia} in star-forming galaxies is well fitted by SNR{sub Ia} = (0.41 {+-} 0.15) Multiplication-Sign 10{sup -10} M{sup 0.72{+-}0.15} + (0.65 {+-} 0.25) Multiplication-Sign 10{sup -3}SFR{sup 1.01{+-}0.22} (statistical errors only), where M is the host galaxy stellar mass (in M{sub Sun }) and SFR is the SFR (in M{sub Sun} yr{sup -1}). We show that our results, for SNe Ia in passive galaxies, are consistent with those at higher redshifts (favoring SNR{sub Ia}{proportional_to}M) when accounting for the difference in the ages of our galaxies. This suggests that the rate of SNe Ia is correlated with the age of the stellar population. The MLCS extinction parameter, A{sub V} , is similar in passive and moderately star-forming galaxies, but we find indications that it is smaller, on average, in highly star-forming galaxies. This result appears to be driven by a deficit of the reddest (A{sub V} > 0.15) SNe Ia in highly star-forming galaxies. We consider that the high levels of dust in these systems may be obscuring the reddest and faintest SNe Ia.
- OSTI ID:
- 22039132
- Journal Information:
- Astrophysical Journal, Vol. 755, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
Similar Records
EVOLUTION IN THE VOLUMETRIC TYPE Ia SUPERNOVA RATE FROM THE SUPERNOVA LEGACY SURVEY
THE TYPE II SUPERNOVA RATE IN z {approx} 0.1 GALAXY CLUSTERS FROM THE MULTI-EPOCH NEARBY CLUSTER SURVEY