Using data from the Sloan Digital Sky Supernova Survey-II, 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
Smith, Mathew, et al. "The SDSS-II Supernova Survey: Parameterizing the Type Ia Supernova Rate as a Function of Host Galaxy Properties." Astrophys.J., vol. 755, Aug. 2011. https://doi.org/10.1088/0004-637X/755/1/61
Smith, Mathew, Nichol, Robert C., Dilday, Benjamin, Marriner, John, Kessler, Richard, Bassett, Bruce, Cinabro, David, Frieman, Joshua, Garnavich, Peter, Jha, Saurabh W., Lampeitl, Hubert, Sako, Masao, Schneider, Donald P., & Sollerman, Jesper (2011). The SDSS-II Supernova Survey: Parameterizing the Type Ia Supernova Rate as a Function of Host Galaxy Properties. Astrophys.J., 755. https://doi.org/10.1088/0004-637X/755/1/61
Smith, Mathew, Nichol, Robert C., Dilday, Benjamin, et al., "The SDSS-II Supernova Survey: Parameterizing the Type Ia Supernova Rate as a Function of Host Galaxy Properties," Astrophys.J. 755 (2011), https://doi.org/10.1088/0004-637X/755/1/61
@article{osti_1967997,
author = {Smith, Mathew and Nichol, Robert C. and Dilday, Benjamin and Marriner, John and Kessler, Richard and Bassett, Bruce and Cinabro, David and Frieman, Joshua and Garnavich, Peter and Jha, Saurabh W. and others},
title = {The SDSS-II Supernova Survey: Parameterizing the Type Ia Supernova Rate as a Function of Host Galaxy Properties},
annote = {Using data from the Sloan Digital Sky Supernova Survey-II, 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 broad-band photometry we use the PEGASE spectral energy distributions (SEDs) to estimate host galaxy stellar masses and recent star-formation rates. We find that the rate of SNe Ia per unit stellar mass is significantly higher (by a factor of ~30) in highly star-forming galaxies compared to passive galaxies. When parameterizing the SN Ia rate (SNR_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 a SNR_Ia proportional to M^0.68 is favored. However, such a parameterization does not describe the observed SN Ia rate in star-forming galaxies. The SN Ia rate in star-forming galaxies is well fit by SNR_Ia = 1.05\pm0.16x10^{-10} M ^{0.68\pm0.01} + 1.01\pm0.09x10^{-3} SFR^{1.00\pm0.05} (statistical errors only), where M is the host galaxy mass and SFR is the star-formation rate. These results are insensitive to the selection criteria used, redshift limit considered and the inclusion of non-spectroscopically confirmed SNe Ia. We also show there is a dependence between the distribution of the MLCS light-curve decline rate parameter, \Delta, and host galaxy type. Passive galaxies host less luminous SNe Ia than seen in moderately and highly star-forming galaxies, although a population of luminous SNe is observed in passive galaxies, contradicting previous assertions that these SNe Ia are only observed in younger stellar systems. The MLCS extinction parameter, A_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. We confirm these results using the SALT2 light-curve fitter.},
doi = {10.1088/0004-637X/755/1/61},
url = {https://www.osti.gov/biblio/1967997},
journal = {Astrophys.J.},
volume = {755},
place = {United States},
year = {2011},
month = {08}}
Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Vol. 362, Issue 2-3https://doi.org/10.1016/0168-9002(95)00274-X