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C.J. Pritchet (U. Victoria), M. Sullivan (U. Toronto), S. Gwyn (U. Victoria), P. Astier (LPNHE, CNRS-IN2P3), E. Aubourg (CEA Saclay), D. Balam (U. Victoria), S. Basa (LAM, CNRS Marseille), R.G. Carlberg, A. Conley (U. Toronto), S. Fabbro (CENTRA, IST Lisbon), D. Fouchez (CPPM, CNRS-IN2P3), J. Guy (LPNHE, CNRS-IN2P3), I. Hook (U. Oxford), D.A. Howell (U. Toronto), H. Lafoux (CEA Saclay), J.D. Neill (U. Victoria), R. Pain, N. Palanque-Delabrouille (LPNHE, CNRS-IN2P3), K. Perrett (U. Toronto), N. Regnault (LPNHE, CNRS-IN2P3), J. Rich (CEA Saclay), R. Taillet, S. Baumont (LPNHE, CNRS-IN2P3), J. Bronder (U. Oxford), V. Lusset (CEA Saclay), P. Ripoche (CPPM, CNRS-IN2P3), A. Mourao (CENTRA, IST Lisbon), S. Perlmutter (LBNL, Berkeley), M. Graham, E. Hsiao (U. Victoria)
Analysis of 150 SNLS Survey Type Ia supernovae (0.2 < z < 0.9, all with spectroscopic identification) shows a strong connection between SNIa rate, normalized per unit mass, and star formation rate or galaxy morphology. This correlation is in the sense that the rate per unit mass in Irr galaxies is more than a factor of 10 higher than that in E/S0 galaxies. This result independently confirms that found for SNLS SNeIa by Sullivan et al (this meeting), but makes use of different photometric redshifts for the field population (Gwyn et al. 2005), and different M/L and star formation rate estimators. The SFR/morphology dependence of SNIa rate is, to first order, independent of redshift. The observations can be explained in terms of one or two component models for the origin of SNeIa (Howell et al., this meeting).
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.