260 K
40 pp.
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TitleThe Distant Type Ia Supernova Rate
Author(s)Pain, R.; Fabbro, S.; Sullivan, M.; Ellis, R. S.; Aldering, G.; Astier, P.; Deustua, S. E.; Fruchter, A. S.; Goldhaber, G.; Goobar, A.; Groom, D. E.; Hardin, D.; Hook, I. M.; Howell, D. A.; Irwin, M. J.; Kim, A. G.; Kim, M. Y.; Knop, R. A.; Lee, J. C.; Perlmutter, S.; Ruiz-Lapuente, P.; Schahmaneche, K.; Schaefer, B.; Walton, N. A.
Publication DateMay 28, 2002
Report NumberLBNL--47887
Unique IdentifierACC0427
Other NumbersLPNHE 02-02; OSTI ID: 807402
Research OrgLawrence Berkeley National Laboratory (LBNL), Berkeley, CA (US)
Contract NoAC03-76SF00098
Sponsoring OrgDirector, Office of Science. Office of High Energy and Nuclear Physics. Division of High Energy Physics, U.S. Department of Energy (DOE); National Science Foundation (NSF) (US)
Subject71 Classical And Quantum Mechanics, General Physics; 72 Physics Of Elementary Particles And Fields; Cosmological Models; Cosmology; Red Shift; Stars; Supernovae
KeywordsCosmology Type Ia Supernovae
Related Web PagesSaul Perlmutter, Distant Supernovae, Dark Energy, and the Accelerating Expansion of the Universe
AbstractWe present a measurement of the rate of distant Type Ia supernovae derived using 4 large subsets of data from the Supernova Cosmology Project. Within this fiducial sample, which surveyed about 12 square degrees, thirty-eight supernovae were detected at redshifts 0.25--0.85. In a spatially flat cosmological model consistent with the results obtained by the Supernova Cosmology Project, we derive a rest-frame Type Ia supernova rate at a mean red shift z {approx_equal} 0.55 of 1.53 {sub -0.25}{sub -0.31}{sup 0.28}{sup 0.32} x 10{sup -4} h{sup 3} Mpc{sup -3} yr{sup -1} or 0.58{sub -0.09}{sub -0.09}{sup +0.10}{sup +0.10} h{sup 2} SNu(1 SNu = 1 supernova per century per 10{sup 10} L{sub B}sun), where the first uncertainty is statistical and the second includes systematic effects. The dependence of the rate on the assumed cosmological parameters is studied and the redshift dependence of the rate per unit comoving volume is contrasted with local estimates in the context of possible cosmic star formation histories and progenitor models.
260 K
40 pp.
View Document 

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