Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:0801.3297)
· References in the article
· Citations to the Article (24) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (64)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
A Measurement of the Rate of Type Ia Supernovae at Redshift z ~ 0.1 from the First Season of the SDSS-II Supernova Survey
Authors:
Dilday, Benjamin; Kessler, Richard; Frieman, Joshua A.; Holtzman, Jon; Marriner, John; Miknaitis, Gajus; Nichol, Robert C.; Romani, Roger; Sako, Masao; Bassett, Bruce; Becker, Andrew; Cinabro, David; DeJongh, Fritz; Depoy, Darren L.; Doi, Mamoru; Garnavich, Peter M.; Hogan, Craig J.; Jha, Saurabh; Konishi, Kohki; Lampeitl, Hubert; Marshall, Jennifer L.; McGinnis, David; Prieto, Jose Luis; Riess, Adam G.; Richmond, Michael W.; Schneider, Donald P.; Smith, Mathew; Takanashi, Naohiro; Tokita, Kouichi; van der Heyden, Kurt; Yasuda, Naoki; Zheng, Chen; Barentine, John; Brewington, Howard; Choi, Changsu; Crotts, Arlin; Dembicky, Jack; Harvanek, Michael; Im, Myunshin; Ketzeback, William; Kleinman, Scott J.; Krzesiński, Jurek; Long, Daniel C.; Malanushenko, Elena; Malanushenko, Viktor; McMillan, Russet J.; Nitta, Atsuko; Pan, Kaike; Saurage, Gabrelle; Snedden, Stephanie A.; Watters, Shannon; Wheeler, J. Craig; York, Donald
Affiliation:
AA(Department of Physics, University of Chicago, Chicago, IL 60637; .; Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637.), AB(Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637.; Enrico Fermi Institute, University of Chicago, Chicago, IL 60637.), AC(Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637.; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637.; Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, IL 60510.), AD(Department of Astronomy, MSC 4500, New Mexico State University, Las Cruces, NM 88003.), AE(Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, IL 60510.), AF(Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, IL 60510.), AG(Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 2EG, UK.), AH(Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305-4060.), AI(Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305-4060.; Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104.), AJ(Department of Mathematics and Applied Mathematics, University of Cape Town, Rondebosch 7701, South Africa.; South African Astronomical Observatory, Observatory 7935, South Africa.), AK(Department of Astronomy, University of Washington, Seattle, WA 98195.), AL(Department of Physics, Wayne State University, Detroit, MI 48202.), AM(Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, IL 60510.), AN(Department of Astronomy, Ohio State University, Columbus, OH 43210-1173.), AO(Institute of Astronomy, Graduate School of Science, University of Tokyo 2-21-1, Osawa, Mitaka, Tokyo 181-0015, Japan.), AP(University of Notre Dame, Notre Dame, IN 46556-5670.), AQ(Department of Astronomy, University of Washington, Seattle, WA 98195.), AR(Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305-4060.; Department of Physics and Astronomy, Rutgers University, Piscataway, NJ 08854.), AS(Institute for Cosmic Ray Research, University of Tokyo, 5-1-5, Kashiwanoha, Kashiwa, Chiba, 277-8582, Japan.), AT(Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 2EG, UK.; Space Telescope Science Institute, Baltimore, MD 21218.), AU(Department of Astronomy, Ohio State University, Columbus, OH 43210-1173.), AV(Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, IL 60510.), AW(Department of Astronomy, Ohio State University, Columbus, OH 43210-1173.), AX(Space Telescope Science Institute, Baltimore, MD 21218.; Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218.), AY(Physics Department, Rochester Institute of Technology, Rochester, NY 14623-5603.), AZ(Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802.), BA(Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 2EG, UK.), BB(Institute of Astronomy, Graduate School of Science, University of Tokyo 2-21-1, Osawa, Mitaka, Tokyo 181-0015, Japan.), BC(Institute of Astronomy, Graduate School of Science, University of Tokyo 2-21-1, Osawa, Mitaka, Tokyo 181-0015, Japan.), BD(South African Astronomical Observatory, Observatory 7935, South Africa.; Department of Astronomy, University of Cape Town, South Africa.), BE(Institute for Cosmic Ray Research, University of Tokyo, 5-1-5, Kashiwanoha, Kashiwa, Chiba, 277-8582, Japan.), BF(Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305-4060.), BG(Department of Astronomy, McDonald Observatory, University of Texas, Austin, TX 78712.; Apache Point Observatory, Sunspot, NM 88349.), BH(Apache Point Observatory, Sunspot, NM 88349.), BI(Department of Astronomy, Seoul National University, Seoul, South Korea.), BJ(Department of Astronomy, Columbia University, New York, NY 10027.), BK(Apache Point Observatory, Sunspot, NM 88349.), BL(Apache Point Observatory, Sunspot, NM 88349.; Lowell Observatory, Flagstaff, AZ 86001.), BM(Department of Astronomy, Seoul National University, Seoul, South Korea.), BN(Apache Point Observatory, Sunspot, NM 88349.), BO(Apache Point Observatory, Sunspot, NM 88349.; Subaru Telescope, Hilo, HI 96720.), BP(Apache Point Observatory, Sunspot, NM 88349.; Obserwatorium Astronomiczne na Suhorze, Akademia Pedagogicazna w Krakowie, ulica Podchorażych 2, PL-30-084 Kraków, Poland.), BQ(Apache Point Observatory, Sunspot, NM 88349.), BR(Apache Point Observatory, Sunspot, NM 88349.), BS(Apache Point Observatory, Sunspot, NM 88349.), BT(Apache Point Observatory, Sunspot, NM 88349.), BU(Apache Point Observatory, Sunspot, NM 88349.; Gemini Observatory, Hilo, HI 96720.), BV(Apache Point Observatory, Sunspot, NM 88349.), BW(Apache Point Observatory, Sunspot, NM 88349.), BX(Apache Point Observatory, Sunspot, NM 88349.), BY(Apache Point Observatory, Sunspot, NM 88349.), BZ(Department of Astronomy, McDonald Observatory, University of Texas, Austin, TX 78712.), CA(Enrico Fermi Institute, University of Chicago, Chicago, IL 60637.; Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637.)
Publication:
The Astrophysical Journal, Volume 682, Issue 1, pp. 262-282. (ApJ Homepage)
Publication Date:
07/2008
Origin:
UCP
ApJ Keywords:
Stars: Supernovae: General
DOI:
10.1086/587733
Bibliographic Code:
2008ApJ...682..262D

Abstract

We present a measurement of the rate of Type Ia supernovae (SNe Ia) from the first of three seasons of data from the SDSS-II Supernova Survey. For this measurement, we include 17 SNe Ia at redshift z<=0.12. Assuming a flat cosmology with Ωm=0.3=1-ΩΛ, we find a volumetric SN Ia rate of [2.93+0.17-0.04(systematic)+0.90-0.71(statistical)]×10-5 SNe Mpc-3 h370 yr-1, at a volume-weighted mean redshift of 0.09. This result is consistent with previous measurements of the SN Ia rate in a similar redshift range. The systematic errors are well controlled, resulting in the most precise measurement of the SN Ia rate in this redshift range. We use a maximum likelihood method to fit SN rate models to the SDSS-II Supernova Survey data in combination with other rate measurements, thereby constraining models for the redshift evolution of the SN Ia rate. Fitting the combined data to a simple power-law evolution of the volumetric SN Ia rate, rV~(1+z)β, we obtain a value of β=1.5+/-0.6, i.e., the SN Ia rate is determined to be an increasing function of redshift at the ~2.5 σ level. Fitting the results to a model in which the volumetric SN rate is rV=Aρ(t)+Bρ˙(t), where ρ(t) is the stellar mass density and ρ˙(t) is the star formation rate, we find A=(2.8+/-1.2)×10-14 SNe M-1solar yr-1, B=(9.3+3.4-3.1)×10-4 SNe M-1solar.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints