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SNLS3: Constraints on Dark Energy Combining the Supernova Legacy Survey Three-year Data with Other Probes

Sullivan, M. and Ellis, R. S. and Neill, J. D. (2011) SNLS3: Constraints on Dark Energy Combining the Supernova Legacy Survey Three-year Data with Other Probes. Astrophysical Journal, 737 (2). Art. No. 102. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20110912-114953536

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Abstract

We present observational constraints on the nature of dark energy using the Supernova Legacy Survey three-year sample (SNLS3) of Guy et al. and Conley et al. We use the 472 Type Ia supernovae (SNe Ia) in this sample, accounting for recently discovered correlations between SN Ia luminosity and host galaxy properties, and include the effects of all identified systematic uncertainties directly in the cosmological fits. Combining the SNLS3 data with the full WMAP7 power spectrum, the Sloan Digital Sky Survey luminous red galaxy power spectrum, and a prior on the Hubble constant H_0 from SHOES, in a flat universe we find Ω_m = 0.269 ± 0.015 and w = –1.061^(+0.069)_(–0.068) (where the uncertainties include all statistical and SN Ia systematic errors)—a 6.5% measure of the dark energy equation-of-state parameter w. The statistical and systematic uncertainties are approximately equal, with the systematic uncertainties dominated by the photometric calibration of the SN Ia fluxes—without these calibration effects, systematics contribute only a ~2% error in w. When relaxing the assumption of flatness, we find Ω_m = 0.271 ± 0.015, Ω_k = –0.002 ± 0.006, and w = –1.069^(+0.091)_(–0.092). Parameterizing the time evolution of w as w(a) = w_0 + w_a (1–a) gives w_0 = –0.905 ± 0.196, w_a = –0.984^(+1.094)_(– 1.097) in a flat universe. All of our results are consistent with a flat, w = –1 universe. The size of the SNLS3 sample allows various tests to be performed with the SNe segregated according to their light curve and host galaxy properties. We find that the cosmological constraints derived from these different subsamples are consistent. There is evidence that the coefficient, β, relating SN Ia luminosity and color, varies with host parameters at >4σ significance (in addition to the known SN luminosity-host relation); however, this has only a small effect on the cosmological results and is currently a subdominant systematic.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/737/2/102 DOIArticle
http://iopscience.iop.org/0004-637X/737/2/102PublisherArticle
ORCID:
AuthorORCID
Neill, J. D.0000-0002-0466-1119
Additional Information:© 2011 The American Astronomical Society. Received 2011 April 7; accepted 2011 June 21; published 2011 August 8. This paper is based in part on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. M.S. acknowledges support from the Royal Society. Canadian collaboration members acknowledge support from NSERC and CIAR; French collaboration members from CNRS/IN2P3, CNRS/INSU, and CEA. This work is based in part on data products produced at the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS. Based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil), and CONICET (Argentina). Based on data from Gemini program IDs: GS-2003B-Q-8, GN-2003B-Q-9, GS-2004A-Q-11, GN-2004A-Q-19, GS-2004B-Q-31, GN-2004B-Q-16, GS-2005A-Q-11, GN-2005A-Q-11, GS-2005BQ-6, GN-2005B-Q-7, GN-2006A-Q-7, and GN-2006B-Q-10. Based in part on observations made with ESO Telescopes at the Paranal Observatory under program IDs 171.A-0486 and 176.A-0589. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
Group:Space Astrophysics Laboratory
Funders:
Funding AgencyGrant Number
Royal SocietyUNSPECIFIED
Natural Sciences and Engineering Research Council of Canada (NSERC)UNSPECIFIED
Canadian Institute for Advanced Research (CIFAR)UNSPECIFIED
Centre National de la Recherche Scientifique (CNRS)UNSPECIFIED
Institut national des sciences de l'Univers (INSU)UNSPECIFIED
Commissariat à l’Energie Atomique (CEA)UNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
NASAUNSPECIFIED
Institut National de Physique Nucléaire et de Physique des Particules (IN2P3)UNSPECIFIED
Subject Keywords:cosmological parameters; cosmology: observations; supernovae: general; surveys
Classification Code:PACS: 95.80+p; 97.60Bw; 95.35.+d; 98.80.Es;
Record Number:CaltechAUTHORS:20110912-114953536
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20110912-114953536
Official Citation:SNLS3: Constraints on Dark Energy Combining the Supernova Legacy Survey Three-year Data with Other Probes M. Sullivan et al. 2011 ApJ 737 102
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:25305
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:13 Sep 2011 20:40
Last Modified:22 May 2017 23:22

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