SNLS3: CONSTRAINTS ON DARK ENERGY COMBINING THE SUPERNOVA LEGACY SURVEY THREE-YEAR DATA WITH OTHER PROBES

被引：388

作者：

Sullivan, M. ^{[1
]}

Guy, J. ^{[2
]}

Conley, A. ^{[3
,4
]}

Regnault, N. ^{[2
]}

Astier, P. ^{[2
]}

Balland, C. ^{[2
,5
]}

Basa, S. ^{[6
]}

Carlberg, R. G. ^{[3
]}

Fouchez, D. ^{[7
]}

Hardin, D. ^{[2
]}

Hook, I. M. ^{[1
,8
]}

Howell, D. A. ^{[9
,10
]}

Pain, R. ^{[2
]}

Palanque-Delabrouille, N. ^{[11
]}

Perrett, K. M. ^{[3
,12
]}

Pritchet, C. J. ^{[13
]}

Rich, J. ^{[11
]}

Ruhlmann-Kleider, V. ^{[11
]}

Balam, D. ^{[13
]}

Baumont, S. ^{[14
]}

Ellis, R. S. ^{[1
,15
]}

Fabbro, S. ^{[13
]}

Fakhouri, H. K. ^{[16
]}

Fourmanoit, N. ^{[2
]}

Gonzalez-Gaitan, S. ^{[3
]}

Graham, M. L. ^{[9
,10
]}

Hudson, M. J. ^{[17
,18
]}

Hsiao, E. ^{[16
]}

Kronborg, T. ^{[2
]}

Lidman, C. ^{[19
]}

Mourao, A. M. ^{[20
,21
]}

Neill, J. D.

Perlmutter, S. ^{[16
,22
]}

Ripoche, P. ^{[2
,16
]}

Suzuki, N. ^{[16
]}

Walker, E. S. ^{[1
,23
]}

机构：

[1] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England

[2] Univ Paris 07, CNRS, Univ Paris 06, IN2P3,LPNHE, F-75252 Paris 05, France

[3] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada

[4] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA

[5] Univ Paris 11, F-91405 Orsay, France

[6] CNRS, LAM, F-13388 Marseille 13, France

[7] Aix Marseille Univ, CNRS, IN2P3, CPPM, Marseille, France

[8] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, PM, Italy

[9] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA

[10] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[11] Irfu SPP, Ctr Saclay, CEA, F-91191 Gif Sur Yvette, France

[12] DRDC Ottawa, Network Informat Operat, Ottawa, ON K1A 0Z4, Canada

[13] Univ Victoria, Dept Phys & Astron, Victoria, BC V8T 1M8, Canada

[14] UJF, LPSC, CNRS, IN2P3,INPG, F-38026 St Martin Dheres, France

[15] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA

[16] LBNL, Berkeley, CA 94720 USA

[17] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada

[18] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada

[19] Australian Astron Observ, Epping, NSW 1710, Australia

[20] CENTRA Ctr Multidisciplinar Astrofis, P-1049001 Lisbon, Portugal

[21] IST, Dep Fis, P-1049001 Lisbon, Portugal

[22] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[23] Scuola Normale Super Pisa, I-56126 Pisa, Italy

来源：

ASTROPHYSICAL JOURNAL | 2011年 / 737卷 / 02期

基金：

加拿大自然科学与工程研究理事会; 美国国家航空航天局;

关键词：

cosmological parameters; cosmology: observations; supernovae: general; surveys; HUBBLE-SPACE-TELESCOPE; BVRI LIGHT CURVES; IA SUPERNOVAE; WMAP OBSERVATIONS; POWER-SPECTRUM; DATA RELEASE; EVOLUTION; SELECTION; SPECTROSCOPY; OSCILLATIONS;

D O I：

10.1088/0004-637X/737/2/102

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 Omega(m) = 0.269 +/- 0.015 and w = -1.061(-0.068)(+0.069) (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 similar to 2% error in w. When relaxing the assumption of flatness, we find Omega(m) = 0.271 +/- 0.015, Omega(k) = -0.002 +/- 0.006, and w = -1.069(-0.092)(+0.091). 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(-1.097)(+1.094) 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, beta, relating SN Ia luminosity and color, varies with host parameters at >4 sigma 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.

引用

页数：19

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