The Complete Light-curve Sample of Spectroscopically Confirmed SNe Ia from Pan-STARRS1 and Cosmological Constraints from the Combined Pantheon Sample

被引：1957

作者：

Scolnic, D. M. ^{[1
]}

Jones, D. O. ^{[2
]}

Rest, A. ^{[2
,3
]}

Pan, Y. C. ^{[4
]}

Chornock, R. ^{[5
]}

Foley, R. J. ^{[4
]}

Huber, M. E. ^{[6
]}

Kessler, R. ^{[1
]}

Narayan, G. ^{[3
]}

Riess, A. G. ^{[2
,3
]}

Rodney, S. ^{[7
]}

Berger, E. ^{[8
]}

Brout, D. J. ^{[9
]}

Challis, P. J. ^{[8
]}

Drout, M. ^{[10
]}

Finkbeiner, D. ^{[11
]}

Lunnan, R. ^{[12
]}

Kirshner, R. P. ^{[8
]}

Sanders, N. E.

Schlafly, E. ^{[13
]}

Smartt, S. ^{[14
]}

Stubbs, C. W. ^{[8
,11
]}

Tonry, J. ^{[6
]}

Wood-Vasey, W. M. ^{[15
]}

Foley, M. ^{[16
]}

Hand, J. ^{[15
]}

Johnson, E. ^{[17
]}

Burgett, W. S. ^{[18
]}

Chambers, K. C. ^{[6
]}

Draper, P. W. ^{[19
]}

Hodapp, K. W. ^{[6
]}

Kaiser, N. ^{[6
]}

Kudritzki, R. P. ^{[6
]}

Magnier, E. A. ^{[6
]}

Metcalfe, N. ^{[19
]}

Bresolin, F. ^{[6
]}

Gall, E. ^{[14
]}

Kotak, R. ^{[14
]}

McCrum, M. ^{[14
]}

Smith, K. W. ^{[14
]}

机构：

[1] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA

[2] Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA

[3] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA

[4] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 92064 USA

[5] Ohio Univ, Dept Phys & Astron, Astrophys Inst, 251B Clippinger Lab, Athens, OH 45701 USA

[6] Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA

[7] Univ South Carolina, Dept Phys & Astron, 712 Main St, Columbia, SC 29208 USA

[8] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[9] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA

[10] Observ Carnegie Inst Sci, 813 Santa Barbara St, Pasadena, CA 91101 USA

[11] Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA

[12] Stockholm Univ, Dept Astron, Stockholm, Sweden

[13] Lawrence Berkeley Natl Lab, One Cyclotron Rd, Berkeley, CA 94720 USA

[14] Queens Univ Belfast, Astrophys Res Ctr, Sch Math & Phys, Belfast BT7 1NN, Antrim, North Ireland

[15] Univ Pittsburgh, Dept Phys & Astron, PITT PACC, Pittsburgh, PA 15260 USA

[16] Univ Notre Dame, Dept Phys, 225 Nieuwland Sci Hall, Notre Dame, IN 46556 USA

[17] Villanova Univ, Dept Astrophys & Planetary Sci, Villanova, PA 19085 USA

[18] GMTO Corp, 251 S Lake Ave,Suite 300, Pasadena, CA 91101 USA

[19] Univ Durham, Dept Phys, Sci Labs, South Rd, Durham DH1 3LE, England

来源：

ASTROPHYSICAL JOURNAL | 2018年 / 859卷 / 02期

基金：

美国国家科学基金会; 美国国家航空航天局;

关键词：

cosmology: observations; dark energy; supernovae: general; HUBBLE-SPACE-TELESCOPE; ESSENCE SUPERNOVA SURVEY; DARK ENERGY; HOST GALAXIES; COSMIC ACCELERATION; VELOCITY-FIELD; LEGACY SURVEY; DATA RELEASE; SPECTROGRAPH; PARAMETERS;

D O I：

10.3847/1538-4357/aab9bb

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present optical light curves, redshifts, and classifications for 365 spectroscopically confirmed Type Ia supernovae (SNe Ia) discovered by the Pan-STARRS1 (PS1) Medium Deep Survey. We detail improvements to the PS1 SN photometry, astrometry, and calibration that reduce the systematic uncertainties in the PS1 SN Ia distances. We combine the subset of 279 PS1 SNe Ia (0.03 < z < 0.68) with useful distance estimates of SNe Ia from the Sloan Digital Sky Survey (SDSS), SNLS, and various low-z and Hubble Space Telescope samples to form the largest combined sample of SNe Ia, consisting of a total of 1048 SNe Ia in the range of 0.01 < z < 2.3, which we call the "Pantheon Sample." When combining Planck 2015 cosmic microwave background (CMB) measurements with the Pantheon SN sample, we find Omega(m) = 0.307 +/- 0.012 and w = -1.026 +/- 0.041 for the wCDM model. When the SN and CMB constraints are combined with constraints from BAO and local H-0 measurements, the analysis yields the most precise measurement of dark energy to date: w(0) = -1.007 +/- 0.089 and w(a) = -0.222 +/- 0.407 for the w(0)w(a) CDM model. Tension with a cosmological constant previously seen in an analysis of PS1 and low-z SNe has diminished after an increase of 2x in the statistics of the PS1 sample, improved calibration and photometry, and stricter light-curve quality cuts. We find that the systematic uncertainties in our measurements of dark energy are almost as large as the statistical uncertainties, primarily due to limitations of modeling the low-redshift sample. This must be addressed for future progress in using SNe Ia to measure dark energy.

引用

页数：28

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