SYSTEMATIC UNCERTAINTIES ASSOCIATED WITH THE COSMOLOGICAL ANALYSIS OF THE FIRST PAN-STARRS1 TYPE Ia SUPERNOVA SAMPLE

被引：90

作者：

Scolnic, D. ^{[1
]}

Rest, A. ^{[2
]}

Riess, A. ^{[1
]}

Huber, M. E. ^{[3
]}

Foley, R. J. ^{[4
,5
,6
]}

Brout, D. ^{[1
]}

Chornock, R. ^{[4
]}

Narayan, G. ^{[7
]}

Tonry, J. L. ^{[3
]}

Berger, E. ^{[4
]}

Soderberg, A. M. ^{[4
]}

Stubbs, C. W. ^{[4
,7
]}

Kirshner, R. P. ^{[4
,7
]}

Rodney, S. ^{[1
]}

Smartt, S. J. ^{[8
]}

Schlafly, E. ^{[9
]}

Botticella, M. T. ^{[8
]}

Challis, P. ^{[4
]}

Czekala, I. ^{[4
]}

Drout, M. ^{[4
]}

Hudson, M. J. ^{[10
]}

Kotak, R. ^{[8
]}

Leibler, C. ^{[11
]}

Lunnan, R. ^{[4
]}

Marion, G. H. ^{[4
]}

McCrum, M. ^{[8
]}

Milisavljevic, D. ^{[4
]}

Pastorello, A. ^{[12
]}

Sanders, N. E. ^{[4
]}

Smith, K. ^{[8
]}

Stafford, E. ^{[1
]}

Thilker, D. ^{[1
]}

Valenti, S. ^{[13
,14
]}

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

Zheng, Z. ^{[1
]}

Burgett, W. S. ^{[3
]}

Chambers, K. C. ^{[3
]}

Denneau, L. ^{[3
]}

Draper, P. W. ^{[16
]}

Flewelling, H. ^{[3
]}

Hodapp, K. W. ^{[3
]}

Kaiser, N. ^{[3
]}

Kudritzki, R. -P. ^{[3
]}

Magnier, E. A. ^{[3
]}

Metcalfe, N. ^{[16
]}

Price, P. A. ^{[17
]}

Sweeney, W. ^{[3
]}

Wainscoat, R. ^{[3
]}

Waters, C. ^{[3
]}

机构：

[1] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[2] Space Telescope Sci Inst, Baltimore, MD 21218 USA

[3] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[4] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

[5] Univ Illinois, Dept Astron, Urbana, IL 61801 USA

[6] Univ Illinois, Dept Phys, Urbana, IL 61801 USA

[7] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA

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

[9] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[10] Univ Waterloo, Waterloo, ON N2L 3G1, Canada

[11] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95060 USA

[12] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[13] Las Cumbres Observ Global Telescope Network Inc, Santa Barbara, CA 93117 USA

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

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

[16] Univ Durham, Sci Labs, Dept Phys, Durham DH1 3LE, England

[17] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA

来源：

ASTROPHYSICAL JOURNAL | 2014年 / 795卷 / 01期

基金：

美国国家科学基金会; 美国国家航空航天局;

关键词：

dark energy; supernovae: general; DARK-ENERGY CONSTRAINTS; HUBBLE-SPACE-TELESCOPE; BVRI LIGHT CURVES; SDSS-II; PECULIAR VELOCITIES; ABSOLUTE MAGNITUDES; IMPROVED DISTANCES; HOST GALAXIES; PHOTOMETRY; DUST;

D O I：

10.1088/0004-637X/795/1/45

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We probe the systematic uncertainties from the 113 Type Ia supernovae (SN Ia) in the Pan-STARRS1 (PS1) sample along with 197 SN Ia from a combination of low-redshift surveys. The companion paper by Rest et al. describes the photometric measurements and cosmological inferences from the PS1 sample. The largest systematic uncertainty stems from the photometric calibration of the PS1 and low-z samples. We increase the sample of observed Calspec standards from 7 to 10 used to define the PS1 calibration system. The PS1 and SDSS-II calibration systems are compared and discrepancies up to similar to 0.02 mag are recovered. We find uncertainties in the proper way to treat intrinsic colors and reddening produce differences in the recovered value of w up to 3%. We estimate masses of host galaxies of PS1 supernovae and detect an insignificant difference in distance residuals of the full sample of 0.037 +/- 0.031 mag for host galaxies with high and low masses. Assuming flatness and including systematic uncertainties in our analysis of only SNe measurements, we find w = -1.120(+0.360)(-0.206)(Stat)(+0.269)(-0.291)(Sys). With additional constraints from Baryon acoustic oscillation, cosmic microwave background (CMB) (Planck) and H-0 measurements, we find w = -1.166(+0.072)(-0.069) and Omega m = 0.280(+0.013)(-0.012) (statistical and systematic errors added in quadrature). The significance of the inconsistency with w = -1 depends on whether we use Planck or Wilkinson Microwave Anisotropy Probe measurements of the CMB: w(BAO+H0+SN+WMAP) = -1.124(+0.083)(-0.065).

引用

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