FIRST-YEAR SLOAN DIGITAL SKY SURVEY-II SUPERNOVA RESULTS: HUBBLE DIAGRAM AND COSMOLOGICAL PARAMETERS-猫眼课题宝

DOI：

10.1088/0067-0049/185/1/32

发表时间：

2009-08

期刊：

The Astrophysical Journal Supplement Series

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中科院分区：

其他

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作者：

R. Kessler;A. Becker;D. Cinabro;J. Vanderplas;J. Frieman;J. Frieman;J. Marriner;T. Davis;T. Davis;B. Dilday;J. Holtzman;S. Jha;H. Lampeitl;M. Sako;Mathew Smith;Mathew Smith;C. Zheng;R. Nichol;B. Bassett;R. Bender;D. Depoy;M. Doi;E. Elson;A. Filippenko;R. Foley;R. Foley;P. Garnavich;U. Hopp;Y. Ihara;W. Ketzeback;W. Kollatschny;K. Konishi;J. Marshall;R. Mcmillan;G. Miknaitis;T. Morokuma;E. Mörtsell;K. Pan;J. Prieto;M. Richmond;A. Riess;A. Riess;R. Romani;D. Schneider;J. Sollerman;J. Sollerman;N. Takanashi;K. Tokita;K. V. D. Heyden;J. Wheeler;N. Yasuda;D. York

我们提供了103颗红移为0.04 < z < 0.42的Ia型超新星（SNe）的哈勃图测量结果，这些超新星是在斯隆数字巡天II（SDSS-II）超新星巡天的第一季（2005年秋季）发现的。这些数据填补了低和高红移超新星Ia巡天之间的红移“沙漠”。在mlcs 2k 2光变曲线拟合方法的框架下，我们利用SDSS-II SN样本，推导出宿主星系的平均红化参数RV = 2.18 ± 0.14stat ± 0.48syst，发现宿主星系消光的内禀分布可用指数函数P（AV）= exp（-AV/τV）拟合，其中τV = 0.334 ± 0.088 mag.我们结合联合收割机的SDSS-II测量与新的距离估计公布的SN数据从ESSENCE调查，超新星遗产调查（SNLS），哈勃太空望远镜（HST），和汇编附近的SN Ia测量。在我们的分析中的一个新功能是使用详细的蒙特卡罗模拟的所有调查，以考虑选择偏差，包括那些从光谱定位。结合SN Hubble图、SDSS亮红星系样品的重子声振荡测量和威尔金森微波各向异性探测器的宇宙微波背景温度各向异性测量，我们在假设空间平坦宇宙模型（FwCDM）具有常数暗能量状态方程参数w的条件下，估计了宇宙学参数w和ΩM.我们还考虑了在w = −1和非零空间曲率的宇宙常数模型（ΛCDM）中对ΩM和ΩΛ的约束。对于FwCDM模型和288个超新星Ia的组合样本，我们发现w = −0.76 ± 0.07（stat）± 0.11（syst），ΩM = 0.307 ± 0.019（stat）± 0.023（syst），使用mlcs 2k 2和w = −0.96 ± 0.06（stat）± 0.12（syst），ΩM = 0.265 ± 0.016（静态）± 0.025（系统）（使用salt-ii拟合器）。我们跟踪这些结果之间的差异，在休息帧UV模型结合不同的亮度校正颜色变化的差异，这些差异主要影响SNLS和HST SNe的距离估计。我们提出了详细的讨论，这两种光变曲线方法的系统误差，发现它们都显示数据模型的差异，在休息帧U带。对于salt-ii方法，我们也看到了色-光度参数（β）红移依赖性的强有力证据。将分析限制在Nearby+SDSS-II样本中的136个Ia超新星，我们发现两种分析方法之间的一致性要好得多，但不确定性更大：对于mlcs 2k 2，w = −0.92 ± 0.13（stat）+0.10 0. 33（syst）;对于salt-ii，w = −0.92 ± 0.11（stat）+0.07 0. 15（syst）。

We present measurements of the Hubble diagram for 103 Type Ia supernovae (SNe) with redshifts 0.04 < z < 0.42, discovered during the first season (Fall 2005) of the Sloan Digital Sky Survey-II (SDSS-II) Supernova Survey. These data fill in the redshift “desert” between low- and high-redshift SN Ia surveys. Within the framework of the mlcs2k2 light-curve fitting method, we use the SDSS-II SN sample to infer the mean reddening parameter for host galaxies, RV = 2.18 ± 0.14stat ± 0.48syst, and find that the intrinsic distribution of host-galaxy extinction is well fitted by an exponential function, P(AV) = exp(−AV/τV), with τV = 0.334 ± 0.088 mag. We combine the SDSS-II measurements with new distance estimates for published SN data from the ESSENCE survey, the Supernova Legacy Survey (SNLS), the Hubble Space Telescope (HST), and a compilation of Nearby SN Ia measurements. A new feature in our analysis is the use of detailed Monte Carlo simulations of all surveys to account for selection biases, including those from spectroscopic targeting. Combining the SN Hubble diagram with measurements of baryon acoustic oscillations from the SDSS Luminous Red Galaxy sample and with cosmic microwave background temperature anisotropy measurements from the Wilkinson Microwave Anisotropy Probe, we estimate the cosmological parameters w and ΩM, assuming a spatially flat cosmological model (FwCDM) with constant dark energy equation of state parameter, w. We also consider constraints upon ΩM and ΩΛ for a cosmological constant model (ΛCDM) with w = −1 and non-zero spatial curvature. For the FwCDM model and the combined sample of 288 SNe Ia, we find w = −0.76 ± 0.07(stat) ± 0.11(syst), ΩM = 0.307 ± 0.019(stat) ± 0.023(syst) using mlcs2k2 and w = −0.96 ± 0.06(stat) ± 0.12(syst), ΩM = 0.265 ± 0.016(stat) ± 0.025(syst) using the salt-ii fitter. We trace the discrepancy between these results to a difference in the rest-frame UV model combined with a different luminosity correction from color variations; these differences mostly affect the distance estimates for the SNLS and HST SNe. We present detailed discussions of systematic errors for both light-curve methods and find that they both show data-model discrepancies in rest-frame U band. For the salt-ii approach, we also see strong evidence for redshift-dependence of the color-luminosity parameter (β). Restricting the analysis to the 136 SNe Ia in the Nearby+SDSS-II samples, we find much better agreement between the two analysis methods but with larger uncertainties: w = −0.92 ± 0.13(stat)+0.10−0.33(syst) for mlcs2k2 and w = −0.92 ± 0.11(stat)+0.07−0.15 (syst) for salt-ii.

FIRST-YEAR SLOAN DIGITAL SKY SURVEY-II SUPERNOVA RESULTS: HUBBLE DIAGRAM AND COSMOLOGICAL PARAMETERS

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