COSMOLOGICAL CONSTRAINTS FROM SUNYAEV–ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg2 OF THE SOUTH POLE TELESCOPE SURVEY
COSMOLOGICAL CONSTRAINTS FROM SUNYAEV–ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg2 OF THE SOUTH POLE TELESCOPE SURVEY
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南极望远镜巡天第一个 178 度2 的 X 射线观测中 SUNYAEVâZELDovich 选定星团的宇宙学约束
DOI：
10.1088/0004-637x/763/2/147
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发表时间：
2013
期刊：
影响因子：
--
通讯作者：
B. A. Benson
中科院分区：
文献类型：
--
作者：
B. A. Benson
我们使用南极望远镜(SPT)Sunyaev-Zel‘dovich(SZ)星团测量的测量结果与X射线测量相结合来约束宇宙学参数。我们提出了一种统计方法，该方法适用于SZ和X射线团簇可观测值与质量的标度关系，同时也适用于宇宙学。该方法可推广到多个星系团可观测值，并自洽地考虑了星系团选择和星团质量定标中的不确定性对导出的宇宙学约束的影响。我们将这种方法应用于一个数据集，该数据集包括从2500°2 SPT-SZ观测的前178°2到z>；0.3处的18个星系团，其中14个星系团有来自Chandra或XMM-牛顿的X射线观测。假设空间平坦的SPTCDM宇宙学模型，我们发现Λ团簇样本约束σ8(Ωm/0.25)0.30=0.785±0.037。结合SPT的宇宙微波背景功率谱测量和7年的威尔金森微波各向异性探测器数据，SPT星团样本约束σ=0.795±0.016和Ωm=0.255±0.016，每个参数比单独的宇宙微波背景数据提高1.5倍。我们考虑了几种对Λ清洁发展机制模型的扩展，包括以下几个自由参数：暗能量状态方程(W)、中微子质量之和(Σmν)、有效相对论物种数(N Ef)和原始非高斯性(F NL)。我们发现，与使用CMB、超新星、重子声振荡和哈勃常数的测量相比，加入SPT星团数据显著改善了对w和Σmν的约束。单独考虑每个扩展，我们最好地约束w=−0.973±0.063和中微子质量之和Σmν<；0.28eV，在95%置信度下，分别比没有簇的约束提高1.25和1.4.假设Λ清洁发展模型有一个自由的N ff和Σmν，我们测得N ff=3.91±0.42，并以95%的置信度约束Σmν<；0.6 3 eV。我们还使用SPT簇样本来约束f_nL=−220±317，与零原始非高斯一致。最后，我们讨论了目前星团质量定标的系统局限性，以及对最近完成的2500°2SPT-SZ调查的未来改进。调查已经探测到∼500星团，其红移中值为∼0.5，质量中值为∼2.3×1014 M☉h−1，与改进的星团质量校准和现有的外部宇宙学数据集相结合，将显著改善对w的约束。
We use measurements from the South Pole Telescope (SPT) Sunyaev–Zel'dovich (SZ) cluster survey in combination with X-ray measurements to constrain cosmological parameters. We present a statistical method that fits for the scaling relations of the SZ and X-ray cluster observables with mass while jointly fitting for cosmology. The method is generalizable to multiple cluster observables, and self-consistently accounts for the effects of the cluster selection and uncertainties in cluster mass calibration on the derived cosmological constraints. We apply this method to a data set consisting of an SZ-selected catalog of 18 galaxy clusters at z> 0.3 from the first 178 deg 2 of the 2500 deg 2 SPT-SZ survey, with 14 clusters having X-ray observations from either Chandra or XMM-Newton. Assuming a spatially flat ΛCDM cosmological model, we find the SPT cluster sample constrains σ 8 (Ω m/0.25) 0.30= 0.785±0.037. In combination with measurements of the cosmic microwave background (CMB) power spectrum from the SPT and the seven-year Wilkinson Microwave Anisotropy Probe data, the SPT cluster sample constrains σ 8= 0.795±0.016 and Ω m= 0.255±0.016, a factor of 1.5 improvement on each parameter over the CMB data alone. We consider several extensions beyond the ΛCDM model by including the following as free parameters: the dark energy equation of state (w), the sum of the neutrino masses (Σm ν), the effective number of relativistic species (N eff), and a primordial non-Gaussianity (f NL). We find that adding the SPT cluster data significantly improves the constraints on w and Σm ν beyond those found when using measurements of the CMB, supernovae, baryon acoustic oscillations, and the Hubble constant. Considering each extension independently, we best constrain w=− 0.973±0.063 and the sum of neutrino masses Σm ν< 0.28 eV at 95% confidence, a factor of 1.25 and 1.4 improvement, respectively, over the constraints without clusters. Assuming a ΛCDM model with a free N eff and Σm ν, we measure N eff= 3.91±0.42 and constrain Σm ν< 0.63 eV at 95% confidence. We also use the SPT cluster sample to constrain f NL=− 220±317, consistent with zero primordial non-Gaussianity. Finally, we discuss the current systematic limitations due to the cluster mass calibration, and future improvements for the recently completed 2500 deg 2 SPT-SZ survey. The survey has detected∼ 500 clusters with a median redshift of∼ 0.5 and a median mass of∼ 2.3× 10 14 M☉ h− 1 and, when combined with an improved cluster mass calibration and existing external cosmological data sets will significantly improve constraints on w.
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星系团X射线标度关系的演化
DOI：
10.1111/j.1365-2966.2010.17267.x
发表时间：
2010
影响因子：
4.8
作者：
C. Short;P. Thomas;O. Young;F. Pearce;A. Jenkins;O. M. U. O. Sussex;UK.;U. Nottingham;U. Durham;Khon Kaen University;Thailand
通讯作者：
Thailand
星系团中电离气体的准确实现：校准反馈
DOI：
10.1086/518432
发表时间：
2006
期刊：
The Astrophysical Journal
影响因子：
--
作者：
P. Bode;J. Ostriker;J. Weller;L. Shaw
通讯作者：
L. Shaw
南极望远镜对次级宇宙微波背景各向异性的测量
DOI：
--
发表时间：
2009
期刊：
影响因子：
--
作者：
M. Lueker;C. Reichardt;K. Schaffer;O. Zahn;P. Ade;K. Aird;B. Benson;B. Benson;L. Bleem;J. Carlstrom;C. Chang;Hsiao;T. Crawford;A. Crites;T. Haan;M. Dobbs;E. George;N. Hall;N. Halverson;G. Holder;W. Holzapfel;J. Hrubeš;M. Joy;R. Keisler;L. Knox;Adrian T. Lee;Adrian T. Lee;E. Leitch;J. McMahon;J. McMahon;J. Mehl;S. Meyer;J. Mohr;T. Montroy;S. Padin;T. Plagge;C. Pryke;J. Ruhl;L. Shaw;L. Shaw;E. Shirokoff;H. Spieler;B. Stalder;Z. Staniszewski;A. Stark;K. Vanderlinde;J. Vieira;R. Williamson
通讯作者：
R. Williamson
DOI：
10.1088/0004-637x/722/2/1180
发表时间：
2010-03
期刊：
The Astrophysical Journal
影响因子：
--
作者：
F. W. High;B. Stalder;J. Song;P. Ade;K. Aird;S. Allam;R. Armstrong;W. Barkhouse;B. Benson;B. Benson;E. Bertin;Suman Bhattacharya;L. Bleem;M. Brodwin;E. Buckley-Geer;J. Carlstrom;P. Challis;C. Chang;T. Crawford;A. Crites;T. Haan;S. Desai;M. Dobbs;J. Dudley;R. Foley;E. George;M. Gladders;N. Halverson;M. Hamuy;S. Hansen;G. Holder;W. Holzapfel;J. Hrubeš;M. Joy;R. Keisler;Adrian T. Lee;Adrian T. Lee;E. Leitch;Huan Lin;Yen-Ting Lin;A. Loehr;M. Lueker;D. Marrone;J. McMahon;J. McMahon;J. Mehl;S. Meyer;J. J. Mohr-J.;T. Montroy;N. Morell;C. Ngeow;S. Padin;T. Plagge;T. Plagge;C. Pryke;C. Reichardt;A. Rest;J. Ruel;J. Ruhl;K. Schaffer;L. Shaw;L. Shaw;E. Shirokoff;R. C. Smith;H. Spieler;Z. Staniszewski;A. Stark;C. Stubbs;D. Tucker;K. Vanderlinde;J. Vieira;R. Williamson;W. M. Wood-Vasey;Y. Yang;O. Zahn;A. Zenteno
通讯作者：
F. W. High;B. Stalder;J. Song;P. Ade;K. Aird;S. Allam;R. Armstrong;W. Barkhouse;B. Benson;B. Benson;E. Bertin;Suman Bhattacharya;L. Bleem;M. Brodwin;E. Buckley-Geer;J. Carlstrom;P. Challis;C. Chang;T. Crawford;A. Crites;T. Haan;S. Desai;M. Dobbs;J. Dudley;R. Foley;E. George;M. Gladders;N. Halverson;M. Hamuy;S. Hansen;G. Holder;W. Holzapfel;J. Hrubeš;M. Joy;R. Keisler;Adrian T. Lee;Adrian T. Lee;E. Leitch;Huan Lin;Yen-Ting Lin;A. Loehr;M. Lueker;D. Marrone;J. McMahon;J. McMahon;J. Mehl;S. Meyer;J. J. Mohr-J.;T. Montroy;N. Morell;C. Ngeow;S. Padin;T. Plagge;T. Plagge;C. Pryke;C. Reichardt;A. Rest;J. Ruel;J. Ruhl;K. Schaffer;L. Shaw;L. Shaw;E. Shirokoff;R. C. Smith;H. Spieler;Z. Staniszewski;A. Stark;C. Stubbs;D. Tucker;K. Vanderlinde;J. Vieira;R. Williamson;W. M. Wood-Vasey;Y. Yang;O. Zahn;A. Zenteno
两种极端合并情况下的规模关系
DOI：
10.1088/0004-637x/729/1/45
发表时间：
2010
期刊：
The Astrophysical Journal
影响因子：
--
作者：
E. Rasia;P. Mazzotta;A. Evrard;M. Markevitch;K. Dolag;M. Meneghetti
通讯作者：
M. Meneghetti