The galaxy cluster X-ray luminosity-gravitational mass relation in the light of the WMAP 3rd year data
The galaxy cluster X-ray luminosity-gravitational mass relation in the light of the WMAP 3rd year data
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根据 WMAP 第三年数据得出的星系团 X 射线光度-引力质量关系
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发表时间：
2006
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通讯作者：
T. Reiprich
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作者：
T. Reiprich
上下文第三年的WMAP结果标志着宇宙学参数的最佳拟合值与第一年的数据和和谐宇宙学模型相比发生了变化。目标。我们测试了新结果与HIFLUGCS星系团样本中宇宙学参数的先前约束的一致性，以及这种变化对X射线光度-引力质量关系的影响。方法.测量的X射线光度函数与观测到的光度-质量关系相结合，与给定宇宙学参数值的质量函数进行比较。结果先前从HIFLUGCS导出的光度函数和光度-质量关系与使用第三年WMAP数据（m = 0：238; 8 = 0：74）的最佳拟合参数值预测的质量函数完全一致，并且与和谐宇宙学模型（m = 0：3; 8 = 0：9）不一致，假设宇宙是平坦的。试图与和谐模型保持一致，需要人为地将光度-质量关系的归一化降低2倍。结论. m和8的最佳拟合值的变化对集群丰度的预测有显着影响。新的WMAP结果现在与先前根据HIFLUGCS星团和其他X射线星团样本的质量函数确定的m-8关系的结果完全一致（“低星团归一化”）。我们的结论是，除非m和8的真实值与第三年WMAP的结果有显著差异，否则光度-质量关系可以很好地描述为之前从星团的X射线观测中确定的结果，偏差因子的保守上限为1.5。这些结论目前正在测试直接在一个完整的后续计划的所有HIFLUGCS集群与钱德拉和XMM-Newton。
Context. The 3rd year WMAP results mark a shift in best fit values of cosmological parameters compared to the 1st year data and the concordance cosmological model. Aims. We test the consistency of the new results with previous constraints on cosmological parameters from the HIFLUGCS galaxy cluster sample and the impact of this shift on the X-ray luminosity‐gravitational mass relation. Methods. The measured X-ray luminosity function combined with the observed luminosity‐mass relation are compared to mass functions predicted for given cosmological parameter values. Results. The luminosity function and luminosity‐mass relation derived previously from HIFLUGCS are in perfect agreement with mass functions predicted using the best fit parameter values from the 3rd year WMAP data ( m = 0:238; 8 = 0:74) and inconsistent with the concordance cosmological model ( m = 0:3; 8 = 0:9), assuming a flat Universe. Trying to force consistency with the concordance model requires artificially decreasing the normalization of the luminosity‐mass relation by a factor of 2. Conclusions. The shift in best fit values for m and 8 has a significant impact on predictions of cluster abundances. The new WMAP results are now in perfect agreement with previous results on the m‐ 8 relation determined from the mass function of HIFLUGCS clusters and other X-ray cluster samples (the “low cluster normalization”). We conclude that ‐ unless the true values of m and 8 di er significantly from the 3rd year WMAP results ‐ the luminosity‐mass relation is well described by their previous determination from X-ray observations of clusters, with a conservative upper limit on the bias factor of 1.5. These conclusions are currently being tested directly in a complete follow-up program of all HIFLUGCS clusters with Chandra and XMM-Newton.