Optimal Chandra and XMM-Newton Bandpasses for Detecting Low-Temperature Groups and Clusters of Galaxies
Optimal Chandra and XMM-Newton Bandpasses for Detecting Low-Temperature Groups and Clusters of Galaxies
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用于探测低温星系团和星系团的最佳钱德拉和 XMM-牛顿带通
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发表时间：
2002
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通讯作者：
C. Scharf
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作者：
C. Scharf
在这篇简短的文章中，我展示了钱德拉和xmm -牛顿天文台探测到的星系团或星系团x射线发射的最大或最佳信噪能带的计算结果。利用观测所得的背景光谱和模型网格，我表明，对于气体温度大于2 keV且红移z < 1的星团，“经典”的0.5-2 keV波段确实接近最佳。然而，对于较冷的系统，这个波段通常远不是最佳的。与最佳频段相比，亚kev等离子体可能遭受20%-60%的信噪比损失，而z >的情况更糟。这意味着，当前和未来的调查应谨慎构建，以尽量减少对群集/群体人口中低质量、低温末端的偏见。
In this short paper I present the results of a calculation that seeks the maximum, or optimal, signal-to-noise energy band for galaxy group or cluster X-ray emission detected by the Chandra and XMM-Newton observatories. Using a background spectrum derived from observations and a grid of models, I show that the "classical" 0.5-2 keV band is indeed close to optimal for clusters with gas temperatures greater than 2 keV and redshifts z < 1. For cooler systems, however, this band is generally far from optimal. Sub-keV plasmas can suffer 20%-60% signal-to-noise loss, compared to an optimal band, and worse for z > 0. The implication is that current and forthcoming surveys should be carefully constructed in order to minimize bias against the low-mass, low-temperature end of the cluster/group population.