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arXiv 1609.08644astro-ph.COastro-ph.GA
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星系团中的标量场暗物质

Scalar field dark matter in clusters of galaxies

Tula Bernal, Victor H. Robles, Tonatiuh Matos

备注：
17 pages, 8 figures. This version matches the published version in MNRAS
发表信息：
MNRAS 468, 3135-3149 (2017)
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摘要：

冷暗物质（CDM）范式的一个替代方案是标量场暗物质（SFDM）模型，该模型假设暗物质是具有典型质量$m\sim10^{-22}\mathrm{eV}/c^2$和正自相互作用的自旋0超轻标量场（SF）。由于超轻玻色子的质量，SFDM可以在非常早期的宇宙中形成玻色-爱因斯坦凝聚体（BEC），这被解释为暗物质晕。虽然在宇宙学上，该模型的行为与CDM相似，但它们在小尺度上有所不同：SFDM自然地预测了更少的卫星晕，矮星系的核心和高红移的大质量星系的形成。零温度下的基态（或BEC）解足以描述低质量星系，但不能描述更大的系统。一个可能的解决方案是增加有限温度修正的SF势，它允许组合的激发态。在这项工作中，我们测试有限温度多态SFDM解决方案在星系团尺度和比较我们的结果与Navarro-Frenk-White（NFW）和BEC配置文件。我们通过拟合13个\textit{Chandra} X射线星系团的质量分布来实现这一点，不包括最亮的星系团。我们发现，SFDM模型准确地描述了集群的DM质量分布提供了一个等价的或更好的协议比NFW配置文件。BEC模型与数据的完全不一致也显示。我们的结论是，理论上动机的多态SFDM配置文件是一个有趣的替代经验配置文件和特设拟合函数，试图耦合渐近NFW下降与内核SFDM。

英文摘要：

One alternative to the cold dark matter (CDM) paradigm is the scalar field dark matter (SFDM) model, which assumes dark matter is a spin-0 ultra-light scalar field (SF) with a typical mass $m\sim10^{-22}\mathrm{eV}/c^2$ and positive self-interactions. Due to the ultra-light boson mass, the SFDM could form Bose-Einstein condensates (BEC) in the very early Universe, which are interpreted as the dark matter haloes. Although cosmologically the model behaves as CDM, they differ at small scales: SFDM naturally predicts fewer satellite haloes, cores in dwarf galaxies and the formation of massive galaxies at high redshifts. The ground state (or BEC) solution at zero temperature suffices to describe low-mass galaxies but fails for larger systems. A possible solution is adding finite-temperature corrections to the SF potential which allows combinations of excited states. In this work, we test the finite-temperature multistate SFDM solution at galaxy cluster scales and compare our results with the Navarro-Frenk-White (NFW) and BEC profiles. We achieve this by fitting the mass distribution of 13 \textit{Chandra} X-ray clusters of galaxies, excluding the region of the brightest cluster galaxy. We show that the SFDM model accurately describes the clusters' DM mass distributions offering an equivalent or better agreement than the NFW profile. The complete disagreement of the BEC model with the data is also shown. We conclude that the theoretically motivated multistate SFDM profile is an interesting alternative to empirical profiles and ad hoc fitting-functions that attempt to couple the asymptotic NFW decline with the inner core in SFDM.

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