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arXiv 1706.08296astro-ph.GA
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在$Λ$ CDM中检验重子诱导的核心形成：星系旋转曲线上DC14和coreNFW暗物质晕模型的比较

Testing baryon-induced core formation in $Λ$CDM: A comparison of the DC14 and coreNFW dark matter halo models on galaxy rotation curves

F. Allaert, G. Gentile, M. Baes

备注：
19 pages, 12 figures, accepted for publication in A&A
发表信息：
A&A 605, A55 (2017)
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摘要：

最近的宇宙流体动力学模拟表明，重子过程，特别是恒星形成爆发后的超新星反馈，可以改变暗物质晕的结构，并将原始尖点转变为较浅的核心。为了评估这种机制是否为尖核争议提供了解决方案，必须将模拟的晕与从星系旋转曲线推断出的真实暗物质晕进行比较。为此，最近从互补质量范围内的星系模拟中获得了两个新的暗物质密度分布：DC 14晕（$10^{10} < M_{\text{halo}}/M_{\odot} < 8 \times 10^{11}$）和核心NFW晕（$10^{7} < M_{\text{halo}}/M_{\odot} < 10^{9}$）。这两种模型已分别被发现，给观察到的旋转曲线很好的拟合。然而，对于DC 14模型，一项研究证实了预测的晕性质与宇宙学标度关系的一致性，但另一项研究强烈反驳了这一点。下一个问题是，这两个模型是否收敛到相同的解决方案，在质量范围内，这两个应该是适当的。为了研究这一点，我们测试了DC 14和cNFW晕模型的旋转曲线的选择星系的晕质量范围内的$4 \times 10^{9}$ - $7 \times 10^{10}$ $M_{\odot}$。我们进一步应用DC 14模型的旋转曲线在较高的晕质量，$9 \times 10^{11}$ $M_{\odot}$，验证协议的宇宙学标度关系。我们发现，这两个模型一般都能够再现观测到的旋转曲线，与早期的结果，和预测的暗物质晕是一致的宇宙学$c-M_{\text{halo}}$和$M_{*}-M_{\text{halo}}$关系。DC 14和cNFW模型也彼此相当好地一致，尽管DC 14倾向于预测比cNFW稍微少延伸的核心和稍微更集中的晕。

英文摘要：

Recent cosmological hydrodynamical simulations suggest that baryonic processes, and in particular supernova feedback after bursts of star formation, can alter the structure of dark matter haloes and transform primordial cusps into shallower cores. To assess whether this mechanism offers a solution to the cusp-core controversy, simulated haloes must be compared to real dark matter haloes inferred from galaxy rotation curves. For this purpose, two new dark matter density profiles were recently derived from simulations of galaxies in complementary mass ranges: the DC14 halo ($10^{10} < M_{\text{halo}}/M_{\odot} < 8 \times 10^{11}$) and the coreNFW halo ($10^{7} < M_{\text{halo}}/M_{\odot} < 10^{9}$). Both models have individually been found to give good fits to observed rotation curves. For the DC14 model, however, the agreement of the predicted halo properties with cosmological scaling relations was confirmed by one study, but strongly refuted by another. A next question is whether the two models converge to the same solution in the mass range where both should be appropriate. To investigate this, we tested the DC14 and cNFW halo models on the rotation curves of a selection of galaxies with halo masses in the range $4 \times 10^{9}$ - $7 \times 10^{10}$ $M_{\odot}$. We further applied the DC14 model to a set of rotation curves at higher halo masses, up to $9 \times 10^{11}$ $M_{\odot}$, to verify the agreement with the cosmological scaling relations. We find that both models are generally able to reproduce the observed rotation curves, in line with earlier results, and the predicted dark matter haloes are consistent with the cosmological $c-M_{\text{halo}}$ and $M_{*}-M_{\text{halo}}$ relations. The DC14 and cNFW models are also in fairly good agreement with each other, even though DC14 tends to predict slightly less extended cores and somewhat more concentrated haloes than cNFW.

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