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Dark matter cores and cusps in spiral galaxies and their explanations
Journal of Cosmology and Astroparticle Physics ( IF 5.3 ) Pub Date : 2020-06-12 , DOI: 10.1088/1475-7516/2020/06/027
Manoj Kaplinghat 1 , Tao Ren 2 , Hai-Bo Yu 2
Affiliation  

Author(s): Kaplinghat, Manoj; Ren, Tao; Yu, Hai-Bo | Abstract: We compare proposed solutions to the core vs cusp issue of spiral galaxies, which has also been framed as a diversity problem, and demonstrate that the cuspiness of dark matter halos is correlated with the stellar surface brightness. We compare the rotation curve fits to the SPARC sample from a self-interacting dark matter (SIDM) model, which self-consistently includes the impact of baryons on the halo profile, and hydrodynamical N-body simulations with cold dark matter (CDM). The SIDM model predicts a strong correlation between the core size and the stellar surface density, and it provides the best global fit to the data. The CDM simulations without strong baryonic feedback effects fail to explain the large dark matter cores seen in low surface brightness galaxies. On the other hand, with strong feedback, CDM simulations do not produce galaxy analogs with high stellar and dark matter densities, and therefore they have trouble in explaining the rotation curves of high surface brightness galaxies. This implies that current feedback implementations need to be modified. We also explicitly show how the concentration-mass and stellar-to-halo mass relations together lead to a radial acceleration relation (RAR) in an averaged sense, and reiterate the point that the RAR does not capture the diversity of galaxy rotation curves in the inner regions. These results make a strong case for SIDM as the explanation for the cores and cusps of field galaxies.

中文翻译:

螺旋星系中的暗物质核心和尖点及其解释

作者(S):Kaplinghat,Manoj;任涛;于海波 | 摘要:我们比较了螺旋星系核心与尖点问题的解决方案,该问题也被视为一个多样性问题,并证明暗物质晕的尖点与恒星表面亮度相关。我们比较了自相互作用暗物质 (SIDM) 模型中 SPARC 样本的旋转曲线拟合,该模型自洽地包括重子对光晕轮廓的影响,以及冷暗物质 (CDM) 的流体动力学 N 体模拟。SIDM 模型预测了核心尺寸和恒星表面密度之间的强相关性,它为数据提供了最佳的全局拟合。没有强重子反馈效应的 CDM 模拟无法解释在低表面亮度星系中看到的大暗物质核心。另一方面,由于反馈很强,CDM 模拟不会产生具有高恒星和暗物质密度的星系类似物,因此它们在解释高表面亮度星系的旋转曲线方面存在困难。这意味着需要修改当前的反馈实现。我们还明确地展示了浓度-质量和恒星-晕质量关系如何共同导致平均意义上的径向加速度关系(RAR),并重申 RAR 没有捕捉到星系旋转曲线的多样性这一点。内部区域。这些结果有力地证明了 SIDM 可以解释场星系的核心和尖端。因此他们难以解释高表面亮度星系的旋转曲线。这意味着需要修改当前的反馈实现。我们还明确地展示了浓度-质量和恒星-晕质量关系如何共同导致平均意义上的径向加速度关系(RAR),并重申 RAR 没有捕捉到星系旋转曲线的多样性这一点。内部区域。这些结果有力地证明了 SIDM 可以解释场星系的核心和尖端。因此他们难以解释高表面亮度星系的旋转曲线。这意味着需要修改当前的反馈实现。我们还明确地展示了浓度-质量和恒星-晕质量关系如何共同导致平均意义上的径向加速度关系(RAR),并重申 RAR 没有捕捉到星系旋转曲线的多样性这一点。内部区域。这些结果有力地证明了 SIDM 可以解释场星系的核心和尖端。并重申 RAR 没有捕捉到内部区域星系旋转曲线的多样性。这些结果有力地证明了 SIDM 可以解释场星系的核心和尖端。并重申 RAR 没有捕捉到内部区域星系旋转曲线的多样性。这些结果有力地证明了 SIDM 可以解释场星系的核心和尖端。
更新日期:2020-06-12
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