Observable tests of self-interacting dark matter in galaxy clusters: BCG wobbles in a constant density core
Observable tests of self-interacting dark matter in galaxy clusters: BCG wobbles in a constant density core
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星系团中自相互作用暗物质的可观测测试：BCG 在恒定密度核心中摆动
DOI：
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发表时间：
2018
影响因子：
4.8
通讯作者：
I. McCarthy
中科院分区：
文献类型：
--
作者：
D. Harvey;A. Robertson;R. Massey;I. McCarthy
冷暗物质模型(CDM)预测，星系团中暗物质的分布应该是尖峰的，集中在中心。恒定密度核心将是超越清洁发展机制物理的有力证据，例如自相互作用暗物质(SIDM)。一个可观测的结果将是最亮的星系团(BCG)在其他松弛的星系团中的振荡。偏移量的BCG确实被观测到了--但只是通过一个简化的振荡解析模型来解释的。我们将这些观测与MASK Sysmtes(巴哈马)-SIDM宇宙学模拟套件的重子和晕进行了比较，其中包括SIDM和恒星形成和反馈的完全流体动力学处理。我们预测，在10kpc范围内，BCGs的中值偏移量随着SIDM截面、星团质量和恒星质量的增加而增加，而CDM的质量没有变化。在模拟截面之间进行内插，我们发现(10个集群的)观测结果与清洁发展机制在∼1.5cm2σ水平上是一致的，在68%(95%)的置信度水平下，更倾向于截面σ/m<；0.12(0.39)/cm2 g−1。这即将排除与速度无关的暗物质自身相互作用作为解决矮小星系预测和观测行为之间差异的解决方案，并将通过欧几里德或超压气球成像望远镜(SuperBIT)进行更大规模的调查来改进。
Models of cold dark matter (CDM) predict that the distribution of dark matter in galaxy clusters should be cuspy, centrally concentrated. Constant density cores would be strong evidence for beyond CDM physics, such as self-interacting dark matter (SIDM). An observable consequence would be oscillations of the brightest cluster galaxy (BCG) in otherwise relaxed galaxy clusters. Offset BCGs have indeed been observed – but only interpreted via a simplified, analytic model of oscillations. We compare these observations to the BAryons and HAloes of MAssive Sysmtes (BAHAMAS)–SIDM suite of cosmological simulations, which include SIDM and a fully hydrodynamical treatment of star formation and feedback. We predict that the median offset of BCGs increases with the SIDM cross-section, cluster mass, and the amount of stellar mass within 10 kpc, while CDM exhibits no trend in mass. Interpolating between the simulated cross-sections, we find that the observations (of 10 clusters) are consistent with CDM at the ∼1.5σ level, and prefer cross-section σ/m < 0.12(0.39) cm2 g−1 at 68 per cent (95 per cent) confidence level. This is on the verge of ruling out velocity-independent dark matter self-interactions as the solution to discrepancies between the predicted and observed behaviour of dwarf galaxies, and will be improved by larger surveys by Euclid or Super-pressure Balloon-borne Imaging Telescope (SuperBIT).
哈勃太空望远镜结合强弱透镜分析碰撞样本：质量和放大率模型以及系统不确定性
DOI：
10.1088/0004-637x/801/1/44
发表时间：
2015
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Zitrin;A. Fabris;J. Merten;P. Melchior;M. Meneghetti;A. Koekemoer;D. Coe;M. Maturi;M. Bartelmann;M. Postman;K. Umetsu;G. Seidel;I. Sendra;T. Broadhurst;I. Balestra;A. Biviano;C. Grillo;A. Mercurio;M. Nonino;P. Rosati;L. Bradley
通讯作者：
L. Bradley
影响因子：
8.6
作者：
Akerib, D. S.;Araujo, H. M.;Zhang, C.
通讯作者：
Zhang, C.