关于ngc4147暗物质形成的场景

IF 1.6 4区 物理与天体物理 Q3 ASTRONOMY & ASTROPHYSICS
Andrés E. Piatti
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引用次数: 0

摘要

我们报告了建立在NGC 4147外围的径向速度色散剖面的结果,NGC 4147是一个探测到强烈潮汐尾的银河系球状星团。从观测的角度来看,最近的模拟表明,在没有潮汐尾的球状星团中,距离星团中心很远的地方,速度分散曲线会上升,因此选择这个星团来探测。从位于NGC 4147潮尾起始处的选定恒星的红外Ca II三重态区域中心的GEMINI@GMOS光谱中,我们测量了它们的径向速度和总体金属丰度。所得的金属丰度被用于最终评估9颗恒星的高排名候选星团,它们位于距离星团中心\(\sim \) 7到33 pc之间,适合测试上述模拟。我们将现有的星系团成员的径向速度与文献中可用的其他速度进行了补充,并建立了星系团速度弥散曲线,该曲线表明,在距离星系团中心较远的地方,星系团速度弥散曲线基本持平或略有上升。这个结果证实了在NGC 4147中可以看到运动热的最外层星团恒星,这反驳了最近的模型预测。然而,最外层星团恒星的平均速度弥散与NGC 4147形成于一个\(10^8\) - \(10^9\)\(\hbox {M}_\odot \)矮星系,其核心是后来被吸积到银河系的暗物质。
本文章由计算机程序翻译,如有差异,请以英文原文为准。

On the dark matter formation scenario of NGC 4147

On the dark matter formation scenario of NGC 4147

We report results on the radial velocity dispersion profile built out to the outskirts of NGC 4147, a Milky Way globular cluster with detected strong tidal tails. The cluster was chosen to probe, from an observational point of view, recent simulations that suggest that rising velocity dispersion profiles at large distances from the clusters’ centers would be seen in globular clusters without tidal tails. From GEMINI@GMOS spectra, centered in the infrared Ca II triplet region, of selected stars located along the onset of NGC 4147’s tidal tails, we measured their radial velocities and overall metallicities. The derived metallicities were used to ultimately assess the highly-ranked cluster candidates of 9 stars, located between \(\sim \)7 and 33 pc from the cluster’s center, suitable for testing the aforementioned simulation. We complemented the present radial velocities with others available in the literature for the cluster’s members, and built a cluster velocity dispersion profile, which suggests a mostly flat or slightly rising profile at large distances from the cluster’s center. This outcome confirms that kinematically hot outermost cluster stars are seen in NGC 4147, which disproves the recent model predictions. Nevertheless, the mean velocity dispersion of the outermost cluster’s stars agrees with NGC 4147 being formed in a \(10^8\)\(10^9\) \(\hbox {M}_\odot \) dwarf galaxy with a cored dark matter profile that was later accreted to the Milky Way.

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来源期刊
Journal of Astrophysics and Astronomy
Journal of Astrophysics and Astronomy 地学天文-天文与天体物理
CiteScore
1.80
自引率
9.10%
发文量
84
审稿时长
>12 weeks
期刊介绍: The journal publishes original research papers on all aspects of astrophysics and astronomy, including instrumentation, laboratory astrophysics, and cosmology. Critical reviews of topical fields are also published. Articles submitted as letters will be considered.
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