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arXiv 1909.02630astro-ph.GA
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御夫座模拟的球状星团系统

The globular cluster system of the Auriga simulations

Timo L. R. Halbesma, Robert J. J. Grand, Facundo A. Gómez, Federico Marinacci, Rüdiger Pakmor, Wilma H. Trick, Philipp Busch, Simon D. M. White

备注：
Accepted by MNRAS 2020 May 15. Received 2020 May 14; in original form 2019 September 5
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摘要：

我们调查是否用于御夫座模拟星系和恒星形成模型可以产生一个现实的球状星团（GC）人口。我们比较了御夫座晕中GC候选恒星粒子的统计数据与银河系（MW）和仙女座（M31）GC种群的目录。我们发现，御夫座模拟产生足够的恒星质量的GC候选人的半径和金属丰度是典型的MW GC系统（GCS）。我们还发现不同的质量比的模拟GC候选人相对于观察到的质量在MW和M31 GC系统的不同箱的银河中心半径金属丰度（r $_{\text{gal}}$ -[Fe/H]）。总体而言，御夫座模拟产生的GC候选者具有比MW和M31 GCS更高的金属丰度，并且它们的半径比观测到的更大。御夫座的模拟要求贫金属GC候选者的束缚团簇形成效率高于10%，而太阳半径内的那些应该经历可以忽略不计的破坏率才能与观测结果一致。另一方面，外晕中的GC候选者要么具有低形成效率，要么经历Auriga模拟的高质量损失，以产生与MW或M31一致的GCS。最后，不同Auriga运行之间的金属丰度和径向分布的分散程度远小于MW和M31 GC之间的差异。御夫座模型不太可能产生与两个星系一致的GCS。

英文摘要：

We investigate whether the galaxy and star formation model used for the Auriga simulations can produce a realistic globular cluster (GC) population. We compare statistics of GC candidate star particles in the Auriga haloes with catalogues of the Milky Way (MW) and Andromeda (M31) GC populations. We find that the Auriga simulations do produce sufficient stellar mass for GC candidates at radii and metallicities that are typical for the MW GC system (GCS). We also find varying mass-ratios of the simulated GC candidates relative to the observed mass in the MW and M31 GC systems for different bins of galactocentric radius-metallicity (r$_{\text{gal}}$ -[Fe/H]). Overall, the Auriga simulations produce GC candidates with higher metallicities than the MW and M31 GCS and they are found at larger radii than observed. The Auriga simulations would require bound cluster formation efficiencies higher than ten percent for the metal-poor GC candidates, and those within the Solar radius should experience negligible destruction rates to be consistent with observations. GC candidates in the outer halo, on the other hand, should either have low formation efficiencies, or experience high mass loss for the Auriga simulations to produce a GCS that is consistent with that of the MW or M31. Finally, the scatter in the metallicity as well as in the radial distribution between different Auriga runs is considerably smaller than the differences between that of the MW and M31 GCSs. The Auriga model is unlikely to give rise to a GCS that can be consistent with both galaxies.

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