Streams on FIRE: Populations of Detectable Stellar Streams in the Milky Way and FIRE-猫眼课题宝

DOI：

10.3847/1538-4357/acc582

发表时间：

2022-08

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

N. Shipp;N. Panithanpaisal;L. Necib;R. Sanderson;D. Erkal;Ting S. Li;I. Santistevan;A. Wetzel;L. Cullinane;A. Ji;Sergey E. Koposov;K. Kuehn;G. Lewis;A. Pace;D. Zucker;J. Bland-Hawthorn;E. Cunningham;Stacy Y. Kim;Sophia Lilleengen;J. Moreno;Sanjib Sharma

我们首次详细比较了在宇宙学模拟和银河系中矮小星系恒星流的数量。特别是，我们比较了在FIRE-2模拟中识别的大约13个银河系类似物的流与南方恒星流光谱调查(S 5)观测到的流。为了进行准确的比较，我们制作了对火流的模拟暗能量调查(DES)观测，并估计了它们的潮汐尾巴和前驱物质的可探测性。可探测恒星流的数量和恒星质量分布在观测和模拟之间是一致的。然而，近心和远心的分布存在差异，平均而言，可探测到的火流形成在较大的近心(到&gt；110kpc)，并且只存在于较大的远点(≳40kpc)，而不是在银河系中观察到的。我们发现银河系中大质量矮星星系流的数量是不完整的。有趣的是，在类似DES的观测中，很大一部分火流只会被检测到是完整的卫星，因为它们的潮汐尾巴表面亮度太低，无法检测到。因此，我们预测了银河系卫星周围尚未检测到的潮汐尾巴的数量，以及完全未检测到的低表面亮度恒星流的数量，并利用鲁宾天文台估计了它们的可探测性。最后，我们讨论了火焰和银河系中流种群差异的原因和意义，并探索了未来在宇宙学模拟中测试卫星干扰的途径。

We present the first detailed comparison of populations of dwarf galaxy stellar streams in cosmological simulations and the Milky Way. In particular, we compare streams identified around 13 Milky Way analogs in the FIRE-2 simulations to streams observed by the Southern Stellar Stream Spectroscopic Survey (S 5). For an accurate comparison, we produce mock Dark Energy Survey (DES) observations of the FIRE streams and estimate the detectability of their tidal tails and progenitors. The number and stellar mass distributions of detectable stellar streams is consistent between observations and simulations. However, there are discrepancies in the distributions of pericenters and apocenters, with the detectable FIRE streams, on average, forming at larger pericenters (out to >110 kpc) and surviving only at larger apocenters (≳40 kpc) than those observed in the Milky Way. We find that the population of high-stellar-mass dwarf galaxy streams in the Milky Way is incomplete. Interestingly, a large fraction of the FIRE streams would only be detected as intact satellites in DES-like observations, since their tidal tails have too low surface brightness to be detectable. We thus predict a population of yet-undetected tidal tails around Milky Way satellites, as well as a population of fully undetected low-surface-brightness stellar streams, and estimate their detectability with the Rubin Observatory. Finally, we discuss the causes and implications of the discrepancies between the stream populations in FIRE and the Milky Way, and explore future avenues for tests of satellite disruption in cosmological simulations.

Streams on FIRE: Populations of Detectable Stellar Streams in the Milky Way and FIRE

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