The weak connection between the stellar haloes and merger histories of Milky Way-mass galaxies
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| Main Authors: | , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866909764292706304 |
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| author | Proctor, Katy L. Ludlow, Aaron D. Lagos, Claudia del P. Robotham, Aaron S. G. |
| author_facet | Proctor, Katy L. Ludlow, Aaron D. Lagos, Claudia del P. Robotham, Aaron S. G. |
| contents | Stellar haloes form through the disruption of satellite galaxies over time, making them a promising observable for constraining galaxy merger histories. We use a dynamical decomposition technique to isolate the stellar haloes of Milky Way-mass galaxies in the $100\,{\rm Mpc}$ EAGLE simulation and study their relationship to the merger histories of their hosts. We define the stellar halo as the stellar mass that is bound to the central subhalo but not associated with the disc or bulge components of a galaxy, and we quantify their merger histories using the most significant merger since $z=1$. Surprisingly, we find that the fraction of a galaxy's total stellar mass in the stellar halo, $f_{\rm SH}$, is not a reliable indicator of its merger activity. Contrary to common assumptions, disc galaxies with low $f_{\rm SH}$ do not necessarily have quiescent merger histories. In fact, roughly one quarter experienced a merger at $z \leq 1$ with a satellite whose stellar mass was at least 10 per cent of the host galaxy's stellar mass. These galaxies undergo mergers with satellites on circular orbits that are roughly co-planar with the pre-existing disc and thereby avoid contributing mass to the stellar halo. Instead, such mergers build thick, extended discs and supply fresh gas that often triggers a significant episode of star formation in the disc. Our results suggest that disc galaxies with low-mass stellar haloes, such as the Milky Way, can have varied and active merger histories, and that stellar haloes may not be a reliable tool for inferring galaxy merger histories. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2407_11444 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | The weak connection between the stellar haloes and merger histories of Milky Way-mass galaxies Proctor, Katy L. Ludlow, Aaron D. Lagos, Claudia del P. Robotham, Aaron S. G. Astrophysics of Galaxies Stellar haloes form through the disruption of satellite galaxies over time, making them a promising observable for constraining galaxy merger histories. We use a dynamical decomposition technique to isolate the stellar haloes of Milky Way-mass galaxies in the $100\,{\rm Mpc}$ EAGLE simulation and study their relationship to the merger histories of their hosts. We define the stellar halo as the stellar mass that is bound to the central subhalo but not associated with the disc or bulge components of a galaxy, and we quantify their merger histories using the most significant merger since $z=1$. Surprisingly, we find that the fraction of a galaxy's total stellar mass in the stellar halo, $f_{\rm SH}$, is not a reliable indicator of its merger activity. Contrary to common assumptions, disc galaxies with low $f_{\rm SH}$ do not necessarily have quiescent merger histories. In fact, roughly one quarter experienced a merger at $z \leq 1$ with a satellite whose stellar mass was at least 10 per cent of the host galaxy's stellar mass. These galaxies undergo mergers with satellites on circular orbits that are roughly co-planar with the pre-existing disc and thereby avoid contributing mass to the stellar halo. Instead, such mergers build thick, extended discs and supply fresh gas that often triggers a significant episode of star formation in the disc. Our results suggest that disc galaxies with low-mass stellar haloes, such as the Milky Way, can have varied and active merger histories, and that stellar haloes may not be a reliable tool for inferring galaxy merger histories. |
| title | The weak connection between the stellar haloes and merger histories of Milky Way-mass galaxies |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2407.11444 |