Mass of the dynamically hot inner stellar halo predicts the ancient accreted stellar mass
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aa42496-21.pdf
Description
Published version
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8.34 MB
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Author(s)
Zhu, Ling
Pillepich, Annalisa
van de Ven, Glenn
Leaman, Ryan
Hernquist, Lars
Nelson, Dylan
Pakmor, Ruediger
Vogelsberger, Mark
Zhang, Le
Date Issued
April 2022
Journal
Astronomy & Astrophysics
Publisher
EDP Sciences
Citation
Zhu, Ling, Pillepich, Annalisa, van de Ven, Glenn, Leaman, Ryan, Hernquist, Lars et al. 2022. "Mass of the dynamically hot inner stellar halo predicts the ancient accreted stellar mass." Astronomy & Astrophysics, 660.
Version
Final published version
Abstract
Galactic dynamical structures are fossil records of the assembly histories of galaxies. By analyzing the cosmological hydrodynamical simulation TNG50, we find that a dynamical structure that we call the “hot inner stellar halo”, defined by stars on dynamically hot orbits with circularity λz < 0.5 at 3.5 kpc < r ≲ 2 Re, is a strong indicator of the mass of accreted satellite galaxies. We find a strong correlation between the mass of this hot inner stellar halo and the total ex situ stellar mass. There is a similarly strong correlation with the stellar mass of the most massive secondary galaxy ever merged. These TNG50 correlations are compatible with those predicted by other simulations, for example by TNG100 across the whole mass range under study (galaxy stellar masses, M*, in the 1010.3 − 11.6 M⊙ range) and by EAGLE for M* ≳ 1010.6 M⊙ galaxies. This shows that our predictions are robust across different galaxy formation and feedback models and hold across a wide range of numerical resolution. The hot inner stellar halo is a product of massive and typically ancient mergers, with inner-halo stars exhibiting three main physical origins: accreted and stripped from massive satellites, dynamically heated by mergers from the bulge and/or disk in the main progenitor, and formed from star formation triggered during mergers. The mass of the hot inner stellar halo defined in this paper is a quantity that can be robustly obtained for real galaxies by applying a population-orbit superposition method to integral-field-unit spectroscopy data, out to a distance of ∼2 Re, which is possible with current observations. Hence, this paper shows that integral-field-unit observations and dynamical models of the inner regions of galaxies provide a way to quantitatively determine the mass of ancient accreted satellites.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1051/0004-6361/202142496
