Left panel: cumulative distributions of Symphony subhalos' z = 0 virial mass, M sub , divided by the largest virial mass achieved along each subhalo's main branch, M peak,sub , stacked over all subhalos from each suite with M sub /M host > 2.7 × 10 −4 . Right panel: same as the left panel, for the ratio of z = 0 maximum circular velocity, V max,sub , to the largest V max,sub achieved along each subhalo's main branch, V peak,sub .

Left panel: cumulative distributions of Symphony subhalos' z = 0 virial mass, M sub , divided by the largest virial mass achieved along each subhalo's main branch, M peak,sub , stacked over all subhalos from each suite with M sub /M host > 2.7 × 10 −4 . Right panel: same as the left panel, for the ratio of z = 0 maximum circular velocity, V max,sub , to the largest V max,sub achieved along each subhalo's main branch, V peak,sub .

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We present Symphony, a compilation of 262 cosmological, cold-dark-matter-only zoom-in simulations spanning four decades of host halo mass, from 10 ¹¹ –10 ¹⁵ M ⊙ . This compilation includes three existing simulation suites at the cluster and Milky Way–mass scales, and two new suites: 39 Large Magellanic Cloud-mass (10 ¹¹ M ⊙ ) and 49 strong-lens-ana...

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... subhalos with earlier infall times, comparable to the half-mass scale factors of the LMC, Milky Way, and Group hosts, are likely to be tidally stripped below this resolution limit by z = 0. Exploring the detailed dependence of subhalo population statistics on accretion time (e.g., following Green et al. 2021) is an interesting area for future work. Figure 16 shows cumulative distributions of M sub /M peak,sub and V V max,sub peak,sub for subhalos above our conservative subto-host halo mass resolution limit of M sub /M host > 2.7 × 10 −4 , stacked over all hosts within each Symphony suite. Subhalos above this limit typically retain ≈50% of their peak mass and ≈80% of their peak maximum circular velocity. ...

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... A. Radial Distribution Figure 1 shows the spatial distribution predicted by galacticus for a 10 13 M ⊙ halo at z = 0.5, with both the evolved and unevolved distributions plotted. Alongside the galacticus prediction, results are shown for Symphony [57] and Han et al. [34] model of the spatial distribution. We plot the ratio of the radial distribution of subhalos to the host's dark matter density in Figure 2. ...
... Similarly, Over the entire virial volume we find similar results, with Symphony predicting around 40% the number of subhalos as galacticus. We note that Symphony and galacticus agree within halo to halo scatter, and N-body simulations such as Symphony and Caterpillar disagree on the 25% level [57]. We also find that the suppression of the subhalo mass function due to the potential of the central galaxy is negligible when compared to the current theoretical uncertainty. ...
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... ntrated hosts in SAGA DR3, while the average SAGA DR3 and ELVES R 50 values are significantly larger than the MW population even at 1-2 Gyr ago. Sausage-Enceladus merger (V. Belokurov et al. 2018;A. Helmi et al. 2018). B24 also study the properties of 45 isolated MW halos from the Symphony Milky Way suite as a control sample (Y.-Y. Mao et al. 2015;E. O. Nadler et al. 2023). Since the MW satellite sample used in this analysis is not complete to the equivalent magnitude of the MW-est resolution limits, 7 we refrain from a quantitative comparison with B24 and instead focus on general trends in our results. ...
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Preprint
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... We resimulate two Milky Way-est hosts (Halo004 and Halo113; Buch et al. 2024) and one Symphony Milky Way host (Halo023; Nadler et al. 2023). We refer to the Milky Way-est hosts as "MW-like," because they contain LMC analog subhalos and merge with Gaia-Sausage-Enceladus (GSE) analogs; we refer to the Symphony Milky Way host as "MW-mass" because it is only constrained to have a host halo mass similar to the MW. ...
... We choose these hosts due to their small Lagrangian volumes, which makes them relatively inexpensive to resimulate. For each simulation, we initialize a region at z = 99 that corresponds to the Lagrangian volume of particles within 10 times the virial radius of the host halo in the parent box at z = 0, following Nadler et al. (2023). Thus, the models we simulate do not suppress P(k) on scales larger than the zoom-in region, which corresponds to a wavenumber k L = 2π/(3 Mpc) ≈ 2 Mpc −1 . ...
Preprint
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... Semi-analytic tools are an efficient way to rapidly generate multiple realizations of disrupted satellite populations, varying host properties (Koposov et al. 2009;Li et al. 2010;Macciò et al. 2010;Guo et al. 2011;Font et al. 2011;Benson 2012;Brooks et al. 2013b;Starkenburg et al. 2013;Barber et al. 2014;Pullen et al. 2014;Guo et al. 2015;Lu et al. 2016;Jiang & van den Bosch 2016;Nadler et al. 2019;Yang et al. 2020;Jiang et al. 2021;Nadler et al. 2023). In this work, we extend SatGen, a semi-analytical satellite galaxy generator that can efficiently produce satellite populations for a large number of host halos (Jiang et al. 2021). ...
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In this work, we study how the abundance and dynamics of populations of disrupting satellite galaxies change systematically as a function of host galaxy properties. We apply a theoretical model of the phase-mixing process to classify intact satellite galaxies, stellar stream-like and shell-like debris in ~1500 Milky Way-mass systems generated by a semi-analytic galaxy formation code, SatGen. In particular, we test the effect of host galaxy halo mass, disk mass, ratio of disk scale height to length, and stellar feedback model on disrupting satellite populations. We find that the counts of tidal debris are consistent across all host galaxy models, within a given host mass range, and that all models can have stream-like debris on low-energy orbits, consistent with those observed around the Milky Way. However, we find a preference for stream-like debris on lower-energy orbits in models with a thicker (lower-density) host disk or on higher-energy orbits in models with a more-massive host disk. Importantly, we observe significant halo-to-halo variance across all models. These results highlight the importance of simulating and observing large samples of Milky Way-mass galaxies and accounting for variations in host properties when using disrupting satellites in studies of near-field cosmology.