Left panel: cumulative distributions of Symphony subhalos' most recent (solid, thick lines) and first (thin, dotted-dashed lines) accretion scale factors into any larger halo, stacked over all subhalos from each suite with M sub /M host > 2.7 × 10 −4 . Top ticks indicate lookback time assuming the cosmological parameters for our LMC, Milky Way, and Group suites. Right panel: same as the left panel, but with accretion scale factors normalized by the half-mass scale factor of each Symphony host. The legend indicates the mean half-mass scale factors for the LMC (pink), Milky Way (blue), Group (green), L-Cluster (gold), and Cluster (red) suites (see Table 1).

Left panel: cumulative distributions of Symphony subhalos' most recent (solid, thick lines) and first (thin, dotted-dashed lines) accretion scale factors into any larger halo, stacked over all subhalos from each suite with M sub /M host > 2.7 × 10 −4 . Top ticks indicate lookback time assuming the cosmological parameters for our LMC, Milky Way, and Group suites. Right panel: same as the left panel, but with accretion scale factors normalized by the half-mass scale factor of each Symphony host. The legend indicates the mean half-mass scale factors for the LMC (pink), Milky Way (blue), Group (green), L-Cluster (gold), and Cluster (red) suites (see Table 1).

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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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Context 1
... Figure 15 shows cumulative infall time distributions for subhalos above our conservative resolution limit of M sub / M host > 2.7 × 10 −4 , stacked over all hosts within each Symphony suite. Infall times are measured using the Acc_Scale (solid, thick distributions) and First_Acc_S-cale (thin, dashed distributions) output by CONSISTENT-TREES. ...
Context 2
... particular, the fraction of splashback subhalos is larger for lower-mass hosts because they are older and accrete more slowly than higher-mass hosts. Thus, we expect a larger difference between the first and most recent accretion scale factors for subhalos of lower-mass hosts, which is consistent with both panels of Figure 15. For the LMC, Milky Way, and Group suites, the flattening of the first accretion scale factor cumulative distributions in the left panel of Figure 15 starts near t lookback ≈ 2 Gyr, roughly one orbital timescale ago, and extends to t lookback ≈ 5 Gyr. ...
Context 3
... we expect a larger difference between the first and most recent accretion scale factors for subhalos of lower-mass hosts, which is consistent with both panels of Figure 15. For the LMC, Milky Way, and Group suites, the flattening of the first accretion scale factor cumulative distributions in the left panel of Figure 15 starts near t lookback ≈ 2 Gyr, roughly one orbital timescale ago, and extends to t lookback ≈ 5 Gyr. This is consistent with the expectation that many subhalos of lowermass hosts accreted within the last few orbital timescales are splashback objects at z = 0 (e.g., Barber et al. 2014). ...
Context 4
... shown in the right panel of Figure 15, the dependence of infall time on host mass is reversed when measured in units of the host's formation time. In particular, relative to their hosts' half-mass scale factors, subhalos of higher-mass hosts accrete earlier than subhalos of lower-mass hosts. ...
Context 5
... above the mass resolution limit, regardless of whether an M sub > 300m part cut is applied. Mass loss is slightly enhanced for subhalos of lower-mass hosts, likely due to a combination of their earlier infall times ( Figure 15) and their hosts' higher concentrations (Figure 3). Meanwhile, subhalos of lower-mass hosts retain slightly more of their peak maximum circular velocity than subhalos of higher-mass hosts. ...

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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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... Ref.[42] analyze SHMFs using peak (rather than present-day) subhalo mass. We measure SHMFs using present-day mass because Galacticus CDM predictions match recent zoom-in simulation results in this regard[47,71], while peak SHMFs are more sensitive to resolution cuts and halo finding algorithms[56]. ...
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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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... 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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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.