Pith. sign in

REVIEW 3 major objections 6 minor 172 references

Mass Modeling the Andromeda Dwarf Galaxies: Andromeda VI and Andromeda XXIII

T0 review · 3 major / 6 minor · reviewed 2026-08-15 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read Dynamical mass modeling of two Andromeda dwarf galaxies places And VI in the cuspy dark-matter regime and And XXIII in a lower-density, possibly tidal regime.

desk verdict Adds two mass-modeled M31 dwarfs, including a claimed cuspy one, but the cusp/core split is prior-driven and needs a wider-prior rerun before I'd trust the classification. read the letter →

arxiv 2505.04475 v3 pith:NWVOZ463 submitted 2025-05-07 astro-ph.GA

Connor S. Pickett , Michelle L.M. Collins , R. Michael Rich , Justin I. Read , Emily J.E. Charles , Nicolas Martin , Scott Chapman , Alan McConnachie
show 2 more authors
Alessandro Savino Daniel R. Weisz
This is my paper · ORCID
classification astro-ph.GA
keywords dwarfspheroidalgalaxiesAndromedadarkmatterdensityprofilescusp-coreproblemJeansmodelingGravSpherestarformationhistorytidalstripping
topics Dark Matter
open problems Dark Matter
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper sets out to measure the dark-matter content of two Andromeda dwarf spheroidal galaxies, Andromeda VI and Andromeda XXIII, using stellar velocities and the dynamical modeling code GravSphere. The authors report that And VI has a central dark-matter density at 150 pc of $(1.4\pm0.5)\times10^8\,M_\odot\,\mathrm{kpc}^{-3}$, high enough to fall in the cuspy regime and the first such result for a mass-modeled M31 satellite. And XXIII comes in lower, at $0.5^{+0.4}_{-0.3}\times10^8\,M_\odot\,\mathrm{kpc}^{-3}$, which the authors read as either a cored inner profile or a density lowered by tides. Because both dwarfs formed most of their stars early and then quenched, the low density of And XXIII is hard to explain by stellar feedback, making external processes or alternative dark-matter models the live options.

What carries the argument

The load-bearing tool is GravSphere, a dynamical model that solves the spherical Jeans equation for tracer stars while fitting a CoreNFWTides dark-matter profile, with the Binulator binning method supplying the velocity and surface-brightness inputs. GravSphere is intended to break the mass-anisotropy degeneracy through virial shape parameters, which use higher-order velocity moments to constrain the orbital anisotropy $\beta(r)$. That step is important because without proper motions the inferred dark-matter density at 150 pc depends on priors on the central and outer anisotropies; the paper's own diagnostic plots show that the virial shape parameters are only weakly constrained for these galaxies.

What would settle it

Measure proper motions for And VI and And XXIII, or collect enough member-star velocities to constrain the velocity-anisotropy shape, and re-run the Jeans fit; if the inferred density at 150 pc for And VI drops below the cusp/core boundary or for And XXIII rises above it, the paper's central classification would be overturned.

Watch

Extended reading notes

Core claim

The paper's central claim is that two Andromeda dwarfs of similar luminosity occupy different dark-matter regimes at 150 pc. And VI is dynamically typical: its enclosed mass within the half-light radius $M(r<r_h)=(4.9\pm1.5)\times10^7\,M_\odot$, its mass-to-light ratio $[M/L]_{r_h}=(27.1\pm8.2)$, and its central dark-matter density are all consistent with a cusped, NFW-like halo, making it the first mass-modeled M31 satellite to fall into the cuspy regime. And XXIII has a comparable enclosed mass, $(3.1\pm1.9)\times10^7\,M_\odot$, but a much lower central dark-matter density, implying either a cored inner profile or a density that tides have lowered. Because And XXIII formed 90 percent of its stars about 7.3 Gyr ago and has shown no significant star formation since, the authors argue that stellar feedback cannot explain its low density and that tidal interaction with M31 is the more plausible external cause. The result adds And XXIII to the short list of M31 dwarfs with low central densities while showing that the cuspy regime is not empty around M31.

Load-bearing premise

The recovered dark-matter densities assume both galaxies are spherical and in dynamical equilibrium, and with no proper-motion measurements the central density depends on assumptions about how stretched the stars' orbits are.

Editorial extensions

If this is right

  • If And VI's cuspy density holds, M31 satellites are not all low-density outliers; at least one is consistent with the standard cold-dark-matter cusp.
  • If And XXIII's low density is caused by tides, it joins And XXI and And XXV as evidence that the M31 environment can strip dark matter before stripping stars.
  • Because And XXIII quenched early, a low-density M31 dwarf with little star formation becomes a sharper test for tidal stripping or alternative dark-matter models rather than feedback-driven core formation.
  • Mass-modeling the remaining unmodeled M31 dwarfs will determine whether low central densities are common in that system and whether the Milky Way versus Andromeda difference is environmental rather than a universal property.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • Editorial inference: a testable extension is to measure proper motions for And VI and And XXIII; if the recovered density at 150 pc shifts across the cusp/core boundary when the anisotropy is allowed to vary, the classification of And VI as cuspy would be fragile.
  • Editorial inference: if future M31 dwarf models keep finding low central densities in early-quenched dwarfs, the most economical explanation would be that tides from M31 are systematically stronger than tides from the Milky Way, a difference that orbit measurements could directly check.
  • Editorial inference: applying the same pipeline to dwarfs with similar luminosity but different projected distances from M31 could separate tidal density lowering from feedback-driven lowering without waiting for full orbits.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. The paper presents dynamical mass modeling of two M31 dwarf spheroidals, Andromeda VI and Andromeda XXIII, using existing Subaru/PAndAS photometry and Keck/DEIMOS spectroscopy. The authors measure systemic velocities and velocity dispersions consistent with Collins et al. (2013), compute enclosed masses within the half-light radius using the Walker et al. (2009) estimator, and then run Binulator+GravSphere with CoreNFWTides models to infer dark matter density profiles. They report rho_DM(150 pc) = (1.4 ± 0.5) × 10^8 M_sun kpc^-3 for And VI and 0.5(+0.4,-0.3) × 10^8 M_sun kpc^-3 for And XXIII, interpreting And VI as cuspy and And XXIII as cored or tidally lowered. Comparisons are made with abundance matching, star formation histories, MOND, and the broader Local Group population; the paper claims And VI is the first mass-modeled M31 satellite in the cuspy regime.

Significance. Extending mass modeling from the Milky Way to the M31 satellite population is a valuable step, and the paper provides new constraints for two dwarfs with publicly available tools and data. The enclosed-mass results are consistent with prior work and rely on a nearly model-independent estimator, and the abundance-matching and MOND comparisons are drawn from independent literature rather than assumed from the inferred densities. However, the headline cusp/core classification depends on velocity-anisotropy priors because proper motions are unavailable, and the paper's own diagnostic plots show that the virial shape parameters v_s1 and v_s2 are poorly constrained. The central density values are therefore not yet robust enough to support the 'first cuspy M31 satellite' claim until wider-prior and robustness tests are supplied.

major comments (3)
  1. [Section 4.3.1, Table 7; Appendix A, Figures A5 and A6] The central-density classification rests on the assumed priors for velocity anisotropy because v_s1 and v_s2 are unconstrained; the figure captions state that these virial shape parameters are 'clearly poor' and 'poor' due to the lack of proper motions. With beta_0 fixed to [-0.01, 0.01] and beta_inf to [-0.1, 1], the recovered beta posterior is effectively the prior, so the quoted uncertainties on rho_DM(150 pc) sample only that prior. Since the cusp/core boundary in Figure 9 is a density threshold, and And VI's rho_DM(150 pc) = 1.4 ± 0.5 × 10^8 M_sun kpc^-3 is described in Section 5 as lying 'within uncertainty, nearer the cusped regime', a systematic shift from differing anisotropy priors could change the classification. Please rerun GravSphere with wider beta priors, including more tangential beta_inf values, and report how rho_DM(150 pc) and the cusp/core assignments change.
  2. [Section 3, Table 1, Appendix A Figure A2] The robustness to the density shape parameter prior n is demonstrated only for And VI; the text states 'We would anticipate a similar result for Andromeda XXIII', but this is not a substitute for the actual test. Because And XXIII's low central density is one of the paper's two central results, and because the GravSphere v1.5 prior 0 < n < 1 excludes steep cusps, please run the broader -1 < n < 1 prior for And XXIII and include the resulting rho_DM(150 pc) value and density profile.
  3. [Sections 4.1 and 4.3] The membership probability threshold P_mem >= 0.10 and the photometric distance cuts (900 pc for And VI, 1800 pc for And XXIII) are asserted to be safe but are not varied. With only 39 member stars for And XXIII, the inferred velocity dispersion, and hence rho_DM(150 pc), could depend on these choices. Please add tests that vary P_mem (for example, 0.05 and 0.15) and the distance cuts, and state whether the inferred densities and cusp/core classifications are stable.
minor comments (6)
  1. [Section 3, after Eq. (2)] The text says 'beta = 0 represents an anisotropic distribution'; this should read 'isotropic distribution'.
  2. [Figure 5 caption] The caption contains typos: 'out MCMC analysis routine' should be 'our MCMC analysis routine', and 'veloicty' should be 'velocity'.
  3. [Section 4.5, And XXIII paragraph] The sentence 'This can be seen in Figure 7' refers to the And XXIII comparison and should cite Figure 8 instead.
  4. [Table 2] The listed apparent V-band magnitude for And VI, mV = 24.6 ± 0.06, is inconsistent with MV = -11.6 at D = 831.8 kpc (which would give mV near 13, not 24.6). Please check whether this entry is a typo or whether 'mV' denotes a different quantity.
  5. [Section 4.3.1] The sentence 'While accounted for when fitting the SBP, final DM density estimations from GravSphere do not change based on solar distance measurements to the dwarf' is unclear and should be rewritten for clarity.
  6. [Equation (8)] The notation nu^2_err,i inside the square root is confusing; please use sigma^2_v,i or explicitly define the velocity uncertainty term.

Circularity Check

0 steps flagged · score 1.0 of 10

No circularity: DM densities are kinematic fit outputs; external benchmarks are independent.

full rationale

The central results — rho_DM(150 pc) for And VI and And XXIII — are outputs of a Jeans-equation fit (GravSphere) to the measured line-of-sight velocity dispersions and surface brightness profiles. They are not assumed or derived from the cusp/core classification the paper then applies. The comparisons to the Walker et al. (2009) mass estimator, to abundance matching (Read & Erkal 2019), and to MOND use independent literature relations that do not take the measured rho_DM as an input, so no fitted quantity is renamed as a prediction. The heavy citation of the authors' own code and prior papers (Read & Steger 2017; Collins et al. 2021; Charles et al. 2023) is self-citation, but the code is public and has been tested on mocks, and the cited prior analyses are not invoked to forbid alternatives or to supply the target result. The acknowledged poor constraints on the virial shape parameters v_s1 and v_s2 (Figures A5 and A6 captions: 'The results of v_s1 and v_s2 are clearly poor for this analysis') make the recovered central densities dependent on the adopted velocity-anisotropy priors, since proper motions are unavailable. That is a genuine robustness limitation, but it is not circular: the data still enter through the likelihood, and a wider prior could change the answer without making the inference tautological. No equation or parameter in the paper reduces by construction to the paper's own inputs, and the cusp/core claim is a comparison to an external theoretical band, not a consequence of the prior itself. The paper is therefore self-contained against external benchmarks, with only minor, non-load-bearing self-citation.

Assumptions & free parameters 7 free parameters · 5 assumptions · 0 invented entities

The central claim rests on the Jeans modeling family and the assumption that the adopted priors are unbiased. The paper is transparent about the equilibrium, sphericity, and stellar population assumptions, but the recovered densities are conditional on these choices.

free parameters (7)
  • M200 (virial mass) = And VI: 12.7 +/- 4.7 x 10^9 M_sun; And XXIII: 3.9 +/- 1.6 x 10^9 M_sun
    Fitted by GravSphere CoreNFWTides; the derived dark matter density profile depends on this mass scale.
  • n (dark matter density shape parameter) = Not reported in text; prior range 0 < n < 1
    Controls cusp/core shape of the inner profile; directly determines whether the dwarf is classified as cuspy or cored.
  • Velocity anisotropy priors (beta_0, beta_inf) = beta_0 in [-0.01, 0.01]; beta_inf in [-0.1, 1]
    Central anisotropy is forced to near-isotropy; the mass-anisotropy degeneracy means the recovered density depends on these priors given the absence of proper motions.
  • Membership probability threshold P_mem = 0.10
    Chosen by hand to balance contamination against losing member stars; affects the velocity dispersion and hence the mass.
  • Photometric distance cut = 900 pc (And VI), 1800 pc (And XXIII)
    Applied to exclude background stars when building the surface brightness profile; could bias the fitted half-light radius.
  • eta_CMD and eta_dist scaling parameters = eta_CMD = 0.1; eta_dist = 5
    Chosen to set the width of the RGB and the spatial membership probability; influence which stars are included as tracers.
  • Stellar mass-to-light ratio M/L = 2 M_sun/L_sun
    Assumed for old stellar populations (Simon 2019) to convert luminosity to stellar mass; affects the baryonic contribution inside 150 pc.
assumptions (5)
  • standard math The spherical Jeans equation relates the observed line-of-sight velocity dispersion to the gravitational potential and velocity anisotropy.
    Used in Equation (1) as the foundation of GravSphere; assumes spherical symmetry and dynamical equilibrium.
  • domain assumption And VI and And XXIII are in dynamical equilibrium and are approximately spherical.
    Stated in Section 6 ('We assumed that both dwarfs are in dynamical equilibrium'); the galaxies have ellipticities ~0.4, so the spherical assumption may bias results, though mock tests are cited.
  • domain assumption The CoreNFWTides model (Read et al. 2018) adequately describes dwarf galaxy dark matter profiles, including tidal truncation.
    Used as the density model in GravSphere; the recovered rho_DM(150 pc) is conditional on this family of profiles.
  • domain assumption The Padova isochrones and adopted stellar parameters correctly identify member stars on the CMD.
    Membership probabilities P_CMD rely on isochrone alignment with age 10 Gyr and [Fe/H] values; mis-matches would alter the member sample.
  • domain assumption The distance measurements from Savino et al. (2022) are correct.
    Distances (831.8 kpc for And VI, 745 kpc for And XXIII) set the physical scale of half-light radii and velocity dispersions.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Mass Modeling the Andromeda Dwarf Galaxies: Andromeda VI and Andromeda XXIII." pith.science (2026). https://pith.science/paper/NWVOZ463

@misc{pith2026250504475,
  author       = {Pith},
  title        = {Pith review of: Mass Modeling the Andromeda Dwarf Galaxies: Andromeda VI and Andromeda XXIII},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NWVOZ463}},
  note         = {Machine review of arXiv:2505.04475}
}
abstract

Accurately mapping the mass profiles of low mass dwarf spheroidal (dSph) galaxies allows us to test predictions made by dark matter (DM) models. To date, such analyses have primarily been performed on Milky Way (MW) satellites. Meanwhile, the Andromeda Galaxy (M31) is home to 35 known dwarf galaxies, yet only two have been successfully mass-modeled so far. A more comprehensive study of Local Group dwarfs is necessary to better understand the nature of dark matter. In this study, we have undertaken a dynamical study of two higher-luminosity Andromeda dwarf galaxies: Andromeda VI (And VI) and Andromeda XXIII (And XXIII). We infer an enclosed mass for And VI of M(r $<$ r$_{h}$) = (4.9 $\pm$ 1.5) $\times$ 10$^{7}$ M$_{\odot}$, corresponding to a mass-to-light ratio of $[M/L]_{r_{\rm{h}}}$ = (27.1 $\pm$ 8.2) M$_{\odot}$/L$_{\odot}$. We infer an enclosed mass for And XXIII of M(r $<$ r$_{h}$) = (3.1 $\pm$ 1.9) $\times$ 10$^{7}$ M$_{\odot}$, corresponding to a mass-to-light ratio of $[M/L]_{r_{\rm{h}}}$ = (90.2 $\pm$ 53.9) M$_{\odot}$/L$_{\odot}$. Using the dynamical Jeans modeling tool, \gravsphere, we determine And VI and And XXIII's dark matter density at 150 pc, finding $\rho_{\rm{DM,VI}}$(150 pc) = (1.4 $\pm$ 0.5) $\times 10^{8}$ M$_{\odot}$ kpc$^{-3}$ and $\rho_{\rm{DM,XXIII}}$(150 pc) = 0.5$\substack{+0.4 \\ -0.3} \times 10^{8}$ M$_{\odot}$ kpc$^{-3}$. Our results make And VI the first mass-modeled M31 satellite to fall into the cuspy regime. And XXIII has a lower density, implying either a more cored central dark matter density, or a lowering of the density through tides. This adds And XXIII to a growing list of M31 dwarfs with a central density lower than most MW dwarfs and lower than expected for isolated dwarfs in the Standard Cosmology. This could be explained by the M31 dwarfs having experienced stronger tides than their MW counterparts.

Figures

Figures reproduced from arXiv: 2505.04475 by the authors.

Figure 1
Figure 1. Half-light radius versus absolute V-band magnitude of Local Group dwarf galaxies. Milky Way dwarfs are denoted by gray triangles, while M31 dwarfs are denoted by gray circles. Andromeda VI and Andromeda XXIII are represented by a magenta diamond and a dark purple diamond, respectively. The black lines represent relations of surface brightness. Note that some uncertainties are too small to be seen but are represented… view at source ↗
Figure 2
Figure 2. Top Left: Histogram of number of stars split into 40 velocity bins of 15 kms−1 each. The light gray bars represent the non-member velocities while the dark gray bars represent member star velocities. The vertical dashed black bar is the systemic velocity of And VI from C13. Bottom Left: Velocity versus radial distance from measured center of And VI. The points are shaded depending on their respective probabilities. … view at source ↗
Figure 3
Figure 3. Same as [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figures from the paper (6 more)
Figure 5
Figure 5. Figure 5: And VI dispersion, as determined via out MCMC analysis routine outlined in § 4.1.2. Both the systemic velocity and veloicty dispersion are shown to converge well at their values of 𝑣 = (-341.6 ± 1.7) kms−1 and 𝜎v = 13.2 +1.4 −1.3 kms−1 , respectively [PITH_FULL_IMAGE:…
Figure 4
Figure 4. Figure 4: Total probability membership of Andromeda VI (top) and An￾dromeda XXIII (bottom), where there is a clear distribution bias at 𝑃tot < 0.10. Therefore, only stars with a total membership probability of 𝑃tot ≥ 0.10 are considered for our analysis. log L = ∑︁ 𝑁 𝑖=1 log 𝑃m…
Figure 6
Figure 6. Figure 6: Same as [PITH_FULL_IMAGE:figures/full_fig_p009_6.png]
Figure 7
Figure 7. Figure 7: Andromeda VI Dark matter density profiles determined by GravSphere (solid black line), with 1 and 2𝜎 being denoted by the dark gray and light gray shaded regions, respectively. The pink shaded region is the density profile created via ⟨SFR⟩ abundance matching. The blue…
Figure 9
Figure 9. Figure 9: Central dark matter density as a function of pre-infall halo mass, 𝑀200. The dark gray region represents a fully cusped profile, while the light gray region represents a fully cored profile (coreNFW from Read et al. (2016)). Each band has a width corresponding to a 1𝜎 …
Figure 10
Figure 10. Figure 10: The luminosity-metallicity relation for Local Group dwarf galax￾ies. Milky Way satellites are denoted by gray triangles, while M31 satellites are denoted by gray circles. The dashed black line represents the relation found by Kirby et al. (2013), with the teal shading…

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

172 extracted references · 5 linked inside Pith

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  2. [2]

    V., Nadler E

    Ahvazi N., Benson A., Sales L. V., Nadler E. O., Weerasooriya S., Du X., Bovill M. S., 2024, @doi [ ] 10.1093/mnras/stae761 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.529.3387A 529, 3387

    doi:10.1093/mnras/stae761 2024

  3. [3]

    D., Zaldivar B., 2020, @doi [ ] 10.1088/1475-7516/2020/09/004 , https://ui.adsabs.harvard.edu/abs/2020JCAP...09..004A 2020, 004

    Alvarez A., Calore F., Genina A., Read J., Serpico P. D., Zaldivar B., 2020, @doi [ ] 10.1088/1475-7516/2020/09/004 , https://ui.adsabs.harvard.edu/abs/2020JCAP...09..004A 2020, 004

    doi:10.1088/1475-7516/2020/09/004 2020

  4. [4]

    Alvey J., et al., 2021, @doi [ ] 10.1093/mnras/staa3640 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.501.1188A 501, 1188

    doi:10.1093/mnras/staa3640 2021

  5. [5]

    R., Becerra-Vergara E

    Arg \"u elles C. R., Becerra-Vergara E. A., Rueda J. A., Ruffini R., 2023, @doi [Universe] 10.3390/universe9040197 , https://ui.adsabs.harvard.edu/abs/2023Univ....9..197A 9, 197

    doi:10.3390/universe9040197 2023

  6. [6]

    E., Jacoby G

    Armandroff T. E., Jacoby G. H., Davies J. E., 1999, @doi [ ] 10.1086/301023 , https://ui.adsabs.harvard.edu/abs/1999AJ....118.1220A 118, 1220

    doi:10.1086/301023 1999

  7. [7]

    Astropy Collaboration et al., 2013, @doi [ ] 10.1051/0004-6361/201322068 , https://ui.adsabs.harvard.edu/abs/2013A&A...558A..33A 558, A33

    doi:10.1051/0004-6361/201322068 2013

  8. [8]

    Astropy Collaboration et al., 2018, @doi [ ] 10.3847/1538-3881/aabc4f , https://ui.adsabs.harvard.edu/abs/2018AJ....156..123A 156, 123

    doi:10.3847/1538-3881/aabc4f 2018

Show all 172 references
  1. [9]

    Astropy Collaboration et al., 2022, @doi [ ] 10.3847/1538-4357/ac7c74 , https://ui.adsabs.harvard.edu/abs/2022ApJ...935..167A 935, 167

    2022 doi

  2. [10]

    Avila-Reese V., Col \' n P., Valenzuela O., D'Onghia E., Firmani C., 2001, @doi [ ] 10.1086/322411 , https://ui.adsabs.harvard.edu/abs/2001ApJ...559..516A 559, 516

    2001 doi

  3. [11]

    K., Glazebrook K., Driver S

    Baldry I. K., Glazebrook K., Driver S. P., 2008, @doi [ ] 10.1111/j.1365-2966.2008.13348.x , https://ui.adsabs.harvard.edu/abs/2008MNRAS.388..945B 388, 945

    2008

  4. [12]

    Battaglia G., Nipoti C., 2022, @doi [Nature Astronomy] 10.1038/s41550-022-01638-7 , https://ui.adsabs.harvard.edu/abs/2022NatAs...6..659B 6, 659

    2022 doi

  5. [13]

    Belokurov V., et al., 2007, @doi [ ] 10.1086/509718 , https://ui.adsabs.harvard.edu/abs/2007ApJ...654..897B 654, 897

    2007 doi

  6. [14]

    A., 1982, @doi [ ] 10.1093/mnras/200.2.361 , https://ui.adsabs.harvard.edu/abs/1982MNRAS.200..361B 200, 361

    Binney J., Mamon G. A., 1982, @doi [ ] 10.1093/mnras/200.2.361 , https://ui.adsabs.harvard.edu/abs/1982MNRAS.200..361B 200, 361

    1982 doi

  7. [15]

    Binney J., Tremaine S., 2008, Galactic Dynamics: Second Edition

    2008

  8. [16]

    R., Lupton R

    Blanton M. R., Lupton R. H., Schlegel D. J., Strauss M. A., Brinkmann J., Fukugita M., Loveday J., 2005, @doi [ ] 10.1086/431416 , https://ui.adsabs.harvard.edu/abs/2005ApJ...631..208B 631, 208

    2005 doi

  9. [17]

    C., Hubeny I., Rauch T., 2020, @doi [ ] 10.3847/1538-3881/ab94b4 , https://ui.adsabs.harvard.edu/abs/2020AJ....160...21B 160, 21

    Bohlin R. C., Hubeny I., Rauch T., 2020, @doi [ ] 10.3847/1538-3881/ab94b4 , https://ui.adsabs.harvard.edu/abs/2020AJ....160...21B 160, 21

    2020 doi

  10. [18]

    F., Errani R., Fattahi A., 2022, @doi [ ] 10.1093/mnras/stac653 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.5247B 512, 5247

    Borukhovetskaya A., Navarro J. F., Errani R., Fattahi A., 2022, @doi [ ] 10.1093/mnras/stac653 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.5247B 512, 5247

    2022 doi

  11. [19]

    S., Kaplinghat M., 2011, @doi [ ] 10.1111/j.1745-3933.2011.01074.x , https://ui.adsabs.harvard.edu/abs/2011MNRAS.415L..40B 415, L40

    Boylan-Kolchin M., Bullock J. S., Kaplinghat M., 2011, @doi [ ] 10.1111/j.1745-3933.2011.01074.x , https://ui.adsabs.harvard.edu/abs/2011MNRAS.415L..40B 415, L40

    2011

  12. [21]

    M., et al., 2014, @doi [ ] 10.1088/0004-637X/796/2/91 , https://ui.adsabs.harvard.edu/abs/2014ApJ...796...91B 796, 91

    Brown T. M., et al., 2014, @doi [ ] 10.1088/0004-637X/796/2/91 , https://ui.adsabs.harvard.edu/abs/2014ApJ...796...91B 796, 91

    2014 doi

  13. [22]

    I., Pawlowski M

    Casetti-Dinescu D. I., Pawlowski M. S., Girard T. M., Kanehisa K. J., Petroski A., Martone M., Kozhurina-Platais V., Platais I., 2024, The Astrophysical Journal, 975, 138

    2024

  14. [23]

    C., Ibata R., Lewis G

    Chapman S. C., Ibata R., Lewis G. F., Ferguson A. M. N., Irwin M., McConnachie A., Tanvir N., 2006, @doi [ ] 10.1086/508599 , https://ui.adsabs.harvard.edu/abs/2006ApJ...653..255C 653, 255

    2006 doi

  15. [24]

    Charles E. J. E., et al., 2023, @doi [ ] 10.1093/mnras/stad752 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.tmp..726C

    2023 doi

  16. [25]

    Chen Y., Girardi L., Bressan A., Marigo P., Barbieri M., Kong X., 2014, @doi [ ] 10.1093/mnras/stu1605 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.444.2525C 444, 2525

    2014 doi

  17. [26]

    Chen Y., Bressan A., Girardi L., Marigo P., Kong X., Lanza A., 2015, @doi [ ] 10.1093/mnras/stv1281 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.452.1068C 452, 1068

    2015 doi

  18. [28]

    Collins M. L. M., et al., 2011, @doi [Monthly Notices of the Royal Astronomical Society] 10.1111/j.1365-2966.2011.19342.x , 417, 1170

    2011

  19. [29]

    Collins M. L. M., et al., 2013, @doi [The Astrophysical Journal] 10.1088/0004-637x/768/2/172 , 768, 172

    2013 doi

  20. [30]

    Collins M. L. M., et al., 2014, @doi [ ] 10.1088/0004-637X/783/1/7 , https://ui.adsabs.harvard.edu/abs/2014ApJ...783....7C 783, 7

    2014 doi

  21. [31]

    Collins M. L. M., Rich R. M., Ibata R., Martin N., Preston J., PAndAS Collaboration 2017, in Gil de Paz A., Knapen J. H., Lee J. C., eds, IAU Symposium Vol. 321, Formation and Evolution of Galaxy Outskirts. pp 16--18 ( @eprint arXiv 1605.03345 ), @doi 10.1017/S1743921316011625

    2017 arXiv

  22. [32]

    Collins M. L. M., Tollerud E. J., Rich R. M., Ibata R. A., Martin N. F., Chapman S. C., Gilbert K. M., Preston J., 2019, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stz3252 , 491, 3496

    2019 doi

  23. [33]

    Collins M. L. M., et al., 2021, @doi [ ] 10.1093/mnras/stab1624 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.505.5686C 505, 5686

    2021 doi

  24. [34]

    R., et al., 2012, @doi [ ] 10.1088/0004-637X/758/1/11 , https://ui.adsabs.harvard.edu/abs/2012ApJ...758...11C 758, 11

    Conn A. R., et al., 2012, @doi [ ] 10.1088/0004-637X/758/1/11 , https://ui.adsabs.harvard.edu/abs/2012ApJ...758...11C 758, 11

    2012 doi

  25. [35]

    A., 2021, @doi [ ] 10.1093/mnras/stab506 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.503..920C 503, 920

    Correa C. A., 2021, @doi [ ] 10.1093/mnras/stab506 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.503..920C 503, 920

    2021 doi

  26. [36]

    J., Hogan C

    Dalcanton J. J., Hogan C. J., 2001, @doi [ ] 10.1086/323207 , https://ui.adsabs.harvard.edu/abs/2001ApJ...561...35D 561, 35

    2001 doi

  27. [37]

    E., Carlsten S., Jiang F., Beaton R., Goulding A

    Danieli S., Greene J. E., Carlsten S., Jiang F., Beaton R., Goulding A. D., 2023, @doi [ ] 10.3847/1538-4357/acefbd , https://ui.adsabs.harvard.edu/abs/2023ApJ...956....6D 956, 6

    2023 doi

  28. [38]

    N., Steinhardt P

    Dav \'e R., Spergel D. N., Steinhardt P. J., Wandelt B. D., 2001, @doi [ ] 10.1086/318417 , https://ui.adsabs.harvard.edu/abs/2001ApJ...547..574D 547, 574

    2001 doi

  29. [39]

    I., No \"e l N

    De Leo M., Read J. I., No \"e l N. E. D., Erkal D., Massana P., Carrera R., 2024, @doi [ ] 10.1093/mnras/stae2428 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.535.1015D 535, 1015

    2024 doi

  30. [40]

    B., Macci \`o A

    Di Cintio A., Brook C. B., Macci \`o A. V., Stinson G. S., Knebe A., Dutton A. A., Wadsley J., 2014, @doi [ ] 10.1093/mnras/stt1891 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.437..415D 437, 415

    2014 doi

  31. [41]

    L., 2018, @doi [ ] 10.1093/mnras/sty091 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.475.5385D 475, 5385

    Di Paolo C., Nesti F., Villante F. L., 2018, @doi [ ] 10.1093/mnras/sty091 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.475.5385D 475, 5385

    2018 doi

  32. [42]

    A., Peter A

    Dooley G. A., Peter A. H. G., Vogelsberger M., Zavala J., Frebel A., 2016, @doi [ ] 10.1093/mnras/stw1309 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.461..710D 461, 710

    2016 doi

  33. [43]

    P., Phillipps S., Davies J

    Driver S. P., Phillipps S., Davies J. I., Morgan I., Disney M. J., 1994, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/266.1.155 , 266, 155

    1994 doi

  34. [44]

    Drlica-Wagner A., et al., 2015, @doi [ ] 10.1088/0004-637X/813/2/109 , https://ui.adsabs.harvard.edu/abs/2015ApJ...813..109D 813, 109

    2015 doi

  35. [45]

    Drlica-Wagner A., et al., 2020, @doi [ ] 10.3847/1538-4357/ab7eb9 , https://ui.adsabs.harvard.edu/abs/2020ApJ...893...47D 893, 47

    2020 doi

  36. [46]

    G., 1991, @doi [ ] 10.1086/170451 , https://ui.adsabs.harvard.edu/abs/1991ApJ...378..496D 378, 496

    Dubinski J., Carlberg R. G., 1991, @doi [ ] 10.1086/170451 , https://ui.adsabs.harvard.edu/abs/1991ApJ...378..496D 378, 496

    1991 doi

  37. [47]

    A., Macci \`o A

    Dutton A. A., Macci \`o A. V., 2014, @doi [ ] 10.1093/mnras/stu742 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.441.3359D 441, 3359

    2014 doi

  38. [48]

    S., 1915, @doi [ ] 10.1093/mnras/75.5.366 , https://ui.adsabs.harvard.edu/abs/1915MNRAS..75..366E 75, 366

    Eddington A. S., 1915, @doi [ ] 10.1093/mnras/75.5.366 , https://ui.adsabs.harvard.edu/abs/1915MNRAS..75..366E 75, 366

    1915 doi

  39. [49]

    M., et al., 2003, in Iye M., Moorwood A

    Faber S. M., et al., 2003, in Iye M., Moorwood A. F. M., eds, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series Vol. 4841, Instrument Design and Performance for Optical/Infrared Ground-based Telescopes. pp 1657--1669, @doi 10.1117/12.460346

    2003 doi

  40. [50]

    A., et al., 2020, @doi [ ] 10.3847/1538-4365/abb82d , https://ui.adsabs.harvard.edu/abs/2020ApJS..251....7F 251, 7

    Flewelling H. A., et al., 2020, @doi [ ] 10.3847/1538-4365/abb82d , https://ui.adsabs.harvard.edu/abs/2020ApJS..251....7F 251, 7

    2020 doi

  41. [51]

    A., Primack J

    Flores R. A., Primack J. R., 1994, @doi [ ] 10.1086/187350 , https://ui.adsabs.harvard.edu/abs/1994ApJ...427L...1F 427, L1

    1994 doi

  42. [52]

    W., Lang D., Goodman J., 2013, @doi [ ] 10.1086/670067 , https://ui.adsabs.harvard.edu/abs/2013PASP..125..306F 125, 306

    Foreman-Mackey D., Hogg D. W., Lang D., Goodman J., 2013, @doi [ ] 10.1086/670067 , https://ui.adsabs.harvard.edu/abs/2013PASP..125..306F 125, 306

    2013 doi

  43. [53]

    W., Simon J

    Fu S. W., Simon J. D., Alarc \'o n Jara A. G., 2019, @doi [ ] 10.3847/1538-4357/ab3658 , https://ui.adsabs.harvard.edu/abs/2019ApJ...883...11F 883, 11

    2019 doi

  44. [54]

    Gaia Collaboration et al., 2018a, @doi [ ] 10.1051/0004-6361/201833051 , https://ui.adsabs.harvard.edu/abs/2018A&A...616A...1G 616, A1

    doi

  45. [55]

    Gaia Collaboration et al., 2018b, @doi [ ] 10.1051/0004-6361/201832698 , https://ui.adsabs.harvard.edu/abs/2018A&A...616A..12G 616, A12

    doi

  46. [56]

    I., Wyse R

    Gallagher John S. I., Wyse R. F. G., 1994, @doi [ ] 10.1086/133500 , https://ui.adsabs.harvard.edu/abs/1994PASP..106.1225G 106, 1225

    1994 doi

  47. [57]

    Garrison-Kimmel S., et al., 2017, @doi [ ] 10.1093/mnras/stx1710 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.471.1709G 471, 1709

    2017 doi

  48. [58]

    Genina A., et al., 2020, @doi [ ] 10.1093/mnras/staa2352 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.498..144G 498, 144

    2020 doi

  49. [59]

    M., et al., 2006, @doi [ ] 10.1086/508643 , https://ui.adsabs.harvard.edu/abs/2006ApJ...652.1188G 652, 1188

    Gilbert K. M., et al., 2006, @doi [ ] 10.1086/508643 , https://ui.adsabs.harvard.edu/abs/2006ApJ...652.1188G 652, 1188

    2006 doi

  50. [60]

    X., Marsh D

    Gonz \'a lez-Morales A. X., Marsh D. J. E., Pe \ n arrubia J., Ure \ n a-L \'o pez L. A., 2017, @doi [ ] 10.1093/mnras/stx1941 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.472.1346G 472, 1346

    2017 doi

  51. [61]

    Goodman J., Weare J., 2010, @doi [Communications in Applied Mathematics and Computational Science] 10.2140/camcos.2010.5.65 , https://ui.adsabs.harvard.edu/abs/2010CAMCS...5...65G 5, 65

    2010 doi

  52. [62]

    K., 2001, @doi [Astrophysics and Space Science Supplement] 10.1023/A:1012742903265 , https://ui.adsabs.harvard.edu/abs/2001ApSSS.277..231G 277, 231

    Grebel E. K., 2001, @doi [Astrophysics and Space Science Supplement] 10.1023/A:1012742903265 , https://ui.adsabs.harvard.edu/abs/2001ApSSS.277..231G 277, 231

    2001 doi

  53. [63]

    K., Gallagher John S

    Grebel E. K., Gallagher John S. I., Harbeck D., 2003, @doi [ ] 10.1086/368363 , https://ui.adsabs.harvard.edu/abs/2003AJ....125.1926G 125, 1926

    2003 doi

  54. [64]

    Groenewegen M. A. T., 2006, @doi [ ] 10.1051/0004-6361:20054163 , https://ui.adsabs.harvard.edu/abs/2006A&A...448..181G 448, 181

    2006 doi

  55. [65]

    Hammer F., et al., 2024, @doi [ ] 10.1093/mnras/stad2922 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.2718H 527, 2718

    2024 doi

  56. [66]

    Hayashi K., Chiba M., Ishiyama T., 2020, @doi [ ] 10.3847/1538-4357/abbe0a , https://ui.adsabs.harvard.edu/abs/2020ApJ...904...45H 904, 45

    2020 doi

  57. [67]

    Hayashi K., Ferreira E. G. M., Chan H. Y. J., 2021, @doi [ ] 10.3847/2041-8213/abf501 , https://ui.adsabs.harvard.edu/abs/2021ApJ...912L...3H 912, L3

    2021 doi

  58. [68]

    Hayashi K., Dobos L., Filion C., Kirby E., Chiba M., Wyse R. F. G., PFS Galactic Archaeology Science Working Group 2023a, @doi [arXiv e-prints] 10.48550/arXiv.2305.11309 , https://ui.adsabs.harvard.edu/abs/2023arXiv230511309H p. arXiv:2305.11309

    doi arXiv

  59. [69]

    Hayashi K., Hirai Y., Chiba M., Ishiyama T., 2023b, @doi [ ] 10.3847/1538-4357/ace33e , https://ui.adsabs.harvard.edu/abs/2023ApJ...953..185H 953, 185

    doi

  60. [70]

    A., Gilmore G., Irwin M

    Ibata R. A., Gilmore G., Irwin M. J., 1994, @doi [ ] 10.1038/370194a0 , https://ui.adsabs.harvard.edu/abs/1994Natur.370..194I 370, 194

    1994 doi

  61. [71]

    C., Dalessandro E., 2011, @doi [ ] 10.1088/0004-637X/738/2/186 , https://ui.adsabs.harvard.edu/abs/2011ApJ...738..186I 738, 186

    Ibata R., Sollima A., Nipoti C., Bellazzini M., Chapman S. C., Dalessandro E., 2011, @doi [ ] 10.1088/0004-637X/738/2/186 , https://ui.adsabs.harvard.edu/abs/2011ApJ...738..186I 738, 186

    2011 doi

  62. [72]

    A., et al., 2014, @doi [ ] 10.1088/0004-637X/780/2/128 , https://ui.adsabs.harvard.edu/abs/2014ApJ...780..128I 780, 128

    Ibata R. A., et al., 2014, @doi [ ] 10.1088/0004-637X/780/2/128 , https://ui.adsabs.harvard.edu/abs/2014ApJ...780..128I 780, 128

    2014 doi

  63. [73]

    Irwin M., Lewis J., 2001, @doi [New Astronomy Reviews] https://doi.org/10.1016/S1387-6473(00)00138-X , 45, 105

    2001 doi

  64. [74]

    J., et al., 2004, in Quinn P

    Irwin M. J., et al., 2004, in Quinn P. J., Bridger A., eds, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series Vol. 5493, Optimizing Scientific Return for Astronomy through Information Technologies. pp 411--422, @doi 10.1117/12.551449

    2004 doi

  65. [75]

    H., 1922, @doi [ ] 10.1093/mnras/82.3.122 , https://ui.adsabs.harvard.edu/abs/1922MNRAS..82..122J 82, 122

    Jeans J. H., 1922, @doi [ ] 10.1093/mnras/82.3.122 , https://ui.adsabs.harvard.edu/abs/1922MNRAS..82..122J 82, 122

    1922 doi

  66. [76]

    P., et al., 2021, @doi [ ] 10.3847/1538-4357/ac1869 , https://ui.adsabs.harvard.edu/abs/2021ApJ...921...32J 921, 32

    Ji A. P., et al., 2021, @doi [ ] 10.3847/1538-4357/ac1869 , https://ui.adsabs.harvard.edu/abs/2021ApJ...921...32J 921, 32

    2021 doi

  67. [77]

    P., et al., 2023, @doi [ ] 10.1051/0004-6361/202346987 , https://ui.adsabs.harvard.edu/abs/2023A&A...678A..38J 678, A38

    J \'u lio M. P., et al., 2023, @doi [ ] 10.1051/0004-6361/202346987 , https://ui.adsabs.harvard.edu/abs/2023A&A...678A..38J 678, A38

    2023 doi

  68. [78]

    S., Di Cintio A., Brook C

    Katz H., Lelli F., McGaugh S. S., Di Cintio A., Brook C. B., Schombert J. M., 2017, @doi [ ] 10.1093/mnras/stw3101 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.466.1648K 466, 1648

    2017 doi

  69. [79]

    Y., Peter A

    Kim S. Y., Peter A. H. G., Wittman D., 2017, @doi [ ] 10.1093/mnras/stx896 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.469.1414K 469, 1414

    2017 doi

  70. [80]

    Y., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2408.15214 , https://ui.adsabs.harvard.edu/abs/2024arXiv240815214K p

    Kim S. Y., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2408.15214 , https://ui.adsabs.harvard.edu/abs/2024arXiv240815214K p. arXiv:2408.15214

    2024 doi arXiv

  71. [81]

    N., Lanfranchi G

    Kirby E. N., Lanfranchi G. A., Simon J. D., Cohen J. G., Guhathakurta P., 2011, @doi [ ] 10.1088/0004-637X/727/2/78 , https://ui.adsabs.harvard.edu/abs/2011ApJ...727...78K 727, 78

    2011 doi

  72. [82]

    N., Cohen J

    Kirby E. N., Cohen J. G., Guhathakurta P., Cheng L., Bullock J. S., Gallazzi A., 2013, @doi [ ] 10.1088/0004-637X/779/2/102 , https://ui.adsabs.harvard.edu/abs/2013ApJ...779..102K 779, 102

    2013 doi

  73. [83]

    Koposov S., et al., 2008, @doi [ ] 10.1086/589911 , https://ui.adsabs.harvard.edu/abs/2008ApJ...686..279K 686, 279

    2008 doi

  74. [84]

    V., Vikhlinin A

    Kravtsov A. V., Vikhlinin A. A., Meshcheryakov A. V., 2018, @doi [Astronomy Letters] 10.1134/S1063773717120015 , https://ui.adsabs.harvard.edu/abs/2018AstL...44....8K 44, 8

    2018 doi

  75. [85]

    Kroupa P., 2001, @doi [ ] 10.1046/j.1365-8711.2001.04022.x , https://ui.adsabs.harvard.edu/abs/2001MNRAS.322..231K 322, 231

    2001

  76. [86]

    Kroupa P., 2002, @doi [Science] 10.1126/science.1067524 , https://ui.adsabs.harvard.edu/abs/2002Sci...295...82K 295, 82

    2002 doi

  77. [87]

    I., et al., 2020, @doi [ ] 10.1093/mnras/staa2541 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.498.2968L 498, 2968

    Libeskind N. I., et al., 2020, @doi [ ] 10.1093/mnras/staa2541 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.498.2968L 498, 2968

    2020 doi

  78. [88]

    R., Frenk C

    Lovell M. R., Frenk C. S., Eke V. R., Jenkins A., Gao L., Theuns T., 2014, @doi [ ] 10.1093/mnras/stt2431 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.439..300L 439, 300

    2014 doi

  79. [91]

    V., 2022, @doi [ ] 10.1093/mnras/stac2452 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.3944M 516, 3944

    Manwadkar V., Kravtsov A. V., 2022, @doi [ ] 10.1093/mnras/stac2452 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.3944M 516, 3944

    2022 doi

  80. [92]

    Marigo P., Girardi L., Bressan A., Groenewegen M. A. T., Silva L., Granato G. L., 2008, @doi [ ] 10.1051/0004-6361:20078467 , https://ui.adsabs.harvard.edu/abs/2008A&A...482..883M 482, 883

    2008 doi

  81. [93]

    L., 2013, @doi [ ] 10.1093/mnras/stt1034 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.434..488M 434, 488

    Marigo P., Bressan A., Nanni A., Girardi L., Pumo M. L., 2013, @doi [ ] 10.1093/mnras/stt1034 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.434..488M 434, 488

    2013 doi

  82. [95]

    F., et al., 2013, @doi [ ] 10.1088/0004-637X/772/1/15 , https://ui.adsabs.harvard.edu/abs/2013ApJ...772...15M 772, 15

    Martin N. F., et al., 2013, @doi [ ] 10.1088/0004-637X/772/1/15 , https://ui.adsabs.harvard.edu/abs/2013ApJ...772...15M 772, 15

    2013 doi

  83. [96]

    F., et al., 2014, @doi [ ] 10.1088/2041-8205/793/1/L14 , https://ui.adsabs.harvard.edu/abs/2014ApJ...793L..14M 793, L14

    Martin N. F., et al., 2014, @doi [ ] 10.1088/2041-8205/793/1/L14 , https://ui.adsabs.harvard.edu/abs/2014ApJ...793L..14M 793, L14

    2014 doi

  84. [97]

    F., et al., 2016, @doi [ ] 10.3847/1538-4357/833/2/167 , https://ui.adsabs.harvard.edu/abs/2016ApJ...833..167M 833, 167

    Martin N. F., et al., 2016, @doi [ ] 10.3847/1538-4357/833/2/167 , https://ui.adsabs.harvard.edu/abs/2016ApJ...833..167M 833, 167

    2016 doi

  85. [98]

    L., 1998, @doi [ ] 10.1146/annurev.astro.36.1.435 , https://ui.adsabs.harvard.edu/abs/1998ARA&A..36..435M 36, 435

    Mateo M. L., 1998, @doi [ ] 10.1146/annurev.astro.36.1.435 , https://ui.adsabs.harvard.edu/abs/1998ARA&A..36..435M 36, 435

    1998 doi

  86. [99]

    W., 2012, @doi [The Astronomical Journal] 10.1088/0004-6256/144/1/4 , 144, 4

    McConnachie A. W., 2012, @doi [The Astronomical Journal] 10.1088/0004-6256/144/1/4 , 144, 4

    2012 doi

  87. [100]

    W., Arimoto N., Irwin M., 2007, @doi [ ] 10.1111/j.1365-2966.2007.11969.x , https://ui.adsabs.harvard.edu/abs/2007MNRAS.379..379M 379, 379

    McConnachie A. W., Arimoto N., Irwin M., 2007, @doi [ ] 10.1111/j.1365-2966.2007.11969.x , https://ui.adsabs.harvard.edu/abs/2007MNRAS.379..379M 379, 379

    2007

  88. [101]

    W., et al., 2009, @doi [ ] 10.1038/nature08327 , https://ui.adsabs.harvard.edu/abs/2009Natur.461...66M 461, 66

    McConnachie A. W., et al., 2009, @doi [ ] 10.1038/nature08327 , https://ui.adsabs.harvard.edu/abs/2009Natur.461...66M 461, 66

    2009 doi

  89. [102]

    W., et al., 2018, @doi [ ] 10.3847/1538-4357/aae8e7 , https://ui.adsabs.harvard.edu/abs/2018ApJ...868...55M 868, 55

    McConnachie A. W., et al., 2018, @doi [ ] 10.3847/1538-4357/aae8e7 , https://ui.adsabs.harvard.edu/abs/2018ApJ...868...55M 868, 55

    2018 doi

  90. [103]

    McGaugh S., Milgrom M., 2013, @doi [ ] 10.1088/0004-637X/766/1/22 , https://ui.adsabs.harvard.edu/abs/2013ApJ...766...22M 766, 22

    2013 doi

  91. [104]

    S., de Blok W

    McGaugh S. S., de Blok W. J. G., Schombert J. M., Kuzio de Naray R., Kim J. H., 2007, @doi [ ] 10.1086/511807 , https://ui.adsabs.harvard.edu/abs/2007ApJ...659..149M 659, 149

    2007 doi

  92. [105]

    McNaught-Roberts T., et al., 2014, @doi [ ] 10.1093/mnras/stu1886 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.445.2125M 445, 2125

    2014 doi

  93. [106]

    Moore B., 1994, @doi [Nature] 10.1038/370629a0 , 370, 629

    1994 doi

  94. [107]

    Moore B., Ghigna S., Governato F., Lake G., Quinn T., Stadel J., Tozzi P., 1999, @doi [ ] 10.1086/312287 , https://ui.adsabs.harvard.edu/abs/1999ApJ...524L..19M 524, L19

    1999 doi

  95. [108]

    P., Somerville R

    Moster B. P., Somerville R. S., Maulbetsch C., van den Bosch F. C., Macci \`o A. V., Naab T., Oser L., 2010, @doi [ ] 10.1088/0004-637X/710/2/903 , https://ui.adsabs.harvard.edu/abs/2010ApJ...710..903M 710, 903

    2010 doi

  96. [109]

    I., Agertz O., Rey M

    Muni C., Pontzen A., Read J. I., Agertz O., Rey M. P., Taylor E., Kim S. Y., Gray E. I., 2025, @doi [ ] 10.1093/mnras/stae2748 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.536..314M 536, 314

    2025 doi

  97. [110]

    O., et al., 2020, @doi [ ] 10.3847/1538-4357/ab846a , https://ui.adsabs.harvard.edu/abs/2020ApJ...893...48N 893, 48

    Nadler E. O., et al., 2020, @doi [ ] 10.3847/1538-4357/ab846a , https://ui.adsabs.harvard.edu/abs/2020ApJ...893...48N 893, 48

    2020 doi

  98. [112]

    F., Eke V

    Navarro J. F., Eke V. R., Frenk C. S., 1996b, @doi [ ] 10.1093/mnras/283.3.L72 , https://ui.adsabs.harvard.edu/abs/1996MNRAS.283L..72N 283, L72

    doi

  99. [113]

    F., Frenk C

    Navarro J. F., Frenk C. S., White S. D. M., 1996c, @doi [ ] 10.1086/177173 , https://ui.adsabs.harvard.edu/abs/1996ApJ...462..563N 462, 563

    doi

  100. [114]

    F., Frenk C

    Navarro J. F., Frenk C. S., White S. D. M., 1997, @doi [ ] 10.1086/304888 , https://ui.adsabs.harvard.edu/abs/1997ApJ...490..493N 490, 493

    1997 doi

  101. [115]

    arXiv:2503.03812

    Nguyen T., Read J., Necib L., Mishra-Sharma S., Faucher-Gigu \`e re C.-A., Wetzel A., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2503.03812 , https://ui.adsabs.harvard.edu/abs/2025arXiv250303812N p. arXiv:2503.03812

    2025 doi arXiv

  102. [116]

    S., Hopkins P

    O \ n orbe J., Boylan-Kolchin M., Bullock J. S., Hopkins P. F., Kere s D., Faucher-Gigu \`e re C.-A., Quataert E., Murray N., 2015, @doi [ ] 10.1093/mnras/stv2072 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.454.2092O 454, 2092

    2015 doi

  103. [117]

    E., 1994, @doi [ ] 10.1086/173713 , https://ui.adsabs.harvard.edu/abs/1994ApJ...422..158O 422, 158

    O'Donnell J. E., 1994, @doi [ ] 10.1086/173713 , https://ui.adsabs.harvard.edu/abs/1994ApJ...422..158O 422, 158

    1994 doi

  104. [118]

    Orkney M. D. A., Taylor E., Read J. I., Rey M. P., Pontzen A., Agertz O., Kim S. Y., Delorme M., 2023, @doi [ ] 10.1093/mnras/stad2516 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.525.3516O 525, 3516

    2023 doi

  105. [119]

    A., Steinwandel U

    O’Leary J. A., Steinwandel U. P., Moster B. P., Martin N., Naab T., 2023, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/stad166 , 520, 897

    2023 doi

  106. [120]

    B., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2411.07424 , https://ui.adsabs.harvard.edu/abs/2024arXiv241107424P p

    Pace A. B., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2411.07424 , https://ui.adsabs.harvard.edu/abs/2024arXiv241107424P p. arXiv:2411.07424

    2024 doi

  107. [121]

    P., Shankar F., 2015, @doi [ ] 10.1051/0004-6361/201424909 , https://ui.adsabs.harvard.edu/abs/2015A&A...574A.113P 574, A113

    Papastergis E., Giovanelli R., Haynes M. P., Shankar F., 2015, @doi [ ] 10.1051/0004-6361/201424909 , https://ui.adsabs.harvard.edu/abs/2015A&A...574A.113P 574, A113

    2015 doi

  108. [122]

    Pascale R., Binney J., Nipoti C., Posti L., 2019, @doi [ ] 10.1093/mnras/stz1617 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.488.2423P 488, 2423

    2019 doi

  109. [123]

    Pastorelli G., et al., 2019, @doi [ ] 10.1093/mnras/stz725 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.485.5666P 485, 5666

    2019 doi

  110. [124]

    Pastorelli G., et al., 2020, @doi [ ] 10.1093/mnras/staa2565 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.498.3283P 498, 3283

    2020 doi

  111. [125]

    S., Tony Sohn S., 2021, @doi [ ] 10.3847/1538-4357/ac2aa9 , https://ui.adsabs.harvard.edu/abs/2021ApJ...923...42P 923, 42

    Pawlowski M. S., Tony Sohn S., 2021, @doi [ ] 10.3847/1538-4357/ac2aa9 , https://ui.adsabs.harvard.edu/abs/2021ApJ...923...42P 923, 42

    2021 doi

  112. [126]

    Peebles P. J. E., 1972, @doi [ ] 10.1086/151797 , https://ui.adsabs.harvard.edu/abs/1972ApJ...178..371P 178, 371

    1972 doi

  113. [127]

    C., 1911, @doi [ ] 10.1093/mnras/71.5.460 , https://ui.adsabs.harvard.edu/abs/1911MNRAS..71..460P 71, 460

    Plummer H. C., 1911, @doi [ ] 10.1093/mnras/71.5.460 , https://ui.adsabs.harvard.edu/abs/1911MNRAS..71..460P 71, 460

    1911 doi

  114. [129]

    Pontzen A., Governato F., 2014, @doi [ ] 10.1038/nature12953 , https://ui.adsabs.harvard.edu/abs/2014Natur.506..171P 506, 171

    2014 doi

  115. [130]

    D., Lima J., Fabris J

    Popolo A. D., Lima J., Fabris J. C., Rodrigues D. C., 2014, @doi [Journal of Cosmology and Astroparticle Physics] 10.1088/1475-7516/2014/04/021 , 2014, 021

    2014 doi

  116. [131]

    E., Zheng Y., Price-Whelan A

    Putman M. E., Zheng Y., Price-Whelan A. M., Grcevich J., Johnson A. C., Tollerud E., Peek J. E. G., 2021, @doi [ ] 10.3847/1538-4357/abe391 , https://ui.adsabs.harvard.edu/abs/2021ApJ...913...53P 913, 53

    2021 doi

  117. [132]

    I., Erkal D., 2019, @doi [ ] 10.1093/mnras/stz1320 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.5799R 487, 5799

    Read J. I., Erkal D., 2019, @doi [ ] 10.1093/mnras/stz1320 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.487.5799R 487, 5799

    2019 doi

  118. [133]

    I., Gilmore G., 2005, @doi [ ] 10.1111/j.1365-2966.2004.08424.x , https://ui.adsabs.harvard.edu/abs/2005MNRAS.356..107R 356, 107

    Read J. I., Gilmore G., 2005, @doi [ ] 10.1111/j.1365-2966.2004.08424.x , https://ui.adsabs.harvard.edu/abs/2005MNRAS.356..107R 356, 107

    2005

  119. [134]

    I., Steger P., 2017, @doi [ ] 10.1093/mnras/stx1798 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.471.4541R 471, 4541

    Read J. I., Steger P., 2017, @doi [ ] 10.1093/mnras/stx1798 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.471.4541R 471, 4541

    2017 doi

  120. [135]

    I., Wilkinson M

    Read J. I., Wilkinson M. I., Evans N. W., Gilmore G., Kleyna J. T., 2006, @doi [ ] 10.1111/j.1365-2966.2005.09959.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.367..387R 367, 387

    2006

  121. [136]

    I., Agertz O., Collins M

    Read J. I., Agertz O., Collins M. L. M., 2016, @doi [ ] 10.1093/mnras/stw713 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.459.2573R 459, 2573

    2016 doi

  122. [137]

    I., Walker M

    Read J. I., Walker M. G., Steger P., 2018, @doi [ ] 10.1093/mnras/sty2286 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.481..860R 481, 860

    2018 doi

  123. [138]

    I., Walker M

    Read J. I., Walker M. G., Steger P., 2019, @doi [ ] 10.1093/mnras/sty3404 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.484.1401R 484, 1401

    2019 doi

  124. [139]

    I., et al., 2021, @doi [ ] 10.1093/mnras/staa3663 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.501..978R 501, 978

    Read J. I., et al., 2021, @doi [ ] 10.1093/mnras/staa3663 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.501..978R 501, 978

    2021 doi

  125. [140]

    C., et al., 2011, @doi [ ] 10.1088/0004-637X/732/2/76 , https://ui.adsabs.harvard.edu/abs/2011ApJ...732...76R 732, 76

    Richardson J. C., et al., 2011, @doi [ ] 10.1088/0004-637X/732/2/76 , https://ui.adsabs.harvard.edu/abs/2011ApJ...732...76R 732, 76

    2011 doi

  126. [141]

    Rocha M., Peter A. H. G., Bullock J. S., Kaplinghat M., Garrison-Kimmel S., O \ n orbe J., Moustakas L. A., 2013, @doi [ ] 10.1093/mnras/sts514 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.430...81R 430, 81

    2013 doi

  127. [142]

    Rodr \' guez-Puebla A., Avila-Reese V., Drory N., 2013, @doi [ ] 10.1088/0004-637X/773/2/172 , https://ui.adsabs.harvard.edu/abs/2013ApJ...773..172R 773, 172

    2013 doi

  128. [143]

    J., Bressan A., Williams B

    Rosenfield P., Marigo P., Girardi L., Dalcanton J. J., Bressan A., Williams B. F., Dolphin A., 2016, @doi [ ] 10.3847/0004-637X/822/2/73 , https://ui.adsabs.harvard.edu/abs/2016ApJ...822...73R 822, 73

    2016 doi

  129. [144]

    C., Ford W

    Rubin V. C., Ford W. K. J., Thonnard N., 1978, @doi [ ] 10.1086/182804 , https://ui.adsabs.harvard.edu/abs/1978ApJ...225L.107R 225, L107

    1978 doi

  130. [145]

    Savino A., et al., 2022, @doi [ ] 10.3847/1538-4357/ac91cb , https://ui.adsabs.harvard.edu/abs/2022ApJ...938..101S 938, 101

    2022 doi

  131. [146]

    Savino A., et al., 2023, @doi [ ] 10.3847/1538-4357/acf46f , https://ui.adsabs.harvard.edu/abs/2023ApJ...956...86S 956, 86

    2023 doi

  132. [147]

    Savino A., et al., 2025, @doi [ ] 10.3847/1538-4357/ada24f , https://ui.adsabs.harvard.edu/abs/2025ApJ...979..205S 979, 205

    2025 doi

  133. [148]

    Schechter P., 1976, @doi [ ] 10.1086/154079 , https://ui.adsabs.harvard.edu/abs/1976ApJ...203..297S 203, 297

    1976 doi

  134. [149]

    J., Finkbeiner D

    Schlegel D. J., Finkbeiner D. P., Davis M., 1998, @doi [ ] 10.1086/305772 , https://ui.adsabs.harvard.edu/abs/1998ApJ...500..525S 500, 525

    1998 doi

  135. [150]

    S., Lake G., 2017, @doi [ ] 10.1093/mnras/stx1294 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.1542S 470, 1542

    Schneider A., Trujillo-Gomez S., Papastergis E., Reed D. S., Lake G., 2017, @doi [ ] 10.1093/mnras/stx1294 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.1542S 470, 1542

    2017 doi

  136. [151]

    S., 2013, @doi [ ] 10.1093/mnras/stt053 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.430.2346S 430, 2346

    Shao S., Gao L., Theuns T., Frenk C. S., 2013, @doi [ ] 10.1093/mnras/stt053 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.430.2346S 430, 2346

    2013 doi

  137. [152]

    D., 2019, @doi [Annual Review of Astronomy and Astrophysics] 10.1146/annurev-astro-091918-104453 , 57, 375

    Simon J. D., 2019, @doi [Annual Review of Astronomy and Astrophysics] 10.1146/annurev-astro-091918-104453 , 57, 375

    2019 doi

  138. [153]

    T., Patel E., Fardal M

    Sohn S. T., Patel E., Fardal M. A., Besla G., van der Marel R. P., Geha M., Guhathakurta P., 2020, @doi [ ] 10.3847/1538-4357/abaf49 , https://ui.adsabs.harvard.edu/abs/2020ApJ...901...43S 901, 43

    2020 doi

  139. [154]

    N., Steinhardt P

    Spergel D. N., Steinhardt P. J., 2000, @doi [Phys. Rev. Lett.] 10.1103/PhysRevLett.84.3760 , 84, 3760

    2000 doi

  140. [155]

    Starkenburg E., et al., 2010, @doi [ ] 10.1051/0004-6361/200913759 , https://ui.adsabs.harvard.edu/abs/2010A&A...513A..34S 513, A34

    2010 doi

  141. [156]

    E., Bullock J

    Strigari L. E., Bullock J. S., Kaplinghat M., Simon J. D., Geha M., Willman B., Walker M. G., 2008, @doi [Nature] 10.1038/nature07222 , 454, 1096

    2008 doi

  142. [157]

    Tang J., Bressan A., Rosenfield P., Slemer A., Marigo P., Girardi L., Bianchi L., 2014, @doi [ ] 10.1093/mnras/stu2029 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.445.4287T 445, 4287

    2014 doi

  143. [158]

    J., et al., 2012, @doi [ ] 10.1088/0004-637X/752/1/45 , https://ui.adsabs.harvard.edu/abs/2012ApJ...752...45T 752, 45

    Tollerud E. J., et al., 2012, @doi [ ] 10.1088/0004-637X/752/1/45 , https://ui.adsabs.harvard.edu/abs/2012ApJ...752...45T 752, 45

    2012 doi

  144. [159]

    J., Boylan-Kolchin M., Bullock J

    Tollerud E. J., Boylan-Kolchin M., Bullock J. S., 2014, @doi [ ] 10.1093/mnras/stu474 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.440.3511T 440, 3511

    2014 doi

  145. [160]

    Tolstoy E., Hill V., Tosi M., 2009, @doi [ ] 10.1146/annurev-astro-082708-101650 , https://ui.adsabs.harvard.edu/abs/2009ARA&A..47..371T 47, 371

    2009 doi

  146. [161]

    E., Belokurov V., Irwin M., 2016, @doi [ ] 10.1093/mnras/stw733 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.459.2370T 459, 2370

    Torrealba G., Koposov S. E., Belokurov V., Irwin M., 2016, @doi [ ] 10.1093/mnras/stw733 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.459.2370T 459, 2370

    2016 doi

  147. [162]

    Torrealba G., et al., 2019, @doi [ ] 10.1093/mnras/stz1624 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.488.2743T 488, 2743

    2019 doi

  148. [163]

    R., Montalb \'a n J., Marigo P., Pastorelli G., Girardi L., 2019, @doi [ ] 10.1093/mnras/sty2745 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.482..929T 482, 929

    Trabucchi M., Wood P. R., Montalb \'a n J., Marigo P., Pastorelli G., Girardi L., 2019, @doi [ ] 10.1093/mnras/sty2745 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.482..929T 482, 929

    2019 doi

  149. [164]

    R., Mowlavi N., Pastorelli G., Marigo P., Girardi L., Lebzelter T., 2021, @doi [ ] 10.1093/mnras/staa3356 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.1575T 500, 1575

    Trabucchi M., Wood P. R., Mowlavi N., Pastorelli G., Marigo P., Girardi L., Lebzelter T., 2021, @doi [ ] 10.1093/mnras/staa3356 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.1575T 500, 1575

    2021 doi

  150. [165]

    Vaz D., et al., 2023, @doi [ ] 10.1051/0004-6361/202346453 , https://ui.adsabs.harvard.edu/abs/2023A&A...678A..59V 678, A59

    2023 doi

  151. [166]

    Virtanen P., et al., 2020, @doi [Nature Methods] 10.1038/s41592-019-0686-2 , https://rdcu.be/b08Wh 17, 261

    2020 doi

  152. [167]

    Vogelsberger M., Zavala J., Loeb A., 2012, @doi [ ] 10.1111/j.1365-2966.2012.21182.x10.1002/asna.19141991009 , https://ui.adsabs.harvard.edu/abs/2012MNRAS.423.3740V 423, 3740

    2012

  153. [168]

    G., Pe \ n arrubia J., 2011, @doi [ ] 10.1088/0004-637X/742/1/20 , https://ui.adsabs.harvard.edu/abs/2011ApJ...742...20W 742, 20

    Walker M. G., Pe \ n arrubia J., 2011, @doi [ ] 10.1088/0004-637X/742/1/20 , https://ui.adsabs.harvard.edu/abs/2011ApJ...742...20W 742, 20

    2011 doi

  154. [169]

    G., Mateo M., Olszewski E

    Walker M. G., Mateo M., Olszewski E. W., Gnedin O. Y., Wang X., Sen B., Woodroofe M., 2007, @doi [ ] 10.1086/521998 , https://ui.adsabs.harvard.edu/abs/2007ApJ...667L..53W 667, L53

    2007 doi

  155. [170]

    G., Mateo M., Olszewski E

    Walker M. G., Mateo M., Olszewski E. W., Pe \ n arrubia J., Evans N. W., Gilmore G., 2009, @doi [ ] 10.1088/0004-637X/704/2/1274 , https://ui.adsabs.harvard.edu/abs/2009ApJ...704.1274W 704, 1274

    2009 doi

  156. [171]

    S., Mamon G

    Wang J., Hammer F., Yang Y., Pawlowski M. S., Mamon G. A., Wang H., 2024, @doi [ ] 10.1093/mnras/stad3651 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.527.7144W 527, 7144

    2024 doi

  157. [172]

    R., et al., 2019, @doi [ ] 10.3847/2041-8213/ab4b52 , https://ui.adsabs.harvard.edu/abs/2019ApJ...885L...8W 885, L8

    Weisz D. R., et al., 2019, @doi [ ] 10.3847/2041-8213/ab4b52 , https://ui.adsabs.harvard.edu/abs/2019ApJ...885L...8W 885, L8

    2019 doi

  158. [173]

    I., Kleyna J

    Wilkinson M. I., Kleyna J. T., Evans N. W., Gilmore G. F., Irwin M. J., Grebel E. K., 2004, @doi [ ] 10.1086/423619 , https://ui.adsabs.harvard.edu/abs/2004ApJ...611L..21W 611, L21

    2004 doi

  159. [174]

    D., Bullock J

    Wolf J., Martinez G. D., Bullock J. S., Kaplinghat M., Geha M., Mu \ n oz R. R., Simon J. D., Avedo F. F., 2010, @doi [ ] 10.1111/j.1365-2966.2010.16753.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.406.1220W 406, 1220

    2010

  160. [175]

    Zimmermann T., Alvey J., Marsh D. J. E., Fairbairn M., Read J. I., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2405.20374 , https://ui.adsabs.harvard.edu/abs/2024arXiv240520374Z p. arXiv:2405.20374

    2024 doi arXiv

  161. [176]

    L., Brinchmann J., Bouch \'e N

    Zoutendijk S. L., Brinchmann J., Bouch \'e N. F., den Brok M., Krajnovi \'c D., Kuijken K., Maseda M. V., Schaye J., 2021, @doi [ ] 10.1051/0004-6361/202040239 , https://ui.adsabs.harvard.edu/abs/2021A&A...651A..80Z 651, A80

    2021 doi

  162. [177]

    de Blok W. J. G., 2010, @doi [Advances in Astronomy] 10.1155/2010/789293 , https://ui.adsabs.harvard.edu/abs/2010AdAst2010E...5D 2010, 789293

    2010 doi

  163. [178]

    P., 1994, @doi [ ] 10.1093/mnras/270.2.271 , https://ui.adsabs.harvard.edu/abs/1994MNRAS.270..271V 270, 271

    van der Marel R. P., 1994, @doi [ ] 10.1093/mnras/270.2.271 , https://ui.adsabs.harvard.edu/abs/1994MNRAS.270..271V 270, 271

    1994 doi

  164. [179]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.stat...

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.