Pith. sign in

REVIEW 2 major objections 5 minor 104 references

Comparing dark-matter slopes at the same physical radii removes most of the cusp-core tension for Milky Way satellites.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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

T0 review · grok-4.5

2026-07-13 06:27 UTC pith:2OT3SNJC

load-bearing objection Fixed-radius, fixed-M★ comparison largely dissolves the cusp-core tension for most MW satellites; the result is real and carefully done. the 2 major comments →

arxiv 2607.08818 v1 pith:2OT3SNJC submitted 2026-07-09 astro-ph.GA

Dark matter density profiles of the Milky Way satellite population: reconciling simulations and observations

Jorge Sarrato-Al\'os , Jos\'e Mar\'ia Arroyo-Polonio This is my paper
classification astro-ph.GA
keywords cusp-core problemdark matter density profilesMilky Way satelliteshydrodynamical simulationsdwarf galaxiesstellar feedbacktidal strippingNFW profile
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper argues that the long-standing cusp-core problem for Milky Way dwarf satellites is largely an artifact of inconsistent measurement. Simulations have usually reported inner dark-matter slopes at a fixed fraction of the virial radius, while observations can only probe limited physical radii set by available stars. When the same physical radii (100–500 pc) and full density profiles are compared at matched stellar mass, NIHAO and FIRE-2 hydrodynamical simulations reproduce the dynamical models of 16 satellites to within roughly 1σ for most systems and outperform a pure NFW expectation. Both data sets show the same mass-dependent core-formation trend: cuspy profiles at the lowest stellar masses give way to cores once stellar mass exceeds about 10^6 solar masses, with satellites showing extra scatter from tides. Inter-model differences among the four observational methods are often as large as the remaining simulation–observation offset, so the residual discrepancies do not yet demand new dark-matter physics. Willman 1 remains the clear outlier that neither suite can match.

Core claim

Evaluating dark-matter density slopes and full profiles at fixed physical radii accessible to observations, rather than at fixed fractions of the virial radius, brings NIHAO and FIRE-2 CDM hydrodynamical simulations into agreement with dynamical models of most Milky Way satellites (within ≲1σ) and reveals a shared stellar-mass-dependent core-formation trend, while a pure NFW profile systematically over-predicts central densities for cored systems.

What carries the argument

The reliability-radius cut: observational slopes and densities are restricted to the radial range actually constrained by spectroscopic tracers (innermost radius enclosing ≥50 member stars or the third velocity-dispersion bin; outer limit set by ≥10 stars), and simulated profiles are evaluated only above their numerical convergence radius at those same physical scales and at matched stellar mass.

Load-bearing premise

The radial ranges treated as reliable for observations rest on practical working thresholds for star counts and bins rather than a unique theoretical limit; if those cuts systematically include unconstrained regions or exclude real signal, the claimed agreement can shift.

What would settle it

A new set of dynamical models for the same 16 satellites that use substantially larger, uniformly selected kinematic samples and still recover slopes or densities that lie systematically outside the mass-matched simulation envelopes at 250–500 pc would falsify the ‘no clear tension’ claim.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Apparent cusp-core discrepancies in the literature that relied on fixed-Rvir slope definitions should be re-examined with matched physical radii before being used to constrain dark-matter models.
  • Satellite comparisons must use the wider scatter of simulated satellites, not centrals, as the theoretical reference because tides naturally produce steeper tails.
  • Density-profile comparisons are more discriminating than slope comparisons and should become the primary metric for future tests.
  • Willman 1, Antlia 2 and Crater 2 remain genuine outliers whose extreme sizes and densities may require either more extreme tidal histories or alternative dark-matter physics.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the reliability cuts are later shown to be too generous, the residual tension that reappears would be largest for the ultra-faints where the kinematic samples are smallest.
  • The same physical-radius protocol applied to field dwarfs (rather than satellites) would test whether the core-formation threshold at 10^6 solar masses is environment-independent.
  • A larger sample of high-resolution simulations of diffuse, heavily stripped satellites could determine whether Antlia 2 and Crater 2 are simply rare tidal products or require non-CDM physics.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. The manuscript argues that much of the apparent cusp–core tension between CDM hydrodynamical simulations and dynamical models of Milky Way dwarf satellites is methodological: slopes have historically been compared at inconsistent radii (fixed fractions of R_vir in simulations versus data-limited radii in observations). Using NIHAO and FIRE-2, the authors recompute simulated dark-matter density and logarithmic-slope profiles at fixed physical radii (100, 250, 500 pc) and compare full profiles to 16 MW satellites modelled by four independent dynamical methods (R19, H20/H23, AP25, P25/P26), restricted to stated reliability ranges. They report a shared mass-dependent core-formation trend (cuspy at M★∼10^5 M⊙ to core-like at ∼10^8 M⊙), agreement within ≲1σ for most systems that outperforms an abundance-matched NFW baseline, larger scatter among satellites consistent with tides, and Willman 1 (plus Antlia 2/Crater 2) as remaining outliers. Inter-model observational scatter is argued to be comparable to the simulation–observation offset.

Significance. If the fixed-physical-radius and fixed-stellar-mass comparison holds, the paper removes a long-standing source of apparent tension in the cusp–core problem and strengthens the case that baryonic feedback in CDM can reproduce the inner structure of most Local Group dwarfs without new dark-matter physics. Strengths include the dual-suite simulation sample, four independent observational pipelines, explicit r_conv,20 and data-driven reliability cuts, Monte-Carlo NFW baseline from Moster+Moliné, and quantitative MAD_σ matching with 68% envelopes. The work is falsifiable: future higher-resolution kinematics or simulations that change the reliability windows or the core-formation threshold would test the claim directly. The result is of clear interest to both the simulation and Local Group dynamics communities.

major comments (2)
  1. Sec. 2 defines observational reliability ranges via practical thresholds (≥50 member stars for the inner limit of star-by-star analyses, ≥10 stars for the outer limit, third bin for binned data, half-light radius always trusted). These cuts gate the ≲1σ agreement and “no clear tension” claim. The paper already marks out-of-range points as empty symbols and notes the thresholds are non-unique, but a short sensitivity test (e.g., 30 vs 50 stars, or 2 vs 3 bins) is still needed to show that the main conclusion does not flip when the cuts are varied within a reasonable range.
  2. Sec. 4.2 and Appendix A: the quantitative MAD_σ matching and 68% envelopes are a strength, yet the abstract and conclusions state agreement “within ≲1σ for most systems” without a clear, tabulated count of how many of the 16 galaxies (and which methods) satisfy that criterion over the full reliable radial range. Adding a short summary table or sentence that lists the systems/methods that remain inside 1σ versus those that exceed it (R19 Fornax/Sculptor/Leo I/II, Willman 1, Antlia 2, Crater 2) would make the central claim fully auditable.
minor comments (5)
  1. Fig. 3 caption and body: empty versus solid symbols for unresolved/extrapolated points are defined, but a one-sentence reminder in the main text of Sec. 4.1 would help readers who inspect only the figure.
  2. Tables 2–4: several entries carry a dagger for radii outside the reliability region; the dagger definition appears only in the table notes. Cross-referencing Sec. 2 in the table notes would improve self-containment.
  3. Sec. 3.3 / Fig. 1: the systematic size offset of simulated galaxies above ∼10^7 M⊙ relative to McConnachie field dwarfs is noted; a brief remark on whether this size bias could affect the half-light-radius reliability cut for the more massive satellites would be useful.
  4. Eq. (1) and Sec. 3.4.1: the double-power-law fit is well motivated, but the radial range used for the fit (from r_conv,20 to R_vir) and any prior or bounds on (α,β,γ) should be stated explicitly so that the slope profiles in Fig. 5 are fully reproducible.
  5. Appendix B: the comparison to centrals alone is valuable; a single sentence in the main text of Sec. 4.2 noting that density deviations are systematically larger for centrals than for satellites would reinforce the environmental argument without forcing readers into the appendix.

Circularity Check

1 steps flagged

No significant circularity: the fixed-radius / fixed-M★ comparison is an external confrontation of independent simulations against published dynamical models and an abundance-matched NFW baseline; only a minor non-load-bearing self-citation of co-authored AP25 data appears.

specific steps
  1. self citation load bearing [Sec. 2 and throughout Results (AP25 models)]
    "we compile inferred dark matter density profiles from four primary literature sources: Hayashi et al. (2020, 2023) (H20/H23), Read et al. (2019) (R19), Arroyo-Polonio et al. (2025) (AP25), and Pascale et al. (2025, 2026) (P25/P26)"

    AP25 shares an author with the present paper and is used as one of the four observational benchmarks. However the citation is not load-bearing: the paper repeatedly notes that observational models already scatter among themselves at a level comparable to any simulation–observation offset, and the “no clear tension” conclusion holds across the other three independent datasets. The step is therefore only a minor self-citation, not a circular reduction of the central claim.

full rationale

The paper’s central claim is methodological and empirical: by evaluating simulated DM slopes and full density profiles at the same physical radii (and stellar masses) that are accessible to four independent dynamical modelling programmes, the apparent cusp-core tension largely disappears and hydrodynamical runs outperform NFW for most of the 16 MW satellites. No free parameter is fitted so that the simulation–observation residual vanishes by construction; the NIHAO/FIRE-2 profiles, the Moster+Moliné NFW proxy, and the reliability cuts are all external to the residual being reported. The sole self-citation of note is AP25 (one co-author), which is treated simply as one of four published observational datasets; the paper itself emphasises that inter-model observational scatter is comparable to the simulation–observation offset, so the agreement claim does not rest on AP25 alone. Reliability radial ranges are acknowledged as practical working definitions, not derived from the simulations. Consequently the derivation chain contains no self-definitional loop, no fitted-input-called-prediction, and no uniqueness or ansatz smuggled via self-citation. Score 1 reflects only the minor, non-load-bearing co-author citation.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 0 invented entities

The central claim rests on standard ΛCDM hydrodynamical modeling, published dynamical inferences, and a set of practical (not theoretically unique) reliability cuts and matching windows. No new physical entities are introduced; free parameters are the numerical thresholds that define ‘reliable’ regions and the mass-matching tolerance.

free parameters (4)
  • inner reliability star count threshold = 50 stars / 3 bins
    Minimum of 50 member stars (or third velocity-dispersion bin) used to set the innermost reliable radius for star-by-star or binned analyses (Sec. 2); described as a practical working definition, not unique.
  • outer reliability star count threshold = 10 stars
    Fewer than 10 member stars defines the outer reliability limit for discrete analyses (Sec. 2).
  • stellar-mass matching window = ±0.25 dex
    Simulated satellites selected within ±0.25 dex of each observed galaxy’s stellar mass for profile comparison (Sec. 4.2).
  • convergence density threshold = f(r)≥0.33 / 200 particles
    r_conv,20 defined via Power/Schaller f(r)≥0.33 (~20 % density convergence) for NIHAO and 200-particle radius for FIRE-2 (Sec. 3.4.1).
axioms (4)
  • domain assumption Baryonic feedback in NIHAO (MaGICC) and FIRE-2 correctly captures the dominant processes that reshape CDM cusps into cores at intermediate stellar masses.
    Invoked throughout Sec. 3–4 when interpreting the mass-dependent core-formation trend as physical rather than numerical.
  • domain assumption The four published dynamical modeling pipelines (H20/H23, R19, AP25, P25/P26) provide meaningful constraints inside the data-driven reliability ranges defined in Sec. 2.
    Explicitly stated as an assumption because ranking techniques by reliability is ‘beyond the scope’ of the paper.
  • domain assumption Projected half-light radii and spectroscopic membership catalogues can be mapped to three-dimensional reliability limits without large bias.
    Sec. 2 notes the approximation is unavoidable because line-of-sight positions are unknown.
  • domain assumption Moster et al. (2013) stellar-to-halo mass relation plus Moliné et al. (2023) subhalo concentration relation supply a fair NFW baseline at fixed stellar mass.
    Used to construct the cyan NFW bands in Fig. 3 and dotted NFW proxies in Figs. 4–5.

pith-pipeline@v1.1.0-grok45 · 28572 in / 3014 out tokens · 26558 ms · 2026-07-13T06:27:24.620700+00:00 · methodology

0 comments
read the original abstract

The cusp-core problem remains a key challenge for the $\Lambda$CDM model. Historically, comparing inner dark matter halo slopes ($d\log\rho/d\log r$) from simulations and observations has suffered from a methodological mismatch: evaluating slopes at different radii creates apparent tensions due to inconsistent definitions rather than genuine physical differences. We rigorously compare dark matter density profiles of Milky Way (MW) dwarf satellites inferred from dynamical modelling against CDM hydrodynamical simulations. Using the NIHAO and FIRE-2 suites ($M_{\star} \sim 10^3$-$10^{11}\,\rm M_\odot$), we confront simulated profiles with dynamical inferences of 16 MW satellites across four methods, strictly within their reliability limits. Crucially, we evaluate simulated slopes at observationally accessible radii, directly comparing profiles at matched stellar mass. Both observed and simulated galaxies exhibit a mass-dependent core-formation trend: inner slopes rise from cuspy values ($\approx -1.5$) at $M_{\star} \sim 10^5\,\rm M_\odot$ to core-like values ($\approx 0$ to $-0.4$) at $M_{\star} \sim 10^8\,\rm M_\odot$. Efficient core formation begins at $M_{\star} \gtrsim 10^6\,\rm M_\odot$ for centrals, where satellites display increased scatter consistent with tidal disruption. Simulated profiles agree with observations within $\lesssim 1\sigma$ for most systems, outperforming a NFW profile. Furthermore, differing observational models present scatter for a given system comparable to the simulation-to-observation offset. Evaluating dark matter density slopes at fixed physical radii significantly improves agreement between hydrodynamical simulations and dynamical models, revealing no clear tension when comparing profiles at fixed stellar mass, but Willman\,1 remains an unresolved outlier.

Figures

Figures reproduced from arXiv: 2607.08818 by Jorge Sarrato-Al\'os, Jos\'e Mar\'ia Arroyo-Polonio.

Figure 1
Figure 1. Figure 1: shows the joint distributions of these parameters. For sim￾ulated galaxies, we calculate the projected half-light radius and effective surface brightness in the V-band5 from 256 projections uniformly distributed along the unit sphere, and plot the median and 1σ range. Simulations exhibit general agreement with observational trends. However, we note that, for stellar masses higher than ∼107M⊙, the half-ligh… view at source ↗
Figure 2
Figure 2. Figure 2: Dark matter density profiles for three galaxies from the FIRE-2 project. The grey shaded region indicates the 1-2% Rvir range, with the black dashed line representing the slope at the logarithmic midpoint. The first panel shows a galaxy selected to match the stellar mass of the Sculptor dwarf; its density is scaled by 1.6 to facilitate the visual comparison of profile shapes with the dynamical analysis by … view at source ↗
Figure 3
Figure 3. Figure 3: Dark matter density slope d log ρ/d log r evaluated at three fixed physical radii versus stellar mass. Each column corresponds to a different radius: 100 pc (left), 250 pc (middle), and 500 pc (right). The upper row shows central (isolated) simulated galaxies, the lower row shows satellites. Grey scale symbols represent simulated galaxies (FIRE-2 and NIHAO): circles for centrals, triangles for satellites. … view at source ↗
Figure 4
Figure 4. Figure 4: Dark matter density profiles versus physical radius. Each panel corresponds to one observed dwarf galaxy and includes all considered literature dynamical model estimates for that galaxy as well as the simulated galaxies whose stellar masses lie within ±0.25 dex of the observed value. Dynamical model density profiles are shown as solid lines (median) with shaded bands (68% credible intervals), colour-coded … view at source ↗
Figure 5
Figure 5. Figure 5: Same layout as [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

104 extracted references · 22 canonical work pages · 18 internal anchors

  1. [1]

    , keywords =

    A Universal Density Profile from Hierarchical Clustering. , keywords =. doi:10.1086/304888 , archivePrefix =. astro-ph/9611107 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/304888

  2. [2]

    High-Resolution Rotation Curves of Low Surface Brightness Galaxies. II. Mass Models. , keywords =. doi:10.1086/323450 , adsurl =

    doi:10.1086/323450

  3. [3]

    Oh, Se-Heon and de Blok, W. J. G. and Brinks, Elias and Walter, Fabian and Kennicutt, Robert C. , year=. DARK AND LUMINOUS MATTER IN THINGS DWARF GALAXIES , volume=. , publisher=. doi:10.1088/0004-6256/141/6/193 , number=

    doi:10.1088/0004-6256/141/6/193

  4. [4]

    , keywords =

    NIHAO - IV: core creation and destruction in dark matter density profiles across cosmic time. , keywords =. doi:10.1093/mnras/stv2856 , archivePrefix =. 1507.03590 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stv2856

  5. [5]

    and Dutton, Aaron A

    Di Cintio, Arianna and Brook, Chris B. and Dutton, Aaron A. and Macciò, Andrea V. and Stinson, Greg S. and Knebe, Alexander , title =. , volume =. 2014 , month =. doi:10.1093/mnras/stu729 , url =

    doi:10.1093/mnras/stu729 2014

  6. [6]

    , keywords =

    The dependence of dark matter profiles on the stellar-to-halo mass ratio: a prediction for cusps versus cores. , keywords =. doi:10.1093/mnras/stt1891 , archivePrefix =. 1306.0898 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stt1891

  7. [7]

    A dark matter profile to model diverse feedback-induced core sizes of $\Lambda$CDM haloes

    A dark matter profile to model diverse feedback-induced core sizes of CDM haloes. , keywords =. doi:10.1093/mnras/staa2101 , archivePrefix =. 2004.10817 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/staa2101 2004

  8. [8]

    , keywords =

    Diversity of Dark Matter Density Profiles in the Galactic Dwarf Spheroidal Satellites. , keywords =. doi:10.3847/1538-4357/abbe0a , archivePrefix =. 2007.13780 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/abbe0a 2007

  9. [9]

    Dark matter halo properties of the Galactic dwarf satellites: implication for chemo-dynamical evolution of the satellites and a challenge to $\Lambda$CDM

    Dark Matter Halo Properties of the Galactic Dwarf Satellites: Implication for Chemo-dynamical Evolution of the Satellites and a Challenge to Lambda Cold Dark Matter. , keywords =. doi:10.3847/1538-4357/ace33e , archivePrefix =. 2206.02821 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ace33e

  10. [10]

    , keywords =

    Cusp-to-core transition of dark matter halos across galaxy mass scales. , keywords =. doi:10.1093/pasj/psag016 , archivePrefix =. 2507.22155 , primaryClass =

    work page doi:10.1093/pasj/psag016

  11. [11]

    , title =

    Hopkins, Philip F. , title =. , volume =. 2015 , month =. doi:10.1093/mnras/stv195 , url =

    doi:10.1093/mnras/stv195 2015

  12. [12]

    FIRE-2 simulations: physics versus numerics in galaxy formation , volume=

    Hopkins, Philip F and Wetzel, Andrew and Kereš, Dušan and Faucher-Giguère, Claude-André and Quataert, Eliot and Boylan-Kolchin, Michael and Murray, Norman and Hayward, Christopher C and Garrison-Kimmel, Shea and Hummels, Cameron and Feldmann, Robert and Torrey, Paul and Ma, Xiangcheng and Anglés-Alcázar, Daniel and Su, Kung-Yi and Orr, Matthew and Schmitz...

    doi:10.1093/mnras/sty1690

  13. [13]

    Planck 2013 results. XVI. Cosmological parameters. , keywords =. doi:10.1051/0004-6361/201321591 , archivePrefix =. 1303.5076 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201321591 2013

  14. [14]

    , keywords =

    The AGORA High-resolution Galaxy Simulations Comparison Project. , keywords =. doi:10.1088/0067-0049/210/1/14 , archivePrefix =. 1308.2669 , primaryClass =

    doi:10.1088/0067-0049/210/1/14

  15. [15]

    , keywords =

    Galaxies at the Extremes: Ultra-diffuse Galaxies in the Virgo Cluster. , keywords =. doi:10.1088/2041-8205/809/2/L21 , archivePrefix =. 1507.02270 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/2041-8205/809/2/l21 2041

  16. [16]

    ELVES I: Structures of Dwarf Satellites of MW-like Galaxies; Morphology, Scaling Relations, and Intrinsic Shapes

    Structures of Dwarf Satellites of Milky Way-like Galaxies: Morphology, Scaling Relations, and Intrinsic Shapes. , keywords =. doi:10.3847/1538-4357/ac2581 , archivePrefix =. 2105.03435 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac2581

  17. [17]

    , keywords =

    The Observed Properties of Dwarf Galaxies in and around the Local Group. , keywords =. doi:10.1088/0004-6256/144/1/4 , archivePrefix =. 1204.1562 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-6256/144/1/4

  18. [18]

    , keywords =

    An almost dark galaxy with the mass of the Small Magellanic Cloud. , keywords =. doi:10.1051/0004-6361/202347667 , archivePrefix =. 2310.12231 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202347667

  19. [19]

    , keywords =

    A Universal Mass Profile for Dwarf Spheroidal Galaxies?. , keywords =. doi:10.1088/0004-637X/704/2/1274 , archivePrefix =. 0906.0341 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/704/2/1274

  20. [20]

    , keywords =

    Accurate masses for dispersion-supported galaxies. , keywords =. doi:10.1111/j.1365-2966.2010.16753.x , archivePrefix =. 0908.2995 , primaryClass =

    doi:10.1111/j.1365-2966.2010.16753.x 2010

  21. [21]

    , keywords =

    Dark matter cores and cusps: the case of multiple stellar populations in dwarf spheroidals. , keywords =. doi:10.1111/j.1365-2966.2011.19684.x , archivePrefix =. 1106.1062 , primaryClass =

    doi:10.1111/j.1365-2966.2011.19684.x 2011

  22. [22]

    , keywords =

    Knowing the unknowns: uncertainties in simple estimators of galactic dynamical masses. , keywords =. doi:10.1093/mnras/stx975 , archivePrefix =. 1603.04443 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stx975

  23. [23]

    , keywords =

    Systematics in virial mass estimators for pressure-supported systems. , keywords =. doi:10.1093/mnras/sty2505 , archivePrefix =. 1805.00484 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty2505

  24. [24]

    , keywords =

    AHF: Amiga's Halo Finder. , keywords =. doi:10.1088/0067-0049/182/2/608 , archivePrefix =. 0904.3662 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0067-0049/182/2/608

  25. [25]

    , keywords =

    AGAMA: action-based galaxy modelling architecture. , keywords =. doi:10.1093/mnras/sty2672 , archivePrefix =. 1802.08239 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty2672

  26. [26]

    Monthly Notices of the Royal Astronomical Society , volume=

    Gasoline2: a modern smoothed particle hydrodynamics code , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2017 , publisher=

    2017

  27. [27]

    Reproducing the inefficiency of galaxy formation across cosmic time with a large sample of cosmological hydrodynamical simulations , author=

    NIHAO project--I. Reproducing the inefficiency of galaxy formation across cosmic time with a large sample of cosmological hydrodynamical simulations , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2015 , publisher=

    2015

  28. [28]

    , archivePrefix = "arXiv", eprint =

    MaGICC discs: matching observed galaxy relationships over a wide stellar mass range. , archivePrefix = "arXiv", eprint =. doi:10.1111/j.1365-2966.2012.21306.x , adsurl =

    doi:10.1111/j.1365-2966.2012.21306.x 2012

  29. [29]

    metal cooling and metal diffusion , volume=

    The enrichment of the intergalactic medium with adiabatic feedback - i. metal cooling and metal diffusion , volume=. , author=. 2010 , pages=. doi:10.1111/j.1365-2966.2010.17047.x , number=

    doi:10.1111/j.1365-2966.2010.17047.x 2010

  30. [30]

    , keywords =

    Halo Expansion in Cosmological Hydro Simulations: Toward a Baryonic Solution of the Cusp/Core Problem in Massive Spirals. , keywords =. doi:10.1088/2041-8205/744/1/L9 , archivePrefix =. 1111.5620 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/2041-8205/744/1/l9 2041

  31. [31]

    , eprint =

    Galactic Stellar and Substellar Initial Mass Function. , eprint =. doi:10.1086/376392 , adsurl =

    doi:10.1086/376392

  32. [32]

    Isolated galaxies

    Star formation and feedback in smoothed particle hydrodynamic simulations - I. Isolated galaxies. , eprint =. doi:10.1111/j.1365-2966.2006.11097.x , adsurl =

    doi:10.1111/j.1365-2966.2006.11097.x 2006

  33. [33]

    , archivePrefix = "arXiv", eprint =

    Making Galaxies In a Cosmological Context: the need for early stellar feedback. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/sts028 , adsurl =

    doi:10.1093/mnras/sts028

  34. [34]

    Chemo-dynamics of the stellar component of the Sculptor dwarf galaxy II: dynamical properties and dark matter halo density

    Chemo-dynamics of the stellar component of the Sculptor dwarf galaxy: II. Dynamical properties and dark matter halo density. , keywords =. doi:10.1051/0004-6361/202554826 , archivePrefix =. 2506.11845 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202554826

  35. [35]

    and Macciò, Andrea V

    Dutton, Aaron A. and Macciò, Andrea V. , year=. Cold dark matter haloes in the Planck era: evolution of structural parameters for Einasto and NFW profiles , volume=. , publisher=. doi:10.1093/mnras/stu742 , number=

    doi:10.1093/mnras/stu742

  36. [36]

    and Bullock, James S

    Fitts, Alex and Boylan-Kolchin, Michael and Elbert, Oliver D. and Bullock, James S. and Hopkins, Philip F. and Oñorbe, Jose and Wetzel, Andrew and Wheeler, Coral and Faucher-Giguère, Claude-André and Kereš, Dušan and Skillman, Evan D. and Weisz, Daniel R. , title =. , volume =. 2017 , month =. doi:10.1093/mnras/stx1757 , url =

    doi:10.1093/mnras/stx1757 2017

  37. [37]

    , keywords =

    Statistical Properties of X-Ray Clusters: Analytic and Numerical Comparisons. , keywords =. doi:10.1086/305262 , archivePrefix =. astro-ph/9710107 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/305262

  38. [38]

    , keywords =

    The impact of star formation histories on the inner dark matter density slopes of galaxies. , keywords =. doi:10.1051/0004-6361/202558718 , archivePrefix =. 2601.17113 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202558718

  39. [39]

    A numerical convergence study

    The inner structure of CDM haloes - I. A numerical convergence study. , keywords =. doi:10.1046/j.1365-8711.2003.05925.x , archivePrefix =. astro-ph/0201544 , primaryClass =

    doi:10.1046/j.1365-8711.2003.05925.x 2003

  40. [40]

    and Wechsler, Risa H

    Behroozi, Peter S. and Wechsler, Risa H. and Wu, Hao-Yi , year=. THE ROCKSTAR PHASE-SPACE TEMPORAL HALO FINDER AND THE VELOCITY OFFSETS OF CLUSTER CORES , volume=. The Astrophysical Journal , publisher=. doi:10.1088/0004-637x/762/2/109 , number=

    doi:10.1088/0004-637x/762/2/109

  41. [41]

    , keywords =

    Dark matter heats up in dwarf galaxies. , keywords =. doi:10.1093/mnras/sty3404 , archivePrefix =. 1808.06634 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty3404

  42. [42]

    and Nipoti, C

    Pascale, R. and Nipoti, C. and Calura, F. and Della Croce, A. , year=. Leo I: The classical dwarf spheroidal galaxy with the highest dark matter density , volume=. doi:10.1051/0004-6361/202555004 , journal=

    doi:10.1051/0004-6361/202555004

  43. [43]

    and Battaglia, G

    Pascale, R. and Battaglia, G. and Arroyo-Polonio, J. M. and Vasiliev, E. and Nipoti, C. and Thomas, G. F. , year=. Multi-component axisymmetric dynamical models of dSphs based on distribution functions: Inferences on dark matter and intermediate-mass black holes in Draco and Ursa Minor , volume=. doi:10.1051/0004-6361/202660016 , journal=

    work page doi:10.1051/0004-6361/202660016

  44. [44]

    and Abraham, Roberto and Merritt, Allison and Zhang, Jielai and Geha, Marla and Conroy, Charlie , year=

    van Dokkum, Pieter G. and Abraham, Roberto and Merritt, Allison and Zhang, Jielai and Geha, Marla and Conroy, Charlie , year=. FORTY-SEVEN MILKY WAY-SIZED, EXTREMELY DIFFUSE GALAXIES IN THE COMA CLUSTER , volume=. The Astrophysical Journal , publisher=. doi:10.1088/2041-8205/798/2/l45 , number=

    doi:10.1088/2041-8205/798/2/l45 2041

  45. [45]

    and Bower, Richard G

    Schaller, Matthieu and Frenk, Carlos S. and Bower, Richard G. and Theuns, Tom and Jenkins, Adrian and Schaye, Joop and Crain, Robert A. and Furlong, Michelle and Dalla Vecchia, Claudio and McCarthy, I. G. , title =. , volume =. 2015 , month =. doi:10.1093/mnras/stv1067 , url =

    doi:10.1093/mnras/stv1067 2015

  46. [46]

    , keywords =

    Galactic star formation and accretion histories from matching galaxies to dark matter haloes. , keywords =. doi:10.1093/mnras/sts261 , archivePrefix =. 1205.5807 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sts261

  47. [47]

    Zhao, H. , year=. Analytical models for galactic nuclei , volume=. Monthly Notices of the Royal Astronomical Society , publisher=. doi:10.1093/mnras/278.2.488 , number=

    doi:10.1093/mnras/278.2.488

  48. [48]

    LCDM halo substructure properties revealed with high resolution and large volume cosmological simulations

    CDM halo substructure properties revealed with high-resolution and large-volume cosmological simulations. , keywords =. doi:10.1093/mnras/stac2930 , archivePrefix =. 2110.02097 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac2930

  49. [49]

    , keywords =

    The Coupling between the Core/Cusp and Missing Satellite Problems. , keywords =. doi:10.1088/2041-8205/759/2/L42 , archivePrefix =. 1207.2772 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/2041-8205/759/2/l42 2041

  50. [50]

    and Di Cintio, Arianna , title =

    Brook, Chris B. and Di Cintio, Arianna , title =. , volume =. 2015 , month =. doi:10.1093/mnras/stv1699 , url =

    doi:10.1093/mnras/stv1699 2015

  51. [51]

    The tidal evolution of dark matter substructure -- I. Subhalo density profiles

    The tidal evolution of dark matter substructure - I. subhalo density profiles. , keywords =. doi:10.1093/mnras/stz2767 , archivePrefix =. 1908.08537 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz2767 1908

  52. [52]

    , keywords =

    The impact of dark matter cusps and cores on the satellite galaxy population around spiral galaxies. , keywords =. doi:10.1111/j.1365-2966.2010.16762.x , archivePrefix =. 1002.3376 , primaryClass =

    doi:10.1111/j.1365-2966.2010.16762.x 2010

  53. [53]

    The Messenger , year = 2006, month = mar, volume =

    The Dwarf galaxy Abundances and Radial-velocities Team (DART) Large Programme - A Close Look at Nearby Galaxies. The Messenger , year = 2006, month = mar, volume =

    2006

  54. [54]

    , keywords =

    Stellar Velocities in the Carina, Fornax, Sculptor, and Sextans dSph Galaxies: Data From the Magellan/MMFS Survey. , keywords =. doi:10.1088/0004-6256/137/2/3100 , archivePrefix =. 0811.0118 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-6256/137/2/3100

  55. [55]

    A 3D view of dwarf galaxies with Gaia and VLT/FLAMES II. The Sextans dwarf spheroidal

    A 3D view of dwarf galaxies with Gaia and VLT/FLAMES: II. The Sextans dwarf spheroidal. , keywords =. doi:10.1051/0004-6361/202554176 , archivePrefix =. 2504.02787 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202554176

  56. [56]

    HSTPROMO Internal Proper-motion Kinematics of Dwarf Spheroidal Galaxies. I. Velocity Anisotropy and Dark Matter Cusp Slope of Draco. , keywords =. doi:10.3847/1538-4357/ad571c , archivePrefix =. 2407.07769 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ad571c

  57. [57]

    , keywords =

    M/L and velocity anisotropy from observations of spherical galaxies, or must M87 have a massive black hole ?. , keywords =. doi:10.1093/mnras/200.2.361 , adsurl =

    doi:10.1093/mnras/200.2.361

  58. [58]

    , keywords =

    The Distribution of Dark Matter in the Coma Cluster. , keywords =. doi:10.1086/164953 , adsurl =

    doi:10.1086/164953

  59. [59]

    The kinematic status and mass content of the Sculptor dwarf spheroidal galaxy

    The Kinematic Status and Mass Content of the Sculptor Dwarf Spheroidal Galaxy. , keywords =. doi:10.1086/590179 , archivePrefix =. 0802.4220 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/590179

  60. [60]

    , keywords =

    A discrete chemo-dynamical model of the dwarf spheroidal galaxy Sculptor: mass profile, velocity anisotropy and internal rotation. , keywords =. doi:10.1093/mnras/stw2081 , archivePrefix =. 1608.08239 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stw2081

  61. [61]

    , keywords =

    Dynamical Models for the Sculptor Dwarf Spheroidal in a CDM Universe. , keywords =. doi:10.3847/1538-4357/aa5c8e , archivePrefix =. 1406.6079 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aa5c8e

  62. [62]

    , keywords =

    GravSphere2: A higher order Jeans method for mass modeling spherical stellar systems. , keywords =. doi:10.1051/0004-6361/202557195 , archivePrefix =. 2509.24103 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/202557195

  63. [63]

    Disentangling gamma-beta: the 4th-order velocity moments based on spherical Jeans analysis

    Disentangling - : The Fourth-order Velocity Moments Based on Spherical Jeans Analysis. , keywords =. doi:10.3847/1538-4357/adb8e4 , archivePrefix =. 2404.12671 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/adb8e4

  64. [64]

    , keywords =

    Model comparison of the dark matter profiles of Fornax, Sculptor, Carina and Sextans. , keywords =. doi:10.1051/0004-6361/201321606 , archivePrefix =. 1304.2976 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201321606

  65. [65]

    , keywords =

    Tidal disruption of dwarf spheroidal galaxies: the strange case of Crater II. , keywords =. doi:10.1093/mnras/sty1278 , archivePrefix =. 1802.09537 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/sty1278

  66. [66]

    , keywords =

    Estimating the dynamical masses of dwarf galaxies in the presence of binary-star contamination. , keywords =. doi:10.1051/0004-6361/202558720 , archivePrefix =. 2603.03129 , primaryClass =

    work page doi:10.1051/0004-6361/202558720

  67. [67]

    Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo

    Magellan/M2FS and MMT/Hectochelle Spectroscopy of Dwarf Galaxies and Faint Star Clusters within the Galactic Halo. , keywords =. doi:10.3847/1538-4365/acdd79 , archivePrefix =. 2312.12738 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4365/acdd79

  68. [68]

    and Kereš, Dušan and Oñorbe, José and Faucher-Giguère, Claude-André and Quataert, Eliot and Murray, Norman and Bullock, James S

    Hopkins, Philip F. and Kereš, Dušan and Oñorbe, José and Faucher-Giguère, Claude-André and Quataert, Eliot and Murray, Norman and Bullock, James S. , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2014 , month =. doi:10.1093/mnras/stu1738 , url =

    doi:10.1093/mnras/stu1738 2014

  69. [69]

    A MegaCam Survey of Outer Halo Satellites. III. Photometric and Structural Parameters. , keywords =. doi:10.3847/1538-4357/aac16b , archivePrefix =. 1806.06891 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aac16b

  70. [70]

    Discovery of a large and diffuse Milky Way dwarf galaxy in the constellation of Crater

    The feeble giant. Discovery of a large and diffuse Milky Way dwarf galaxy in the constellation of Crater. , keywords =. doi:10.1093/mnras/stw733 , archivePrefix =. 1601.07178 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stw733

  71. [71]

    , keywords =

    The hidden giant: discovery of an enormous Galactic dwarf satellite in Gaia DR2. , keywords =. doi:10.1093/mnras/stz1624 , archivePrefix =. 1811.04082 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stz1624

  72. [72]

    , keywords =

    The BaSTI Stellar Evolution Database: models for extremely metal-poor and super-metal-rich stellar populations. , keywords =. doi:10.1051/0004-6361/201321950 , archivePrefix =. 1308.3850 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201321950

  73. [73]

    Cuspy dark matter density profiles in massive dwarf galaxies

    Cuspy dark matter density profiles in massive dwarf galaxies. , keywords =. doi:10.1093/mnras/stac588 , archivePrefix =. 2203.00694 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac588

  74. [74]

    , keywords =

    Bulgeless dwarf galaxies and dark matter cores from supernova-driven outflows. , keywords =. doi:10.1038/nature08640 , archivePrefix =. 0911.2237 , primaryClass =

    Pith/arXiv arXiv doi:10.1038/nature08640

  75. [75]

    , keywords =

    How supernova feedback turns dark matter cusps into cores. , keywords =. doi:10.1111/j.1365-2966.2012.20571.x , archivePrefix =. 1106.0499 , primaryClass =

    doi:10.1111/j.1365-2966.2012.20571.x 2012

  76. [76]

    , keywords =

    The Dark Matter Content of Milky Way Dwarf Spheroidal Galaxies: Draco, Sextans, and Ursa Minor. , keywords =. doi:10.3847/1538-4357/ae07ce , archivePrefix =. 2507.02284 , primaryClass =

    doi:10.3847/1538-4357/ae07ce

  77. [77]

    , keywords =

    Observational Evidence for Self-Interacting Cold Dark Matter. , keywords =. doi:10.1103/PhysRevLett.84.3760 , archivePrefix =. astro-ph/9909386 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/physrevlett.84.3760

  78. [78]

    Local Group and Nearby Dwarf Galaxies Catalog

  79. [79]

    , keywords =

    The tidal stripping of satellites. , keywords =. doi:10.1111/j.1365-2966.2005.09861.x , archivePrefix =. astro-ph/0506687 , primaryClass =

    doi:10.1111/j.1365-2966.2005.09861.x 2005

  80. [80]

    and Kang, Xi , title =

    Chang, Jiang and Macciò, Andrea V. and Kang, Xi , title =. Monthly Notices of the Royal Astronomical Society , volume =. 2013 , month =. doi:10.1093/mnras/stt434 , url =

    work page doi:10.1093/mnras/stt434 2013

Showing first 80 references.