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arxiv: 2605.18975 · v1 · pith:NNTS5T76new · submitted 2026-05-18 · 🌌 astro-ph.GA

Bulgeless Evolution And the Rise of Discs (BEARD) III. A numerical simulation view of satellites around Milky-Way analogues

Salvador Cardona-Barrero , Jairo M\'endez-Abreu , Adriana de Lorenzo-C\'aceres , Carlos Marrero de la Rosa , Yetli Rosas-Guevara , Elena Arjona-G\'alvez , Mario Chamorro Cazorla , Nelvy Choque-Challapa
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Enrico Maria Corsini Arianna Di Cintio David Fernandez Daniele Gasparri Divakara Mayya Lorenzo Morelli Francesca Pinna Alessandro Pizzella Javier Rom\'an Daniel Rosa Gonzalez Olga Vega Stefano Zarattini
This is my paper

Pith reviewed 2026-05-20 08:35 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords bulgeless galaxiessatellite populationsorbital alignmentgalaxy morphologycosmological hydrodynamical simulationMilky Way analoguesmerger historydisc galaxies
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The pith

Bulgeless galaxies host satellite systems that are more centrally concentrated, orbitally aligned with the disc, and dynamically colder than those around bulge-dominated galaxies.

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

This paper compares the satellite populations of bulgeless disc galaxies to those of bulge-dominated galaxies with matched stellar masses in a high-resolution cosmological simulation. Satellite numbers turn out similar, but the bulgeless hosts show satellites that cluster closer to the center, align more closely with the host disc plane, and follow more orderly orbits. These differences arise because the host galaxy and its satellites evolve together, so a quieter merger history for bulgeless systems imprints itself on the satellites. A reader would care because the result offers a way to trace how galaxies assembled by looking at their surrounding satellites rather than only at the central structure itself.

Core claim

Using the TNG50-1 simulation, the satellite systems of 135 bulgeless galaxies were compared to a control sample of bulge-dominated galaxies with similar stellar masses. Satellite abundance does not depend strongly on morphology, but satellites around bulgeless galaxies display a steeper faint-end luminosity function, greater central concentration, and stronger alignment with the host disc plane. This orbital alignment results from coherent post-infall dynamical evolution that is sensitive to the host morphology, though infall of massive satellites can disrupt or stall the alignment. The results indicate that the morphology of the central galaxy imprints on its satellite system through their共

What carries the argument

Co-evolution of host galaxy morphology and post-infall satellite orbital dynamics, which transfers central structural properties to the satellite population's spatial and kinematic traits.

If this is right

  • Satellite abundance is largely independent of whether the host galaxy has a bulge.
  • Satellites around bulgeless galaxies exhibit a steeper faint-end slope in their luminosity function.
  • Satellites are more centrally concentrated around bulgeless hosts.
  • Orbital alignment with the disc plane is stronger for satellites of bulgeless galaxies due to morphology-dependent post-infall evolution.
  • Infall of massive satellites can temporarily weaken or stall the secular alignment process.

Where Pith is reading between the lines

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

  • Satellite alignment and concentration statistics could serve as indirect indicators of host bulge fraction in surveys where central morphology is difficult to measure directly.
  • The results connect to questions of assembly bias by suggesting that quieter merger environments preserve more coherent satellite systems around disc galaxies.
  • Extending the comparison to higher redshifts in simulations might reveal when the morphological imprint on satellites first appears during galaxy growth.
  • Accurate modeling of central potential effects on satellite orbits will be required in future simulations to match observed satellite distributions around real bulgeless galaxies.

Load-bearing premise

The simulation accurately captures how a host galaxy's central morphology shapes the orbits and distributions of its satellites after they fall in.

What would settle it

A large observational survey of Milky Way analogue galaxies finding no difference in satellite orbital alignment angles or radial concentration between bulgeless and bulge-dominated hosts.

Figures

Figures reproduced from arXiv: 2605.18975 by Adriana de Lorenzo-C\'aceres, Alessandro Pizzella, Arianna Di Cintio, Carlos Marrero de la Rosa, Daniele Gasparri, Daniel Rosa Gonzalez, David Fernandez, Divakara Mayya, Elena Arjona-G\'alvez, Enrico Maria Corsini, Francesca Pinna, Jairo M\'endez-Abreu, Javier Rom\'an, Lorenzo Morelli, Mario Chamorro Cazorla, Nelvy Choque-Challapa, Olga Vega, Salvador Cardona-Barrero, Stefano Zarattini, Yetli Rosas-Guevara.

Figure 1
Figure 1. Figure 1: Top panel: Distribution of host galaxy stellar mass. Bot [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Face-on color-composite images of randomly selected galaxies from the samples used in this work. Images have been [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Number of satellite galaxies as function of the host’s [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Colourmagnitude diagram of satellite galaxies. Satellites [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of the ratio between the stellar mass of the [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 5
Figure 5. Figure 5: Stacked satellite LFs of the BD (orange), BL (blue) and [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: Stacked empirical cumulative distribution function of the [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Satellite infall time distribution. Infall times are estimated [PITH_FULL_IMAGE:figures/full_fig_p010_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Top panel: Distribution of satellite orbital alignment, at [PITH_FULL_IMAGE:figures/full_fig_p011_10.png] view at source ↗
read the original abstract

$Aims$. The existence of massive disc galaxies with little or no bulge challenges conventional $\Lambda$ cold dark matter model, which typically favours dynamically hot central structures due to early collapse and mergers. The study of these bulgeless disc galaxies is the aim of the Bulgeless Evolution And the Rise of Discs (BEARD) survey, as they offer a unique opportunity to investigate the link between galaxy morphology and the properties of their satellite systems. $Methods$. Using the high-resolution cosmological hydrodynamical simulation TNG50-1, we studied the satellite populations of 135 bulgeless galaxies. We compared their satellite properties to those of a bulge-dominated control sample with matched stellar masses. Our analysis focuses on satellite abundance, luminosity functions, spatial distribution, orbital alignment, and infall histories. $Results$. We find that satellite abundance is largely independent of host galaxy morphology. However, satellites around bulgeless galaxies exhibit luminosity functions with a steeper faint-end slope, are more centrally concentrated, and show stronger orbital alignment with the host disc plane. The orbital alignment originates from coherent post-infall dynamical evolution that depends on host galaxy morphology. The infall of more massive satellites can additionally perturb this process, contributing to a weakening or temporary stalling of the secular alignment. $Conclusions$. Due to the co-evolution of the host galaxy and the satellite system, the morphology of the central galaxy leaves a clear imprint on its satellite system. Bulgeless galaxies tend to have dynamically colder, more aligned, and more centrally concentrated satellite populations. These trends reflect a more quiet merger history and support the use of satellite properties as tracers of host galaxy formation pathways.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 1 minor

Summary. The manuscript uses the TNG50-1 cosmological hydrodynamical simulation to compare the satellite populations of 135 bulgeless galaxies against a stellar-mass-matched control sample of bulge-dominated galaxies. It reports that satellite abundance is largely independent of host morphology, while bulgeless hosts exhibit satellites with steeper faint-end luminosity functions, greater central concentration, and stronger orbital alignment with the host disc plane. These differences are attributed to co-evolution, with orbital alignment arising from coherent post-infall dynamical evolution that depends on host morphology and is modulated by massive satellite infall.

Significance. If robust, the results provide a controlled numerical view of how central galaxy morphology imprints on satellite system properties, supporting the use of satellites as tracers of host formation history in the context of the BEARD survey. The direct comparison of simulation outputs for abundance, luminosity functions, spatial distributions, and alignments is a clear strength, as is the focus on post-infall processes rather than fitted parameters.

major comments (1)
  1. [Methods and Results (orbital alignment and spatial distribution)] The central claim that differences in satellite alignment, concentration, and faint-end slope arise from morphology-dependent post-infall co-evolution (Results and Conclusions) requires that TNG50-1 accurately captures orbital evolution for low-mass satellites. The simulation has baryonic mass resolution ~8.5e4 Msun and softening ~0.3 kpc; satellites driving the steeper faint-end slope experience rapid decay and stripping whose rates depend on central potential shape. Bulgeless hosts have shallower potentials, so numerical heating or force inaccuracies could preferentially affect alignment and concentration relative to bulge-dominated hosts. The manuscript should include explicit resolution convergence tests or comparisons to higher-resolution runs to rule out artifacts.
minor comments (1)
  1. [Methods] The exact criteria used to classify bulgeless galaxies in the simulation and the precise matching procedure for the control sample (stellar mass, redshift range, etc.) would benefit from a concise summary table or explicit list in the Methods to aid reproducibility.

Simulated Author's Rebuttal

1 responses · 1 unresolved

We thank the referee for their careful and constructive review of our manuscript. We address the major comment on numerical resolution and potential artifacts below, providing our honest assessment while committing to revisions where feasible.

read point-by-point responses

  1. Referee: The central claim that differences in satellite alignment, concentration, and faint-end slope arise from morphology-dependent post-infall co-evolution (Results and Conclusions) requires that TNG50-1 accurately captures orbital evolution for low-mass satellites. The simulation has baryonic mass resolution ~8.5e4 Msun and softening ~0.3 kpc; satellites driving the steeper faint-end slope experience rapid decay and stripping whose rates depend on central potential shape. Bulgeless hosts have shallower potentials, so numerical heating or force inaccuracies could preferentially affect alignment and concentration relative to bulge-dominated hosts. The manuscript should include explicit resolution convergence tests or comparisons to higher-resolution runs to rule out artifacts.

    Authors: We appreciate the referee highlighting this important caveat regarding TNG50-1's resolution for low-mass satellite orbital evolution. The quoted mass resolution and softening length are accurate, and we agree that dynamical friction, tidal stripping, and numerical heating could in principle be influenced by the shallower central potentials in bulgeless hosts. However, the morphological differences in the potential are physical, and our reported trends in alignment and concentration arise from the coherent post-infall evolution we measure directly in the simulation. Prior TNG50 studies have validated satellite dynamics in this mass regime against both observations and higher-resolution zoom simulations. To address the concern, we will add a new paragraph in the Methods section discussing resolution limitations, citing relevant TNG convergence literature on satellite stripping and orbits, and explicitly noting that the trends are unlikely to be dominated by numerical artifacts. We cannot add new explicit convergence tests, as no higher-resolution run with a comparable statistical sample of bulgeless galaxies is available. revision: partial

standing simulated objections not resolved
  • We lack access to higher-resolution cosmological hydrodynamical simulations containing a statistically equivalent sample of bulgeless Milky Way analogues, preventing direct resolution convergence tests.

Circularity Check

0 steps flagged

No significant circularity in simulation-based satellite comparison

full rationale

The paper reports direct outputs from the TNG50-1 simulation: satellite abundance, luminosity functions, spatial distributions, orbital alignments, and infall histories are measured for 135 bulgeless galaxies versus a mass-matched bulge-dominated control sample. No parameters are fitted to data subsets and then re-predicted, no quantities are defined in terms of the results they are claimed to produce, and no load-bearing steps reduce to self-citations or imported uniqueness theorems. The central claim that host morphology imprints on satellite properties follows from the numerical experiment itself rather than any re-derivation or renaming of inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim depends on the validity of the TNG50-1 hydrodynamical simulation for reproducing realistic satellite orbital evolution and on the assumption that the simulated bulgeless galaxies are comparable to observed ones; no additional free parameters are introduced in the abstract.

axioms (1)
  • domain assumption The TNG50-1 simulation provides a sufficiently accurate model of galaxy and satellite co-evolution in a Lambda-CDM cosmology.
    All reported differences in satellite properties are interpreted as physical outcomes of the simulation rather than numerical artifacts.

pith-pipeline@v0.9.0 · 5950 in / 1395 out tokens · 54095 ms · 2026-05-20T08:35:52.130644+00:00 · methodology

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Reference graph

Works this paper leans on

115 extracted references · 115 canonical work pages · 46 internal anchors

  1. [1]

    , keywords =

    Baryonic imprints on DM haloes: population statistics from dwarf galaxies to galaxy clusters. , keywords =. doi:10.1093/mnras/stab3177 , archivePrefix =. 2109.02713 , primaryClass =

    work page doi:10.1093/mnras/stab3177

  2. [2]

    , keywords =

    Rigorous luminosity function determination in the presence of a background: theory and application to two intermediate redshift clusters ^ *. , keywords =. doi:10.1111/j.1365-2966.2005.09063.x , archivePrefix =. astro-ph/0503704 , primaryClass =

    work page doi:10.1111/j.1365-2966.2005.09063.x 2005

  3. [3]

    Frequency and properties of bars in cluster and field galaxies at intermediate redshifts

    Frequency and properties of bars in cluster and field galaxies at intermediate redshifts. , keywords =. doi:10.1051/0004-6361/200810352 , archivePrefix =. 0902.4080 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200810352

  4. [4]

    Bulge Formation via Mergers in Cosmological Simulations

    Bulge Formation via Mergers in Cosmological Simulations. Galactic Bulges , year = 2016, editor =. doi:10.1007/978-3-319-19378-6_12 , archivePrefix =. 1511.04095 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/978-3-319-19378-6_12 2016

  5. [5]

    Stellar population synthesis at the resolution of 2003

    , year =. arXiv , doi =:astro-ph/0309134 , keywords =

    work page internal anchor Pith review Pith/arXiv arXiv

  6. [6]

    L., & Norman, M

    , year =. arXiv , doi =:astro-ph/9710107 , keywords =

    work page internal anchor Pith review Pith/arXiv arXiv

  7. [7]

    , keywords =

    Milky Way-est: Cosmological Zoom-in Simulations with Large Magellanic Cloud and Gaia Sausage Enceladus Analogs. , keywords =. doi:10.3847/1538-4357/ad554c , archivePrefix =. 2404.08043 , primaryClass =

    work page doi:10.3847/1538-4357/ad554c

  8. [8]

    A universal angular momentum profile for galactic halos

    A Universal Angular Momentum Profile for Galactic Halos. , keywords =. doi:10.1086/321477 , archivePrefix =. astro-ph/0011001 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/321477

  9. [9]

    Reionization and the abundance of galactic satellites

    Reionization and the Abundance of Galactic Satellites. , keywords =. doi:10.1086/309279 , archivePrefix =. astro-ph/0002214 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/309279

  10. [10]

    Journal of Statistical Software , author=

    Bambi: A Simple Interface for Fitting Bayesian Linear Models in Python , volume=. Journal of Statistical Software , author=. 2022 , pages=. doi:10.18637/jss.v103.i15 , number=

    work page doi:10.18637/jss.v103.i15 2022

  11. [11]

    , author Padovani, P

    Dark halo response and the stellar initial mass function in early-type and late-type galaxies. , keywords =. doi:10.1111/j.1365-2966.2011.19038.x , archivePrefix =. 1012.5859 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.19038.x 2011

  12. [12]

    , keywords =

    The dependence of the galaxy stellar-to-halo mass relation on galaxy morphology. , keywords =. doi:10.1093/mnras/staa3053 , archivePrefix =. 2010.01186 , primaryClass =

    work page doi:10.1093/mnras/staa3053 2010

  13. [13]

    , keywords =

    Dynamical evidence for a morphology-dependent relation between the stellar and halo masses of galaxies. , keywords =. doi:10.1051/0004-6361/202040256 , archivePrefix =. 2102.11282 , primaryClass =

    work page doi:10.1051/0004-6361/202040256

  14. [14]

    On the Lack of Evolution in Galaxy Star Formation Efficiency

    On the Lack of Evolution in Galaxy Star Formation Efficiency. , keywords =. doi:10.1088/2041-8205/762/2/L31 , archivePrefix =. 1209.3013 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/762/2/l31 2041

  15. [15]

    Galactic star formation and accretion histories from matching galaxies to dark matter haloes

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sts261

  16. [16]

    Symfind: Addressing the Fragility of Subhalo Finders and Revealing the Durability of Subhalos

    SYMFIND : Addressing the Fragility of Subhalo Finders and Revealing the Durability of Subhalos. , keywords =. doi:10.3847/1538-4357/ad4e33 , archivePrefix =. 2308.10926 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ad4e33

  17. [17]

    , keywords =

    Radial Distributions of Dwarf Satellite Systems in the Local Volume. , keywords =. doi:10.3847/1538-4357/abb60b , archivePrefix =. 2006.02444 , primaryClass =

    work page doi:10.3847/1538-4357/abb60b 2006

  18. [18]

    , keywords =

    The Exploration of Local VolumE Satellites (ELVES) Survey: A Nearly Volume-limited Sample of Nearby Dwarf Satellite Systems. , keywords =. doi:10.3847/1538-4357/ac6fd7 , archivePrefix =. 2203.00014 , primaryClass =

    work page doi:10.3847/1538-4357/ac6fd7

  19. [19]

    Galactic Stellar and Substellar Initial Mass Function

    Galactic Stellar and Substellar Initial Mass Function. , keywords =. doi:10.1086/376392 , archivePrefix =. astro-ph/0304382 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/376392

  20. [20]

    , url =. in prep. , note =. doi:, abstract =

    work page

  21. [21]

    , keywords =

    A Duality in the Origin of Bulges and Spheroidal Galaxies. , keywords =. doi:10.3847/1538-4357/abef72 , archivePrefix =. 2103.10438 , primaryClass =

    work page doi:10.3847/1538-4357/abef72

  22. [22]

    , keywords =

    From Naked Spheroids to Disky Galaxies: How Do Massive Disk Galaxies Shape Their Morphology?. , keywords =. doi:10.3847/1538-4357/ac5a57 , archivePrefix =. 2202.02332 , primaryClass =

    work page doi:10.3847/1538-4357/ac5a57

  23. [23]

    Astronomy & Astrophysics , author =

    Untangling stellar components of galaxies:. Astronomy & Astrophysics , author =. 2024 , pages =. doi:10.1051/0004-6361/202451202 , abstract =

    work page doi:10.1051/0004-6361/202451202 2024

  24. [24]

    , author Padovani, P

    Times, environments and channels of bulge formation in a Lambda cold dark matter cosmology. , keywords =. doi:10.1111/j.1365-2966.2011.18475.x , archivePrefix =. 1102.3186 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.18475.x 2011

  25. [25]

    NIHAO XXI: The emergence of Low Surface Brightness galaxies

    NIHAO XXI: the emergence of low surface brightness galaxies. , keywords =. doi:10.1093/mnras/stz985 , archivePrefix =. 1901.08559 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz985 1901

  26. [26]

    , keywords =

    Dark matter halos and scaling relations of extremely massive spiral galaxies from extended H I rotation curves. , keywords =. doi:10.1093/mnras/stac3424 , archivePrefix =. 2207.02906 , primaryClass =

    work page doi:10.1093/mnras/stac3424

  27. [27]

    2018 , publisher=

    An introduction to generalized linear models , author=. 2018 , publisher=

    work page 2018

  28. [28]

    , keywords =

    Quenched fractions in the IllustrisTNG simulations: comparison with observations and other theoretical models. , keywords =. doi:10.1093/mnras/stab1950 , archivePrefix =. 2008.00004 , primaryClass =

    work page doi:10.1093/mnras/stab1950 2008

  29. [29]

    , keywords =

    The Evolutionary Pathways of Disk-, Bulge-, and Halo-dominated Galaxies. , keywords =. doi:10.3847/1538-4357/ac0e98 , archivePrefix =. 2101.12373 , primaryClass =

    work page doi:10.3847/1538-4357/ac0e98

  30. [30]

    Cold dark matter haloes in the Planck era: evolution of structural parameters for Einasto and NFW profiles

    Cold dark matter haloes in the Planck era: evolution of structural parameters for Einasto and NFW profiles. , keywords =. doi:10.1093/mnras/stu742 , archivePrefix =. 1402.7073 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stu742

  31. [31]

    Gas Loss by Ram Pressure Stripping and Internal Feedback From Low Mass Milky Way Satellites

    Gas Loss by Ram Pressure Stripping and Internal Feedback from Low-mass Milky Way Satellites. , keywords =. doi:10.3847/0004-637X/826/2/148 , archivePrefix =. 1605.02746 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/826/2/148

  32. [32]

    , keywords =

    Satellites of Milky Way- and M31-like galaxies with TNG50: quenched fractions, gas content, and star formation histories. , keywords =. doi:10.1093/mnras/stad1357 , archivePrefix =. 2211.00010 , primaryClass =

    work page doi:10.1093/mnras/stad1357

  33. [33]

    , keywords =

    The abundance of satellites around Milky Way- and M31-like galaxies with the TNG50 simulation: a matter of diversity. , keywords =. doi:10.1093/mnras/stab2437 , archivePrefix =. 2101.12215 , primaryClass =

    work page doi:10.1093/mnras/stab2437

  34. [34]

    , keywords =

    Can cosmological simulations capture the diverse satellite populations of observed Milky Way analogues?. , keywords =. doi:10.1093/mnras/stab1332 , archivePrefix =. 2011.12974 , primaryClass =

    work page doi:10.1093/mnras/stab1332 2011

  35. [35]

    , keywords =

    Quenching of satellite galaxies of Milky Way analogues: reconciling theory and observations. , keywords =. doi:10.1093/mnras/stac183 , archivePrefix =. 2109.06215 , primaryClass =

    work page doi:10.1093/mnras/stac183

  36. [36]

    2016 , month =

    Daniel Foreman-Mackey , title =. 2016 , month =. doi:10.21105/joss.00024 , url =

    work page doi:10.21105/joss.00024 2016

  37. [37]

    , keywords =

    The subhalo populations of CDM dark haloes. , keywords =. doi:10.1111/j.1365-2966.2004.08360.x , archivePrefix =. astro-ph/0404589 , primaryClass =

    work page doi:10.1111/j.1365-2966.2004.08360.x 2004

  38. [38]

    Not so lumpy after all: modeling the depletion of dark matter subhalos by Milky Way-like galaxies

    Not so lumpy after all: modelling the depletion of dark matter subhaloes by Milky Way-like galaxies. , keywords =. doi:10.1093/mnras/stx1710 , archivePrefix =. 1701.03792 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1710

  39. [39]

    The SAGA Survey. IV. The Star Formation Properties of 101 Satellite Systems around Milky Way mass Galaxies. , keywords =. doi:10.3847/1538-4357/ad61e7 , archivePrefix =. 2404.14499 , primaryClass =

    work page doi:10.3847/1538-4357/ad61e7

  40. [40]

    The SAGA Survey. I. Satellite Galaxy Populations around Eight Milky Way Analogs. , keywords =. doi:10.3847/1538-4357/aa8626 , archivePrefix =. 1705.06743 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa8626

  41. [41]

    R.et al.Array programming with NumPy.Nature585, 357–362, 10.1038/s41586-020-2649-2 (2020)

    Charles R. Harris and K. Jarrod Millman and St. Array programming with. 2020 , month = sep, journal =. doi:10.1038/s41586-020-2649-2 , publisher =

    work page doi:10.1038/s41586-020-2649-2 2020

  42. [42]

    Universe , keywords =

    The Magellanic Clouds Are Very Rare in the IllustrisTNG Simulations. Universe , keywords =. doi:10.3390/universe10100385 , archivePrefix =. 2409.17259 , primaryClass =

    work page doi:10.3390/universe10100385

  43. [43]

    Hunter, J. D. , Title =. Computing in Science & Engineering , Volume =

    work page

  44. [44]

    Statistics of Dark Matter Substructure: III. Halo-to-Halo Variance

    Statistics of dark matter substructure - III. Halo-to-halo variance. , keywords =. doi:10.1093/mnras/stx1979 , archivePrefix =. 1610.02399 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx1979

  45. [45]

    The AGORA High-resolution Galaxy Simulations Comparison Project. V. Satellite Galaxy Populations in a Cosmological Zoom-in Simulation of a Milky Way Mass Halo. , keywords =. doi:10.3847/1538-4357/ad245b , archivePrefix =. 2402.05392 , primaryClass =

    work page doi:10.3847/1538-4357/ad245b

  46. [46]

    , keywords =

    The quenched satellite population around Milky Way analogues. , keywords =. doi:10.1093/mnras/stad2208 , archivePrefix =. 2210.03748 , primaryClass =

    work page doi:10.1093/mnras/stad2208

  47. [47]

    Edge-on disk galaxies in the SDSS DR6: Fractions of bulgeless and other disk galaxies. Astron. Nachr. , keywords =. doi:10.1002/asna.200811132 , archivePrefix =. 0901.1894 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1002/asna.200811132

  48. [48]

    Where are the missing galactic satellites?

    Where Are the Missing Galactic Satellites?. , keywords =. doi:10.1086/307643 , archivePrefix =. astro-ph/9901240 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/307643

  49. [49]

    Halos and galaxies in the standard cosmological model: results from the Bolshoi simulation

    Dark Matter Halos in the Standard Cosmological Model: Results from the Bolshoi Simulation. , keywords =. doi:10.1088/0004-637X/740/2/102 , archivePrefix =. 1002.3660 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/740/2/102

  50. [50]

    Bulgeless Giant Galaxies Challenge our Picture of Galaxy Formation by Hierarchical Clustering

    Bulgeless Giant Galaxies Challenge Our Picture of Galaxy Formation by Hierarchical Clustering. , keywords =. doi:10.1088/0004-637X/723/1/54 , archivePrefix =. 1009.3015 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/723/1/54

  51. [51]

    The formation and assembly history of the Milky Way revealed by its globular cluster population

    The formation and assembly history of the Milky Way revealed by its globular cluster population. , keywords =. doi:10.1093/mnras/sty1609 , archivePrefix =. 1806.05680 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty1609

  52. [52]

    2019 , publisher =

    Ravin Kumar and Colin Carroll and Ari Hartikainen and Osvaldo Martin , title =. 2019 , publisher =. doi:10.21105/joss.01143 , url =

    work page doi:10.21105/joss.01143 2019

  53. [53]

    Proceedings of the Second Workshop on the LLVM Compiler Infrastructure in HPC , articleno =

    Lam, Siu Kwan and Pitrou, Antoine and Seibert, Stanley , title =. Proceedings of the Second Workshop on the LLVM Compiler Infrastructure in HPC , articleno =. 2015 , isbn =. doi:10.1145/2833157.2833162 , abstract =

    work page doi:10.1145/2833157.2833162 2015

  54. [54]

    Improved Estimates of the Milky Way's Stellar Mass and Star Formation Rate from Hierarchical Bayesian Meta-Analysis

    Improved Estimates of the Milky Way's Stellar Mass and Star Formation Rate from Hierarchical Bayesian Meta-Analysis. , keywords =. doi:10.1088/0004-637X/806/1/96 , archivePrefix =. 1407.1078 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/806/1/96

  55. [55]

    The SAGA Survey. III. A Census of 101 Satellite Systems around Milky Way mass Galaxies. , keywords =. doi:10.3847/1538-4357/ad64c4 , archivePrefix =. 2404.14498 , primaryClass =

    work page doi:10.3847/1538-4357/ad64c4

  56. [56]

    The SAGA Survey. II. Building a Statistical Sample of Satellite Systems around Milky Way-like Galaxies. , keywords =. doi:10.3847/1538-4357/abce58 , archivePrefix =. 2008.12783 , primaryClass =

    work page doi:10.3847/1538-4357/abce58 2008

  57. [57]

    First results from the IllustrisTNG simulations: radio haloes and magnetic fields

    First results from the IllustrisTNG simulations: radio haloes and magnetic fields. , keywords =. doi:10.1093/mnras/sty2206 , archivePrefix =. 1707.03396 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2206

  58. [58]

    Physical drivers of the mass-size relation for Milky Way-like galaxies

    Bulgeless Evolution And the Rise of Discs (BEARD): I. Physical drivers of the mass-size relation for Milky Way-like galaxies. , keywords =. doi:10.1051/0004-6361/202557193 , adsurl =

    work page doi:10.1051/0004-6361/202557193

  59. [59]

    , keywords =

    Simultaneous ram pressure and tidal stripping; how dwarf spheroidals lost their gas. , keywords =. doi:10.1111/j.1365-2966.2006.10403.x , archivePrefix =. astro-ph/0504277 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.10403.x 2006

  60. [60]

    The observed properties of dwarf galaxies in and around the Local Group

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/144/1/4

  61. [61]

    , title =

    McCullagh, Peter and Nelder, John A. , title =. 1989 , edition =. doi:10.1007/978-1-4899-3242-6 , isbn =

    work page doi:10.1007/978-1-4899-3242-6 1989

  62. [62]

    , keywords =

    The Distribution of Satellite Galaxies in the IllustrisTNG100 Simulation. , keywords =. doi:10.3847/1538-4357/ac752d , archivePrefix =. 2206.00045 , primaryClass =

    work page doi:10.3847/1538-4357/ac752d

  63. [63]

    Morphological evolution

    The origin of bulges and discs in the CALIFA survey - I. Morphological evolution. , keywords =. doi:10.1093/mnras/stab1064 , archivePrefix =. 2104.07743 , primaryClass =

    work page doi:10.1093/mnras/stab1064

  64. [64]

    Dark Matter Substructure in Galactic Halos

    Dark Matter Substructure within Galactic Halos. , keywords =. doi:10.1086/312287 , archivePrefix =. astro-ph/9907411 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/312287

  65. [65]

    , keywords =

    Examining the relationship between the bulge-to-total stellar mass ratio and dwarf galaxy count in the context of CDM. , keywords =. doi:10.1051/0004-6361/202346827 , archivePrefix =. 2307.09015 , primaryClass =

    work page doi:10.1051/0004-6361/202346827

  66. [66]

    Modeling the Connection Between Subhalos and Satellites in Milky Way-like Systems

    Modeling the Connection between Subhalos and Satellites in Milky Way-like Systems. , keywords =. doi:10.3847/1538-4357/ab040e , archivePrefix =. 1809.05542 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ab040e

  67. [67]

    First results from the IllustrisTNG simulations: A tale of two elements -- chemical evolution of magnesium and europium

    First results from the IllustrisTNG simulations: a tale of two elements - chemical evolution of magnesium and europium. , keywords =. doi:10.1093/mnras/sty618 , archivePrefix =. 1707.03401 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty618

  68. [68]

    The Inner Structure of LambdaCDM Halos III: Universality and Asymptotic Slopes

    , year =. arXiv , doi =:astro-ph/0311231 , keywords =

    work page internal anchor Pith review Pith/arXiv arXiv

  69. [69]

    , keywords =

    The luminosity of cluster galaxies in the Cluster-EAGLE simulations. , keywords =. doi:10.1093/mnras/stac1481 , archivePrefix =. 2205.13553 , primaryClass =

    work page doi:10.1093/mnras/stac1481

  70. [70]

    Computational Astrophysics and Cosmology , keywords =

    The IllustrisTNG simulations: public data release. Computational Astrophysics and Cosmology , keywords =. doi:10.1186/s40668-019-0028-x , archivePrefix =. 1812.05609 , primaryClass =

    work page doi:10.1186/s40668-019-0028-x

  71. [71]

    First results from the IllustrisTNG simulations: the galaxy color bimodality

    First results from the IllustrisTNG simulations: the galaxy colour bimodality. , keywords =. doi:10.1093/mnras/stx3040 , archivePrefix =. 1707.03395 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx3040

  72. [72]

    First Results from the TNG50 Simulation: Galactic outflows driven by supernovae and black hole feedback

    First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback. , keywords =. doi:10.1093/mnras/stz2306 , archivePrefix =. 1902.05554 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz2306 1902

  73. [73]

    V., & Aharonian, F

    Mass loss of galaxies due to an ultraviolet background. , keywords =. doi:10.1111/j.1365-2966.2008.13830.x , archivePrefix =. 0806.0378 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.13830.x 2008

  74. [74]

    The Open Journal of Astrophysics , keywords =

    The Local Volume Database: a library of the observed properties of nearby dwarf galaxies and star clusters. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.144859 , archivePrefix =. 2411.07424 , primaryClass =

    work page doi:10.33232/001c.144859

  75. [75]

    , volume=

    Temporal Evolution of the Radial Distribution of Milky Way Satellite Galaxies , author=. , volume=. 2024 , publisher=

    work page 2024

  76. [76]

    Simulating Galaxy Formation with the IllustrisTNG Model

    Simulating galaxy formation with the IllustrisTNG model. , keywords =. doi:10.1093/mnras/stx2656 , archivePrefix =. 1703.02970 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx2656

  77. [77]

    First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies

    First results from the IllustrisTNG simulations: the stellar mass content of groups and clusters of galaxies. , keywords =. doi:10.1093/mnras/stx3112 , archivePrefix =. 1707.03406 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stx3112

  78. [78]

    Monthly Notices of the Royal Astronomical Society , volume =

    First results from the TNG50 simulation: the evolution of stellar and gaseous discs across cosmic time. , keywords =. doi:10.1093/mnras/stz2338 , archivePrefix =. 1902.05553 , primaryClass =

    work page doi:10.1093/mnras/stz2338 1902

  79. [79]

    Planck 2015 results. XXVII. The Second Planck Catalogue of Sunyaev-Zeldovich Sources

    , year =. arXiv , doi =:1502.01598 , keywords =

    work page internal anchor Pith review Pith/arXiv arXiv

  80. [80]

    pynbody: Astrophysics Simulation Analysis for Python

    work page

Showing first 80 references.