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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
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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

discussion (0)

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