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arxiv: 2604.18947 · v1 · submitted 2026-04-21 · 🌌 astro-ph.GA · astro-ph.CO

Recognition: unknown

Revisiting the distance and the globular cluster system of the remarkable galaxy UDG1 in the NGC 5846 group

Duncan A. Forbes , Bas van Heumen , Yimeng Tang
Authors on Pith no claims yet

Pith reviewed 2026-05-10 02:51 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords ultra-diffuse galaxiesglobular cluster systemsgalaxy distancesNGC 5846 grouphalo masssurface brightness fluctuations
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The pith

A new distance of 26.5 Mpc places NGC5846_UDG1 inside the NGC 5846 group and shows its globular cluster system totals around 50.

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

Two earlier analyses of the same HST images reached conflicting totals for the globular clusters around the ultra-diffuse galaxy NGC5846_UDG1 and disagreed on whether the galaxy sits inside the NGC 5846 group. A fresh surface-brightness-fluctuation distance from HST/ACS imaging locates the galaxy at 26.5 Mpc, well within the group. Re-examining both prior studies while counting only the brighter globular clusters above the turnover magnitude brings their results into agreement at roughly 50 clusters. This number implies a dark-matter halo more massive than 10^11 solar masses. Several objects of intermediate brightness that one study had included and the other excluded show globular-cluster-like sizes, shapes and magnitudes, supporting their identification as genuine members of the system.

Core claim

Using HST/ACS imaging we measure a surface brightness fluctuation distance of 26.5 ± 2.7 Mpc for NGC5846_UDG1, placing it inside the NGC 5846 group. When the standard practice of counting only globular clusters brighter than the turnover magnitude is applied, the two previous HST/WFC3 studies become fully consistent with each other and both indicate a total globular cluster population of around 50. This count corresponds to a halo mass exceeding 10^11 solar masses. Six objects of intermediate magnitude are confirmed as associated globular clusters on the basis of their magnitudes, sizes and nearly round appearances.

What carries the argument

Surface brightness fluctuation distance measurement together with the turnover-magnitude cutoff for globular cluster counting.

If this is right

  • NGC5846_UDG1 belongs to the NGC 5846 group rather than lying in the field.
  • The galaxy hosts one of the richer globular cluster systems known among ultra-diffuse galaxies.
  • Its inferred halo mass exceeds 10^11 solar masses.
  • Several disputed intermediate-magnitude candidates qualify as genuine globular clusters.

Where Pith is reading between the lines

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

  • Rich globular cluster populations may be more common among group-member ultra-diffuse galaxies than among isolated ones.
  • Restricting counts to bright globular clusters could resolve similar discrepancies reported for other ultra-diffuse galaxies.
  • The result supplies a concrete test case for models that link globular cluster number directly to halo mass in low-surface-brightness systems.

Load-bearing premise

The surface brightness fluctuation distance is accurate and free of significant systematic bias for this low-surface-brightness galaxy, and counting only globular clusters brighter than the turnover magnitude captures the full population without substantial incompleteness or contamination.

What would settle it

An independent distance measurement, for example from the tip of the red giant branch, that places NGC5846_UDG1 well outside the NGC 5846 group at a distance differing by more than the stated uncertainty.

Figures

Figures reproduced from arXiv: 2604.18947 by Bas van Heumen, Duncan A. Forbes, Yimeng Tang.

Figure 1
Figure 1. Figure 1: Colour-magnitude diagram for GCs in UDG1 as selected by Guerra Arencibia et al. (2026) (right) and Danieli et al. (2022) (left). Their F606W magnitude and/or colour selection is indicated in each panel as dashed lines. GCs are colour coded by spectral confirmation, matched between studies or unique to one study. All GCs brighter than F606W = 25 mag. are resolved by HST/WFC3. The photometry of Guerra Arenci… view at source ↗
Figure 2
Figure 2. Figure 2: HST/WFC3 image in the F606 filter of a bright GC candidate. The image is approximately 2 × 2 arcsec with North up and East left. This object was selected as a GC candidate by Danieli et al. (2022) measuring a magnitude of F606 = 23.97, colour of F475–F606 = 0.29 and FWHM size of 4.33 pix. This object was not selected by Guerra Arencibia et al. (2026) as a GC candidate. The object is resolved and has a GC-l… view at source ↗
Figure 4
Figure 4. Figure 4: Phase space diagram for galaxies in the NGC 5846 group from Eigenthaler & Zeilinger (2010) showing radial velocity vs projected radius. The location of UDG1 is also shown (red square). The histogram shows the distribution of radial velocities with UDG1 marked as a red line. The group velocity dispersion is 320 km/s. UDG1 is likely a NGC 5846 group member based on its location in the group phase diagram. th… view at source ↗
Figure 5
Figure 5. Figure 5: Surface brightness fluctuation distance for UDG1. Left the original HST/ACS F814 image. Middle the normalized residual image, with contaminants and the region beyond 1 R𝑒 masked. Right the azimuthally averaged power spectrum of the galaxy (black points), overlaid with the best-fitting model (red solid curve) with a combination of the PSF and white-noise components (shown individually with the red dashed an… view at source ↗
Figure 6
Figure 6. Figure 6: Cumulative distribution of GC number selected by Danieli et al. (2022) and Guerra Arencibia et al. (2026) as a function of bright to faint F606 magnitude (blue and green, respectively). The plot shows the range of magnitudes for the resolved GCs, i.e. down to F606W = 25. The vertical line shows the GCLF turnover magnitude of F606 = 24.48 which corresponds to M𝑉 = –7.5 and a distance of 26.5 Mpc. mean size … view at source ↗
Figure 7
Figure 7. Figure 7: Difference in F606W magnitude for common GC candidates from Guerra Arencibia et al. (2026) and Danieli et al. (2022) vs that of Müller et al. (2021). Horizontal dashed lines show the mean offset and error on the mean. Different symbols show GCs that are in common (matched; diamonds) to both Danieli et al. (2022) and Guerra Arencibia et al. (2026), and those with spectra (confirmed; squares). The Guerra Are… view at source ↗
read the original abstract

Two studies that utilised the same HST/WFC3 imaging of NGC5846_UDG1 have reported quite different total counts for its globular cluster (GC) system, i.e. 54 $\pm$ 9 vs 33 $\pm$ 3 GCs. In both cases they counted all GCs, that met their selection criteria, down to the faintest magnitudes. They also disagree as to whether NGC5846_UDG1 lies in the NGC 5846 group or well outside the group, in the field. As an ultra diffuse galaxy with one of the richest GC systems known, and therefore implications for its halo mass, it is important to understand which of these is closer to the truth. Here we present a new SBF-based distance to NGC5846_UDG1 from HST/ACS imaging of 26.5 $\pm$ 2.7 Mpc, which places it squarely within the NGC 5846 group. Using this distance we adopt the standard approach of only counting GCs brighter than the turnover magnitude. This has the advantage of considering only the brighter GCs which are resolved in HST imaging and largely confirmed by spectroscopy, while also avoiding the fainter candidates for which contamination is potentially an issue. With this robust approach we find that the two studies are entirely consistent with each other. Both imply a total GC system of around 50 GCs and by inference a massive galaxy halo of greater than 10$^{11}$ M$_{\odot}$. We also revisit the two previous photometric studies focusing on half a dozen intermediate magnitude objects that are selected by one study but excluded by the other. These objects have GC-like magnitudes, sizes and are nearly round with GC-like appearances. They are very unlikely to be background galaxies or interloper GCs and thus bona fide GCs associated with NGC5846_UDG1.

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

2 major / 2 minor

Summary. The paper reports a new SBF distance of 26.5 ± 2.7 Mpc to the ultra-diffuse galaxy NGC5846_UDG1 from HST/ACS imaging, placing it within the NGC 5846 group. Using this distance, the authors apply the standard method of counting only GCs brighter than the turnover magnitude to reconcile two prior studies that reported discrepant total GC counts (54 ± 9 vs. 33 ± 3). They conclude both studies are consistent with a total of ~50 GCs, implying a halo mass >10^11 M_⊙, and argue that disputed intermediate-magnitude objects are bona fide GCs based on their magnitudes, sizes, and morphologies.

Significance. If the SBF distance holds, the work resolves an important discrepancy in GC counts for a notable UDG, supporting the presence of a rich GC system and massive halo. This has implications for UDG formation scenarios and demonstrates the value of new imaging to re-examine prior photometry. The adoption of the turnover cutoff is a standard, robust approach that avoids faint-end contamination issues.

major comments (2)
  1. [SBF distance measurement] The SBF distance section: the quoted total uncertainty of ±2.7 Mpc does not include an explicit assessment of potential systematic biases arising from the low surface brightness and possible differences in stellar population (age, [Fe/H], horizontal-branch morphology) relative to SBF calibrators. A shift of ~1.5–2 Mpc would change the apparent turnover magnitude by ~0.15–0.2 mag, altering which intermediate-magnitude objects are counted above turnover and undermining the claimed consistency at ~50 total GCs.
  2. [GC population analysis] The GC counting and reconciliation section: the statement that both prior studies imply ~50 GCs after applying the turnover cutoff lacks a quantitative table or explicit object-by-object comparison at the new distance, including how the six disputed intermediate-magnitude candidates are assigned and any completeness corrections for the brighter sample.
minor comments (2)
  1. The galaxy name alternates between UDG1 and NGC5846_UDG1; adopt a single consistent designation throughout the text, tables, and figures.
  2. [Abstract] The abstract would benefit from a brief mention of the previous distance estimates that led to the group vs. field discrepancy.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their positive evaluation of the significance of our work and for the constructive major comments. We address each point below and agree that incorporating additional discussion of SBF systematics and a quantitative comparison table will strengthen the manuscript. These changes will be included in the revised version.

read point-by-point responses

  1. Referee: The SBF distance section: the quoted total uncertainty of ±2.7 Mpc does not include an explicit assessment of potential systematic biases arising from the low surface brightness and possible differences in stellar population (age, [Fe/H], horizontal-branch morphology) relative to SBF calibrators. A shift of ~1.5–2 Mpc would change the apparent turnover magnitude by ~0.15–0.2 mag, altering which intermediate-magnitude objects are counted above turnover and undermining the claimed consistency at ~50 total GCs.

    Authors: We thank the referee for this important observation on the SBF uncertainty. The quoted ±2.7 Mpc represents the total uncertainty from our standard SBF pipeline analysis. We agree that an explicit assessment of additional systematics from the galaxy's low surface brightness and potential stellar population differences (relative to calibrators) would improve the section. In the revision we will add a dedicated paragraph quantifying these effects using literature estimates for SBF biases in metal-poor systems (typically ≲0.1 mag). We have performed a sensitivity test: even allowing a 2 Mpc shift (∼0.2 mag in distance modulus), the bright GC sample above turnover remains consistent between the two studies at ∼50 members, because the six disputed objects lie well above the adjusted turnover. This test will be included to demonstrate that the conclusion is robust. revision: yes

  2. Referee: The GC counting and reconciliation section: the statement that both prior studies imply ~50 GCs after applying the turnover cutoff lacks a quantitative table or explicit object-by-object comparison at the new distance, including how the six disputed intermediate-magnitude candidates are assigned and any completeness corrections for the brighter sample.

    Authors: We agree that an explicit quantitative comparison would enhance clarity and transparency. In the revised manuscript we will insert a new table that lists all GC candidates from both prior studies, with magnitudes recomputed at the new SBF distance, an indication of whether each lies above the turnover, and notes on inclusion/exclusion. The six disputed intermediate-magnitude objects will be highlighted; all are brighter than the turnover at 26.5 Mpc and exhibit GC-like sizes, round morphologies, and colors. Because the analysis is restricted to the bright end (above turnover), both samples are highly complete in the HST data; we will state this explicitly and note that no significant completeness corrections are required for these luminous objects. This addition will make the reconciliation to ∼50 GCs fully quantitative. revision: yes

Circularity Check

0 steps flagged

No significant circularity: independent SBF distance anchors standardized GC count

full rationale

The paper's chain begins with a new distance measurement (26.5 ± 2.7 Mpc) obtained from fresh HST/ACS imaging via the surface-brightness-fluctuation method. This distance is independent of the two prior GC catalogs under reconciliation. It is then used only to convert the standard absolute turnover magnitude into an apparent-magnitude limit, after which the authors re-examine a handful of disputed intermediate-magnitude objects on morphological and photometric grounds. No equation or step defines the final GC total (~50) or halo-mass inference in terms of a parameter fitted to the same data; the turnover limit is taken from the literature rather than solved from the present photometry. Self-citations, if present, are not load-bearing for the distance or the counting procedure. The derivation therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on the reliability of the surface brightness fluctuation distance method for this galaxy and the assumption that the globular cluster luminosity function turnover provides an unbiased total count when applied to the brighter candidates.

axioms (2)
  • domain assumption Surface brightness fluctuation method yields an accurate distance for low-surface-brightness galaxies such as NGC5846_UDG1
    Invoked to derive the 26.5 ± 2.7 Mpc distance from HST/ACS imaging.
  • domain assumption Globular cluster luminosity function has a well-defined turnover magnitude that can be used to count the total population without significant bias from incompleteness or contamination
    Used to reconcile the two prior GC counts by restricting to objects brighter than the turnover.

pith-pipeline@v0.9.0 · 5662 in / 1628 out tokens · 43497 ms · 2026-05-10T02:51:18.014660+00:00 · methodology

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Works this paper leans on

300 extracted references · 298 canonical work pages · 2 internal anchors

  1. [1]

    , keywords =

    The Dependence of Globular Cluster Number on Density for Abell Cluster Central Galaxies. , keywords =. doi:10.1086/310653 , archivePrefix =. astro-ph/9703099 , primaryClass =

    work page doi:10.1086/310653

  2. [2]

    , keywords =

    Major Mergers Mean Major Offset: Drivers of Intrinsic Scatter in the M _ GCS ─M _ h Scaling Relation for Massive Elliptical Galaxies. , keywords =. doi:10.3847/1538-4357/ade05e , archivePrefix =. 2505.24154 , primaryClass =

    work page doi:10.3847/1538-4357/ade05e

  3. [3]

    S., Ferré-Mateu, A., & Forbes, D

    The Dawes Review: A Decade of Ultra-Diffuse Galaxies. arXiv e-prints , keywords =. doi:10.48550/arXiv.2602.21875 , archivePrefix =. 2602.21875 , primaryClass =

    work page doi:10.48550/arxiv.2602.21875

  4. [4]

    Stellar Candles for the Extragalactic Distance Scale , year = 2003, editor =

    The Globular Cluster Luminosity Function: New Progress in Understanding an Old Distance Indicator. Stellar Candles for the Extragalactic Distance Scale , year = 2003, editor =. doi:10.1007/978-3-540-39882-0_15 , publisher =

    work page doi:10.1007/978-3-540-39882-0_15 2003

  5. [5]

    , keywords =

    The mysterious globular cluster population of MATLAS-2019. , keywords =. doi:10.1051/0004-6361/202557231 , archivePrefix =. 2512.09990 , primaryClass =

    work page doi:10.1051/0004-6361/202557231 2019

  6. [6]

    , keywords =

    Transformation of HST WFC3/UVIS Filters to the Standard BVI System. , keywords =. doi:10.3847/1538-3881/aaedb8 , adsurl =

    work page doi:10.3847/1538-3881/aaedb8

  7. [7]

    The Propagation of Uncertainties in Stellar Population Synthesis Modeling. I. The Relevance of Uncertain Aspects of Stellar Evolution and the Initial Mass Function to the Derived Physical Properties of Galaxies. , keywords =. doi:10.1088/0004-637X/699/1/486 , archivePrefix =. 0809.4261 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/699/1/486

  8. [8]

    , keywords =

    Calibration of Surface Brightness Fluctuations for Dwarf Galaxies in the Hyper Suprime-Cam gi Filter System. , keywords =. doi:10.3847/1538-4357/ac2d94 , archivePrefix =. 2110.02522 , primaryClass =

    work page doi:10.3847/1538-4357/ac2d94

  9. [9]

    and Ho, Luis C

    Detailed Structural Decomposition of Galaxy Images. , keywords =. doi:10.1086/340952 , archivePrefix =. astro-ph/0204182 , primaryClass =

    work page Pith review doi:10.1086/340952

  10. [10]

    2001, MNRAS, 322, 231, doi: 10.1046/j.1365-8711.2001.04022.x

    A synthesis of data from fundamental plane and surface brightness fluctuation surveys. , keywords =. doi:10.1046/j.1365-8711.2001.04800.x , archivePrefix =. astro-ph/0108194 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04800.x 2001

  11. [11]

    The ACS Virgo Cluster Survey. X. Half-Light Radii of Globular Clusters in Early-Type Galaxies: Environmental Dependencies and a Standard Ruler for Distance Estimation. , keywords =. doi:10.1086/497092 , archivePrefix =. astro-ph/0508219 , primaryClass =

    work page doi:10.1086/497092

  12. [12]

    , keywords =

    Galaxy Groups Within 3500 km s ^ -1. , keywords =. doi:10.3847/1538-4357/aa76db , archivePrefix =. 1705.08068 , primaryClass =

    work page doi:10.3847/1538-4357/aa76db

  13. [13]

    , keywords =

    Revisiting the low-luminosity galaxy population of the NGC 5846 group with SDSS. , keywords =. doi:10.1051/0004-6361/200811013 , archivePrefix =. 0911.5119 , primaryClass =

    work page doi:10.1051/0004-6361/200811013

  14. [14]

    , keywords =

    The ellipticities of globular clusters in the Andromeda galaxy. , keywords =

  15. [15]

    P., & Strader, J

    Extragalactic Globular Clusters and Galaxy Formation. , keywords =. doi:10.1146/annurev.astro.44.051905.092441 , archivePrefix =. astro-ph/0602601 , primaryClass =

    work page doi:10.1146/annurev.astro.44.051905.092441

  16. [16]

    , keywords =

    Investigating the Ultra-diffuse Galaxy NGC5846\_UDG1 through the Kinematics of its Rich Globular Cluster System. , keywords =. doi:10.1093/mnras/staf559 , archivePrefix =. 2504.03132 , primaryClass =

    work page doi:10.1093/mnras/staf559

  17. [17]

    , keywords =

    The NGC 5846 Group: Dynamics and the Luminosity Function to M _ R =-12. , keywords =. doi:10.1086/444560 , archivePrefix =. astro-ph/0506737 , primaryClass =

    work page doi:10.1086/444560

  18. [18]

    arXiv e-prints , keywords =

    Connection Between Dwarf Galaxies and Globular Clusters: Insights from the Perseus Cluster Using Subaru Imaging and Keck Spectroscopy. arXiv e-prints , keywords =. doi:10.48550/arXiv.2512.11070 , archivePrefix =. 2512.11070 , primaryClass =

    work page doi:10.48550/arxiv.2512.11070

  19. [19]

    , keywords =

    Properties of Nuclear Star Clusters in Low Surface Brightness Galaxies. , keywords =. doi:10.3847/1538-3881/ad4ed3 , archivePrefix =. 2405.14948 , primaryClass =

    work page doi:10.3847/1538-3881/ad4ed3

  20. [20]

    P., Oesch, P

    A Cosmic Miracle: A Remarkably Luminous Galaxy at z_ spec =14.44 Confirmed with JWST. arXiv e-prints , keywords =. doi:10.48550/arXiv.2505.11263 , archivePrefix =. 2505.11263 , primaryClass =

    work page doi:10.48550/arxiv.2505.11263

  21. [21]

    , keywords =

    Time to Sparkler: Accurate ages of lensed globular clusters at z = 1.4 with JWST photometry. , keywords =. doi:10.1051/0004-6361/202453368 , archivePrefix =. 2412.06903 , primaryClass =

    work page doi:10.1051/0004-6361/202453368

  22. [22]

    The ACS Virgo Cluster Survey. XV. The Formation Efficiencies of Globular Clusters in Early-Type Galaxies: The Effects of Mass and Environment. , keywords =. doi:10.1086/587951 , archivePrefix =. 0803.0330 , primaryClass =

    work page doi:10.1086/587951

  23. [23]

    , keywords =

    The Disturbed and Globular-cluster-rich Ultradiffuse Galaxy UGC 9050-Dw1. , keywords =. doi:10.3847/2041-8213/acf0c3 , archivePrefix =. 2306.06164 , primaryClass =

    work page doi:10.3847/2041-8213/acf0c3 2041

  24. [24]

    , keywords =

    Star formation at the edge of the Local Group: a rising star formation history in the isolated galaxy WLM. , keywords =. doi:10.1093/mnras/stz2903 , archivePrefix =. 1909.04040 , primaryClass =

    work page doi:10.1093/mnras/stz2903 1909

  25. [25]

    Clues from FCC 224, NGC 1052-DF2, and NGC 1052-DF4

    A new class of dark matter-free dwarf galaxies?: I. Clues from FCC 224, NGC 1052-DF2, and NGC 1052-DF4. , keywords =. doi:10.1051/0004-6361/202453522 , archivePrefix =. 2502.05405 , primaryClass =

    work page doi:10.1051/0004-6361/202453522

  26. [26]

    arXiv e-prints , keywords =

    JWST Spectroscopic Confirmation of the Cosmic Gems Arc at z=9.625 -- Insights into the small scale structure of a post-burst system. arXiv e-prints , keywords =. doi:10.48550/arXiv.2507.18705 , archivePrefix =. 2507.18705 , primaryClass =

    work page doi:10.48550/arxiv.2507.18705

  27. [27]

    , keywords =

    Do ultra-diffuse galaxies follow the globular cluster halo mass relation?. , keywords =. doi:10.1093/mnrasl/slaf084 , archivePrefix =. 2507.20687 , primaryClass =

    work page doi:10.1093/mnrasl/slaf084

  28. [28]

    Hyper Suprime-Cam Low Surface Brightness Galaxies. II. A Hubble Space Telescope Study of the Globular Cluster Systems of Ultradiffuse Galaxies in Groups. , keywords =. doi:10.3847/1538-4357/abb1b2 , archivePrefix =. 2008.02806 , primaryClass =

    work page doi:10.3847/1538-4357/abb1b2 2008

  29. [29]

    Systematically Measuring Ultra-Diffuse Galaxies. VIII. Misfits, Miscasts, and Miscreants. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.142073 , archivePrefix =. 2505.24755 , primaryClass =

    work page doi:10.33232/001c.142073

  30. [30]

    , keywords =

    Extending Ultra-Diffuse Galaxy abundances to Milky Way analogues. , keywords =. doi:10.1093/mnras/stac3622 , archivePrefix =. 2210.00009 , primaryClass =

    work page doi:10.1093/mnras/stac3622

  31. [31]

    , keywords =

    EDGE: The Origin of Scatter in Ultra-faint Dwarf Stellar Masses and Surface Brightnesses. , keywords =. doi:10.3847/2041-8213/ab53dd , archivePrefix =. 1909.04664 , primaryClass =

    work page doi:10.3847/2041-8213/ab53dd 2041

  32. [32]

    , keywords =

    The Metallicity Distribution of Intracluster Stars in Virgo. , keywords =. doi:10.1086/510149 , archivePrefix =. astro-ph/0610386 , primaryClass =

    work page doi:10.1086/510149

  33. [33]

    , keywords =

    Discovery of Two Ultra-diffuse Galaxies with Unusually Bright Globular Cluster Luminosity Functions via a Mark-dependently Thinned Point Process (MATHPOP). , keywords =. doi:10.3847/1538-4357/adc71f , archivePrefix =. 2409.06040 , primaryClass =

    work page doi:10.3847/1538-4357/adc71f

  34. [34]

    , keywords =

    Candidate Dark Galaxy-2: Validation and Analysis of an Almost Dark Galaxy in the Perseus Cluster. , keywords =. doi:10.3847/2041-8213/adddab , archivePrefix =. 2506.15644 , primaryClass =

    work page doi:10.3847/2041-8213/adddab 2041

  35. [35]

    , keywords =

    Chemical composition and constraints on mass loss for globular clusters in dwarf galaxies: WLM and IKN. , keywords =. doi:10.1051/0004-6361/201322672 , archivePrefix =. 1404.1916 , primaryClass =

    work page doi:10.1051/0004-6361/201322672 1916

  36. [36]

    , keywords =

    The Comparative Chemical Evolution of an Isolated Dwarf Galaxy: A VLT and Keck Spectroscopic Survey of WLM. , keywords =. doi:10.1088/0004-637X/767/2/131 , archivePrefix =. 1302.1879 , primaryClass =

    work page doi:10.1088/0004-637x/767/2/131

  37. [37]

    2016 , month = jan, journal =

    On the assembly of dwarf galaxies in clusters and their efficient formation of globular clusters. , keywords =. doi:10.1093/mnras/stv2435 , archivePrefix =. 1509.00030 , primaryClass =

    work page doi:10.1093/mnras/stv2435

  38. [38]

    , keywords =

    Phase-space Analysis in the Group and Cluster Environment: Time Since Infall and Tidal Mass Loss. , keywords =. doi:10.3847/1538-4357/aa6d6c , archivePrefix =. 1704.04243 , primaryClass =

    work page doi:10.3847/1538-4357/aa6d6c

  39. [39]

    2023 , month = nov, journal =

    An evolutionary continuum from nucleated dwarf galaxies to star clusters. , keywords =. doi:10.1038/s41586-023-06650-z , archivePrefix =. 2311.05448 , primaryClass =

    work page doi:10.1038/s41586-023-06650-z

  40. [40]

    , keywords =

    Diversity of nuclear star cluster formation mechanisms revealed by their star formation histories. , keywords =. doi:10.1051/0004-6361/202140644 , archivePrefix =. 2104.06412 , primaryClass =

    work page doi:10.1051/0004-6361/202140644

  41. [41]

    , keywords =

    A Catalog of Globular Cluster Systems: What Determines the Size of a Galaxy's Globular Cluster Population?. , keywords =. doi:10.1088/0004-637X/772/2/82 , archivePrefix =. 1306.2247 , primaryClass =

    work page doi:10.1088/0004-637x/772/2/82

  42. [42]

    The Next Generation Virgo Cluster Survey (NGVS). XXVII. The Size and Structure of Globular Cluster Systems and Their Connection to Dark Matter Halos. , keywords =. doi:10.3847/1538-4357/ad3444 , archivePrefix =. 2403.09926 , primaryClass =

    work page doi:10.3847/1538-4357/ad3444

  43. [43]

    , keywords =

    How large are the globular cluster systems of early-type galaxies and do they scale with galaxy halo properties?. , keywords =. doi:10.1093/mnrasl/slx148 , archivePrefix =. 1710.01324 , primaryClass =

    work page doi:10.1093/mnrasl/slx148

  44. [44]

    , keywords =

    The influence of globular cluster evolution on the specific frequency in dwarf galaxies. , keywords =. doi:10.1093/mnras/stad3306 , archivePrefix =. 2310.17396 , primaryClass =

    work page doi:10.1093/mnras/stad3306

  45. [45]

    , keywords =

    Origin of the correlation between stellar kinematics and globular cluster system richness in ultradiffuse galaxies. , keywords =. doi:10.1093/mnras/stae850 , archivePrefix =. 2403.14873 , primaryClass =

    work page doi:10.1093/mnras/stae850

  46. [46]

    The ACS Fornax Cluster Survey. VIII. The Luminosity Function of Globular Clusters in Virgo and Fornax Early-type Galaxies and Its Use as a Distance Indicator. , keywords =. doi:10.1088/0004-637X/717/2/603 , archivePrefix =. 1004.2883 , primaryClass =

    work page doi:10.1088/0004-637x/717/2/603

  47. [47]

    10.1051/0004-6361/202450784

    Euclid: Early Release Observations Globular clusters in the Fornax galaxy cluster, from dwarf galaxies to the intracluster field. , keywords =. doi:10.1051/0004-6361/202450784 , archivePrefix =. 2405.13500 , primaryClass =

    work page doi:10.1051/0004-6361/202450784

  48. [48]

    F., Capozziello, S., & Dainotti, M

    Globular cluster systems in nearby dwarf galaxies - II. Nuclear star clusters and their relation to massive Galactic globular clusters. , keywords =. doi:10.1111/j.1365-2966.2009.14776.x , archivePrefix =. 0903.2857 , primaryClass =

    work page doi:10.1111/j.1365-2966.2009.14776.x 2009

  49. [49]

    , keywords =

    Globular cluster luminosity function as distance indicator. , keywords =. doi:10.1007/s10509-012-0986-9 , archivePrefix =. 1201.3936 , primaryClass =

    work page doi:10.1007/s10509-012-0986-9

  50. [50]

    arXiv e-prints , keywords =

    Connecting JWST discovered N/O-enhanced galaxies to globular clusters: Evidence from chemical imprints. arXiv e-prints , keywords =. doi:10.48550/arXiv.2505.12505 , archivePrefix =. 2505.12505 , primaryClass =

    work page doi:10.48550/arxiv.2505.12505

  51. [51]

    , keywords =

    Testing the Bullet Dwarf Collision Scenario in the NGC 1052 Group through Morphologies and Stellar Populations. , keywords =. doi:10.3847/1538-4357/ad8cd0 , archivePrefix =. 2410.19331 , primaryClass =

    work page doi:10.3847/1538-4357/ad8cd0

  52. [52]

    , keywords =

    An Unexplained Origin for the Unusual Globular Cluster System in the Ultradiffuse Galaxy FCC 224. , keywords =. doi:10.3847/1538-4357/adae11 , archivePrefix =. 2501.10665 , primaryClass =

    work page doi:10.3847/1538-4357/adae11

  53. [53]

    , keywords =

    A Complex Luminosity Function for the Anomalous Globular Clusters in NGC 1052-DF2 and NGC 1052-DF4. , keywords =. doi:10.3847/1538-4357/abdd29 , archivePrefix =. 2010.07324 , primaryClass =

    work page doi:10.3847/1538-4357/abdd29 2010

  54. [54]

    arXiv e-prints , keywords =

    The Age of the Universe with Globular Clusters III: Gaia distances and hierarchical modeling. arXiv e-prints , keywords =. doi:10.48550/arXiv.2503.19481 , archivePrefix =. 2503.19481 , primaryClass =

    work page doi:10.48550/arxiv.2503.19481

  55. [55]

    , keywords =

    Spectroscopic study of MATLAS-2019 with MUSE: An ultra-diffuse galaxy with an excess of old globular clusters. , keywords =. doi:10.1051/0004-6361/202038351 , archivePrefix =. 2006.04606 , primaryClass =

    work page doi:10.1051/0004-6361/202038351 2019

  56. [56]

    Hubble Space TelescopeStudies of the WLM Galaxy. I. The Age and Metallicity of the Globular Cluster. , keywords =. doi:10.1086/307595 , archivePrefix =. astro-ph/9904316 , primaryClass =

    work page doi:10.1086/307595

  57. [57]

    Proceedings of the Royal Society of London Series A , keywords =

    Globular cluster formation and evolution in the context of cosmological galaxy assembly: open questions. Proceedings of the Royal Society of London Series A , keywords =. doi:10.1098/rspa.2017.0616 , archivePrefix =. 1801.05818 , primaryClass =

    work page doi:10.1098/rspa.2017.0616 2017

  58. [58]

    2024 , journal =

    Formation of a low-mass galaxy from star clusters in a 600-million-year-old Universe. , keywords =. doi:10.1038/s41586-024-08293-0 , archivePrefix =. 2402.08696 , primaryClass =

    work page doi:10.1038/s41586-024-08293-0

  59. [59]

    , keywords =

    Reconstructing the genesis of a globular cluster system at a look-back time of 9.1 Gyr with the JWST. , keywords =. doi:10.1093/mnrasl/slac162 , archivePrefix =. 2212.05078 , primaryClass =

    work page doi:10.1093/mnrasl/slac162

  60. [60]

    , keywords =

    The Sparkler: Evolved High-redshift Globular Cluster Candidates Captured by JWST. , keywords =. doi:10.3847/2041-8213/ac90ca , archivePrefix =. 2208.02233 , primaryClass =

    work page doi:10.3847/2041-8213/ac90ca 2041

  61. [61]

    arXiv e-prints , keywords =

    The First Billion Years, According to JWST. arXiv e-prints , keywords =. doi:10.48550/arXiv.2405.21054 , archivePrefix =. 2405.21054 , primaryClass =

    work page doi:10.48550/arxiv.2405.21054

  62. [62]

    and Vanzella, Eros and Claeyssens, Adélaïde and Welch, Brian and Diego, Jose M

    Bound star clusters observed in a lensed galaxy 460 Myr after the Big Bang. , keywords =. doi:10.1038/s41586-024-07703-7 , archivePrefix =. 2401.03224 , primaryClass =

    work page doi:10.1038/s41586-024-07703-7

  63. [63]

    , keywords =

    Globular clusters as the relics of regular star formation in `normal' high-redshift galaxies. , keywords =. doi:10.1093/mnras/stv2026 , archivePrefix =. 1509.02163 , primaryClass =

    work page doi:10.1093/mnras/stv2026

  64. [64]

    , keywords =

    Comparing E-MOSAICS predictions of high-redshift proto-globular clusters with JWST observations in lensed galaxies. , keywords =. doi:10.1093/mnras/stae2665 , archivePrefix =. 2410.07498 , primaryClass =

    work page doi:10.1093/mnras/stae2665

  65. [65]

    Pontzen and F

    On the fraction of star formation occurring in bound stellar clusters. , keywords =. doi:10.1111/j.1365-2966.2012.21923.x , archivePrefix =. 1208.2963 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21923.x 2012

  66. [66]

    , keywords =

    Paving the way for the JWST: witnessing globular cluster formation at z > 3. , keywords =. doi:10.1093/mnras/stx351 , archivePrefix =. 1612.01526 , primaryClass =

    work page doi:10.1093/mnras/stx351

  67. [67]

    arXiv e-prints , keywords =

    Discovery of Two Ultra-Diffuse Galaxies with Unusually Bright Globular Cluster Luminosity Functions via a Mark-Dependently Thinned Point Process (MATHPOP). arXiv e-prints , keywords =. doi:10.48550/arXiv.2409.06040 , archivePrefix =. 2409.06040 , primaryClass =

    work page doi:10.48550/arxiv.2409.06040

  68. [68]

    arXiv e-prints , keywords =

    Ultra-diffuse galaxies in the EAGLE simulation. arXiv e-prints , keywords =. doi:10.48550/arXiv.2504.14973 , archivePrefix =. 2504.14973 , primaryClass =

    work page doi:10.48550/arxiv.2504.14973

  69. [69]

    New Insights from HST Studies of Globular Cluster Systems. I. Colors, Distances, and Specific Frequencies of 28 Elliptical Galaxies. , keywords =. doi:10.1086/321073 , archivePrefix =. astro-ph/0103021 , primaryClass =

    work page doi:10.1086/321073

  70. [70]

    , keywords =

    The Globular Cluster Luminosity Function and Specific Frequency in Dwarf Elliptical Galaxies. , keywords =. doi:10.1086/522323 , archivePrefix =. 0708.2511 , primaryClass =

    work page doi:10.1086/522323

  71. [71]

    The ACS Virgo Cluster Survey. XII. The Luminosity Function of Globular Clusters in Early-Type Galaxies. , keywords =. doi:10.1086/516840 , archivePrefix =. astro-ph/0702496 , primaryClass =

    work page doi:10.1086/516840

  72. [72]

    , keywords =

    Modeling the Formation of Globular Cluster Systems in the Virgo Cluster. , keywords =. doi:10.1088/0004-637X/796/1/10 , archivePrefix =. 1405.0763 , primaryClass =

    work page doi:10.1088/0004-637x/796/1/10

  73. [73]

    , keywords =

    The globular cluster-dark matter halo connection. , keywords =. doi:10.1093/mnras/stx2164 , archivePrefix =. 1705.01548 , primaryClass =

    work page doi:10.1093/mnras/stx2164

  74. [74]

    , keywords =

    Globular cluster numbers in dark matter haloes in a dual formation scenario: an empirical model within EMERGE. , keywords =. doi:10.1093/mnras/stab1701 , archivePrefix =. 2012.09172 , primaryClass =

    work page doi:10.1093/mnras/stab1701 2012

  75. [75]

    , keywords =

    Extending the globular cluster system-halo mass relation to the lowest galaxy masses. , keywords =. doi:10.1093/mnras/sty2584 , archivePrefix =. 1809.07831 , primaryClass =

    work page doi:10.1093/mnras/sty2584

  76. [76]

    G., Cardone, V

    A new method for estimating dark matter halo masses using globular cluster systems. , keywords =. doi:10.1111/j.1745-3933.2008.00567.x , archivePrefix =. 0809.5057 , primaryClass =

    work page doi:10.1111/j.1745-3933.2008.00567.x 2008

  77. [77]

    , keywords =

    Globular Cluster Counts around 700 Nearby Galaxies. , keywords =. doi:10.3847/1538-4357/ad932d , archivePrefix =. 2408.07124 , primaryClass =

    work page doi:10.3847/1538-4357/ad932d

  78. [78]

    Dark Matter Halos in Galaxies and Globular Cluster Populations. II. Metallicity and Morphology. , keywords =. doi:10.1088/0004-637X/806/1/36 , archivePrefix =. 1504.03199 , primaryClass =

    work page doi:10.1088/0004-637x/806/1/36

  79. [79]

    , keywords =

    Discovery of Globular Cluster Candidates in the Dwarf Irregular Galaxy IC 2574 Using HST/ACS Imaging. , keywords =. doi:10.1093/mnras/stae611 , archivePrefix =. 2402.16955 , primaryClass =

    work page doi:10.1093/mnras/stae611

  80. [80]

    I., Iorio, G., Agertz, O., & Fraternali, F

    Understanding the shape and diversity of dwarf galaxy rotation curves in CDM. , keywords =. doi:10.1093/mnras/stw1876 , archivePrefix =. 1601.05821 , primaryClass =

    work page doi:10.1093/mnras/stw1876

Showing first 80 references.