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Constructing a Pristine View of Extended Globular Cluster Structure

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read Adding photometric metallicities from the Pristine-Gaia-Synthetic catalogue to Gaia astrometry reveals extended structure around 22 of 30 Milky Way globular clusters, six of them new tentative detections.

desk verdict A careful, honest extension of the KI25 method to 30 globular clusters, but the six new tentative detections rest on uncalibrated significance levels and need a null-field control before they can be fully trusted. read the letter →

arxiv 2507.05590 v1 pith:A23PCJEV submitted 2025-07-08 astro-ph.GA

Pete B. Kuzma , Miho N. Ishigaki , Takanobu Kirihara , Itsuki Ogami This is my paper · ORCID
classification astro-ph.GA
keywords globularclusterstidaltailsextra-tidalstarsphotometricmetallicitiesPristinesurveyGaiaastrometryunsupervisedmachinelearningMilkyWaystellarhalo
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper claims that adding a photometric-metallicity dimension to Gaia astrometry can expose stars tidally stripped from Milky Way globular clusters, even at large angular separations. Applying an unsupervised machine-learning membership classifier to the Pristine-Gaia-Synthetic catalogue around 30 clusters, the authors find 22 clusters with extended structure within five degrees of their centres, six of which are new tentative detections. The high-probability stars beyond the Jacobi radius carry photometric metallicities consistent with the cluster values, supporting the interpretation that they were stripped from the cluster. The result matters because it demonstrates a homogeneous, all-sky route to building candidate lists of extra-tidal stars that upcoming multi-object spectrographs can confirm.

What carries the argument

The load-bearing object is the Pristine-Gaia-Synthetic (PGS) catalogue, which supplies all-sky synthetic CaHK-band photometry and photometric $[\mathrm{Fe/H}]$ for Gaia sources, giving a metallicity-sensitive colour index $(\mathrm{CaHK}-G_0)-2.5(G_{\mathrm{BP}}-G_{\mathrm{RP}})_0$. The membership machinery is an unsupervised k-nearest-neighbour likelihood that combines three parameter spaces — Gaia proper motion, Gaia colour–magnitude, and PGS colour–colour — to assign each star a probability of belonging to the cluster rather than the Milky Way field. A conservative sample ($P_{\mathrm{mem}} > 0.99$) provides the cleanest extra-tidal candidates, and a variable smoothing radius plus first-order field subtraction turns those candidates into density maps whose position angles are then fit as a function of radius and compared with orbits and N-body models.

What would settle it

Obtain moderate-resolution spectra of the conservative-sample stars beyond the Jacobi radius for the six new tentative detections: if the measured line-of-sight velocities do not cluster around each cluster's systemic velocity, or the spectroscopic metallicities disagree with the photometric values, the claimed extra-tidal structure would be revealed as field contamination rather than stripped cluster stars.

Watch

Extended reading notes

Core claim

Within five degrees of each of 30 Milky Way globular clusters, the authors combine Gaia proper motions and photometry with synthetic CaHK-band photometric metallicities ($[\mathrm{Fe/H}]$) from the Pristine-Gaia-Synthetic catalogue. A k-nearest-neighbour likelihood assigns each star a membership probability in proper-motion, colour-magnitude, and colour-colour spaces, and adaptive smoothing of the high-probability stars produces two-dimensional density maps. After subtracting a first-order Milky Way field gradient and excluding eight clusters with incomplete coverage or too few high-probability stars, 22 clusters show extended structure; six of these are new tentative detections. Four clusters present diffuse envelope-like features and the rest show tidal tail-like structure, with position angles broadly consistent with cluster orbits and N-body disruption models. The mean photometric metallicities of conservative high-probability samples outside the Jacobi radius agree with their clusters' metallicities, indicating the stars are likely genuinely stripped.

Load-bearing premise

The analysis assumes that the Milky Way field density across each five-degree field is smooth enough to be removed by subtracting a fitted first-order polynomial, so any residual overdensity is attributed to cluster debris; if the field contains real substructure such as other streams or halo clumps, some of the detected excess could be spurious.

Editorial extensions

If this is right

  • If the central claim holds, photometric metallicities from narrowband CaHK surveys become a general tool for finding stripped stars around globular clusters, not just for Omega Centauri.
  • The candidate lists for the six new tentative detections (NGC 6101, NGC 6205, NGC 6218, NGC 6541, NGC 6752, NGC 6934) are concrete targets for spectroscopic follow-up that can confirm membership with line-of-sight velocities.
  • Broad agreement between measured position angles and cluster orbits implies that the morphology of extended structure can be mapped from density maps alone in many clusters, enabling population-wide studies of globular cluster disruption.
  • The consistency of metallicities inside and outside the Jacobi radius suggests that extra-tidal stars trace the same stellar populations as their progenitors, so chemistry can be used to link debris to parent clusters.

Reading between the lines

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

  • Because PGS reaches only about $G = 17$, the detected tails are likely the bright tips of longer structures; deeper CaHK photometry should reveal that several new tentative detections are longer streams than the current maps show.
  • If spectroscopic follow-up confirms the six tentative detections at the predicted metallicities, the same classifier could be run on future all-sky narrowband surveys to build a complete census of dissolving globular clusters in the Milky Way.
  • The disagreement between observed debris orientation and N-body predictions for NGC 1261, NGC 1851, NGC 2808 and NGC 6934 suggests the comparison itself is a probe of the Milky Way potential; fitting these data with flexible potentials might constrain the bar or halo shape more sharply than the paper's fixed-potential comparison does.
  • The roughly 20 percent contamination fraction at $P_{\mathrm{mem}} > 0.5$ outside the Jacobi radius implies that membership-probability thresholds alone cannot separate true members from field stars that mimic cluster properties; radial velocities are required before individual stars can be claimed as members.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. This paper presents a search for extra-tidal structure around 30 Milky Way globular clusters using the Pristine-Gaia-Synthetic catalogue, which provides photometric [Fe/H] estimates from synthetic CaHK photometry combined with Gaia astrometry and photometry. The authors define a probabilistic membership model in proper-motion, colour-magnitude, and colour-colour spaces, using cluster stars inside the tidal radius as a template and field stars outside two degrees as a contrast. They build 2D surface density maps with adaptive smoothing, subtract a first-order polynomial to remove the Milky Way field gradient, and identify 22 clusters with extended structure within 5 degrees, six of which are new tentative detections. They also measure mean [Fe/H] in three radial ranges and find broad consistency, and they compare position angles of the extended structure with eTidals N-body models, particle-spray models, and Galstreams tracks.

Significance. If the detections are secure, this would be one of the largest homogeneous censuses of extra-tidal structure in GCs and would demonstrate the power of adding CaHK-based photometric metallicities to Gaia astrometry for this purpose. The paper is careful about photometric depth and contamination, releases membership probabilities as online material, and makes a useful comparison to dynamical models. However, the two main quantitative claims—the detection statistics of the overdensities and the metallicity consistency of the outer populations—are weakened by an uncalibrated significance estimator and by a selection that uses a metallicity-sensitive dimension, respectively. The six new detections are explicitly tentative, but the paper's headline count of 22 clusters with extended structure depends on the same uncalibrated maps.

major comments (3)
  1. [Section 3, Eq. (8) and Section 4.2, Fig. 4] The significance of the residual overdensities that underlie the claim of 22 GCs with extended structure (six of them new) is not calibrated against the null hypothesis. The adaptive-knot estimator in Eq. (8) sets Rloc from the distance to the nearest P_mem-weighted stars, producing spatially correlated knot densities; the first-order polynomial is fitted to and subtracted from these same knots, and the reported σ levels are computed from the RMS of the residuals of that fit. No null-field control is run, so the σ values do not measure the probability that a residual overdensity arises from a smooth Milky Way field. The authors' own statement in Section 5.3 that "regions could just as easily be residual fluctuations in the MW field around the GCs observed" applies directly to the six new tentative detections (NGC 6101, NGC 6205, NGC 6218, NGC 6541, NGC 6752, NGC 6934). I request that the authors run the full pipeline on null fields (e.g., off-cluster positions with the same footprint and quality cuts) or on randomized P_mem assignments, and report the false-positive rate as a function of the claimed σ threshold.
  2. [Section 3, Eqs. (3)-(6); Section 4.1, Table 2] The finding that high-probability stars outside the Jacobi radius have metallicities consistent with the cluster is partly circular. The membership likelihood includes a colour-colour space built on the CaHK index, which is a direct photometric metallicity proxy, and the GC reference sample defines the locus in that space. Stars with high P_mem are therefore selected because they lie near the cluster locus in a metallicity-sensitive dimension, so the agreement between [Fe/H]_PGS outside r_J and inside r_t is not an independent test that these stars are stripped cluster members. To support this claim, the authors should either demonstrate that the outer [Fe/H] distribution is narrower or more peaked than what the selection function alone would produce (e.g., by applying the same P_mem cut to a field-only control sample), or explicitly re-frame the metallicity comparison as a consistency check rather than a confirmation of membership.
  3. [Section 4.2.1, Fig. 5] The split between tidal-tail-like and diffuse-envelope structures is based on the threshold σθ < 8 deg, where σθ is the weighted uncertainty of position angles measured from the same uncalibrated 2D density maps. For the six new tentative detections, this classification is provisional at best; reporting fractions such as "17 GCs have tidal tail structure and 4 have envelope structure" as quantitative results gives these provisional classifications more weight than the data support. The authors should either tie the classification to a calibrated detection significance or present it as a morphological description of the candidate maps only.
minor comments (5)
  1. [Section 2] The word "Specifcally" is a typo; the sentence should read "Specifically."
  2. [Section 5, COMPARISON TO MODELS] The text "theeTidalsGCs9 project" contains a typo and should be "the eTidals GCs project" or "the eTidalsGCs project."
  3. [References] The reference list contains a duplicated entry for Massari, Koppelman, and Helmi (2019), with one version garbled as "r 1/4ap"; the duplicate should be removed.
  4. [Section 4.1] The contamination estimate at P_mem > 0.5 is described as the ratio of stars with [Fe/H] consistent with the cluster to all stars present; this does not measure contamination in the usual sense (the fraction of apparent members that are field stars) because both the numerator and denominator are already filtered by a metallicity-sensitive selection, and the wording should be adjusted accordingly.
  5. [Appendix A] In the criterion for whether a cluster is suitable for 2D density map analysis, "P Pmem > 5" should be written as "Σ P_mem > 5" to avoid confusion.

Circularity Check

1 steps flagged · score 5.0 of 10

Metallicity agreement is partly self-consistent by construction; extended-structure detections remain independent.

  1. fitted input called prediction [Section 3 (Methods, Eqs. 6-7) and Section 4.1 (Results, Fig. 3)]
    "The latter space utilises the PGS CaHK-band, which is sensitive to [Fe/H]... can be used to identify [Fe/H]-similar groups. ... There is a predominantly clear one-to-one relationship between the mean measurements across the three radial regions, which supports our assumption that the stars are excited/stripped from the GC central regions."

    The conservative sample used for the outside-Jacobi-radius metallicity is defined by P_mem > 0.99, and P_mem (Eq. 7) is the ratio of cluster to field likelihoods whose cluster term includes P_CC, a k-NN density in (G_BP - G_RP, CaHK ind) space around a reference built from stars inside the tidal radius. CaHK ind is the same photometric dimension that drives the Pristine [Fe/H] estimate, so high-P_mem stars are, by construction, confined to the cluster's CaHK locus and hence to the cluster's [Fe/H]_PGS. The agreement reported in Fig. 3 is therefore a self-consistency of the selection, not an independent test that stripped stars share the cluster metallicity; the paper itself notes the selection 'may directly influence our findings.'

full rationale

The main structural claim—22 GCs with 2D density overdensities, six new—is not circular: it is a spatial clustering signal in a sample selected by PM, CMD, and CaHK-ind similarity, and it is compared against external Galstreams tracks, eTidals N-body models, and particle-spray models. However, the supporting claim that high-probability stars beyond the Jacobi radius have PGS metallicities consistent with the cluster is partly constructed: the membership probability includes the CaHK-ind (metallicity-sensitive) dimension, with the cluster reference defined by stars inside the tidal radius, so the conservative extra-tidal sample must populate the same CaHK locus. The Fig. 3 one-to-one relation is thus a selection echo rather than an independent confirmation. The paper's Section 5.3 admission that field stars can match PM, CMD, and [Fe/H]_PGS simultaneously and be indistinguishable reinforces that the metallicity dimension alone does not break the degeneracy. The uncalibrated field-subtraction sigma levels are an in-sample statistic; the authors concede 'regions could just as easily be residual fluctuations in the MW field around the GCs observed,' which is a null-test limitation, not a definitional circularity. No load-bearing self-citation chain is present: KI25 is a methodological inheritance and the model comparisons are external.

Assumptions & free parameters 7 free parameters · 6 assumptions · 0 invented entities

The analysis rests on the reliability of the PGS catalogue, the cleanliness of the internal reference samples, and the smoothness of the Milky Way field model. No new physical entities are introduced. The free parameters are mostly hand-chosen thresholds and mixture weights; f_cl is fitted per cluster. These are standard for a mixture-model search, but the arbitrary sigma_theta=8 deg split and the P_mem thresholds should be sensitivity-tested.

free parameters (7)
  • f_cl (cluster-to-field ratio) = fit per GC, values not reported
    Normalizes the membership likelihood (Eq. 6); fitted to each GC's 5-degree field.
  • k (nearest neighbors) = 10
    Hand-chosen; k-th nearest neighbour density in CMD and CC spaces (Eq. 3).
  • CMD weighting metric ratio = 1:10 (colour:mag)
    Hand-chosen to reflect uncertainty ratio between Gaia colours and G-band photometry.
  • CC weighting metric ratio = 1:2 (CaHK ind:colour)
    Hand-chosen for colour-colour space.
  • P_mem selection thresholds = 0.5 and 0.99
    Thresholds for membership display and conservative sample.
  • sigma_theta tail/envelope split = 8 deg
    Hand-chosen cut separating tightly constrained position angles (tails) from diffuse envelopes.
  • minimum summed P_mem per density knot = 2
    Adaptive smoothing parameter in Eq. 8.
assumptions (6)
  • domain assumption PGS synthetic CaHK photometry yields reliable photometric [Fe/H] for -4<[Fe/H]<0
    Taken from Pristine DR1 papers (Starkenburg 2017; Martin 2024); underlies the CC-space discriminator.
  • domain assumption Reference GC sample inside the tidal radius with PM within 1 mas/yr of the cluster is clean
    Used to build the cluster likelihood; contamination is 'very little' (Section 3).
  • domain assumption Field sample outside 2 degrees is dominated by MW stars, not cluster debris
    Section 3: extra-tidal stars are 'severely outnumbered by the field'.
  • domain assumption MW field density across each 5-degree field varies smoothly (first-order polynomial)
    Section 3: 2D first-order polynomial fit and subtraction; if field has substructure, overdensities can be spurious.
  • domain assumption Cluster tidal and Jacobi radii from cited catalogues are accurate
    Used to define radial bins and outer regions; from de Boer et al. 2019 and Balbinot & Gieles 2018.
  • domain assumption Orbital integration with MWPotential2014 approximates true GC orbits
    Used for position angle comparisons; from Bovy 2014, not re-derived here.

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Pith. "Pith review of Constructing a Pristine View of Extended Globular Cluster Structure." pith.science (2026). https://pith.science/paper/A23PCJEV

@misc{pith2026250705590,
  author       = {Pith},
  title        = {Pith review of: Constructing a Pristine View of Extended Globular Cluster Structure},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/A23PCJEV}},
  note         = {Machine review of arXiv:2507.05590}
}
read the original abstract

Globular Clusters (GCs) displaying extended structures are becoming increasingly ubiquitous in the Milky Way (MW). Despite their low surface brightness, which makes disentangling the true structure from the MW overwhelmingly difficult, the increasing availability of multi-dimensional data sets has allowed for new detections of extended GC structure. This work utilises the Pristine-Gaia-Synthetic catalogue released as part of the Pristine Surveys first data release to search for tidally stripped stars in the peripheries of MW GCs. Pristine provides photometric [Fe/H] measurements based on CaHK-band photometry. Using unsupervised machine learning techniques, we provided lists of extra-tidal stars for 30 GCs, one of the largest surveys of its kind. We find that (1) 22 GCs that passed our quality cut have extended structure within 5 deg from the cluster centers of which six are new tentative detections, (2) four of those GCs exhibit diffuse envelope-like extra-tidal features, while the remaining GCs exhibit tidal tail-like structures. We measure the position angles of the extended structures, find broad consistency between the position angles and the GC orbits, and discuss our results concerning N-body models. This work demonstrates the effectiveness of adding photometric metallicities to the multi-dimensional search of extended tidal structure and how the upcoming multi-object spectrographs will be crucial for exploring GC peripheries in the coming years.

Figures

Figures reproduced from arXiv: 2507.05590 by the authors.

Figure 1
Figure 1. Demonstration of the parameter spaces explored for the two reference sets with respect to NGC 7089. Points in red belong to the cluster sample, and the black points are the field sample. Left: CMD space. Center: The colour-colour space. Right: The proper motion space in tangential coordinates. An extended version of this figure for all GCs is located in the appendix. average knot density (ρ) and associated standard … view at source ↗
Figure 2
Figure 2. Radial distribution of [Fe/H]PGS for our sampled GCs. Stars with Pmem > 0.5 are displayed and coloured by their membership probability (top colour bar). Underplotted is a density diagram that demonstrates the distribution of stars with Pmem < 0.1 (most likely field members). Each star that is part of the conservative sample for each GC is marked with a black circle, along with their [Fe/H]PGS uncertainty displayed w… view at source ↗
Figure 2
Figure 2. Radial distribution of [Fe/H]PGS for our sampled GCs. A continuation of [PITH_FULL_IMAGE:figures/full_fig_p010_2.png] view at source ↗
Figures from the paper (18 more)
Figure 3
Figure 3. Figure 3: Comparison of the mean [Fe/H]PGS measurements across the three radial ranges for each GC. The radial ranges explored are deonted by the x- and y- axis labels, where [Fe/H]rcl PGS denotes the radial range that covers within the tidal radius, [Fe/H]rt PGS between the tid…
Figure 4
Figure 4. Figure 4: 2D density distribution of our analysed GCs. Each GC, labelled in the top right, contains their surface density distribution coloured by σ level on the top row. The contours indicate 1, 2 and 3 σ levels. Additionally plotted are the GCs orbit (forward/backward orbits a…
Figure 4
Figure 4. Figure 4: 2D Density distribution of our analysis GCs. A continuation of [PITH_FULL_IMAGE:figures/full_fig_p013_4.png]
Figure 5
Figure 5. Figure 5: Demonstration of the separation between ex￾tended tidal structure that is highly constrained (green), and those that are less constrained (red), designated by σθ as a function of heliocentric distance, R⊙. The pointing direction of the arrows (triangles) indicated whet…
Figure 6
Figure 6. Figure 6: The same as [PITH_FULL_IMAGE:figures/full_fig_p015_6.png]
Figure 6
Figure 6. Figure 6: A continuation of [PITH_FULL_IMAGE:figures/full_fig_p016_6.png]
Figure 7
Figure 7. Figure 7: Position angle as a function of radius for our GCs with 2D surface density distributions. Each GC, labelled in the top right corner, has its radial position angle profile demonstrated by the blue points. Also demonstrated are the forward/backward orbits as solid/dashed…
Figure 7
Figure 7. Figure 7: Position angle as a function of radius for our GCs with 2D surface density distributions. A continuation of [PITH_FULL_IMAGE:figures/full_fig_p018_7.png]
Figure 8
Figure 8. Figure 8: Corner plot of GC parameters used to explore potential predictors of extended structure and its form. Points share colours and triangle orientations with [PITH_FULL_IMAGE:figures/full_fig_p019_8.png]
Figure 9
Figure 9. Figure 9: Demonstration of the eTidalGCs N-body models (top row) the Y. Chen et al. (2025) particle spray models in both forward and backward trajectories in the under four selected MW potentials: McMillan17 (P. J. McMillan 2017), Cautan20 (M. Cautun et al. 2020), and a MWpotent…
Figure 10
Figure 10. Figure 10: The same as [PITH_FULL_IMAGE:figures/full_fig_p024_10.png]
Figure 10
Figure 10. Figure 10: A continuation of [PITH_FULL_IMAGE:figures/full_fig_p025_10.png]
Figure 11
Figure 11. Figure 11: Extended version of [PITH_FULL_IMAGE:figures/full_fig_p026_11.png]
Figure 11
Figure 11. Figure 11: Extended version of [PITH_FULL_IMAGE:figures/full_fig_p027_11.png]
Figure 11
Figure 11. Figure 11: Extended version of [PITH_FULL_IMAGE:figures/full_fig_p028_11.png]
Figure 11
Figure 11. Figure 11: Extended version of [PITH_FULL_IMAGE:figures/full_fig_p029_11.png]
Figure 11
Figure 11. Figure 11: Extended version of [PITH_FULL_IMAGE:figures/full_fig_p030_11.png]
Figure 11
Figure 11. Figure 11: Extended version of [PITH_FULL_IMAGE:figures/full_fig_p031_11.png]

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Works this paper leans on

110 extracted references · 19 canonical work pages

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ur...

  3. [3]

    ?;^nk*6 Oۄ ][wv P;|dq Sn u<urS =j O?rlo&Q= :ƚ9<[)7/I cU[K& 縏9,1 >Dt 1듣 :o y

    thebibliography [1] 20pt to REFERENCES 6pt =0pt \@twocolumntrue 12pt -12pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key o...

    arXiv 2017

  4. [4]

    D., & Baumgardt, H

    Arnold, A. D., & Baumgardt, H. 2025, title Direct N-body simulations of NGC 6397 and its tidal tails, Monthly Notices of the Royal Astronomical Society, 537, 1807–1817, 10.1093/mnras/staf121

    doi:10.1093/mnras/staf121 2025

  5. [5]

    S., Erkal , D., et al

    Awad , P., Li , T. S., Erkal , D., et al. 2025, title S ^ 5 : New insights from deep spectroscopic observations of the tidal tails of the globular clusters NGC 1261 and NGC 1904 , , 693, A69, 10.1051/0004-6361/202451930

    doi:10.1051/0004-6361/202451930 2025

  6. [6]

    2022, title Evidence for C and Mg variations in the GD-1 stellar stream , , 515, 5802, 10.1093/mnras/stac1953

    Balbinot , E., Cabrera-Ziri , I., & Lardo , C. 2022, title Evidence for C and Mg variations in the GD-1 stellar stream , , 515, 5802, 10.1093/mnras/stac1953

    work page doi:10.1093/mnras/stac1953 2022

  7. [7]

    2018, title The devil is in the tails: the role of globular cluster mass evolution on stream properties , , 474, 2479, 10.1093/mnras/stx2708

    Balbinot , E., & Gieles , M. 2018, title The devil is in the tails: the role of globular cluster mass evolution on stream properties , , 474, 2479, 10.1093/mnras/stx2708

    doi:10.1093/mnras/stx2708 2018

  8. [8]

    2018, title Multiple Stellar Populations in Globular Clusters , , 56, 83, 10.1146/annurev-astro-081817-051839

    Bastian , N., & Lardo , C. 2018, title Multiple Stellar Populations in Globular Clusters , , 56, 83, 10.1146/annurev-astro-081817-051839

    doi:10.1146/annurev-astro-081817-051839 2018

Show all 110 references
  1. [9]

    2018, title A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters , , 478, 1520, 10.1093/mnras/sty1057

    Baumgardt , H., & Hilker , M. 2018, title A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters , , 478, 1520, 10.1093/mnras/sty1057

    2018 doi

  2. [10]

    2021, title Accurate distances to Galactic globular clusters through a combination of Gaia EDR3 , HST , and literature data, , 505, 5957, 10.1093/mnras/stab1474

    Baumgardt, H., & Vasiliev, E. 2021, title Accurate distances to Galactic globular clusters through a combination of Gaia EDR3 , HST , and literature data, , 505, 5957, 10.1093/mnras/stab1474

    2021 doi

  3. [11]

    Bonaca, A., Geha, M., K\" u pper, A. H. W., et al. 2014, title MILKY WAY MASS AND POTENTIAL RECOVERY USING TIDAL STREAMS IN A REALISTIC HALO, The Astrophysical Journal, 795, 94, 10.1088/0004-637x/795/1/94

    2014 doi

  4. [12]

    Bonaca , A., & Price-Whelan , A. M. 2025, title Stellar streams in the Gaia era , , 100, 101713, 10.1016/j.newar.2024.101713

    2025

  5. [13]

    2014, title DYNAMICAL MODELING OF TIDAL STREAMS, The Astrophysical Journal, 795, 95, 10.1088/0004-637x/795/1/95

    Bovy, J. 2014, title DYNAMICAL MODELING OF TIDAL STREAMS, The Astrophysical Journal, 795, 95, 10.1088/0004-637x/795/1/95

    2014 doi

  6. [14]

    2015, title galpy: A python LIBRARY FOR GALACTIC DYNAMICS, The Astrophysical Journal Supplement Series, 216, 29, 10.1088/0067-0049/216/2/29

    Bovy, J. 2015, title galpy: A python LIBRARY FOR GALACTIC DYNAMICS, The Astrophysical Journal Supplement Series, 216, 29, 10.1088/0067-0049/216/2/29

    2015 doi

  7. [15]

    K., & Kallivayalil, N

    Bovy, J., Bahmanyar, A., Fritz, T. K., & Kallivayalil, N. 2016, title THE SHAPE OF THE INNER MILKY WAY HALO FROM OBSERVATIONS OF THE PAL 5 AND GD–1 STELLAR STREAMS, The Astrophysical Journal, 833, 31, 10.3847/1538-4357/833/1/31

    2016 doi

  8. [16]

    2019, title Collaborative Nested Sampling: Big Data versus Complex Physical Models , , 131, 108005, 10.1088/1538-3873/aae7fc

    Buchner , J. 2019, title Collaborative Nested Sampling: Big Data versus Complex Physical Models , , 131, 108005, 10.1088/1538-3873/aae7fc

    2019 doi

  9. [17]

    2021, title UltraNest - a robust, general purpose Bayesian inference engine , The Journal of Open Source Software, 6, 3001, 10.21105/joss.03001

    Buchner , J. 2021, title UltraNest - a robust, general purpose Bayesian inference engine , The Journal of Open Source Software, 6, 3001, 10.21105/joss.03001

    2021 doi

  10. [18]

    2014, title X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue, A & A, 564, A125, 10.1051/0004-6361/201322971

    Buchner, J., Georgakakis, A., Nandra, K., et al. 2014, title X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue, A & A, 564, A125, 10.1051/0004-6361/201322971

    2014 doi

  11. [19]

    M., Cautun , M., Deason , A

    Callingham , T. M., Cautun , M., Deason , A. J., et al. 2022, title The chemo-dynamical groups of Galactic globular clusters , , 513, 4107, 10.1093/mnras/stac1145

    2022 doi

  12. [20]

    Carballo-Bello, J. A. 2019, title Using Gaia DR2 to detect extratidal structures around the Galactic globular cluster NGC 362, Monthly Notices of the Royal Astronomical Society, 486, 1667–1671, 10.1093/mnras/stz962

    2019 doi

  13. [21]

    A., Martínez-Delgado, D., Navarrete, C., et al

    Carballo-Bello, J. A., Martínez-Delgado, D., Navarrete, C., et al. 2017, title Tails and streams around the Galactic globular clusters NGC 1851, NGC 1904, NGC 2298 and NGC 2808, Monthly Notices of the Royal Astronomical Society, 474, 683–695, 10.1093/mnras/stx2767

    2017 doi

  14. [22]

    A., Salinas, R., & Piatti, A

    Carballo-Bello, J. A., Salinas, R., & Piatti, A. E. 2020, title The disruption of the low-mass globular cluster E 3, Monthly Notices of the Royal Astronomical Society, 499, 2157–2161, 10.1093/mnras/staa2864

    2020 doi

  15. [23]

    G., & Grillmair , C

    Carlberg , R. G., & Grillmair , C. J. 2021, title Testing for Dark Matter in the Outskirts of Globular Clusters , , 922, 104, 10.3847/1538-4357/ac289f

    2021 doi

  16. [24]

    G., & Grillmair , C

    Carlberg , R. G., & Grillmair , C. J. 2022, title The Dark Matter Halo of M54 , , 935, 14, 10.3847/1538-4357/ac7d54

    2022 doi

  17. [25]

    2009, title Intrinsic iron spread and a new metallicity scale for globular clusters, A & A, 508, 695–706, 10.1051/0004-6361/200913003

    Carretta, E., Bragaglia, A., Gratton, R., D’Orazi, V., & Lucatello, S. 2009, title Intrinsic iron spread and a new metallicity scale for globular clusters, A & A, 508, 695–706, 10.1051/0004-6361/200913003

    2009 doi

  18. [26]

    J., et al

    Cautun , M., Ben \' tez-Llambay , A., Deason , A. J., et al. 2020, title The milky way total mass profile as inferred from Gaia DR2 , , 494, 4291, 10.1093/mnras/staa1017

    2020 doi

  19. [27]

    Y., & Ash , N

    Chen , Y., Valluri , M., Gnedin , O. Y., & Ash , N. 2025, title Improved Particle Spray Algorithm for Modeling Globular Cluster Streams , , 276, 32, 10.3847/1538-4365/ad9904

    2025 doi

  20. [28]

    C., Abrams, D

    Dalton, G., Trager, S. C., Abrams, D. C., et al. 2012, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 8446, Ground-based and Airborne Instrumentation for Astronomy IV, ed. I. S. McLean, S. K. Ramsay, & H. Takami, 84460P, 10.1117/12.925950

    2012 doi

  21. [29]

    de Boer, T. J. L., Gieles, M., Balbinot, E., et al. 2019, title Globular cluster number density profiles using Gaia DR2 , , 485, 4906, 10.1093/mnras/stz651

    2019 doi

  22. [30]

    1999, title The Pattern Speed of the Galactic Bar , , 524, L35, 10.1086/312299

    Dehnen , W. 1999, title The Pattern Speed of the Galactic Bar , , 524, L35, 10.1086/312299

    1999 doi

  23. [31]

    K., & Rix, H.-W

    Dehnen, W., Odenkirchen, M., Grebel, E. K., & Rix, H.-W. 2004, title Modeling the Disruption of the Globular Cluster Palomar 5 by Galactic Tides, The Astronomical Journal, 127, 2753–2770, 10.1086/383214

    2004 doi

  24. [32]

    2018, title On the Solar Velocity , Research Notes of the American Astronomical Society, 2, 210, 10.3847/2515-5172/aaef8b

    Drimmel , R., & Poggio , E. 2018, title On the Solar Velocity , Research Notes of the American Astronomical Society, 2, 210, 10.3847/2515-5172/aaef8b

    2018 doi

  25. [33]

    F., Ibata , R., et al

    Errani , R., Navarro , J. F., Ibata , R., et al. 2022, title The Pristine survey - XVIII. C-19: tidal debris of a dark matter-dominated globular cluster? , , 514, 3532, 10.1093/mnras/stac1516

    2022 doi

  26. [34]

    2023, title The e-TidalGCs project

    Ferrone , S., Di Matteo , P., Mastrobuono-Battisti , A., et al. 2023, title The e-TidalGCs project. Modeling the extra-tidal features generated by Galactic globular clusters , , 673, A44, 10.1051/0004-6361/202244141

    2023 doi

  27. [35]

    Gaia Collaboration , Prusti, T., de Bruijne, J. H. J., et al. 2016, title The Gaia mission , A & A, 595, A1, 10.1051/0004-6361/201629272

    2016 doi

  28. [36]

    2018, title Gaia Data Release 2

    Gaia Collaboration , Helmi, A., van Leeuwen, F., et al. 2018, title Gaia Data Release 2. Kinematics of globular clusters and dwarf galaxies around the Milky Way , A & A, 616, A12, 10.1051/0004-6361/201832698

    2018 doi

  29. [37]

    Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2023, title Gaia Data Release 3. Summary of the content and survey properties , , 674, A1, 10.1051/0004-6361/202243940

    2023 doi

  30. [38]

    2021, title A supra-massive population of stellar-mass black holes in the globular cluster Palomar 5 , Nature Astronomy, 5, 957, 10.1038/s41550-021-01392-2

    Gieles , M., Erkal , D., Antonini , F., Balbinot , E., & Pe \ n arrubia , J. 2021, title A supra-massive population of stellar-mass black holes in the globular cluster Palomar 5 , Nature Astronomy, 5, 957, 10.1038/s41550-021-01392-2

    2021 doi

  31. [39]

    M., Brasseur, C

    Ginsburg, A., Sip o cz, B. M., Brasseur, C. E., et al. 2019, title astroquery: An Astronomical Web-querying Package in Python , AJ, 157, 98, 10.3847/1538-3881/aafc33

    2019 doi

  32. [40]

    2019, title What is a globular cluster? An observational perspective , , 27, 8, 10.1007/s00159-019-0119-3

    Gratton , R., Bragaglia , A., Carretta , E., et al. 2019, title What is a globular cluster? An observational perspective , , 27, 8, 10.1007/s00159-019-0119-3

    2019 doi

  33. [41]

    2004, title Abundance Variations within Globular Clusters, Annual Review of Astronomy and Astrophysics, 42, 385–440, 10.1146/annurev.astro.42.053102.133945

    Gratton, R., Sneden, C., & Carretta, E. 2004, title Abundance Variations within Globular Clusters, Annual Review of Astronomy and Astrophysics, 42, 385–440, 10.1146/annurev.astro.42.053102.133945

    2004

  34. [42]

    G., Carretta, E., & Bragaglia, A

    Gratton, R. G., Carretta, E., & Bragaglia, A. 2012, title Multiple populations in globular clusters: Lessons learned from the Milky Way globular clusters, The Astronomy and Astrophysics Review, 20, 10.1007/s00159-012-0050-3

    2012 doi

  35. [43]

    Grillmair , C. J. 2019, title Detection of a 50 long Trailing Tidal Tail for the Globular Cluster M5 , , 884, 174, 10.3847/1538-4357/ab441d

    2019 doi

  36. [44]

    M., Webb , J

    Grondin , S. M., Webb , J. J., Lane , J. M. M., Speagle , J. S., & Leigh , N. W. C. 2024, title A catalogue of Galactic GEMS: Globular cluster Extra-tidal Mock Stars , , 528, 5189, 10.1093/mnras/stae203

    2024 doi

  37. [45]

    2015, title Development of multiple tidal tails around globular clusters and dwarf satellite galaxies , , 446, 3100

    Hozumi, S., & Burkert, A. 2015, title Development of multiple tidal tails around globular clusters and dwarf satellite galaxies , , 446, 3100

    2015

  38. [46]

    Hunter, J. D. 2007, title Matplotlib: A 2D Graphics Environment, Computing in Science & Engineering, 9, 90–95, 10.1109/mcse.2007.55

    2007 doi

  39. [47]

    2021, title Charting the Galactic Acceleration Field

    Ibata , R., Malhan , K., Martin , N., et al. 2021, title Charting the Galactic Acceleration Field. I. A Search for Stellar Streams with Gaia DR2 and EDR3 with Follow-up from ESPaDOnS and UVES , , 914, 123, 10.3847/1538-4357/abfcc2

    2021 doi

  40. [48]

    2024, title Charting the Galactic Acceleration Field

    Ibata , R., Malhan , K., Tenachi , W., et al. 2024, title Charting the Galactic Acceleration Field. II. A Global Mass Model of the Milky Way from the STREAMFINDER Atlas of Stellar Streams Detected in Gaia DR3 , , 967, 89, 10.3847/1538-4357/ad382d

    2024 doi

  41. [49]

    A., Lewis , G

    Ibata , R. A., Lewis , G. F., Irwin , M. J., & Quinn , T. 2002, title Uncovering cold dark matter halo substructure with tidal streams , , 332, 915, 10.1046/j.1365-8711.2002.05358.x

    2002

  42. [50]

    2017, title On the kinematic detection of accreted streams in the Gaia era: a cautionary tale , , 604, A106, 10.1051/0004-6361/201629691

    Jean-Baptiste , I., Di Matteo , P., Haywood , M., et al. 2017, title On the kinematic detection of accreted streams in the Gaia era: a cautionary tale , , 604, A106, 10.1051/0004-6361/201629691

    2017 doi

  43. [51]

    W., et al

    Jensen, J., Thomas, G., McConnachie, A. W., et al. 2021, title Uncovering fossils of the distant Milky Way with UNIONS: NGC 5466 and its stellar stream, Monthly Notices of the Royal Astronomical Society, 507, 1923, 10.1093/mnras/stab2325

    2021 doi

  44. [52]

    C., Dalton , G

    Jin , S., Trager , S. C., Dalton , G. B., et al. 2024, title The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation , , 530, 2688, 10.1093/mnras/stad557

    2024 doi

  45. [53]

    S., Agertz, O., Berbel, A

    Jong De de Jong, R. S., Agertz, O., Berbel, A. A., et al. 2019, title 4MOST: Project overview and information for the First Call for Proposals , The Messenger, 175, 3, 10.18727/0722-6691/5117

    2019 doi

  46. [54]

    Jordi, K., & Grebel, E. K. 2010, title Search for extratidal features around 17 globular clusters in the Sloan Digital Sky Survey , A & A, 522, A71, 10.1051/0004-6361/201014392

    2010 doi

  47. [55]

    Kraft , R. P. 1994, title Abundance Differences among Globular Cluster Giants: Primordial vs. Evolutionary Scenarios , , 106, 553, 10.1086/133416

    1994 doi

  48. [56]

    B., Da Costa, G

    Kuzma, P. B., Da Costa, G. S., & Mackey, A. D. 2018, title The outer envelopes of globular clusters. II. NGC 1851, NGC 5824 and NGC 1261* , , 473, 2881, 10.1093/mnras/stx2353

    2018 doi

  49. [57]

    B., Ferguson , A

    Kuzma , P. B., Ferguson , A. M. N., & Pe \ n arrubia , J. 2021, title Detecting globular cluster tidal extensions with Bayesian inference - I. Analysis of Centauri with Gaia EDR3 , , 507, 1127, 10.1093/mnras/stab2280

    2021 doi

  50. [58]

    B., Ferguson , A

    Kuzma , P. B., Ferguson , A. M. N., Varri , A. L., et al. 2022, title Forward and back: kinematics of the Palomar 5 tidal tails , , 512, 315, 10.1093/mnras/stac381

    2022 doi

  51. [59]

    B., & Ishigaki , M

    Kuzma , P. B., & Ishigaki , M. N. 2025, title A pristine view of galactic globular clusters and their peripheries: Omega Centauri , , 537, 2752, 10.1093/mnras/staf212

    2025 doi

  52. [60]

    Küpper, A. H. W., Kroupa, P., Baumgardt, H., & Heggie, D. C. 2010, title Tidal tails of star clusters, , 401, 105, 10.1111/j.1365-2966.2009.15690.x

    2010

  53. [61]

    Küpper, A. H. W., Lane, R. R., & Heggie, D. C. 2012, title More on the structure of tidal tails, , 420, 2700, 10.1111/j.1365-2966.2011.20242.x

    2012

  54. [62]

    2000, title Tidal tails around 20 Galactic globular clusters

    Leon, S., Meylan, G., & Combes, F. 2000, title Tidal tails around 20 Galactic globular clusters. Observational evidence for gravitational disk/bulge shocking , A & A, 359, 907, 10.48550/ARXIV.ASTRO-PH/0006100

    2000 doi

  55. [63]

    2018, title Gaia Data Release 2

    Lindegren, L., Hern \'a ndez, J., Bombrun, A., et al. 2018, title Gaia Data Release 2. The astrometric solution , A & A, 616, A2, 10.1051/0004-6361/201832727

    2018 doi

  56. [64]

    A., Hern \'a ndez , J., et al

    Lindegren , L., Klioner , S. A., Hern \'a ndez , J., et al. 2021, title Gaia Early Data Release 3. The astrometric solution , , 649, A2, 10.1051/0004-6361/202039709

    2021 doi

  57. [65]

    A., Sharma, S., et al

    Malhan, K., Ibata, R. A., Sharma, S., et al. 2022, title The Global Dynamical Atlas of the Milky Way Mergers : Constraints from Gaia EDR3 -based Orbits of Globular Clusters , Stellar Streams , and Satellite Galaxies , apj, 926, 107, 10.3847/1538-4357/ac4d2a

    2022 doi

  58. [66]

    F., Starkenburg , E., Yuan , Z., et al

    Martin , N. F., Starkenburg , E., Yuan , Z., et al. 2024, title The Pristine survey: XXIII. Data Release 1 and an all-sky metallicity catalogue based on Gaia DR3 BP/RP spectro-photometry , , 692, A115, 10.1051/0004-6361/202347633

    2024 doi

  59. [67]

    2025, title Origin of the system of globular clusters in the Milky Way -- Gaia eDR3 edition , arXiv e-prints, arXiv:2503.14657, 10.48550/arXiv.2503.14657

    Massari , D. 2025, title Origin of the system of globular clusters in the Milky Way -- Gaia eDR3 edition , arXiv e-prints, arXiv:2503.14657, 10.48550/arXiv.2503.14657

    2025 doi arXiv

  60. [69]

    H., & Helmi, A

    Massari, D., Koppelman, H. H., & Helmi, A. 2019, title Origin of the system of globular clusters in the Milky Way , åp, 630, L4, 10.1051/0004-6361/201936135

    2019 doi

  61. [70]

    Massari, D., Dalessandro, E., Erkal, D., et al. 2025, title Euclid: Early Release Observations – Unveiling the morphology of two Milky Way globular clusters out to their periphery, Astronomy & Astrophysics, 697, A8, 10.1051/0004-6361/202449696

    2025 doi

  62. [71]

    2023, title galstreams: A library of Milky Way stellar stream footprints and tracks, Monthly Notices of the Royal Astronomical Society, 520, 5225, 10.1093/mnras/stad321

    Mateu, C. 2023, title galstreams: A library of Milky Way stellar stream footprints and tracks, Monthly Notices of the Royal Astronomical Society, 520, 5225, 10.1093/mnras/stad321

    2023 doi

  63. [72]

    McMillan, P. J. 2017, title The mass distribution and gravitational potential of the Milky Way , , 465, 76, 10.1093/mnras/stw2759

    2017 doi

  64. [73]

    P., & Marino , A

    Milone , A. P., & Marino , A. F. 2022, title Multiple Populations in Star Clusters , Universe, 8, 359, 10.3390/universe8070359

    2022 doi

  65. [74]

    2024, title Metallicity distributions of halo stars: do they trace the Galactic accretion history? , , 690, A136, 10.1051/0004-6361/202449291

    Mori , A., Di Matteo , P., Salvadori , S., et al. 2024, title Metallicity distributions of halo stars: do they trace the Galactic accretion history? , , 690, A136, 10.1051/0004-6361/202449291

    2024 doi

  66. [75]

    K., Rockosi, C

    Odenkirchen, M., Grebel, E. K., Rockosi, C. M., et al. 2001, title Detection of Massive Tidal Tails around the Globular Cluster Palomar 5 with Sloan Digital Sky Survey Commissioning Data , apjl, 548, L165, 10.1086/319095

    2001 doi

  67. [76]

    W., Saha, A., Knezek, P., et al

    Olszewski, E. W., Saha, A., Knezek, P., et al. 2009, title A 500 Parsec Halo Surrounding the Galactic Globular NGC 1851 , AJ, 138, 1570

    2009

  68. [77]

    2023, title The distribution of globular clusters in kinematic spaces does not trace the accretion history of the host galaxy , , 673, A86, 10.1051/0004-6361/202245128

    Pagnini , G., Di Matteo , P., Khoperskov , S., et al. 2023, title The distribution of globular clusters in kinematic spaces does not trace the accretion history of the host galaxy , , 673, A86, 10.1051/0004-6361/202245128

    2023 doi

  69. [78]

    2025, title Abundance ties: Nephele and the globular cluster population accreted with Cen: Based on APOGEE DR17 and Gaia EDR3 , , 693, A155, 10.1051/0004-6361/202450264

    Pagnini , G., Di Matteo , P., Haywood , M., et al. 2025, title Abundance ties: Nephele and the globular cluster population accreted with Cen: Based on APOGEE DR17 and Gaia EDR3 , , 693, A155, 10.1051/0004-6361/202450264

    2025 doi

  70. [79]

    G., & Miralda-Escud \'e , J

    Palau , C. G., & Miralda-Escud \'e , J. 2019, title Statistical detection of a tidal stream associated with the globular cluster M68 using Gaia data , , 488, 1535, 10.1093/mnras/stz1790

    2019 doi

  71. [80]

    G., & Miralda-Escud \'e , J

    Palau , C. G., & Miralda-Escud \'e , J. 2021, title The tidal stream generated by the globular cluster NGC 3201 , , 504, 2727, 10.1093/mnras/stab1024

    2021 doi

  72. [81]

    2011, title Scikit-learn: Machine Learning in P ython, Journal of Machine Learning Research, 12, 2825, 10.48550/ARXIV.1201.0490

    Pedregosa, F., Varoquaux, G., Gramfort, A., et al. 2011, title Scikit-learn: Machine Learning in P ython, Journal of Machine Learning Research, 12, 2825, 10.48550/ARXIV.1201.0490

    2011 doi arXiv

  73. [82]

    L., Breen, P

    Peñarrubia, J., Varri, A. L., Breen, P. G., Ferguson, A. M. N., & Sánchez-Janssen, R. 2017, title Stellar envelopes of globular clusters embedded in dark mini-haloes, , 471, L31, 10.1093/mnrasl/slx094

    2017 doi

  74. [83]

    Piatti , A. E. 2019, title Formation Imprints in the Kinematics of the Milky Way Globular Cluster System , , 882, 98, 10.3847/1538-4357/ab3574

    2019 doi

  75. [84]

    Piatti , A. E. 2024 a , title Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355 , , 167, 279, 10.3847/1538-3881/ad4704

    2024 doi

  76. [85]

    Piatti , A. E. 2024 b , title First deep search of tidal tails in the Milky Way globular cluster NGC 6362 , , 683, A151, 10.1051/0004-6361/202348534

    2024 doi

  77. [86]

    E., & Carballo-Bello, J

    Piatti, A. E., & Carballo-Bello, J. A. 2019, title Extra-tidal structures around the Gaia Sausage candidate globular cluster NGC 6779 (M56) , , 485, 1029, 10.1093/mnras/stz500

    2019 doi

  78. [87]

    E., & Carballo-Bello , J

    Piatti , A. E., & Carballo-Bello , J. A. 2020, title The tidal tails of Milky Way globular clusters , , 637, L2, 10.1051/0004-6361/202037994

    2020 doi

  79. [88]

    E., Mestre , M

    Piatti , A. E., Mestre , M. F., Carballo-Bello , J. A., et al. 2021, title Signatures of tidal disruption in the Milky Way globular cluster NGC 6981 (M72) , , 646, A176, 10.1051/0004-6361/202040038

    2021 doi

  80. [89]

    2020, title adrn/gala: v1.3, , v1.3 Zenodo, 10.5281/zenodo.4159870

    Price-Whelan, A., Sipőcz, B., Lenz, D., et al. 2020, title adrn/gala: v1.3, , v1.3 Zenodo, 10.5281/zenodo.4159870

    2020 doi

  81. [90]

    Price-Whelan, A. M. 2017, title Gala: A Python package for galactic dynamics, The Journal of Open Source Software, 2, 10.21105/joss.00388

    2017 doi

  82. [91]

    M., Johnston , K

    Price-Whelan , A. M., Johnston , K. V., Valluri , M., et al. 2016, title Chaotic dispersal of tidal debris , , 455, 1079, 10.1093/mnras/stv2383

    2016 doi

  83. [92]

    W., et al

    Riello , M., De Angeli , F., Evans , D. W., et al. 2021, title Gaia Early Data Release 3. Photometric content and validation , , 649, A3, 10.1051/0004-6361/202039587

    2021 doi

  84. [93]

    Roberts , D., Gieles , M., Erkal , D., & Sanders , J. L. 2025, title Stellar streams from black hole-rich star clusters , , 538, 454, 10.1093/mnras/staf321

    2025 doi

  85. [94]

    2020, title The eye of Gaia on globular clusters structure: tidal tails , , 495, 2222

    Sollima, A. 2020, title The eye of Gaia on globular clusters structure: tidal tails , , 495, 2222

    2020

  86. [95]

    2019, title The eye of Gaia on globular clusters kinematics: internal rotation , , 485, 1460, 10.1093/mnras/stz505

    Sollima, A., Baumgardt, H., & Hilker, M. 2019, title The eye of Gaia on globular clusters kinematics: internal rotation , , 485, 1460, 10.1093/mnras/stz505

    2019 doi

  87. [96]

    2017, title The Pristine survey - I

    Starkenburg , E., Martin , N., Youakim , K., et al. 2017, title The Pristine survey - I. Mining the Galaxy for the most metal-poor stars , , 471, 2587, 10.1093/mnras/stx1068

    2017 doi

  88. [97]

    2023, title Classifying Globular Clusters and Applying them to Estimate the mass of the Milky Way , Research in Astronomy and Astrophysics, 23, 015013, 10.1088/1674-4527/ac9e91

    Sun , G., Wang , Y., Liu , C., et al. 2023, title Classifying Globular Clusters and Applying them to Estimate the mass of the Milky Way , Research in Astronomy and Astrophysics, 23, 015013, 10.1088/1674-4527/ac9e91

    2023 doi

  89. [98]

    S., Chiba , M., et al

    Takada , M., Ellis , R. S., Chiba , M., et al. 2014, title Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph , , 66, R1, 10.1093/pasj/pst019

    2014 doi

  90. [99]

    2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol

    Tamura , N., Takato , N., Shimono , A., et al. 2016, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 9908, Ground-based and Airborne Instrumentation for Astronomy VI, ed. C. J. Evans , L. Simard , & H. Takami , 99081M, 10.1117/12.2232103

    2016 doi

  91. [100]

    Tavangar , K., & Price-Whelan , A. M. 2025, title Inferring the density and membership of stellar streams with flexible models: The GD-1 stream in Gaia Data Release 3 , arXiv e-prints, arXiv:2502.13236, 10.48550/arXiv.2502.13236

    2025 doi

  92. [101]

    P., Tollerud, E

    The Astropy Collaboration , Robitaille, T. P., Tollerud, E. J., et al. 2013, title Astropy: A community Python package for astronomy , A & A, 558, A33

    2013

  93. [102]

    M., Sip o cz, B

    The Astropy Collaboration , Price-Whelan, A. M., Sip o cz, B. M., et al. 2018, title The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package , AJ, 156, 123

    2018

  94. [103]

    2021, title Gaia EDR3 view on galactic globular clusters , , 505, 5978, 10.1093/mnras/stab1475

    Vasiliev , E., & Baumgardt , H. 2021, title Gaia EDR3 view on galactic globular clusters , , 505, 5978, 10.1093/mnras/stab1475

    2021 doi

  95. [104]

    E., et al

    Virtanen, P., Gommers, R., Oliphant, T. E., et al. 2020, title SciPy 1.0: Fundamental Algorithms for Scientific Computing in Python , Nature Methods, 17, 261

    2020

  96. [105]

    C., & Varoquaux, G

    Walt van van der Walt, S., Colbert, S. C., & Varoquaux, G. 2011, title The NumPy Array: A Structure for Efficient Numerical Computation , arXiv, 13, 22

    2011

  97. [106]

    H., Baumgardt, H., et al

    Wan, Z., Oliver, W. H., Baumgardt, H., et al. 2021, title The dynamics of the globular cluster NGC 3201 out to the Jacobi radius, , 502, 4513, 10.1093/mnras/stab306

    2021 doi

  98. [107]

    D., Oliver, W

    Wan, Z., Arnold, A. D., Oliver, W. H., et al. 2022, title Dynamics in the outskirts of four Milky Way globular clusters: it's the tides that dominate, Monthly Notices of the Royal Astronomical Society, 519, 192, 10.1093/mnras/stac3566

    2022 doi

  99. [108]

    C., K ro g lu , F., Fragione , G., et al

    Weatherford , N. C., K ro g lu , F., Fragione , G., et al. 2023, title Stellar Escape from Globular Clusters. I. Escape Mechanisms and Properties at Ejection , , 946, 104, 10.3847/1538-4357/acbcc1

    2023 doi

  100. [109]

    2023, title The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272) , , 953, 130, 10.3847/1538-4357/acdee2

    Yang , Y., Zhao , J.-K., Tang , X.-Z., Ye , X.-H., & Zhao , G. 2023, title The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272) , , 953, 130, 10.3847/1538-4357/acdee2

    2023 doi

  101. [110]

    D., Johnston , K

    Yavetz , T. D., Johnston , K. V., Pearson , S., Price-Whelan , A. M., & Hamilton , C. 2023, title Stream Fanning and Bifurcations: Observable Signatures of Resonances in Stellar Stream Morphology , , 954, 215, 10.3847/1538-4357/ace7b9

    2023 doi

  102. [111]

    2012, title LAMOST spectral survey An overview , Research in Astronomy and Astrophysics, 12, 723, 10.1088/1674-4527/12/7/002

    Zhao , G., Zhao , Y.-H., Chu , Y.-Q., Jing , Y.-P., & Deng , L.-C. 2012, title LAMOST spectral survey An overview , Research in Astronomy and Astrophysics, 12, 723, 10.1088/1674-4527/12/7/002

    2012 doi

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Reviewed August 6, 2026 · model on record in the stance chip above.