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arxiv: 2605.07918 · v1 · submitted 2026-05-08 · 🌌 astro-ph.GA

Recognition: no theorem link

Constraining the Galactic bar using the M92 stellar stream

Amanda Bystr\"om , Sergey E. Koposov , Ting. S. Li , Constance M. Rockosi , Arjun Dey , Guillaume F. Thomas , Raymond G. Carlberg , Oleg Y. Gnedin
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Namitha Kizhuprakkat Mika Lambert Nasser Mohammed Gustavo E. Medina Joan Najita Alexander H. Riley Nathan R. Sandford Leandro Beraldo e Silva Jessica N. Aguilar Steven Ahlen Davide Bianchi David Brooks Todd Claybaugh Andrew P. Cooper Andrei Cuceu Axel de la Macorra Peter Doel Jaime E. Forero-Romero Satya Gontcho A Gontcho Gaston Gutierrez Richard Joyce Stephanie Juneau Anthony Kremin Martin Landriau Laurent Le Guillou Aaron Meisner Ramon Miquel Will J. Percival Francisco Prada Ignasi P\'erez-R\`afols Graziano Rossi Eusebio Sanchez David Schlegel Joseph H. Silber Gregory Tarl\'e Benjamin A. Weaver Hu Zou
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Pith reviewed 2026-05-11 03:31 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Milky Waystellar streamgalactic barpattern speedM92DESIglobular clustergalactic dynamics
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The pith

The M92 stellar stream constrains the Milky Way bar's pattern speed to 29.1 km s^{-1} kpc^{-1}.

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

Using new spectroscopic observations from DESI, the paper identifies members of the diffuse stellar stream associated with the globular cluster M92. These data reveal clear gradients in distance, proper motion, and radial velocity that match expectations for a stream perturbed by the galactic bar. By generating mock streams in a range of barred potentials and comparing them to the observations, the authors derive the bar's pattern speed and its rate of change. This provides an independent constraint on the inner Milky Way potential using a stellar stream for the first time.

Core claim

The M92 stream's observed spatial and kinematic properties are best matched by mock streams evolved in a Milky Way potential with a bar pattern speed of Ω = 29.1^{+0.7}_{-0.4} km s^{-1} kpc^{-1} and a time derivative Ω̇ = 0.7^{+3.5}_{-2.3} km s^{-1} kpc^{-1} Gyr^{-1}. This inference is obtained through probabilistic comparison of the stream data to simulations in different barred models, establishing stellar streams as viable probes for bar properties.

What carries the argument

Probabilistic matching of observed M92 stream members to mock streams simulated in barred galactic potentials with varying pattern speeds.

Load-bearing premise

The mock streams accurately represent the real M92 stream's evolution under the influence of the galactic bar's time-dependent potential.

What would settle it

If additional observations reveal that the stream's velocity gradients or spatial extent deviate significantly from those predicted by the best-fit bar model, the estimated pattern speed would be invalidated.

Figures

Figures reproduced from arXiv: 2605.07918 by Aaron Meisner, Alexander H. Riley, Amanda Bystr\"om, Andrei Cuceu, Andrew P. Cooper, Anthony Kremin, Arjun Dey, Axel de la Macorra, Benjamin A. Weaver, Constance M. Rockosi, David Brooks, Davide Bianchi, David Schlegel, Eusebio Sanchez, Francisco Prada, Gaston Gutierrez, Graziano Rossi, Gregory Tarl\'e, Guillaume F. Thomas, Gustavo E. Medina, Hu Zou, Ignasi P\'erez-R\`afols, Jaime E. Forero-Romero, Jessica N. Aguilar, Joan Najita, Joseph H. Silber, Laurent Le Guillou, Leandro Beraldo e Silva, Martin Landriau, Mika Lambert, Namitha Kizhuprakkat, Nasser Mohammed, Nathan R. Sandford, Oleg Y. Gnedin, Peter Doel, Ramon Miquel, Raymond G. Carlberg, Richard Joyce, Satya Gontcho A Gontcho, Sergey E. Koposov, Stephanie Juneau, Steven Ahlen, Ting. S. Li, Todd Claybaugh, Will J. Percival.

Figure 1
Figure 1. Figure 1: The density of the DECaLS photometric sample, after the initial stream selections described in Sec. 3.1 have been applied, shown in greyscale, and the DESI spectroscopic tertiary programme tiles are shown in blue. These DESI tiles are labelled from 1 to 6. The M92 GC is at the centre of the DESI tiles. MNRAS 000, 1–24 (2026) [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The initial selection of M92 stream stars. Left: The distribution of Gaia proper motions of the photometric sample, after a cut in parallax, Eq. 1, and CMD (shown on the right, Eq. 3), has been applied. The magenta dashed circle shows the cut in proper motion with a radius of 0.5 mas yr−1 , as given in Eq. 2. Right: The CMD of the photometric sample, after a cut in parallax, Eq. 1, and proper motions (show… view at source ↗
Figure 3
Figure 3. Figure 3: The distance modulus distribution computed using Eq. 5 as a function of 𝜙1 for all SGB candidate stars (grey points) and the spectro￾scopically selected stream members (black points), with the corresponding distance given on the right axis. The distance modulus track given in Eq. 6 is shown as a blue line and the integrated GC orbit is given as a dark blue dashed line. The five stars used for interpolating… view at source ↗
Figure 4
Figure 4. Figure 4: The CAMD of all stream star candidates, selected using the astrometric criteria given in Eqs. 1 and 2 and their distances corrected using Eq. 6, shown as a two-dimensional histogram. The overlaid dashed magenta box shows the CMD selection applied to the stream stars. 𝜇𝜙1 ,0 (𝜙1) = −0.09𝜙1 − 5, and (7) 𝜇𝜙2 ,0 (𝜙1) = 0.26𝜙1 + 0.25, (8) and they are subtracted from the respective proper motion directions. The… view at source ↗
Figure 5
Figure 5. Figure 5: Top row: The distribution in proper motions as a function of stream longitude 𝜙1, along the stream longitude (𝜇𝜙1 , top left) and stream latitude (𝜇𝜙2 , top right), after the selections in Eqs. 1 and 4 as well as the CMD selection have been applied. The two-dimensional histograms have been column-normalised. Bottom row: Same as the top row, but for when stars inside the dashed magenta lines in the other pr… view at source ↗
Figure 7
Figure 7. Figure 7: The radial velocity distribution as a function of stream longitude 𝜙1 of the spectroscopic sample after the astrometric selections in Eqs. 1, and 10 and 11 with 𝑛 = 2, as well as the metallicity selection given in Eq. 12, has been applied. The magenta dashed lines show the velocity selection region, given by Eq. 14 when 𝑛 = 2. data is not symmetric in 𝜙1, as it is longer and broader at 𝜙1 > 0 deg, which ca… view at source ↗
Figure 6
Figure 6. Figure 6: The metallicity and radial velocity distribution of the spectroscopic sample. Top: The entire sample, without any selections. Bottom: The sample, after photometric and astrometric selections have been applied, which makes the M92 overdensity around [Fe/H] = −2.35 dex and 𝑣𝑅 = −120 km s−1 stand out even more strongly, showing the efficacy of these stream selections. selections to the spectroscopic sample is… view at source ↗
Figure 8
Figure 8. Figure 8: The stream morphology of the spectroscopic sample after selections in parallax, CMD, proper motions, metallicity and radial velocity have been applied. In blue, the outline of the DESI tertiary programme tiles are shown. The integrated GC orbit is shown as a dark blue dashed line. The direction of the Galactic centre has been marked with an arrow. extending below the progenitor is matched very well by the … view at source ↗
Figure 9
Figure 9. Figure 9: Means and dispersions of the four stream observables stream latitude (top row), proper motion along the stream longitude (middle top row), proper motion along the stream latitude (middle bottom row) and radial velocity (bottom row), obtained by fitting Eq. 16 to stream members in bins of 𝜙1. Each row shows each of the four fitted observables as black points with corresponding error bars for each 𝜙1 bin. No… view at source ↗
Figure 10
Figure 10. Figure 10: The velocity dispersions of the stream as seen in [PITH_FULL_IMAGE:figures/full_fig_p013_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: The log-likelihoods from Eq. 18 across the (Ω¤ , Ω) grid of bar potential parameters in which we integrate our mock streams. Redder colours denote higher likelihood, and bluer colours denote lower likelihood. The bottom panel shows the area within the grey rectangle in the top panel (note also the change in colour scale). To estimate the bar parameters Ω¤ and Ω, we sample their joint posterior 𝑝(Ω¤ , Ω| ®… view at source ↗
Figure 12
Figure 12. Figure 12: The posteriors on the bar parameters Ω¤ (left panel) and Ω (right panel), shown in solid black. The grey solid and dashed lines show the median and percentiles of each parameter respectively. 4 2 0 2 2 [deg] 5.4 5.2 5.0 4.8 4.6 1 [mas yr 1 ] 4 2 0 2 4 1 [deg] 1.0 0.5 0.0 0.5 1.0 2 [mas yr 1 ] 4 2 0 2 4 1 [deg] 140 130 120 110 100 vR [k m s 1 ] [PITH_FULL_IMAGE:figures/full_fig_p016_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Mock stream generated in a potential with the best-fitting bar parameters, shown as a column-normalised histogram, The results from the mixture modelling of the observed stream is shown as aquamarine points, which corresponds to the left column of [PITH_FULL_IMAGE:figures/full_fig_p016_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: The stream progenitor orbit in different barred potentials, indicated at the top of each panel, in the bar co-rotating frame, colour-coded by lookback time. The bluest point shows the current position of M92. The bar density is shown as a black contour, and the bar’s major axis is shown as a dashed grey line. Top row: Orbits in potentials with bar parameters from the ridge of high likelihood bar parameter… view at source ↗
read the original abstract

Stellar streams are excellent probes of the gravitational potential in which they evolve. In the Milky Way (MW), globular cluster (GC) streams are routinely used to infer properties about time-dependent perturbations of the underlying potential. This implies that streams with Galactocentric radii small enough to be perturbed by the MW bar should offer constraints on it, such as its pattern speed, which currently has a wide range of values reported in the literature and is important when studying stellar kinematics. The GC M92 has a small pericentre and should be affected by the bar. It has a diffuse stellar stream, but confirming stream members has previously been hindered by a lack of spectroscopic data. In this paper, we use Dark Energy Spectroscopic Instrument (DESI) observations together with photometric and astrometric data to obtain spectroscopic members of the M92 stream for the first time. We identify a clear spatial distribution and gradients in distance moduli, proper motions, and radial velocities that confirm the stream's existence. We compare the observed stream to mock streams generated in different barred potentials and estimate the MW bar's pattern speed $\Omega = 29.1^{+0.7}_{-0.4}$ km s$^{-1}$ kpc$^{-1}$ and $\dot \Omega = 0.7^{+3.5}_{-2.3}$ km s$^{-1}$ kpc$^{-1}$ Gyr$^{-1}$. This is the first time a stellar stream is used to probabilistically infer these bar properties, and it opens up an exciting realm of inner Galactic potential characterisation using stellar streams.

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 / 3 minor

Summary. The paper reports the first spectroscopic confirmation of the M92 globular cluster stellar stream using DESI observations combined with photometric and astrometric data. It identifies a clear spatial distribution along with gradients in distance moduli, proper motions, and radial velocities. By generating and comparing mock streams evolved in different barred Galactic potentials to the observed data, the authors derive constraints on the Milky Way bar pattern speed of Ω = 29.1^{+0.7}_{-0.4} km s^{-1} kpc^{-1} and its derivative dot{Ω} = 0.7^{+3.5}_{-2.3} km s^{-1} kpc^{-1} Gyr^{-1}, presenting this as the first probabilistic inference of these bar properties from a stellar stream.

Significance. If the modeling assumptions hold, this work provides a novel and potentially powerful method for constraining the time-dependent inner Milky Way potential using stellar streams, which could help reconcile the wide range of bar pattern speed values reported in the literature from other techniques. The approach is extensible to other inner-Galaxy streams and represents a clear methodological advance, with the narrow uncertainty on Ω being a notable outcome of the probabilistic comparison.

major comments (2)
  1. [Mock stream generation and fitting] Mock stream generation (methods section): the inference of Ω and dot{Ω} is obtained by fitting mock streams evolved in barred potentials where bar shape, mass, orientation, and functional form are held fixed from literature values while only Ω and dot{Ω} are varied. No sensitivity tests or variations of these fixed parameters are shown; a mismatch between the assumed bar model and reality could systematically bias the recovered Ω value and its quoted 1σ interval, which is load-bearing for the central claim.
  2. [Data selection] Data selection and member identification (results section): the criteria used to select DESI spectroscopic members, including any cuts on radial velocity, proper motion, or metallicity, and quantitative estimates of contamination or completeness, are not presented in sufficient detail to assess whether the reported gradients could be affected by selection effects or interlopers.
minor comments (3)
  1. [Abstract] The abstract states that mock streams were generated in 'different barred potentials' but does not specify the number of models, the exact parameter variations, or the bar potential functional form employed.
  2. [Notation] Notation for the pattern speed derivative is inconsistent between the abstract (dot{Ω}) and the reported value; a uniform symbol should be used throughout.
  3. [Methods] The paper would benefit from an explicit statement of the assumed bar mass and orientation values taken from the literature in the mock generation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments and positive assessment of the significance of our work. We address each major comment below and are prepared to revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [Mock stream generation and fitting] Mock stream generation (methods section): the inference of Ω and dot{Ω} is obtained by fitting mock streams evolved in barred potentials where bar shape, mass, orientation, and functional form are held fixed from literature values while only Ω and dot{Ω} are varied. No sensitivity tests or variations of these fixed parameters are shown; a mismatch between the assumed bar model and reality could systematically bias the recovered Ω value and its quoted 1σ interval, which is load-bearing for the central claim.

    Authors: We thank the referee for this important observation. Our analysis deliberately fixed the bar shape, mass, orientation, and functional form to standard literature values in order to isolate the constraints on pattern speed Ω and its time derivative, which are the quantities of primary interest for probing the time-dependent inner potential. We agree, however, that the absence of sensitivity tests leaves open the possibility of systematic bias in the reported Ω interval if the adopted bar model differs from reality. In the revised manuscript we will add an appendix (or expanded methods subsection) presenting results from additional mock-stream runs in which bar mass and shape are varied within published ranges; we will quantify the resulting shifts in the recovered Ω posterior and discuss the robustness of our central value. revision: yes

  2. Referee: [Data selection] Data selection and member identification (results section): the criteria used to select DESI spectroscopic members, including any cuts on radial velocity, proper motion, or metallicity, and quantitative estimates of contamination or completeness, are not presented in sufficient detail to assess whether the reported gradients could be affected by selection effects or interlopers.

    Authors: We agree that the current description of the spectroscopic member selection is insufficient for full reproducibility and for evaluating possible selection biases. In the revised results section we will provide the precise numerical cuts applied to the DESI data (radial velocity, proper-motion, metallicity, and any additional quality or photometric criteria), together with quantitative estimates of contamination (e.g., expected field-star or interloper fractions derived from control fields or statistical modeling) and completeness (e.g., recovery rates from injected mock members). These additions will allow readers to assess whether the reported spatial and kinematic gradients are robust against selection effects. revision: yes

Circularity Check

0 steps flagged

No significant circularity; inference is data-driven fitting of bar parameters

full rationale

The derivation proceeds by identifying M92 stream members via DESI spectroscopy plus photometry/astrometry, then generating mock streams in barred potentials and performing probabilistic comparison to constrain Ω and dotΩ. This is a standard parameter inference step whose output values are not equivalent to the inputs by construction; the mocks are forward models, not tautological rearrangements of the data. No load-bearing self-citations, uniqueness theorems, or ansatzes imported from prior author work are invoked to force the result. The central claim remains an empirical constraint whose validity rests on the fidelity of the mock generation rather than definitional equivalence.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on the assumption that the M92 stream's observed phase-space distribution is dominated by the bar's time-dependent perturbation rather than other effects such as the disk or halo substructure. The bar potential model parameters (shape, strength, pattern speed) are fitted rather than derived. No new particles or forces are introduced.

free parameters (2)
  • bar pattern speed Ω
    Fitted to match the observed stream gradients; reported as the primary result with asymmetric uncertainties.
  • bar pattern speed derivative dot{Ω}
    Fitted simultaneously; allows for a slowly changing bar speed.
axioms (2)
  • domain assumption The gravitational potential can be decomposed into a time-dependent barred component plus a static axisymmetric background.
    Invoked when generating mock streams in different barred potentials.
  • domain assumption Identified spectroscopic members accurately trace the true stream orbit without significant contamination.
    Required for the spatial and velocity gradients to constrain the bar.

pith-pipeline@v0.9.0 · 5803 in / 1427 out tokens · 35600 ms · 2026-05-11T03:31:10.488348+00:00 · methodology

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Works this paper leans on

172 extracted references · 172 canonical work pages · 3 internal anchors

  1. [1]

    , keywords =

    BV Photometry of RR Lyrae Variables in the Globular Cluster M92. , keywords =. doi:10.1086/132956 , adsurl =

    work page doi:10.1086/132956

  2. [2]

    , keywords =

    Gaia EDR3 view on galactic globular clusters. , keywords =. doi:10.1093/mnras/stab1475 , archivePrefix =. 2102.09568 , primaryClass =

    work page doi:10.1093/mnras/stab1475

  3. [3]

    1999, XSPEC: An X-ray spectral fitting package,, Astrophysics Source Code Library, record ascl:9910.005 http://ascl.net/9910.005 Astropy Collaboration, Robitaille, T

    Astropy: A community Python package for astronomy. , keywords =. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page doi:10.1051/0004-6361/201322068

  4. [4]

    The Astronomical Journal , author =

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    work page doi:10.3847/1538-3881/aabc4f

  5. [5]

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/ac7c74

  6. [6]

    R., Millman, K

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

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

  7. [7]

    Price-Whelan , title =

    Adrian M. Price-Whelan , title =. doi:10.21105/joss.00388 , url =

    work page doi:10.21105/joss.00388

  8. [8]

    Adrian Price-Whelan and Brigitta Sipőcz and Daniel Lenz and Johnny Greco and Nathaniel Starkman and Dan Foreman-Mackey and P. L. Lim and Semyeong Oh and Sergey Koposov and Syrtis Major , title =. doi:10.5281/zenodo.4159870 , url =

    work page doi:10.5281/zenodo.4159870

  9. [9]

    Eric Jones and Travis Oliphant and Pearu Peterson and others , title =

    work page

  10. [10]

    and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and

    Virtanen, Pauli and Gommers, Ralf and Oliphant, Travis E. and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and. Nature Methods , year =

    work page

  11. [11]

    C., Varoquaux G., 2011, @doi [Computing in Science Engineering] 10.1109/MCSE.2011.37 , 13, 22

    The NumPy Array: A Structure for Efficient Numerical Computation. Computing in Science and Engineering , keywords =. doi:10.1109/MCSE.2011.37 , archivePrefix =. 1102.1523 , primaryClass =

    work page doi:10.1109/mcse.2011.37 2011

  12. [12]

    D., 2007, @doi [Computing in Science Engineering] 10.1109/MCSE.2007.55 , 9, 90

    Matplotlib: A 2D Graphics Environment. Computing in Science and Engineering , keywords =. doi:10.1109/MCSE.2007.55 , adsurl =

    work page doi:10.1109/mcse.2007.55 2007

  13. [13]

    , keywords =

    Constraining the Milky Way Potential with a Six-Dimensional Phase-Space Map of the GD-1 Stellar Stream. , keywords =. doi:10.1088/0004-637X/712/1/260 , archivePrefix =. 0907.1085 , primaryClass =

    work page doi:10.1088/0004-637x/712/1/260

  14. [14]

    , keywords =

    Broken into Pieces: ATLAS and Aliqa Uma as One Single Stream. , keywords =. doi:10.3847/1538-4357/abeb18 , archivePrefix =. 2006.10763 , primaryClass =

    work page doi:10.3847/1538-4357/abeb18 2006

  15. [15]

    The Astrophysical Journal , volume=

    The field of streams: Sagittarius and its siblings , author=. The Astrophysical Journal , volume=. 2006 , publisher=

    work page 2006

  16. [16]

    Martin and Nick Kaiser and Klaus Hodapp and Kenneth C

    Nina Hernitschek and Branimir Sesar and Hans-Walter Rix and Vasily Belokurov and David Martinez-Delgado and Nicolas F. Martin and Nick Kaiser and Klaus Hodapp and Kenneth C. Chambers and Richard Wainscoat and Eugene Magnier and Rolf-Peter Kudritzki and Nigel Metcalfe and Peter W. Draper , title =. 2017 , month =. doi:10.3847/1538-4357/aa960c , url =

    work page doi:10.3847/1538-4357/aa960c 2017

  17. [17]

    Charting the Galactic Acceleration Field. I. A Search for Stellar Streams with Gaia DR2 and EDR3 with Follow-up from ESPaDOnS and UVES. , keywords =. doi:10.3847/1538-4357/abfcc2 , archivePrefix =. 2012.05245 , primaryClass =

    work page doi:10.3847/1538-4357/abfcc2 2012

  18. [18]

    , keywords =

    A deeper look at the GD1 stream: density variations and wiggles. , keywords =. doi:10.1093/mnras/sty677 , archivePrefix =. 1801.08948 , primaryClass =

    work page doi:10.1093/mnras/sty677

  19. [19]

    , keywords =

    S ^ 5 : The Orbital and Chemical Properties of One Dozen Stellar Streams. , keywords =. doi:10.3847/1538-4357/ac46d3 , archivePrefix =. 2110.06950 , primaryClass =

    work page doi:10.3847/1538-4357/ac46d3

  20. [20]

    , keywords =

    Exploring the interaction between the MW and LMC with a large sample of blue horizontal branch stars from the DESI survey. , keywords =. doi:10.1093/mnras/staf1219 , archivePrefix =. 2410.09149 , primaryClass =

    work page doi:10.1093/mnras/staf1219

  21. [21]

    , keywords =

    The Hidden Past of M92: Detection and Characterization of a Newly Formed 17 Long Stellar Stream Using the Canada-France Imaging Survey. , keywords =. doi:10.3847/1538-4357/abb6f7 , archivePrefix =. 2009.04487 , primaryClass =

    work page doi:10.3847/1538-4357/abb6f7 2009

  22. [22]

    , keywords =

    Mean proper motions, space orbits, and velocity dispersion profiles of Galactic globular clusters derived from Gaia DR2 data. , keywords =. doi:10.1093/mnras/sty2997 , archivePrefix =. 1811.01507 , primaryClass =

    work page doi:10.1093/mnras/sty2997

  23. [23]

    , keywords =

    Intrinsic iron spread and a new metallicity scale for globular clusters. , keywords =. doi:10.1051/0004-6361/200913003 , archivePrefix =. 0910.0675 , primaryClass =

    work page doi:10.1051/0004-6361/200913003

  24. [24]

    , keywords =

    The eye of Gaia on globular clusters structure: tidal tails. , keywords =. doi:10.1093/mnras/staa1209 , archivePrefix =. 2004.13754 , primaryClass =

    work page doi:10.1093/mnras/staa1209 2004

  25. [25]

    , keywords =

    Testing kinematic distances under a realistic Galactic potential: Investigating systematic errors in the kinematic distance method arising from a non-axisymmetric potential. , keywords =. doi:10.1051/0004-6361/202450000 , archivePrefix =. 2403.18000 , primaryClass =

    work page doi:10.1051/0004-6361/202450000

  26. [26]

    2019, MNRAS, 482, 1525, doi: 10.1093/mnras/sty2672

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

    work page doi:10.1093/mnras/sty2672

  27. [27]

    2017, MNRAS, 465, 1621, doi: 10.1093/mnras/stw2819

    Dynamical modelling of the galactic bulge and bar: the Milky Way's pattern speed, stellar and dark matter mass distribution. , keywords =. doi:10.1093/mnras/stw2819 , archivePrefix =. 1608.07954 , primaryClass =

    work page doi:10.1093/mnras/stw2819

  28. [28]

    2022b, MNRAS, 514, L1, doi: 10.1093/mnrasl/slac046

    The stellar mass distribution of the Milky Way's bar: an analytical model. , keywords =. doi:10.1093/mnrasl/slac046 , archivePrefix =. 2204.13114 , primaryClass =

    work page doi:10.1093/mnrasl/slac046

  29. [29]

    , keywords =

    Rotation Curve of the Milky Way from Classical Cepheids. , keywords =. doi:10.3847/2041-8213/aaf73f , archivePrefix =. 1810.02131 , primaryClass =

    work page doi:10.3847/2041-8213/aaf73f 2041

  30. [30]

    , keywords =

    The Circular Velocity Curve of the Milky Way from 5 to 25 kpc. , keywords =. doi:10.3847/1538-4357/aaf648 , archivePrefix =. 1810.09466 , primaryClass =

    work page doi:10.3847/1538-4357/aaf648

  31. [31]

    Weighing the Galactic disk using phase-space spirals. III. Probing distant regions of the disk using the Gaia EDR3 proper motion sample. , keywords =. doi:10.1051/0004-6361/202142819 , archivePrefix =. 2111.13707 , primaryClass =

    work page doi:10.1051/0004-6361/202142819

  32. [32]

    2013, ApJ, 779, 115, doi: 10.1088/0004-637X/779/2/115 Chanam´ e, J., Kleyna, J., & van der Marel, R

    A Direct Dynamical Measurement of the Milky Way's Disk Surface Density Profile, Disk Scale Length, and Dark Matter Profile at 4 kpc < -0.5ex R < -0.5ex 9 kpc. , keywords =. doi:10.1088/0004-637X/779/2/115 , archivePrefix =. 1309.0809 , primaryClass =

    work page doi:10.1088/0004-637x/779/2/115

  33. [33]

    , keywords =

    Milky Way dynamics in light of Gaia. , keywords =. doi:10.1016/j.newar.2024.101721 , archivePrefix =. 2501.04075 , primaryClass =

    work page doi:10.1016/j.newar.2024.101721 2024

  34. [34]

    , keywords =

    Improved Particle Spray Algorithm for Modeling Globular Cluster Streams. , keywords =. doi:10.3847/1538-4365/ad9904 , archivePrefix =. 2408.01496 , primaryClass =

    work page doi:10.3847/1538-4365/ad9904

  35. [35]

    Monthly Notices of the Royal Astronomical Society , author =

    A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters. , keywords =. doi:10.1093/mnras/sty1057 , archivePrefix =. 1804.08359 , primaryClass =

    work page doi:10.1093/mnras/sty1057

  36. [36]

    , keywords =

    S ^ 5 : Probing the Milky Way and Magellanic Clouds potentials with the 6D map of the Orphan-Chenab stream. , keywords =. doi:10.1093/mnras/stad551 , archivePrefix =. 2211.04495 , primaryClass =

    work page doi:10.1093/mnras/stad551

  37. [37]

    dynesty: a dynamic nested sampling package for estimating Bayesian posteriors and evidences

    DYNESTY: a dynamic nested sampling package for estimating Bayesian posteriors and evidences. , keywords =. doi:10.1093/mnras/staa278 , archivePrefix =. 1904.02180 , primaryClass =

    work page doi:10.1093/mnras/staa278 1904

  38. [38]

    doi:10.5281/zenodo.12537467 , version =

    joshspeagle/dynesty: v2.1.4. doi:10.5281/zenodo.12537467 , version =

    work page doi:10.5281/zenodo.12537467

  39. [39]

    Nested Sampling. Bayesian Inference and Maximum Entropy Methods in Science and Engineering: 24th International Workshop on Bayesian Inference and Maximum Entropy Methods in Science and Engineering , year = 2004, editor =. doi:10.1063/1.1835238 , adsurl =

    work page doi:10.1063/1.1835238 2004

  40. [40]

    Bayesian Analysis , author =

    Nested sampling for general. Bayesian Analysis , author =. 2006 , note =. doi:10.1214/06-BA127 , abstract =

    work page doi:10.1214/06-ba127 2006

  41. [41]

    arXiv:1704.03459

    Dynamic nested sampling: an improved algorithm for parameter estimation and evidence calculation , volume =. Statistics and Computing , author =. 2019 , pages =. doi:10.1007/s11222-018-9844-0 , abstract =

    work page doi:10.1007/s11222-018-9844-0 2019

  42. [42]

    , keywords =

    ESCARGOT: Mapping Vertical Phase Spiral Characteristics Throughout the Real and Simulated Milky Way. , keywords =. doi:10.3847/1538-4357/acf1fc , archivePrefix =. 2302.09086 , primaryClass =

    work page doi:10.3847/1538-4357/acf1fc

  43. [43]

    adrn/gala: v1.9.1 , url =

    Price-Whelan, Adrian and Souchereau, Harrison and Wagg, Tom and Sipőcz, Brigitta and Starkman, Nathaniel and Chen, Yingtian and Lilleengen, Sophia and. adrn/gala: v1.9.1 , url =. 2024 , doi =

    work page 2024

  44. [44]

    The Southern clusters and overview

    Homogeneous analysis of globular clusters from the APOGEE survey with the BACCHUS code - II. The Southern clusters and overview. , keywords =. doi:10.1093/mnras/stz3496 , archivePrefix =. 1912.04839 , primaryClass =

    work page doi:10.1093/mnras/stz3496 1912

  45. [45]

    2010 , month = jul, journal =

    Was the progenitor of the Sagittarius stream a disc galaxy?. , keywords =. doi:10.1111/j.1745-3933.2010.00921.x , archivePrefix =. 1007.1485 , primaryClass =

    work page doi:10.1111/j.1745-3933.2010.00921.x 2010

  46. [46]

    Implementing the Nelder-Mead simplex algorithm with adaptive parameters , volume =

    Gao, Fuchang and Han, Lixing , year =. Implementing the Nelder-Mead simplex algorithm with adaptive parameters , volume =. Computational Optimization and Applications , doi =

    work page

  47. [47]

    , keywords =

    galstreams: A library of Milky Way stellar stream footprints and tracks. , keywords =. doi:10.1093/mnras/stad321 , archivePrefix =. 2204.10326 , primaryClass =

    work page doi:10.1093/mnras/stad321

  48. [48]

    , keywords =

    Stellar streams in the Gaia era. , keywords =. doi:10.1016/j.newar.2024.101713 , archivePrefix =. 2405.19410 , primaryClass =

    work page doi:10.1016/j.newar.2024.101713 2024

  49. [49]

    , keywords =

    Insights into Pre-enrichment of Star Clusters and Self-enrichment of Dwarf Galaxies from Their Intrinsic Metallicity Dispersions. , keywords =. doi:10.1088/0004-6256/144/6/183 , archivePrefix =. 1209.4648 , primaryClass =

    work page doi:10.1088/0004-6256/144/6/183

  50. [50]

    , keywords =

    Connecting the Milky Way potential profile to the orbital time-scales and spatial structure of the Sagittarius Stream. , keywords =. doi:10.1093/mnras/sty3428 , archivePrefix =. 1804.04995 , primaryClass =

    work page doi:10.1093/mnras/sty3428

  51. [51]

    , keywords =

    Constraining the potential of the Milky Way using stellar streams and the Inverse Time Integration method. , keywords =. doi:10.1093/mnras/staf658 , archivePrefix =. 2412.15091 , primaryClass =

    work page doi:10.1093/mnras/staf658

  52. [52]

    , keywords =

    Galactic Accelerations from the GD-1 Stream Suggest a Tilted Dark Matter Halo. , keywords =. doi:10.3847/2041-8213/add0a9 , archivePrefix =. 2504.07187 , primaryClass =

    work page doi:10.3847/2041-8213/add0a9 2041

  53. [53]

    W., & Ebeling, H

    The mechanics of tidal streams. , keywords =. doi:10.1111/j.1365-2966.2011.18270.x , archivePrefix =. 1011.3672 , primaryClass =

    work page doi:10.1111/j.1365-2966.2011.18270.x 2011

  54. [54]

    W., & Ebeling, H

    More on the structure of tidal tails , volume =. , author =. 2012 , note =. doi:10.1111/j.1365-2966.2011.20242.x , abstract =

    work page doi:10.1111/j.1365-2966.2011.20242.x 2012

  55. [55]

    and Wilkinson, M

    On the structure of tidal tails , volume =. , author =. 2008 , pages =. doi:10.1111/j.1365-2966.2008.13323.x , abstract =

    work page doi:10.1111/j.1365-2966.2008.13323.x 2008

  56. [56]

    Nature Astronomy , keywords =

    Gaps and length asymmetry in the stellar stream Palomar 5 as effects of Galactic bar rotation. Nature Astronomy , keywords =. doi:10.1038/s41550-017-0220-3 , archivePrefix =. 1703.04627 , primaryClass =

    work page doi:10.1038/s41550-017-0220-3

  57. [57]

    The case of the tidal stream of the Hyades

    Impact of the Galactic bar on tidal streams within the Galactic disc. The case of the tidal stream of the Hyades. , keywords =. doi:10.1051/0004-6361/202346650 , archivePrefix =. 2309.05733 , primaryClass =

    work page doi:10.1051/0004-6361/202346650

  58. [58]

    , keywords =

    Spending Too Much Time at the Galactic Bar: Chaotic Fanning of the Ophiuchus Stream. , keywords =. doi:10.3847/0004-637X/824/2/104 , archivePrefix =. 1601.06790 , primaryClass =

    work page doi:10.3847/0004-637x/824/2/104

  59. [59]

    , keywords =

    Gaps in globular cluster streams: giant molecular clouds can cause them too. , keywords =. doi:10.1093/mnrasl/slw148 , archivePrefix =. 1606.02715 , primaryClass =

    work page doi:10.1093/mnrasl/slw148

  60. [60]

    , keywords =

    A sharper view of Pal 5's tails: discovery of stream perturbations with a novel non-parametric technique. , keywords =. doi:10.1093/mnras/stx1208 , archivePrefix =. 1609.01282 , primaryClass =

    work page doi:10.1093/mnras/stx1208

  61. [61]

    , keywords =

    Effects of baryonic and dark matter substructure on the Pal 5 stream. , keywords =. doi:10.1093/mnras/stz142 , archivePrefix =. 1809.09640 , primaryClass =

    work page doi:10.1093/mnras/stz142

  62. [62]

    , keywords =

    The effect of the deforming dark matter haloes of the Milky Way and the Large Magellanic Cloud on the Orphan-Chenab stream. , keywords =. doi:10.1093/mnras/stac3108 , archivePrefix =. 2205.01688 , primaryClass =

    work page doi:10.1093/mnras/stac3108

  63. [63]

    , keywords =

    LMC Calls, Milky Way Halo Answers: Disentangling the Effects of the MW LMC Interaction on Stellar Stream Populations. , keywords =. doi:10.3847/1538-4357/ad93a7 , archivePrefix =. 2410.02574 , primaryClass =

    work page doi:10.3847/1538-4357/ad93a7

  64. [64]

    arXiv e-prints , keywords =

    Dancing Streams In Merging Halos: Stellar Streams in a MW--LMC-like merger. arXiv e-prints , keywords =. doi:10.48550/arXiv.2505.14792 , archivePrefix =. 2505.14792 , primaryClass =

    work page doi:10.48550/arxiv.2505.14792

  65. [65]

    , keywords =

    GD-1 and the Milky Way Starless Dark Matter Subhalos. , keywords =. doi:10.3847/1538-4357/adec91 , archivePrefix =. 2503.13290 , primaryClass =

    work page doi:10.3847/1538-4357/adec91

  66. [66]

    H., et al

    The merger that led to the formation of the Milky Way's inner stellar halo and thick disk. , keywords =. doi:10.1038/s41586-018-0625-x , archivePrefix =. 1806.06038 , primaryClass =

    work page doi:10.1038/s41586-018-0625-x

  67. [67]

    , keywords =

    A Comparative Study between M30 and M92: M92 is a Merger Remnant with a Large Helium Enhancement. , keywords =. doi:10.3847/1538-4357/ad12ca , archivePrefix =. 2312.02442 , primaryClass =

    work page doi:10.3847/1538-4357/ad12ca

  68. [68]

    , keywords =

    M92 (NGC 6341) Is a Metal-complex Globular Cluster with an Atypical Primordial Population. , keywords =. doi:10.3847/2041-8213/acd05a , archivePrefix =. 2305.02983 , primaryClass =

    work page doi:10.3847/2041-8213/acd05a 2041

  69. [69]

    A new algorithm for detecting stellar streams

    STREAMFINDER - I. A new algorithm for detecting stellar streams. , keywords =. doi:10.1093/mnras/sty912 , archivePrefix =. 1804.11338 , primaryClass =

    work page doi:10.1093/mnras/sty912

  70. [70]

    A., Ramsay, G., Andronov, I., et al

    Mass models of the Milky Way. , keywords =. doi:10.1046/j.1365-8711.1998.01282.x10.1111/j.1365-8711.1998.01282.x , archivePrefix =. astro-ph/9612059 , primaryClass =

    work page doi:10.1046/j.1365-8711.1998.01282.x10.1111/j.1365-8711.1998.01282.x 1998

  71. [71]

    , keywords =

    Disentangling the Galaxy's Gordian knot: evidence from APOGEE Gaia for a knotted and slower bar in the Milky Way. , keywords =. doi:10.1093/mnras/staf348 , archivePrefix =. 2402.07986 , primaryClass =

    work page doi:10.1093/mnras/staf348

  72. [72]

    , keywords =

    Riding the kinematic waves in the Milky Way disk with Gaia. , keywords =. doi:10.1051/0004-6361/201833494 , archivePrefix =. 1805.09790 , primaryClass =

    work page doi:10.1051/0004-6361/201833494

  73. [73]

    , keywords =

    Shepherding tidal debris with the Galactic bar: the Ophiuchus stream. , keywords =. doi:10.1093/mnras/stw1006 , archivePrefix =. 1512.04536 , primaryClass =

    work page doi:10.1093/mnras/stw1006

  74. [74]

    , keywords =

    Flipping of the Tidal Tails of the Ophiuchus Stream due to the Decelerating Galactic Bar. , keywords =. doi:10.3847/1538-4357/adc57c , archivePrefix =. 2503.19221 , primaryClass =

    work page doi:10.3847/1538-4357/adc57c

  75. [75]

    , keywords =

    A Larger Extent for the Ophiuchus Stream. , keywords =. doi:10.3847/1538-3881/ab8cbf , archivePrefix =. 2004.14350 , primaryClass =

    work page doi:10.3847/1538-3881/ab8cbf 2004

  76. [76]

    , keywords =

    The X-shaped Bulge of the Milky Way Revealed by WISE. , keywords =. doi:10.3847/0004-6256/152/1/14 , archivePrefix =. 1603.00026 , primaryClass =

    work page doi:10.3847/0004-6256/152/1/14

  77. [77]

    , keywords =

    The structure of the Milky Way's bar outside the bulge. , keywords =. doi:10.1093/mnras/stv745 , archivePrefix =. 1504.01401 , primaryClass =

    work page doi:10.1093/mnras/stv745

  78. [78]

    G., Hauser, M

    Morphology, Near-Infrared Luminosity, and Mass of the Galactic Bulge from COBE DIRBE Observations. , keywords =. doi:10.1086/175734 , adsurl =

    work page doi:10.1086/175734

  79. [79]

    , keywords =

    Dynamical streams in the local stellar halo. , keywords =. doi:10.1093/mnras/staf965 , archivePrefix =. 2503.02926 , primaryClass =

    work page doi:10.1093/mnras/staf965

  80. [80]

    , keywords =

    Stellar halo substructure generated by bar resonances. , keywords =. doi:10.1093/mnras/stad2136 , archivePrefix =. 2303.00008 , primaryClass =

    work page doi:10.1093/mnras/stad2136

Showing first 80 references.