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Mapping the Milky Way with Gaia Bp/Rp spectra-IV: the broken and asymmetric density profile of the stellar disk traced by a large sample of red clumps

T0 review · 3 major / 3 minor · reviewed 2026-05-08 · grok-4.3

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Pith's one-line read Gaia red clump stars map the Milky Way stellar disk as having four distinct radial density segments plus inner thickening and a localized bump.

desk verdict Gaia red-clump mapping gives a four-break radial disk profile plus inner flaring and a 5-7 kpc density bump, but everything rests on whether the selection and distance corrections are clean. read the letter →

arxiv 2604.24456 v1 submitted 2026-04-27 astro-ph.GA

Wenbo Wu , Yuqin Chen , Jianhui Lian , Martín López-Corredoira , Chengdong Li , Xianhao Ye , C. Allende Prieto , Xiang-Xiang Xue
show 5 more authors
Gang Zhao Jingkun Zhao David S. Aguado Jonay I. González Hernández Rafael Rebolo
This is my paper · ORCID
classification astro-ph.GA
keywords redclumpstarsMilkyWaystellardiskdensityprofileGaiaBp/Rpspectraradialbreaksflaringazimuthalasymmetrymetallicitybump
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

The paper uses roughly 8.4 million red clump stars selected from Gaia Bp/Rp spectra to trace the three-dimensional density of the Galactic stellar disk. After applying corrections for selection biases and distance errors, the authors model the vertical structure as a sum of geometrically thin and thick disks and extract the radial and azimuthal dependence. This yields a radial profile that breaks into a steep exponential decline inside 3 kpc, a nearly flat plateau between 3 and 7 kpc, a moderate exponential falloff out to 13 kpc, and a steeper cutoff beyond 13 kpc, with parameters that change with galactic azimuth. The thin disk also shows smooth thickening toward smaller radii inside 6.4 kpc, and a sector between 5 and 7 kpc and -30 to 15 degrees in azimuth contains both a density excess and a metallicity excess. A reader would care because these features record the combined effects of the central bar, radial migration, and past dynamical heating on the disk's present-day shape.

What carries the argument

Two-component vertical density model (thin plus thick geometrically defined disks) applied to selection-corrected star counts, which isolates the radial and azimuthal dependence of the underlying stellar density.

What would settle it

An independent re-derivation of distances or selection functions on the same Gaia red-clump sample that removes the reported radial breaks or shifts the location of the inner flaring and density bump by more than 1 kpc.

Watch

Extended reading notes

Core claim

Using approximately 8.4 million red clump stars from Gaia Bp/Rp spectra, after correcting for selection effects and distance uncertainties, the vertical stellar density profile of the Galactic disk is fit with a two-component model of geometrically thin and thick disks. The resulting radial density profile exhibits four breaks: a steep exponential inside R ~ 3 kpc, a nearly flat plateau from R ~ 3 to ~7 kpc, an exponential decline beyond the solar radius to around 13 kpc, and a sharper exponential drop-off beyond R ~ 13 kpc. The thin disk additionally shows a smooth thickening or flaring feature toward the Galactic center at R < 6.4 kpc, while a localized density bump appears in the region 5

Load-bearing premise

The corrections for selection effects and distance uncertainties are complete and unbiased so that the observed star counts accurately reflect the true underlying density profile.

Editorial extensions

If this is right

  • The termination radius of the steep inner component varies with azimuth, pointing to dynamical interaction with the bar or bulge.
  • The thin-disk thickening inside 6.4 kpc occurs near the bar's co-rotation radius and is therefore likely produced by bar-driven heating.
  • The localized density and metallicity bump between 5 and 7 kpc and -30° to 15° in azimuth is consistent with radial migration of super metal-rich stars.
  • All four radial components have azimuth-dependent parameters, so the disk density is not axisymmetric.

Reading between the lines

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

  • The broken profile supplies a concrete target for N-body simulations of Milky Way-like galaxies to reproduce without fine-tuning.
  • Repeating the same analysis with other Gaia tracers such as main-sequence turnoff stars could test whether the breaks are population-dependent.
  • The reported azimuthal asymmetry implies that local kinematic samples near the Sun may not represent the disk at other longitudes.
  • If the inner flaring is bar-driven, similar thickening should appear in external barred galaxies observed edge-on.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 3 minor

Summary. The manuscript analyzes ~8.4 million red-clump stars selected from Gaia Bp/Rp spectra to map the radial and azimuthal stellar density profile of the Milky Way disk. After applying corrections for selection effects and distance uncertainties, the authors fit a two-component (geometrically thin and thick) vertical density model and report four radial regimes: a steep exponential inside R~3 kpc, a plateau from ~3 to ~7 kpc, an exponential decline from the solar radius to ~13 kpc, and a sharper drop beyond 13 kpc. They additionally identify inner flaring of the thin disk at R<6.4 kpc, azimuthal dependence of the component parameters, and a localized density plus metallicity bump in the 5<R<7 kpc, -30°<φ<15° region, which they link to bar dynamics and radial migration.

Significance. If the selection-function and distance corrections prove unbiased, the work supplies one of the largest homogeneous samples for disk mapping and offers concrete observational constraints on bar-disk coupling and radial migration. The explicit use of public Gaia data and a two-component vertical decomposition are positive features that allow direct comparison with simulations.

major comments (3)
  1. [§3] §3 (Correction pipeline): The reported breaks at R≈3, 7, and 13 kpc and the 5–7 kpc azimuthal bump are derived directly from binned counts after the selection and distance corrections. No recovery tests on mock catalogs with known input density profiles are described, leaving open the possibility that residual radial dependence in completeness or distance posterior shifts could fabricate or suppress these features.
  2. [§4.2] §4.2 (Inner flaring): The claim that the thin disk exhibits smooth thickening toward the Galactic center at R<6.4 kpc (interpreted as bar-induced heating near co-rotation) rests on the two-component scale-height fit. No propagation of distance uncertainties into the fitted h_z(R) or quantitative comparison with an alternative single-component model is provided, which is load-bearing for the dynamical interpretation.
  3. [§4.3] §4.3 (Localized bump): The density and metallicity bump in 5<R<7 kpc, -30°<φ<15° is presented as a distinct feature potentially linked to radial migration. The manuscript does not report Poisson uncertainties on the binned counts, a statistical significance test against a smooth model, or a control test excluding the metallicity selection, making it difficult to assess whether the feature is robust.
minor comments (3)
  1. [Figure 3] Figure 3: The radial density profiles are shown without overlaid model curves or residual panels, making it hard to judge the quality of the four-component fit.
  2. [Notation] Notation: The symbol φ is used for azimuth without an explicit definition or reference to the adopted Galactic coordinate convention in the text.
  3. [Abstract] Abstract: The statement that 'the parameters of these four main components depend on φ to some extent' is not accompanied by a quantitative measure (e.g., fractional variation) in the main body.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive and detailed comments. We address each major point below and will incorporate revisions to strengthen the validation of our results.

read point-by-point responses

  1. Referee: [§3] §3 (Correction pipeline): The reported breaks at R≈3, 7, and 13 kpc and the 5–7 kpc azimuthal bump are derived directly from binned counts after the selection and distance corrections. No recovery tests on mock catalogs with known input density profiles are described, leaving open the possibility that residual radial dependence in completeness or distance posterior shifts could fabricate or suppress these features.

    Authors: We agree that explicit recovery tests using mock catalogs are a valuable addition for validating the correction pipeline. While the manuscript includes internal consistency checks (varying selection criteria and comparing distance methods), we did not describe full end-to-end recovery tests. In the revised version we will add a new subsection to §3 that generates mock catalogs with known input density profiles (including the reported breaks and bump), applies the full selection function and distance uncertainty model, and demonstrates recovery of the input features to within the reported uncertainties. This will directly address the concern that the features could be artifacts. revision: yes

  2. Referee: [§4.2] §4.2 (Inner flaring): The claim that the thin disk exhibits smooth thickening toward the Galactic center at R<6.4 kpc (interpreted as bar-induced heating near co-rotation) rests on the two-component scale-height fit. No propagation of distance uncertainties into the fitted h_z(R) or quantitative comparison with an alternative single-component model is provided, which is load-bearing for the dynamical interpretation.

    Authors: The two-component vertical model was adopted after explicit model comparison using BIC values, which favored the two-component fit over a single-component model by a large margin. Distance uncertainties for the red-clump sample are modest (∼5–10 %). In the revision we will propagate these uncertainties into the h_z(R) profiles via Monte Carlo resampling of the distance posteriors and will add a quantitative side-by-side comparison of the single- versus two-component fits, including the radial dependence of the scale heights. These additions will make the inner-flaring claim more robust and will support the dynamical interpretation. revision: yes

  3. Referee: [§4.3] §4.3 (Localized bump): The density and metallicity bump in 5<R<7 kpc, -30°<φ<15° is presented as a distinct feature potentially linked to radial migration. The manuscript does not report Poisson uncertainties on the binned counts, a statistical significance test against a smooth model, or a control test excluding the metallicity selection, making it difficult to assess whether the feature is robust.

    Authors: We will add Poisson uncertainties to all binned density counts in the revised figures and text. A formal statistical test comparing the observed counts against a smooth radial-plus-azimuthal model (with χ² or likelihood-ratio statistics) will be included. We will also present a control analysis that repeats the density mapping after removing the metallicity cut, confirming that the bump remains visible in the purely photometric/density selection. These changes will allow readers to evaluate the feature’s significance directly. revision: yes

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity in observational density mapping from corrected Gaia star counts

full rationale

The paper's derivation chain selects ~8.4 million red clump stars from Gaia Bp/Rp spectra, applies corrections for selection effects and distance uncertainties, bins the data radially and azimuthally, and fits a two-component (thin+thick) vertical density model to the corrected counts. The reported radial breaks (steep inner exponential, plateau 3-7 kpc, outer decline, sharp drop beyond 13 kpc), inner flaring, and localized 5-7 kpc bump are direct outputs of this empirical pipeline rather than quantities defined in terms of themselves, fitted parameters renamed as predictions, or load-bearing self-citations. No uniqueness theorems, ansatzes smuggled via prior work, or renaming of known results are invoked; the central claims remain self-contained mappings from the observed (corrected) star counts.

Assumptions & free parameters 2 free parameters · 2 assumptions · 0 invented entities

The central claims rest on empirical fitting of multiple parameters to corrected star counts and domain assumptions about the tracer population and data corrections.

free parameters (2)
  • radial break radii = 3 kpc, 7 kpc, 13 kpc
    Positions at approximately 3, 7, and 13 kpc determined by fitting the observed density profile
  • disk scale lengths and heights = various values
    Parameters for the thin and thick disk components fitted at different radii and azimuths
assumptions (2)
  • domain assumption Red clump stars serve as reliable tracers of the underlying stellar population density after selection
    Basis for using the 8.4 million stars selected from Gaia Bp/Rp spectra
  • domain assumption Selection effects and distance uncertainties can be corrected without introducing significant bias
    Explicitly stated as performed prior to fitting the density profile

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Cite this review

Pith. "Pith review of Mapping the Milky Way with Gaia Bp/Rp spectra-IV: the broken and asymmetric density profile of the stellar disk traced by a large sample of red clumps." pith.science (2026). https://pith.science/paper/2604.24456

@misc{pith2026260424456,
  author       = {Pith},
  title        = {Pith review of: Mapping the Milky Way with Gaia Bp/Rp spectra-IV: the broken and asymmetric density profile of the stellar disk traced by a large sample of red clumps},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/2604.24456}},
  note         = {Machine review of arXiv:2604.24456}
}
abstract

This study explores the density profile of the stellar disk, radially and azimuthally, based on approximately 8.4 million red clump stars selected from Gaia Bp/Rp spectra. After correcting for selection effects and distance uncertainties, we fit the vertical stellar density profile of the Galactic disk with a two-component model consisting of geometrically thin and thick disks. Our derived density profile shows several breaks radially: (1) a steep exponential inside R$\sim3$ kpc; (2) a nearly flat plateau from R$\sim3$ to $\sim7$ kpc; (3) an exponential decline beyond the solar radius to around 13 kpc; (4) a sharper exponential drop-off beyond R$\sim$13 kpc. The parameters of these four main components depend on $\phi$ to some extent. Variation of the termination radius of the first component suggests an interaction with the bar/bulge. Besides the typical flaring at $R>6.4$ kpc, we find that the thin disk also exhibits a similar and smooth thickening/flaring feature toward the Galactic center at $R<6.4$ kpc. The observed inner flaring may indicate heating effects introduced by the Galactic bar, since $R=6.4$ kpc lies close to the co-rotation radius where the bar's dynamical influence becomes significant. Additionally, we identify a localized density bump in the region $5<R<7$ kpc and $-30^\circ<\phi<15^\circ$, where a corresponding metallicity bump is also visible near the Galactic plane. This density/metallicity bump may be related to the recently reported bimodal distribution of the guiding radius of super metal-rich stars in the solar vicinity through radial migration.

Figures

Figures reproduced from arXiv: 2604.24456 by the authors.

Figure 1
Figure 1. Distributions of the primary RC (blue points), secondary RC (orange points), and RGB (green points) identified by M. Vrard et al. (2016) in the Teff −log g diagram. The stellar atmospheric parameters are provided by the APOGEE DR17 (top panel) and the An23 Gaia XP catalog (bottom panel). Two types of the dust map are frequently used in the astronomical researches: (1) a two-dimensional (2D) map where the extinction … view at source ↗
Figure 2
Figure 2. Selection of RCs in two specific metallicity bins. Top left panel shows the distributions of RGBs (blue points) and RCs (orange points) identified by Y.-S. Ting et al. (2018) in a bin of 0.2 < [M/H] < 0.3. A linear fit is applied to derive the Teff –log g relation for these RC stars. Two dashed lines, offset by ±0.15 dex in log g from the fitting line (shown in black), are used to include the majority of RCs within … view at source ↗
Figure 3
Figure 3. Density distributions of log g for the non-duplicated sources satisfying the Teff − log g selection criteria. According to the Ting18 catalog, some of them are identified as RCs (blue hist), while others are possibly RGBs (orange hist). We only retain the region where RCs dominate by requiring 2.3 < log g < 2.8. deviations of RCs differ slightly but all are around 0.2, which is a typical value of the intrinsic dispe… view at source ↗
Figures from the paper (23 more)
Figure 4
Figure 4. Figure 4: Density distribution of the RCs (top panel) and RGBs (bottom panel) on a logarithmic scale in [M/H]-MKs diagram. The black point represents the mean value, and the dashed black line is a cubic polynomial that describes MKs as a function of [M/H]. 3. SELECTION FUNCTION …
Figure 5
Figure 5. Figure 5: Comparison between our calculated heliocentric distance (drc) and the dist50 from F. Anders et al. (2022) for the selected RC sample. The two dashed lines indicates the boundaries of a 30% difference between the two types of distance ( |drc−dist50| drc = 0.3). We only …
Figure 6
Figure 6. Figure 6: Density distribution of the RC sample in the Sky positions (l, b) on a logarithmic scale with base 10. 0.0 2.5 5.0 7.5 10.0 12.5 15.0 17.5 20.0 R (kpc) 4 2 0 2 4 Z (kpc) 10 0 10 1 10 2 10 3 10 4
Figure 7
Figure 7. Figure 7: Density distribution of the RC sample in the R − Z diagram on a logarithmic scale. The location of the Sun is marked by a blue star
Figure 8
Figure 8. Figure 8: Density distribution of our RC candidates in the Galactocentric X − Y diagram, where the position of the Sun is indicated by a blue star. In this right-handed coordinate system, the azimuthal angle ϕ is measured from the center-Sun-an￾ticenter direction and rotates clo…
Figure 9
Figure 9. Figure 9: Azimuthal distribution (ϕ) of RC samples selected from the APOGEE survey (blue hist, J. Bovy et al. (2016b)), the LAMOST survey (orange hist, Y. Huang et al. (2020)), and Gaia XP spectra (green hist). RC sample obtained from Gaia XP spectra has a more completed coverag…
Figure 10
Figure 10. Figure 10: Map of the selection function for Gaia XP spectra using Gaia DR3 photometry as the reference for a bright (top panel) and a faint (bottom panel) magnitude. In the bottom panel we can see a lack of faint stars within |b| < 10◦ for XP spectra, which causes the deficienc…
Figure 11
Figure 11. Figure 11: Normalized density distributions of the RCs selected from XP spectra (blue normalized histogram, by us) and the combined LAMOST/APOGEE survey (orange histogram, by Y.-S. Ting et al. (2018)) in G − GRP (top panel) color and G (bottom panel) band magnitude. The green hi…
Figure 12
Figure 12. Figure 12: Completeness (black dashed lines) and purity (black solid lines) as a function of G estimated from a direct comparison with the Ting18 catalog. A one-dimensional quadratic polynomial fit is applied to both completeness and purity, and the resulting functions are used …
Figure 13
Figure 13. Figure 13: Averaged SRC in X − Y panel of our RC sample. The pixel size is 0.1 × 0.1. as follows: mKs − MKs ∼ P(G)N (⟨mKs ⟩ − ⟨MKs ⟩, σmKs 2 + σMKs 2 ) + (1 − P(G))N (⟨mKs ⟩ − ⟨MKs;RGB⟩, σmKs 2 + σMKs;RGB 2 ) (7) where P(G) is the purity as a function of G magnitude. In
Figure 14
Figure 14. Figure 14: Density distribution of RCs in three certain bins of 3.75 < R < 4.0 kpc (top panel, near the bar/bulge), 7.75 < R < 8.0 kpc (middle panel, in the solar neighborhood),and 14.5 < R < 15.5 kpc (bottom panel, in the outer disk) in Z − ln ν panel. The black points represen…
Figure 15
Figure 15. Figure 15: Corner plot of the five free parameters in the regions of 7.75 < R < 8.0 kpc. The dashed lines show the 16th, 50th, and 84th percentiles of the marginalized distribution of each parameter. R thanks to the large number of stars inside the solar radius. From R = 8 to 11…
Figure 16
Figure 16. Figure 16: Vertical density distribution (points) and best fitting results (black lines) for RC sample of different bins of ϕ. In each sub figure, the differently colored points represent the vertical density distributions at increasing radii from the inner to outer disk: R =2.1…
Figure 17
Figure 17. Figure 17: Scale height of the thin disk as a function of R for different bins of ϕ, which presents a V-shaped pattern flaring both inside and outside. Yellow lines are results of M. L´opez-Corredoira et al. (2004) with an systematic offset of -0.04 corrected, which also display…
Figure 18
Figure 18. Figure 18: Scale height of the thick disk as a function of R for different bins of ϕ. It increases steadily from ∼ 0.50 kpc at R = 2 kpc to ∼ 0.75 kpc in the solar neighborhood
Figure 19
Figure 19. Figure 19: Fraction of the geometric thin disk as a function of R for different bins of ϕ. However, we note that f0 has a large uncertainty at R > 12 kpc for several bins, which might be caused by the worse fitting in the remoter disk as shown in
Figure 20
Figure 20. Figure 20: Warp parameter Z0 as a function of R. We can see a clear down warp at bins of ϕ < 15◦ beyond R ∼ 8 kpc. However, at bins of ϕ > 15◦ , the upward warp is absent at R > 12 kpc, which might be introduced by the lack of near-plane stars and the bad fitting of the vertical…
Figure 21
Figure 21. Figure 21: Mid-plane (ln ν0, top panel) and surface (ln Σ, bottom panel) density profiles as a function of R. Both of them can be well described by a combination of four main components with an additional density bump at 5 < R < 7 kpc. hR;bar is the scale length of the first com…
Figure 22
Figure 22. Figure 22: Surface density profile ln Σ as a function of R for six different bins of ϕ. Except for the bin of −60◦ < ϕ < −30◦ , the conclusion that ln Σ is composed of four main components remains unchanged, but the specific parameters exhibit some degree of dependence on the az…
Figure 23
Figure 23. Figure 23: Distributions of mean metallicity ⟨[M/H]⟩ in the X − Y diagram for RCs with |Z| < 1 kpc, |Z| < 0.15 kpc, 0.15 < |Z| < 1 kpc, and 0.5 < |Z| < 1 kpc (in each row, respectively). We can notice a metallicity bump at around −7 < X < −5 kpc and −4 < Y < 2 kpc in the left tw…
Figure 24
Figure 24. Figure 24: Surface density profile ln Σ as a function of R for six different bins of ϕ after removing data points of |Z| < 0.15 kpc during the fitting process. The density bump and the additional break mentioned in
Figure 25
Figure 25. Figure 25: Normalized density distributions of Rg (top panel) and R (bottom panel) for stars of 0.25 < [M/H] < 0.5 (left panel), 0.1 < [M/H] < 0.25 (middle panel), and [M/H] < 0.1 (right panel) in two different bins of 0◦ < ϕ < 15◦ (blue hist) and −15◦ < ϕ < 0 ◦ (orange hist). T…
Figure 26
Figure 26. Figure 26: Normalized density distributions of Rg (top panel) and R (bottom panel) for stars with 0.25 < [M/H] < 0.5 (left panel), 0.1 < [M/H] < 0.25 (middle panel), and [M/H] < 0.1 (right panel) in two different bins of 15◦ < ϕ < 30◦ (blue hist) and −30◦ < ϕ < −15◦ (orange hist…

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Works this paper leans on

150 extracted references · 150 canonical work pages

  1. [1]

    K., Ag¨ ueros, M

    Abazajian, K., Adelman-McCarthy, J. K., Ag¨ ueros, M. A., et al. 2004, AJ, 128, 502, doi: 10.1086/421365

    work page doi:10.1086/421365 2004

  2. [2]

    THE EIGHTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST DATA FROM SDSS-III

    Aihara, H., Allende Prieto, C., An, D., et al. 2011, ApJS, 193, 29, doi: 10.1088/0067-0049/193/2/29

    work page doi:10.1088/0067-0049/193/2/29 2011

  3. [3]

    Alves, D. R. 2000, ApJ, 539, 732, doi: 10.1086/309278 Amˆ ores, E. B., Robin, A. C., & Reyl´ e, C. 2017, A&A, 602, A67, doi: 10.1051/0004-6361/201628461

    work page doi:10.1086/309278 2000

  4. [4]

    C., & Chiti , A

    An, D., Beers, T. C., & Chiti, A. 2024, ApJS, 272, 20, doi: 10.3847/1538-4365/ad3641

    work page doi:10.3847/1538-4365/ad3641 2024

  5. [5]

    Anders, F., Khalatyan, A., Queiroz, A. B. A., et al. 2022, A&A, 658, A91, doi: 10.1051/0004-6361/202142369

    work page doi:10.1051/0004-6361/202142369 2022

  6. [6]

    Robust Data-driven Metallicities for 175 Million Stars from Gaia XP Spectra

    Andrae, R., Rix, H.-W., & Chandra, V. 2023, ApJS, 267, 8, doi: 10.3847/1538-4365/acd53e Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-3881/aabc4f

    work page doi:10.3847/1538-4365/acd53e 2023

  7. [7]

    10.1051/0004-6361/200810860

    Auvergne, M., Bodin, P., Boisnard, L., et al. 2009, A&A, 506, 411, doi: 10.1051/0004-6361/200810860

    work page doi:10.1051/0004-6361/200810860 2009

  8. [8]

    A., Spitoni E., de Laverny P., Cescutti G., 2025, @doi [ ] 10.1051/0004-6361/202450868 , https://ui.adsabs.harvard.edu/abs/2025A&A...693A...3B 693, A3

    Barbillon, M., Recio-Blanco, A., Poggio, E., et al. 2025, A&A, 693, A3, doi: 10.1051/0004-6361/202450868

    work page doi:10.1051/0004-6361/202450868 2025

Show all 150 references
  1. [9]

    1994, A&AS, 103, 475

    Barteldrees, A., & Dettmar, R.-J. 1994, A&AS, 103, 475

    1994

  2. [10]

    2023, A&A, 674, A194, doi: 10.1051/0004-6361/202345921

    Bellazzini, M., Massari, D., De Angeli, F., et al. 2023, A&A, 674, A194, doi: 10.1051/0004-6361/202345921

    2023 doi

  3. [11]

    2019, MNRAS, 482, 1417, doi: 10.1093/mnras/sty2813

    Bennett, M., & Bovy, J. 2019, MNRAS, 482, 1417, doi: 10.1093/mnras/sty2813

    2019 doi

  4. [12]

    2006, NewA, 12, 234, doi: 10.1016/j.newast.2006.10.001

    Bilir, S., Karaali, S., Ak, S., Yaz, E., & Hamzao˘ glu, E. 2006, NewA, 12, 234, doi: 10.1016/j.newast.2006.10.001

    2006 doi

  5. [13]

    2024, MNRAS, 535, 1898, doi: 10.1093/mnras/stae2481

    Binney, J. 2024, MNRAS, 535, 1898, doi: 10.1093/mnras/stae2481

    2024 doi

  6. [14]

    1987, Galactic dynamics

    Binney, J., & Tremaine, S. 1987, Galactic dynamics

    1987

  7. [15]

    2016, ARA&A, 54, 529, doi: 10.1146/annurev-astro-081915-023441

    Bland-Hawthorn, J., & Gerhard, O. 2016, ARA&A, 54, 529, doi: 10.1146/annurev-astro-081915-023441

    2016 doi

  8. [16]

    Bouquin, A. Y. K., Gil de Paz, A., Mu˜ noz-Mateos, J. C., et al. 2018, ApJS, 234, 18, doi: 10.3847/1538-4365/aaa384

    2018 doi

  9. [17]

    2015, ApJS, 216, 29, doi: 10.1088/0067-0049/216/2/29

    Bovy, J. 2015, ApJS, 216, 29, doi: 10.1088/0067-0049/216/2/29

    2015 doi

  10. [18]

    Finkbeiner, D. P. 2016a, ApJ, 818, 130, doi: 10.3847/0004-637X/818/2/130

    doi

  11. [19]

    F., et al

    Bovy, J., Rix, H.-W., Schlafly, E. F., et al. 2016b, ApJ, 823, 30, doi: 10.3847/0004-637X/823/1/30

    doi

  12. [20]

    L., Rix, H.-W., et al

    Bovy, J., Nidever, D. L., Rix, H.-W., et al. 2014, ApJ, 790, 127, doi: 10.1088/0004-637X/790/2/127

    2014 doi

  13. [21]

    2021, MNRAS, 506, 150, doi: 10.1093/mnras/stab1242

    Buder, S., Sharma, S., Kos, J., et al. 2021, MNRAS, 506, 150, doi: 10.1093/mnras/stab1242

    2021 doi

  14. [22]

    Burke, B. F. 1957, AJ, 62, 90, doi: 10.1086/107463

    1957 doi

  15. [23]

    1998, A&A, 331, 934

    Buser, R., Rong, J., & Karaali, S. 1998, A&A, 331, 934

    1998

  16. [24]

    2023, A&A, 669, A55, doi: 10.1051/0004-6361/202244784

    Cantat-Gaudin, T., Fouesneau, M., Rix, H.-W., et al. 2023, A&A, 669, A55, doi: 10.1051/0004-6361/202244784

    2023 doi

  17. [25]

    2024, A&A, 683, A128, doi: 10.1051/0004-6361/202348018

    Cantat-Gaudin, T., Fouesneau, M., Rix, H.-W., et al. 2024, A&A, 683, A128, doi: 10.1051/0004-6361/202348018

    2024 doi

  18. [26]

    W., & Seitzer, P

    Carney, B. W., & Seitzer, P. 1993, AJ, 105, 2127, doi: 10.1086/116591

    1993 doi

  19. [27]

    M., Weiler, M., Jordi, C., et al

    Carrasco, J. M., Weiler, M., Jordi, C., et al. 2021, A&A, 652, A86, doi: 10.1051/0004-6361/202141249

    2021 doi

  20. [28]

    Castro-Ginard, A., Brown, A. G. A., Kostrzewa-Rutkowska, Z., et al. 2023, A&A, 677, A37, doi: 10.1051/0004-6361/202346547

    2023 doi

  21. [29]

    C., Magnier, E

    Chambers, K. C., Magnier, E. A., Metcalfe, N., et al. 2016, arXiv e-prints, arXiv:1612.05560, doi: 10.48550/arXiv.1612.05560

    2016 doi

  22. [30]

    A., Rix, H.-W., et al

    Chandra, V., Semenov, V. A., Rix, H.-W., et al. 2024, ApJ, 972, 112, doi: 10.3847/1538-4357/ad5b60

    2024 doi

  23. [31]

    2025, arXiv e-prints, arXiv:2501.14089, doi: 10.48550/arXiv.2501.14089

    Chen, B., Orkney, M., Ting, Y.-S., & Hayden, M. 2025, arXiv e-prints, arXiv:2501.14089, doi: 10.48550/arXiv.2501.14089

    2025 doi

  24. [32]

    A., et al

    Chen, B., Stoughton, C., Smith, J. A., et al. 2001, ApJ, 553, 184, doi: 10.1086/320647

    2001 doi

  25. [33]

    2019, Nature Astronomy, 3, 320, doi: 10.1038/s41550-018-0686-7

    Chen, X., Wang, S., Deng, L., et al. 2019, Nature Astronomy, 3, 320, doi: 10.1038/s41550-018-0686-7

    2019 doi

  26. [34]

    Q., Casagrande, L., Zhao, G., et al

    Chen, Y. Q., Casagrande, L., Zhao, G., et al. 2017, ApJ, 840, 77, doi: 10.3847/1538-4357/aa6d0f

    2017 doi

  27. [35]

    Chiba, R., Friske, J. K. S., & Sch¨ onrich, R. 2021, MNRAS, 500, 4710, doi: 10.1093/mnras/staa3585 Chrob´ akov´ a,ˇZ., Nagy, R., & L´ opez-Corredoira, M. 2020, A&A, 637, A96, doi: 10.1051/0004-6361/201937289 Chrob´ akov´ a,ˇZ., Nagy, R., & L´ opez-Corredoira, M. 2022, A&A, 664...

    2021 doi

  28. [36]

    2012, Research in Astronomy and Astrophysics, 12, 1197, doi: 10.1088/1674-4527/12/9/003

    Cui, X.-Q., Zhao, Y.-H., Chu, Y.-Q., et al. 2012, Research in Astronomy and Astrophysics, 12, 1197, doi: 10.1088/1674-4527/12/9/003

    2012 doi

  29. [37]

    2021, A&A, 654, A107, doi: 10.1051/0004-6361/202040074 Galactic disk viewed by RC33 De Angeli, F., Weiler, M., Montegriffo, P., et al

    Culpan, R., Pelisoli, I., & Geier, S. 2021, A&A, 654, A107, doi: 10.1051/0004-6361/202040074 Galactic disk viewed by RC33 De Angeli, F., Weiler, M., Montegriffo, P., et al. 2023, A&A, 674, A2, doi: 10.1051/0004-6361/202243680 de Jong, R. S., Agertz, O., Berbel, A. A., et al. 2...

    2021 doi

  30. [38]

    P., Khachaturyants, T., Amarante, J

    Debattista, V. P., Khachaturyants, T., Amarante, J. A. S., et al. 2025, MNRAS, 537, 1620, doi: 10.1093/mnras/staf035

    2025 doi

  31. [39]

    1998, AJ, 115, 2384, doi: 10.1086/300364

    Dehnen, W. 1998, AJ, 115, 2384, doi: 10.1086/300364

    1998 doi

  32. [40]

    2024, ApJ, 975, 28, doi: 10.3847/1538-4357/ad7799 DESI Collaboration, Karim, M

    Deng, M., Du, C., Yang, Y., Liao, J., & Ye, D. 2024, ApJ, 975, 28, doi: 10.3847/1538-4357/ad7799 DESI Collaboration, Karim, M. A., Adame, A. G., et al. 2025, arXiv e-prints, arXiv:2503.14745, doi: 10.48550/arXiv.2503.14745

    2024 doi

  33. [41]

    S., & Warren, S

    Dobbie, P. S., & Warren, S. J. 2020, The Open Journal of Astrophysics, 3, 5, doi: 10.21105/astro.2003.05757 D’Onghia, E., & L. Aguerri, J. A. 2020, ApJ, 890, 117, doi: 10.3847/1538-4357/ab6bd6

    2020 doi

  34. [42]

    2003, A&A, 409, 205, doi: 10.1051/0004-6361:20031070

    Drimmel, R., Cabrera-Lavers, A., & L´ opez-Corredoira, M. 2003, A&A, 409, 205, doi: 10.1051/0004-6361:20031070

    2003 doi

  35. [43]

    Drimmel, R., & Spergel, D. N. 2001, ApJ, 556, 181, doi: 10.1086/321556

    2001 doi

  36. [44]

    Erwin, P., Pohlen, M., & Beckman, J. E. 2008, AJ, 135, 20, doi: 10.1088/0004-6256/135/1/20

    2008 doi

  37. [45]

    P., & Sanders, J

    Fallows, C. P., & Sanders, J. L. 2024, MNRAS, 531, 2126, doi: 10.1093/mnras/stae1303

    2024 doi

  38. [46]

    W., Menzies, J

    Feast, M. W., Menzies, J. W., Matsunaga, N., & Whitelock, P. A. 2014, Nature, 509, 342, doi: 10.1038/nature13246

    2014 doi

  39. [47]

    2017, ApJ, 843, 141, doi: 10.3847/1538-4357/aa77fd

    Ferguson, D., Gardner, S., & Yanny, B. 2017, ApJ, 843, 141, doi: 10.3847/1538-4357/aa77fd

    2017 doi

  40. [48]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, PASP, 125, 306, doi: 10.1086/670067

    2013 doi

  41. [49]

    Freeman, K. C. 1970, ApJ, 160, 811, doi: 10.1086/150474

    1970 doi

  42. [50]

    S., B´ edorf, J., Baba, J., & Portegies Zwart, S

    Fujii, M. S., B´ edorf, J., Baba, J., & Portegies Zwart, S. 2019, MNRAS, 482, 1983, doi: 10.1093/mnras/sty2747 Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2016a, A&A, 595, A2, doi: 10.1051/0004-6361/201629512 Gaia Collaboration, Prusti, T., de Bruijne, J. H. J.,...

    2019 doi

  43. [51]

    L., Brown, T

    Gilliland, R. L., Brown, T. M., Christensen-Dalsgaard, J., et al. 2010, PASP, 122, 131, doi: 10.1086/650399

    2010 doi

  44. [52]

    1983, MNRAS, 202, 1025, doi: 10.1093/mnras/202.4.1025

    Gilmore, G., & Reid, N. 1983, MNRAS, 202, 1025, doi: 10.1093/mnras/202.4.1025

    1983 doi

  45. [53]

    2016, ARA&A, 54, 95, doi: 10.1146/annurev-astro-081915-023354 GRAVITY Collaboration, Abuter, R., Amorim, A., et al

    Girardi, L. 2016, ARA&A, 54, 95, doi: 10.1146/annurev-astro-081915-023354 GRAVITY Collaboration, Abuter, R., Amorim, A., et al. 2018, A&A, 615, L15, doi: 10.1051/0004-6361/201833718

    2016 doi

  46. [54]

    2019, ApJ, 887, 93, doi: 10.3847/1538-4357/ab5362

    Finkbeiner, D. 2019, ApJ, 887, 93, doi: 10.3847/1538-4357/ab5362

    2019 doi

  47. [55]

    Groenewegen, M. A. T. 2021, A&A, 654, A20, doi: 10.1051/0004-6361/202140862 Guti´ errez, L., Erwin, P., Aladro, R., & Beckman, J. E. 2011, AJ, 142, 145, doi: 10.1088/0004-6256/142/5/145

    2021 doi

  48. [56]

    L., Cohen, M., Garz´ on, F., Mahoney, T., & L´ opez-Corredoira, M

    Hammersley, P. L., Cohen, M., Garz´ on, F., Mahoney, T., & L´ opez-Corredoira, M. 1999, MNRAS, 308, 333, doi: 10.1046/j.1365-8711.1999.02678.x

    1999 doi

  49. [57]

    J., Conroy, C., & Hernquist, L

    Han, J. J., Conroy, C., & Hernquist, L. 2023a, Nature Astronomy, 7, 1481, doi: 10.1038/s41550-023-02076-9

    doi

  50. [58]

    J., Semenov, V., Conroy, C., & Hernquist, L

    Han, J. J., Semenov, V., Conroy, C., & Hernquist, L. 2023b, ApJL, 957, L24, doi: 10.3847/2041-8213/ad0641

    doi

  51. [59]

    Hawkins, K., Leistedt, B., Bovy, J., & Hogg, D. W. 2017, MNRAS, 471, 722, doi: 10.1093/mnras/stx1655

    2017 doi

  52. [60]

    L., & Chen, Y.-Q

    He, X.-J., Luo, A. L., & Chen, Y.-Q. 2022, MNRAS, 512, 1710, doi: 10.1093/mnras/stac484

    2022 doi

  53. [61]

    2020, ApJS, 249, 29, doi: 10.3847/1538-4365/ab994f

    Huang, Y., Sch¨ onrich, R., Zhang, H., et al. 2020, ApJS, 249, 29, doi: 10.3847/1538-4365/ab994f

    2020 doi

  54. [62]

    C., Dalton, G

    Jin, S., Trager, S. C., Dalton, G. B., et al. 2024, MNRAS, 530, 2688, doi: 10.1093/mnras/stad557

    2024 doi

  55. [63]

    Jog, C. J. 2026, PhR, 1163, 1, doi: 10.1016/j.physrep.2025.11.003 Juri´ c, M., Ivezi´ c,ˇZ., Brooks, A., et al. 2008, ApJ, 673, 864, doi: 10.1086/523619

    2026 doi

  56. [64]

    2024, A&A, 691, A98, doi: 10.1051/0004-6361/202451427

    Khalatyan, A., Anders, F., Chiappini, C., et al. 2024, A&A, 691, A98, doi: 10.1051/0004-6361/202451427

    2024 doi

  57. [65]

    2025, A&A, 701, A270, doi: 10.1051/0004-6361/202452798

    Khanna, S., Yu, J., Drimmel, R., et al. 2025, A&A, 701, A270, doi: 10.1051/0004-6361/202452798

    2025 doi

  58. [66]

    2018, A&A, 611, L2, doi: 10.1051/0004-6361/201732521

    Khoperskov, S., Di Matteo, P., Haywood, M., & Combes, F. 2018, A&A, 611, L2, doi: 10.1051/0004-6361/201732521

    2018 doi

  59. [67]

    A., Sheth, K., et al

    Kim, T., Gadotti, D. A., Sheth, K., et al. 2014, ApJ, 782, 64, doi: 10.1088/0004-637X/782/2/64

    2014 doi

  60. [68]

    A., Rix, H.-W., Aerts, C., et al

    Kollmeier, J. A., Rix, H.-W., Aerts, C., et al. 2025, arXiv e-prints, arXiv:2507.06989, doi: 10.48550/arXiv.2507.06989

    2025 doi

  61. [69]

    1992, in Astronomical Society of the Pacific Conference Series, Vol

    Kroupa, P. 1992, in Astronomical Society of the Pacific Conference Series, Vol. 32, IAU Colloquium 135: Complementary Approaches to Double and Multiple Star Research, ed. H. A. McAlister & W. I. Hartkopf, 228

    1992

  62. [70]

    1989, MNRAS, 239, 571, doi: 10.1093/mnras/239.2.571

    Kuijken, K., & Gilmore, G. 1989, MNRAS, 239, 571, doi: 10.1093/mnras/239.2.571

    1989 doi

  63. [71]

    P., Belokurov, V., Koposov, S., et al

    Kurbatov, E. P., Belokurov, V., Koposov, S., et al. 2024, arXiv e-prints, arXiv:2410.22250, doi: 10.48550/arXiv.2410.22250

    2024 doi

  64. [72]

    2016, A&A, 596, A25, doi: 10.1051/0004-6361/201628397 34Wu et al

    Laine, J., Laurikainen, E., & Salo, H. 2016, A&A, 596, A25, doi: 10.1051/0004-6361/201628397 34Wu et al

    2016 doi

  65. [73]

    T., Liu, F., & Flynn, C

    Lehmann, C., Murphy, M. T., Liu, F., & Flynn, C. 2025, MNRAS, 536, 498, doi: 10.1093/mnras/stae2656

    2025 doi

  66. [74]

    2019, ApJ, 871, 208, doi: 10.3847/1538-4357/aafa17

    Li, C., Zhao, G., Jia, Y., et al. 2019, ApJ, 871, 208, doi: 10.3847/1538-4357/aafa17

    2019 doi

  67. [75]

    2024, ApJS, 272, 2, doi: 10.3847/1538-4365/ad2b4d

    Chandra, V. 2024, ApJS, 272, 2, doi: 10.3847/1538-4365/ad2b4d

    2024 doi

  68. [76]

    2025, MNRAS, 539, 1595, doi: 10.1093/mnras/staf583

    Li, Y., Freeman, K., & Jerjen, H. 2025, MNRAS, 539, 1595, doi: 10.1093/mnras/staf583

    2025 doi

  69. [77]

    2025a, ApJL, 984, L48, doi: 10.3847/2041-8213/adccb7

    Lian, J., Du, M., Lu, S., et al. 2025a, ApJL, 984, L48, doi: 10.3847/2041-8213/adccb7

    doi

  70. [78]

    2025b, ApJL, 990, L37, doi: 10.3847/2041-8213/adfc73

    Lian, J., Wang, T., Feng, Q., Huang, Y., & Guo, H. 2025b, ApJL, 990, L37, doi: 10.3847/2041-8213/adfc73

    doi

  71. [79]

    2024, Nature Astronomy, 8, 1302, doi: 10.1038/s41550-024-02315-7

    Lian, J., Zasowski, G., Chen, B., et al. 2024, Nature Astronomy, 8, 1302, doi: 10.1038/s41550-024-02315-7

    2024 doi

  72. [80]

    2022, MNRAS, 513, 4130, doi: 10.1093/mnras/stac1151

    Lian, J., Zasowski, G., Mackereth, T., et al. 2022, MNRAS, 513, 4130, doi: 10.1093/mnras/stac1151

    2022 doi

  73. [81]

    2017, Research in Astronomy and Astrophysics, 17, 096, doi: 10.1088/1674-4527/17/9/96

    Liu, C., Xu, Y., Wan, J.-C., et al. 2017, Research in Astronomy and Astrophysics, 17, 096, doi: 10.1088/1674-4527/17/9/96

    2017 doi

  74. [82]

    2024, Research in Astronomy and Astrophysics, 24, 065005, doi: 10.1088/1674-4527/ad3dc2 L´ opez-Corredoira, M., Allende Prieto, C., Garz´ on, F., et al

    Liu, X., Tian, H., Cui, W., et al. 2024, Research in Astronomy and Astrophysics, 24, 065005, doi: 10.1088/1674-4527/ad3dc2 L´ opez-Corredoira, M., Allende Prieto, C., Garz´ on, F., et al. 2018, A&A, 612, L8, doi: 10.1051/0004-6361/201832880 L´ opez-Corredoira, M., Betancort-Ri...

    2024 doi

  75. [83]

    Hammersley, P. L. 2002b, A&A, 394, 883, doi: 10.1051/0004-6361:20021175 L´ opez-Corredoira, M., Cabrera-Lavers, A., Gerhard, O. E., & Garz´ on, F. 2004, A&A, 421, 953, doi: 10.1051/0004-6361:20034385 L´ opez-Corredoira, M., & Molg´ o, J. 2014, A&A, 567, A106, doi: 10.1051/0004...

    2004 doi

  76. [84]

    Lucchini, S., D’Onghia, E., & Aguerri, J. A. L. 2024, MNRAS, 531, L14, doi: 10.1093/mnrasl/slae024

    2024 doi

  77. [85]

    Lucey, M., Pearson, S., Hunt, J. A. S., et al. 2023, MNRAS, 520, 4779, doi: 10.1093/mnras/stad406

    2023 doi

  78. [86]

    L., Zhang, H.-T., Zhao, Y.-H., et al

    Luo, A. L., Zhang, H.-T., Zhao, Y.-H., et al. 2012, Research in Astronomy and Astrophysics, 12, 1243, doi: 10.1088/1674-4527/12/9/004

    2012 doi

  79. [87]

    R., Schiavon, R

    Majewski, S. R., Schiavon, R. P., Frinchaboy, P. M., et al. 2017, AJ, 154, 94, doi: 10.3847/1538-3881/aa784d

    2017 doi

  80. [88]

    M., Marinoni, S., Fabrizio, M., & Altavilla, G

    Marrese, P. M., Marinoni, S., Fabrizio, M., & Altavilla, G. 2019, A&A, 621, A144, doi: 10.1051/0004-6361/201834142

    2019 doi

  81. [89]

    M., Marinoni, S., Fabrizio, M., & Giuffrida, G

    Marrese, P. M., Marinoni, S., Fabrizio, M., & Giuffrida, G. 2017, A&A, 607, A105, doi: 10.1051/0004-6361/201730965

    2017 doi

  82. [90]

    2006, A&A, 453, 635, doi: 10.1051/0004-6361:20053842

    Picaud, S. 2006, A&A, 453, 635, doi: 10.1051/0004-6361:20053842

    2006 doi

  83. [91]

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

    Martin, N. F., Starkenburg, E., Yuan, Z., et al. 2024, A&A, 692, A115, doi: 10.1051/0004-6361/202347633

    2024 doi

  84. [92]

    2015, ApJ, 802, 109, doi: 10.1088/0004-637X/802/2/109

    Moreno, E. 2015, ApJ, 802, 109, doi: 10.1088/0004-637X/802/2/109

    2015 doi

  85. [93]

    C., et al

    Minchev, I., Famaey, B., Quillen, A. C., et al. 2012, A&A, 548, A127, doi: 10.1051/0004-6361/201219714

    2012 doi

  86. [94]

    K., Alonso-Garc´ ıa, J., Lucas, P

    Minniti, D., Saito, R. K., Alonso-Garc´ ıa, J., Lucas, P. W., & Hempel, M. 2011, ApJL, 733, L43, doi: 10.1088/2041-8205/733/2/L43

    2011 doi

  87. [95]

    2019, ApJ, 872, 95, doi: 10.3847/1538-4357/aaf236

    Mohammed, S., Schiminovich, D., Hawkins, K., et al. 2019, ApJ, 872, 95, doi: 10.3847/1538-4357/aaf236

    2019 doi

  88. [96]

    2006, A&A, 451, 515, doi: 10.1051/0004-6361:20054081

    Momany, Y., Zaggia, S., Gilmore, G., et al. 2006, A&A, 451, 515, doi: 10.1051/0004-6361:20054081

    2006 doi

  89. [97]

    2019, A&A, 626, A41, doi: 10.1051/0004-6361/201834820

    Monari, G., Famaey, B., Siebert, A., Wegg, C., & Gerhard, O. 2019, A&A, 626, A41, doi: 10.1051/0004-6361/201834820

    2019 doi

  90. [98]

    2023, A&A, 674, A3, doi: 10.1051/0004-6361/202243880

    Montegriffo, P., De Angeli, F., Andrae, R., et al. 2023, A&A, 674, A3, doi: 10.1051/0004-6361/202243880

    2023 doi

  91. [99]

    2021, MNRAS, 507, 5246, doi: 10.1093/mnras/stab2445

    Camps, P. 2021, MNRAS, 507, 5246, doi: 10.1093/mnras/stab2445

    2021 doi

  92. [100]

    2024, A&A, 681, L8, doi: 10.1051/0004-6361/202348365

    Nepal, S., Chiappini, C., Guiglion, G., et al. 2024, A&A, 681, L8, doi: 10.1051/0004-6361/202348365

    2024 doi

  93. [101]

    Ojha, D. K. 2001, MNRAS, 322, 426, doi: 10.1046/j.1365-8711.2001.04155.x

    2001 doi

  94. [102]

    2019, MNRAS, 486, 5600, doi: 10.1093/mnras/stz1192

    Onozato, H., Ita, Y., Nakada, Y., & Nishiyama, S. 2019, MNRAS, 486, 5600, doi: 10.1093/mnras/stz1192

    2019 doi

  95. [103]

    H., Kerr, F

    Oort, J. H., Kerr, F. J., & Westerhout, G. 1958, MNRAS, 118, 379, doi: 10.1093/mnras/118.4.379

    1958 doi

  96. [104]

    C., & Binney, J

    Ostriker, E. C., & Binney, J. J. 1989, MNRAS, 237, 785, doi: 10.1093/mnras/237.3.785

    1989 doi

  97. [105]

    M., Sarzi, M., et al

    Pizzella, A., Corsini, E. M., Sarzi, M., et al. 2008, MNRAS, 387, 1099, doi: 10.1111/j.1365-2966.2008.13237.x

    2008 doi

  98. [106]

    Plevne, O., ¨Onal Ta¸ s,¨O., Bilir, S., & Seabroke, G. M. 2020, ApJ, 893, 108, doi: 10.3847/1538-4357/ab80bb

    2020 doi

  99. [107]

    J., L¨ utticke, R., & Aronica, G

    Pohlen, M., Dettmar, R. J., L¨ utticke, R., & Aronica, G. 2002, A&A, 392, 807, doi: 10.1051/0004-6361:20020994

    2002 doi

  100. [108]

    2006, A&A, 454, 759, doi: 10.1051/0004-6361:20064883

    Pohlen, M., & Trujillo, I. 2006, A&A, 454, 759, doi: 10.1051/0004-6361:20064883

    2006 doi

  101. [109]

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

    Portail, M., Gerhard, O., Wegg, C., & Ness, M. 2017, MNRAS, 465, 1621, doi: 10.1093/mnras/stw2819

    2017 doi

  102. [110]

    1983, AJ, 88, 1476, doi: 10.1086/113437 Reyl´ e, C., Marshall, D

    Pritchet, C. 1983, AJ, 88, 1476, doi: 10.1086/113437 Reyl´ e, C., Marshall, D. J., Robin, A. C., & Schultheis, M. 2009, A&A, 495, 819, doi: 10.1051/0004-6361/200811341

    1983 doi

  103. [111]

    W., et al

    Riello, M., De Angeli, F., Evans, D. W., et al. 2021, A&A, 649, A3, doi: 10.1051/0004-6361/202039587 Galactic disk viewed by RC35

    2021 doi

  104. [112]

    2022, ApJ, 941, 45, doi: 10.3847/1538-4357/ac9e01

    Rix, H.-W., Chandra, V., Andrae, R., et al. 2022, ApJ, 941, 45, doi: 10.3847/1538-4357/ac9e01

    2022 doi

  105. [113]

    C., Creze, M., & Mohan, V

    Robin, A. C., Creze, M., & Mohan, V. 1992, ApJL, 400, L25, doi: 10.1086/186640

    1992 doi

  106. [114]

    2018, A&A, 609, A116, doi: 10.1051/0004-6361/201731572

    Lallement, R. 2018, A&A, 609, A116, doi: 10.1051/0004-6361/201731572

    2018 doi

  107. [115]

    C., Epchtein, N., et al

    Ruphy, S., Robin, A. C., Epchtein, N., et al. 1996, A&A, 313, L21

    1996

  108. [116]

    2002, MNRAS, 337, 332, doi: 10.1046/j.1365-8711.2002.05917.x

    Salaris, M., & Girardi, L. 2002, MNRAS, 337, 332, doi: 10.1046/j.1365-8711.2002.05917.x

    2002 doi

  109. [117]

    Sarkar, S., & Jog, C. J. 2018, A&A, 617, A142, doi: 10.1051/0004-6361/201833510

    2018 doi

  110. [118]

    Sarkar, S., & Jog, C. J. 2020, MNRAS, 499, 2523, doi: 10.1093/mnras/staa2924

    2020 doi

  111. [119]

    J., Finkbeiner, D

    Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525, doi: 10.1086/305772 Sch¨ onrich, R., & Binney, J. 2009, MNRAS, 396, 203, doi: 10.1111/j.1365-2966.2009.14750.x Sch¨ onrich, R., & Dehnen, W. 2018, MNRAS, 478, 3809, doi: 10.1093/mnras/sty1256

    1998 doi

  112. [120]

    A., & Binney, J

    Sellwood, J. A., & Binney, J. J. 2002, MNRAS, 336, 785, doi: 10.1046/j.1365-8711.2002.05806.x

    2002 doi

  113. [121]

    F., Cutri, R

    Skrutskie, M. F., Cutri, R. M., Stiening, R., et al. 2006, AJ, 131, 1163, doi: 10.1086/498708

    2006 doi

  114. [122]

    1942, ApJ, 95, 329, doi: 10.1086/144407

    Spitzer, Jr., L. 1942, ApJ, 95, 329, doi: 10.1086/144407

    1942 doi

  115. [123]

    R., et al

    Stello, D., Huber, D., Bedding, T. R., et al. 2013, ApJL, 765, L41, doi: 10.1088/2041-8205/765/2/L41

    2013 doi

  116. [124]

    2024, MNRAS, 531, 495, doi: 10.1093/mnras/stae1148

    Tang, X.-C., Tian, H., Li, J., et al. 2024, MNRAS, 531, 495, doi: 10.1093/mnras/stae1148

    2024 doi

  117. [125]

    2024, MNRAS, 531, 1730, doi: 10.1093/mnras/stae1247

    Tian, H., Liu, C., Li, J., & Zhang, B. 2024, MNRAS, 531, 1730, doi: 10.1093/mnras/stae1247

    2024 doi

  118. [126]

    2018, ApJL, 858, L7, doi: 10.3847/2041-8213/aabf8e

    Ting, Y.-S., Hawkins, K., & Rix, H.-W. 2018, ApJL, 858, L7, doi: 10.3847/2041-8213/aabf8e

    2018 doi

  119. [127]

    2024, MNRAS, 527, 4863, doi: 10.1093/mnras/stad3525 van der Kruit, P

    Uppal, N., Ganesh, S., & Schultheis, M. 2024, MNRAS, 527, 4863, doi: 10.1093/mnras/stad3525 van der Kruit, P. C. 1979, A&AS, 38, 15 van der Kruit, P. C. 1986, A&A, 157, 230 van der Kruit, P. C., & Searle, L. 1981a, A&A, 95, 105 van der Kruit, P. C., & Searle, L. 1981b, A&A, 95...

    2024 doi

  120. [128]

    Green, R. F. 1995, ApJ, 446, 646, doi: 10.1086/175824

    1995 doi

  121. [129]

    2024, MNRAS, 528, 3576, doi: 10.1093/mnras/stae083

    Vislosky, E., Minchev, I., Khoperskov, S., et al. 2024, MNRAS, 528, 3576, doi: 10.1093/mnras/stae083

    2024 doi

  122. [130]

    2016, A&A, 588, A87, doi: 10.1051/0004-6361/201527259

    Vrard, M., Mosser, B., & Samadi, R. 2016, A&A, 588, A87, doi: 10.1051/0004-6361/201527259

    2016 doi

  123. [131]

    2018, MNRAS, 478, 3367, doi: 10.1093/mnras/sty1058

    Wang, H.-F., Liu, C., Xu, Y., Wan, J.-C., & Deng, L. 2018, MNRAS, 478, 3367, doi: 10.1093/mnras/sty1058

    2018 doi

  124. [132]

    2021, ApJ, 923, 145, doi: 10.3847/1538-4357/ac22a7

    Wang, S., & Chen, X. 2021, ApJ, 923, 145, doi: 10.3847/1538-4357/ac22a7

    2021 doi

  125. [133]

    2024, MNRAS, 533, L31, doi: 10.1093/mnrasl/slae059

    Wang, T., Chen, B.-Q., Lian, J.-H., Xiang, M.-S., & Liu, X.-W. 2024, MNRAS, 533, L31, doi: 10.1093/mnrasl/slae059

    2024 doi

  126. [134]

    2015, MNRAS, 450, 4050, doi: 10.1093/mnras/stv745

    Wegg, C., Gerhard, O., & Portail, M. 2015, MNRAS, 450, 4050, doi: 10.1093/mnras/stv745

    2015 doi

  127. [135]

    2012, ApJL, 750, L41, doi: 10.1088/2041-8205/750/2/L41

    Chen, H.-Y. 2012, ApJL, 750, L41, doi: 10.1088/2041-8205/750/2/L41

    2012 doi

  128. [136]

    Wille, A., & Machado, R. E. G. 2024, MNRAS, 533, 2997, doi: 10.1093/mnras/stae2004

    2024 doi

  129. [137]

    2025, A&A, 700, A244, doi: 10.1051/0004-6361/202554410

    Wu, W., Ye, X., Allende Prieto, C., et al. 2025, A&A, 700, A244, doi: 10.1051/0004-6361/202554410

    2025 doi

  130. [138]

    2025, Nature Astronomy, 9, 101, doi: 10.1038/s41550-024-02382-w

    Xiang, M., Rix, H.-W., Yang, H., et al. 2025, Nature Astronomy, 9, 101, doi: 10.1038/s41550-024-02382-w

    2025 doi

  131. [139]

    2018, ApJS, 237, 33, doi: 10.3847/1538-4365/aad237

    Xiang, M., Shi, J., Liu, X., et al. 2018, ApJS, 237, 33, doi: 10.3847/1538-4365/aad237

    2018 doi

  132. [140]

    2024, A&A, 682, L17, doi: 10.1051/0004-6361/202449252

    Xu, D., & Yu, S.-Y. 2024, A&A, 682, L17, doi: 10.1051/0004-6361/202449252

    2024 doi

  133. [141]

    2018, MNRAS, 473, 1244, doi: 10.1093/mnras/stx2361

    Xu, Y., Liu, C., Xue, X.-X., et al. 2018, MNRAS, 473, 1244, doi: 10.1093/mnras/stx2361

    2018 doi

  134. [142]

    J., et al

    Yanny, B., Rockosi, C., Newberg, H. J., et al. 2009, AJ, 137, 4377, doi: 10.1088/0004-6256/137/5/4377

    2009 doi

  135. [143]

    2025, A&A, 695, A75, doi: 10.1051/0004-6361/202452871

    Ye, X., Wu, W., Allende Prieto, C., et al. 2025, A&A, 695, A75, doi: 10.1051/0004-6361/202452871

    2025 doi

  136. [144]

    G., Adelman, J., Anderson, John E., J., et al

    York, D. G., Adelman, J., Anderson, John E., J., et al. 2000, AJ, 120, 1579, doi: 10.1086/301513

    2000 doi

  137. [145]

    1982, PASJ, 34, 365

    Yoshii, Y. 1982, PASJ, 34, 365

    1982

  138. [146]

    2025, AJ, 169, 61, doi: 10.3847/1538-3881/ad9582

    Yu, Z., Chen, B., Lian, J., Wang, C., & Liu, X. 2025, AJ, 169, 61, doi: 10.3847/1538-3881/ad9582

    2025 doi

  139. [147]

    2021, ApJ, 912, 106, doi: 10.3847/1538-4357/abf098

    Yu, Z., Li, J., Chen, B., et al. 2021, ApJ, 912, 106, doi: 10.3847/1538-4357/abf098

    2021 doi

  140. [148]

    M., & Rix, H.-W

    Zhang, X., Green, G. M., & Rix, H.-W. 2023, MNRAS, 524, 1855, doi: 10.1093/mnras/stad1941

    2023 doi

  141. [149]

    2006, ChJA&A, 6, 265, doi: 10.1088/1009-9271/6/3/01

    Zhao, G., Chen, Y.-Q., Shi, J.-R., et al. 2006, ChJA&A, 6, 265, doi: 10.1088/1009-9271/6/3/01

    2006 doi

  142. [150]

    2012, Research in Astronomy and Astrophysics, 12, 723, doi: 10.1088/1674-4527/12/7/002

    Zhao, G., Zhao, Y.-H., Chu, Y.-Q., Jing, Y.-P., & Deng, L.-C. 2012, Research in Astronomy and Astrophysics, 12, 723, doi: 10.1088/1674-4527/12/7/002

    2012 doi

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