pith. machine review for the scientific record. sign in

arxiv: 2605.14308 · v1 · submitted 2026-05-14 · 🌌 astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

Reconstructing the Stripping History of the Sagittarius Stream with Neural Networks

Jian Zhang , Cuihua Du , Mingji Deng , Zhongcheng Li , Haoyang Liu
Authors on Pith no claims yet

Pith reviewed 2026-05-15 02:36 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Sagittarius Streamstripping timeneural networksmetallicity gradientglobular clustersN-body simulationsstellar halodwarf galaxy disruption
0
0 comments X

The pith

A neural network trained on simulations infers when Sagittarius Stream stars were stripped from their dwarf galaxy, revealing a clear metallicity gradient with time.

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

The paper trains a neural network on N-body simulations of the Sagittarius dwarf disruption so that the network can estimate the stripping time of any stream star from its present-day position and velocity alone. When the trained network is run on real stars selected from Gaia, APOGEE, SEGUE and LAMOST data, it recovers a steady rise in metallicity for stars that left the dwarf more recently. This linear trend implies the progenitor continued to form stars and enrich its gas until late in its disruption. The same model also returns specific stripping epochs for globular clusters previously linked to the Sagittarius system, distinguishing those still bound from those removed in earlier orbits.

Core claim

A neural network trained on N-body simulations of the Sagittarius dwarf spheroidal can recover the time at which each stream star was stripped from its phase-space coordinates alone. Real data yield a clear linear metallicity-stripping-time relation with slope approximately 0.3 dex Gyr^{-1}. The network places M54, Terzan 7, Terzan 8 and Arp 2 as still bound, while dating Pal 12 to 0.9 Gyr ago, Whiting 1 to 1.1 Gyr ago and NGC 2419 to 2.1 Gyr ago.

What carries the argument

Neural network that maps observed phase-space coordinates directly to stripping time, trained on N-body simulations of the Sagittarius dwarf disruption.

If this is right

  • Metallicity increases linearly with more recent stripping time at roughly 0.3 dex per Gyr.
  • M54, Terzan 7, Terzan 8 and Arp 2 remain bound to the Sagittarius remnant today.
  • Pal 12, Whiting 1 and NGC 2419 left the dwarf 0.9, 1.1 and 2.1 Gyr ago respectively.
  • NGC 4147 and NGC 5634, if confirmed as members, were stripped about 1.1 Gyr ago.
  • Data-driven stripping-time estimates can reconstruct both the dynamical orbit and the chemical history of the stream.

Where Pith is reading between the lines

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

  • The identical training procedure could be repeated for other known stellar streams to date their own stripping sequences.
  • A confirmed gradient would constrain how long the Sagittarius dwarf continued forming stars before its gas was exhausted.
  • Adding future high-precision radial-velocity or abundance data would allow the method to map changes in the dwarf's orbital decay rate.
  • The approach may help identify additional faint members that current selection cuts miss.

Load-bearing premise

The neural network trained only on simulations produces unbiased stripping-time estimates when applied to real stars despite differences in dynamics or selection.

What would settle it

A large independent sample of stream stars with direct age or abundance measurements showing no correlation between metallicity and the network-predicted stripping time.

Figures

Figures reproduced from arXiv: 2605.14308 by Cuihua Du, Haoyang Liu, Jian Zhang, Mingji Deng, Zhongcheng Li.

Figure 1
Figure 1. Figure 1: Results on the test set. The x-axis shows the true stripping time Ts of V21 simulation particles, and the y-axis shows the stripping time predicted from the neural network (Tˆs). Blue dots with error bars correspond to the adopted value and uncertainty of the NN-predicted results. The grey dashed line corresponds to y=x. Here, E⃗xt|⃗xo [·] and Var⃗xt|⃗xo [·] denote the expectation and variance taken with r… view at source ↗
Figure 2
Figure 2. Figure 2: Combined results from SEGUE, APOGEE, and LAMOST surveys. The main panels show the line-of-sight velocity relative to Λ⊙ for the Sgr Stream across four metallicity bins. Background gray, orange, and green scatter points represent particles from the V21 simulation classified as still-bound, young wrap (0 > Ts ≥ −2 Gyr), and old wrap (Ts < −2 Gyr), re￾spectively. Overlaid symbols show observed Sgr Stream memb… view at source ↗
Figure 3
Figure 3. Figure 3: Directed Acyclic Graph (DAG) for our hierarchical Bayesian mixture-plus-regression model. Latent variables are shown as unfilled circles, observed quantities as filled gray circles, and fixed parameters are shown in rectangles. The model infers the true stripping time Ts,i from the NN prediction Tˆs,i and its uncertainty σTs,i . A Gaussian mixture model with three components (k = 1, 2, 3), parameterized by… view at source ↗
Figure 4
Figure 4. Figure 4: The x-axis shows NN-predicted stripping time Tˆs, and the y-axis shows metallicity. Blue, orange, and green dots correspond to data from SEGUE, APOGEE, and LAMOST. The red line shows the metallicity gradient, with the shaded region representing the 1σ credible interval. As expected, M 54, Ter 7, Ter 8, and Arp 2 exhibit stripping times consistent with zero within uncertainties, confirm￾ing that they are cu… view at source ↗
Figure 5
Figure 5. Figure 5: Corner plot of the slope, intercept, and dispersion of the metallicity gradient [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
read the original abstract

The Sagittarius (Sgr) Stream is produced by the ongoing disruption of the Sgr dwarf spheroidal (dSph) galaxy and is thought to contain multiple wraps that were stripped during different pericentric passages. In this study, we introduce a neural-network--based method trained on $N$-body simulations to infer the stripping time of Sgr Stream stars directly from their phase-space coordinates. We combine spectroscopic data from SEGUE, APOGEE DR17, and LAMOST DR7 LRS with \textit{Gaia} EDR3 astrometry and distance estimates from the latest \texttt{StarHorse} catalog to identify high-quality Sgr Stream members. Applying our method to these stars, we measure a clear metallicity gradient with stripping time, well described by a linear relation with slope $\sim 0.3~\mathrm{dex~Gyr^{-1}}$. We further predict the stripping times of globular clusters previously suggested to originate from the Sgr dSph. M 54, Terzan 7, Terzan 8, and Arp 2 exhibit stripping times consistent with being currently bound to the Sgr remnant. Pal 12, Whiting 1, and NGC 2419 are inferred to have been stripped $0.9 \pm 0.1$, $1.1 \pm 0.2$, and $2.1 \pm 0.2$ Gyr ago, respectively. For NGC 4147 and NGC 5634, whose membership in the Sgr system remains uncertain, our analysis suggests stripping times of $1.1 \pm 0.4$ and $1.1 \pm 0.1$ Gyr, respectively, if they are ultimately confirmed as genuine Sgr members. These results demonstrate that data-driven models of dynamical stripping histories offer a promising approach for reconstructing the formation and chemical evolution of the Sgr Stream.

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 / 1 minor

Summary. The paper introduces a neural-network method trained on N-body simulations to infer the stripping times of Sagittarius Stream stars directly from phase-space coordinates. Combining SEGUE, APOGEE, LAMOST, Gaia EDR3, and StarHorse data, the authors identify high-quality stream members and report a metallicity gradient with stripping time of slope ~0.3 dex Gyr^{-1}. They further predict stripping times for several globular clusters previously linked to the Sgr dSph, including values such as 0.9 Gyr for Pal 12 and 2.1 Gyr for NGC 2419.

Significance. If the neural network generalizes reliably, the work provides a novel data-driven route to reconstruct the multi-wrap stripping history of the Sgr stream and to link chemical gradients to dynamical epochs. The reported linear metallicity-stripping-time relation and the specific GC age predictions constitute falsifiable outputs that could be tested with future spectroscopic surveys or improved simulations.

major comments (2)
  1. [Abstract and §3] Abstract and §3 (Methods): no performance metrics, cross-validation scores, or recovery tests on held-out simulations are reported for the neural network's ability to predict known stripping times. Without these, the central claim that the network accurately maps observed (x, v) to stripping time remains only moderately supported.
  2. [§4] §4 (Application to observations): the training set consists of noise-free N-body particles, yet the manuscript does not describe injection of realistic Gaia/StarHorse uncertainties (distance errors ~10-20%, proper-motion and RV errors) during training or Monte-Carlo propagation at inference. This omission directly affects the reliability of the reported ~0.3 dex Gyr^{-1} gradient and the GC stripping times (e.g., NGC 2419 at 2.1 Gyr).
minor comments (1)
  1. [Abstract] The abstract states the gradient is 'well described by a linear relation' but does not quote the intercept or the formal uncertainty on the slope; these should be added for reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed report. Their comments have identified areas where the original manuscript could be strengthened through additional validation and clearer description of uncertainty handling. We address each major comment below and have revised the manuscript accordingly.

read point-by-point responses

  1. Referee: [Abstract and §3] Abstract and §3 (Methods): no performance metrics, cross-validation scores, or recovery tests on held-out simulations are reported for the neural network's ability to predict known stripping times. Without these, the central claim that the network accurately maps observed (x, v) to stripping time remains only moderately supported.

    Authors: We agree that quantitative performance metrics were not presented in the original submission. In the revised manuscript we have expanded §3 with a new subsection on validation. This includes 5-fold cross-validation results on the simulation training set and recovery tests on held-out N-body particles, together with quantitative metrics (mean absolute error and correlation coefficient between predicted and true stripping times) and new figures showing the recovery performance. These additions directly support the claim that the network maps phase-space coordinates to stripping time. revision: yes

  2. Referee: [§4] §4 (Application to observations): the training set consists of noise-free N-body particles, yet the manuscript does not describe injection of realistic Gaia/StarHorse uncertainties (distance errors ~10-20%, proper-motion and RV errors) during training or Monte-Carlo propagation at inference. This omission directly affects the reliability of the reported ~0.3 dex Gyr^{-1} gradient and the GC stripping times (e.g., NGC 2419 at 2.1 Gyr).

    Authors: We agree that the original text did not adequately describe uncertainty handling. The training was performed on noise-free particles to learn the clean dynamical mapping; observational errors are instead propagated at inference via Monte Carlo sampling of each star's phase-space coordinates within their reported uncertainties. In the revised manuscript we have added a detailed description of this procedure in §4, including the number of realizations drawn and how the resulting distributions are used to obtain the reported stripping times and their uncertainties. We have also included a robustness test in which realistic Gaia/StarHorse-level noise was injected into simulation particles, confirming that the recovered metallicity gradient remains consistent. These changes improve the presentation of the reliability of the ~0.3 dex Gyr^{-1} gradient and the globular-cluster ages. revision: yes

Circularity Check

0 steps flagged

No significant circularity: NN trained on independent N-body simulations applied to external observations

full rationale

The derivation trains a neural network on N-body simulations (independent of observations) to map phase-space coordinates to stripping times, then applies the model to real SEGUE/APOGEE/LAMOST+Gaia+StarHorse data. The metallicity gradient (~0.3 dex Gyr^{-1}) and GC stripping-time predictions are computed from these inferred times plus observed metallicities, without reducing to the training inputs by construction. No self-definitional steps, fitted inputs renamed as predictions, load-bearing self-citations, uniqueness theorems, or ansatzes appear in the abstract or described method. The chain remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on the assumption that N-body simulations capture the essential phase-space evolution of stripped stars and that the trained network generalizes without major domain shift to real data.

free parameters (1)
  • neural network weights and hyperparameters
    Fitted during supervised training on simulation outputs to map phase-space to stripping time.
axioms (1)
  • domain assumption N-body simulations faithfully reproduce the phase-space distributions of stars stripped at different pericentric passages
    The training dataset is generated from these simulations.

pith-pipeline@v0.9.0 · 5660 in / 1315 out tokens · 49800 ms · 2026-05-15T02:36:26.654522+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

111 extracted references · 111 canonical work pages · 60 internal anchors

  1. [1]

    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

  2. [2]

    The Astropy Project: Building an inclusive, open-science project and status of the v2.0 core package

    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 internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/aabc4f

  3. [3]

    Astropy: A Community Python Package for Astronomy

    Astropy: A community Python package for astronomy. , keywords =. 2013. doi:10.1051/0004-6361/201322068 , archivePrefix =. 1307.6212 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201322068 2013

  4. [4]

    , keywords =

    Core condensation in heavy halos: a two-stage theory for galaxy formation and clustering. , keywords =. doi:10.1093/mnras/183.3.341 , adsurl =

    work page doi:10.1093/mnras/183.3.341

  5. [5]

    Simulating the joint evolution of quasars, galaxies and their large-scale distribution

    Simulations of the formation, evolution and clustering of galaxies and quasars. , keywords =. doi:10.1038/nature03597 , archivePrefix =. astro-ph/0504097 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/nature03597

  6. [6]

    A Two Micron All Sky Survey View of the Sagittarius Dwarf Galaxy. I. Morphology of the Sagittarius Core and Tidal Arms. , keywords =. doi:10.1086/379504 , archivePrefix =. astro-ph/0304198 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/379504

  7. [7]

    , year = 1994, month = jul, volume =

    A dwarf satellite galaxy in Sagittarius. , year = 1994, month = jul, volume =. doi:10.1038/370194a0 , adsurl =

    work page doi:10.1038/370194a0 1994

  8. [8]

    Revising members and candidates with Gaia DR2

    Globular clusters in the Sagittarius stream. Revising members and candidates with Gaia DR2. , keywords =. doi:10.1051/0004-6361/202037621 , archivePrefix =. 2003.07871 , primaryClass =

    work page doi:10.1051/0004-6361/202037621 2003

  9. [9]

    , keywords =

    Tango for three: Sagittarius, LMC, and the Milky Way. , keywords =. doi:10.1093/mnras/staa3673 , archivePrefix =. 2009.10726 , primaryClass =

    work page doi:10.1093/mnras/staa3673 2009

  10. [10]

    R., & Wynn, G

    Building up the stellar halo of the Galaxy. , keywords =. doi:10.1046/j.1365-8711.1999.02616.x , archivePrefix =. astro-ph/9901102 , primaryClass =

    work page doi:10.1046/j.1365-8711.1999.02616.x 1999

  11. [11]

    Co-formation of the Galactic disc and the stellar halo

    Co-formation of the disc and the stellar halo. , keywords =. doi:10.1093/mnras/sty982 , archivePrefix =. 1802.03414 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty982

  12. [12]

    The merger that led to the formation of the Milky Way's inner stellar halo and thick disk

    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 internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41586-018-0625-x

  13. [13]

    , keywords =

    Multiple retrograde substructures in the Galactic halo: A shattered view of Galactic history. , keywords =. doi:10.1051/0004-6361/201936738 , archivePrefix =. 1909.08924 , primaryClass =

    work page doi:10.1051/0004-6361/201936738 1909

  14. [14]

    Evidence for Two Early Accretion Events That Built the Milky Way Stellar Halo

    Evidence for two early accretion events that built the Milky Way stellar halo. , keywords =. doi:10.1093/mnras/stz1770 , archivePrefix =. 1904.03185 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1770 1904

  15. [15]

    , keywords =

    Evidence from the H3 Survey That the Stellar Halo Is Entirely Comprised of Substructure. , keywords =. doi:10.3847/1538-4357/abaef4 , archivePrefix =. 2006.08625 , primaryClass =

    work page doi:10.3847/1538-4357/abaef4 2006

  16. [16]

    A Tail of Two Populations: Chemo-dynamics of the Sagittarius Stream and Implications for its Original Mass

    A tail of two populations: chemo-dynamics of the Sagittarius stream and implications for its original mass. , keywords =. doi:10.1093/mnras/stw2328 , archivePrefix =. 1607.00803 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2328

  17. [17]

    , keywords =

    A Diffuse Metal-poor Component of the Sagittarius Stream Revealed by the H3 Survey. , keywords =. doi:10.3847/1538-4357/abab08 , archivePrefix =. 2007.14408 , primaryClass =

    work page doi:10.3847/1538-4357/abab08 2007

  18. [18]

    , keywords =

    Phase-space Properties and Chemistry of the Sagittarius Stellar Stream Down to the Extremely Metal-poor ([Fe/H] -3) Regime. , keywords =. doi:10.3847/1538-4357/acb694 , archivePrefix =. 2212.08249 , primaryClass =

    work page doi:10.3847/1538-4357/acb694

  19. [19]

    , 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

  20. [20]

    , keywords =

    Evidence for the Sagittarius Dwarf Galaxy at Low Galactic Latitudes. , keywords =. doi:10.1086/309917 , adsurl =

    work page doi:10.1086/309917

  21. [21]

    , keywords =

    Discovery of a Tidal Extension of the Sagittarius Dwarf Spheroidal Galaxy. , keywords =. doi:10.1086/309919 , adsurl =

    work page doi:10.1086/309919

  22. [22]

    Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees

    Tracing the Outer Structure of the Sagittarius Dwarf Galaxy:Detections at Angular Distances between 10 and 34. , keywords =. doi:10.1086/311720 , archivePrefix =. astro-ph/9810015 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/311720

  23. [23]

    MACHO Project Photometry of RR Lyrae Stars in the Sgr Dwarf Galaxy

    MACHO Project Photometry of RR Lyrae Stars in the Sagittarius Dwarf Galaxy. , keywords =. doi:10.1086/303467 , archivePrefix =. astro-ph/9605148 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/303467

  24. [24]

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

    The APM survey for cool carbon stars in the Galactic halo - I. , keywords =. doi:10.1046/j.1365-8711.1998.01086.x , adsurl =

    work page doi:10.1046/j.1365-8711.1998.01086.x 1998

  25. [25]

    Starcounts Redivivus. III. A Possible Detection of the Sagittarius Dwarf Spheroidal Galaxy at B=-40 deg. , keywords =. doi:10.1086/301036 , archivePrefix =. astro-ph/9906455 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/301036

  26. [26]

    Galactic Halo substructure in the Sloan Digital Sky Survey: the ancient tidal stream from the Sagittarius dwarf galaxy

    Galactic Halo Substructure in the Sloan Digital Sky Survey: The Ancient Tidal Stream from the Sagittarius Dwarf Galaxy. , keywords =. doi:10.1086/318894 , archivePrefix =. astro-ph/0004255 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/318894

  27. [27]

    Sagittarius Tidal Debris 90 kpc from the Galactic Center

    Sagittarius Tidal Debris 90 Kiloparsecs from the Galactic Center. , keywords =. doi:10.1086/379316 , archivePrefix =. astro-ph/0309162 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/379316

  28. [28]

    The Field of Streams: Sagittarius and its Siblings

    The Field of Streams: Sagittarius and Its Siblings. , keywords =. doi:10.1086/504797 , archivePrefix =. astro-ph/0605025 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/504797

  29. [29]

    Precession of the Sagittarius stream

    Precession of the Sagittarius stream. , keywords =. doi:10.1093/mnras/stt1862 , archivePrefix =. 1301.7069 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stt1862

  30. [30]

    The Geometry of Sagittarius Stream from Pan-STARRS1 3$\pi$ RR Lyrae

    The Geometry of the Sagittarius Stream from Pan-STARRS1 3 RR Lyrae. , keywords =. doi:10.3847/1538-4357/aa960c , archivePrefix =. 1710.09436 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/aa960c

  31. [31]

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

    Simple dynamical models of the Sagittarius dwarf galaxy. , keywords =. doi:10.1046/j.1365-8711.2001.04238.x , archivePrefix =. astro-ph/0002482 , primaryClass =

    work page doi:10.1046/j.1365-8711.2001.04238.x 2001

  32. [32]

    Velocity trends in the debris of Sagittarius and the shape of the dark-matter halo of the Galaxy

    Velocity Trends in the Debris of Sagittarius and the Shape of the Dark Matter Halo of Our Galaxy. , keywords =. doi:10.1086/423340 , archivePrefix =. astro-ph/0406396 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/423340

  33. [33]

    A Two Micron All Sky Survey View of the Sagittarius Dwarf Galaxy. III. Constraints on the Flattening of the Galactic Halo. , keywords =. doi:10.1086/426777 , archivePrefix =. astro-ph/0407565 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/426777

  34. [34]

    A Two Micron All-Sky Survey View of the Sagittarius Dwarf Galaxy. IV. Modeling the Sagittarius Tidal Tails. , keywords =. doi:10.1086/426779 , archivePrefix =. astro-ph/0407566 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/426779

  35. [35]

    The Origin of the Bifurcation in the Sagittarius Stream

    The Origin of the Bifurcation in the Sagittarius Stream. , keywords =. doi:10.1086/507128 , archivePrefix =. astro-ph/0605026 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/507128

  36. [36]

    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

  37. [37]

    The Sagittarius Dwarf Galaxy: a Model for Evolution in a Triaxial Milky Way Halo

    The Sagittarius Dwarf Galaxy: A Model for Evolution in a Triaxial Milky Way Halo. , keywords =. doi:10.1088/0004-637X/714/1/229 , archivePrefix =. 1003.1132 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/714/1/229

  38. [38]

    The Gaia mission

    The Gaia mission. , keywords =. doi:10.1051/0004-6361/201629272 , archivePrefix =. 1609.04153 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629272

  39. [39]

    Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties

    Gaia Data Release 1. Summary of the astrometric, photometric, and survey properties. , keywords =. doi:10.1051/0004-6361/201629512 , archivePrefix =. 1609.04172 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201629512

  40. [40]

    2018, , 616, A1, 10.1051/0004-6361/201833051

    Gaia Data Release 2. Summary of the contents and survey properties. , keywords =. doi:10.1051/0004-6361/201833051 , archivePrefix =. 1804.09365 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833051

  41. [41]

    Summary of the contents and survey properties

    Gaia Early Data Release 3. Summary of the contents and survey properties. , keywords =. doi:10.1051/0004-6361/202039657 , archivePrefix =. 2012.01533 , primaryClass =

    work page doi:10.1051/0004-6361/202039657 2012

  42. [42]

    , keywords =

    An all-sky proper-motion map of the Sagittarius stream using Gaia DR2. , keywords =. doi:10.1051/0004-6361/201937145 , archivePrefix =. 2001.10012 , primaryClass =

    work page doi:10.1051/0004-6361/201937145 2001

  43. [43]

    , keywords =

    A Panoramic Landscape of the Sagittarius Stream in Gaia DR2 Revealed with the STREAMFINDER Spyglass. , keywords =. doi:10.3847/2041-8213/ab77c7 , archivePrefix =. 2002.11121 , primaryClass =

    work page doi:10.3847/2041-8213/ab77c7 2041

  44. [44]

    , keywords =

    The Sagittarius stream in Gaia Early Data Release 3 and the origin of the bifurcations. , keywords =. doi:10.1051/0004-6361/202142830 , archivePrefix =. 2112.02105 , primaryClass =

    work page doi:10.1051/0004-6361/202142830

  45. [45]

    , keywords =

    StarHorse results for spectroscopic surveys and Gaia DR3: Chrono-chemical populations in the solar vicinity, the genuine thick disk, and young alpha-rich stars. , keywords =. doi:10.1051/0004-6361/202245399 , archivePrefix =. 2303.09926 , primaryClass =

    work page doi:10.1051/0004-6361/202245399

  46. [46]

    2023 , month = jun, journal =

    Gaia Data Release 3. Summary of the content and survey properties. , keywords =. doi:10.1051/0004-6361/202243940 , archivePrefix =. 2208.00211 , primaryClass =

    work page doi:10.1051/0004-6361/202243940

  47. [47]

    Properties and validation of the radial velocities

    Gaia Data Release 3. Properties and validation of the radial velocities. , keywords =. doi:10.1051/0004-6361/202244220 , archivePrefix =. 2206.05902 , primaryClass =

    work page doi:10.1051/0004-6361/202244220

  48. [48]

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

    The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST). Research in Astronomy and Astrophysics , year = 2012, month = sep, volume =. doi:10.1088/1674-4527/12/9/003 , adsurl =

    work page doi:10.1088/1674-4527/12/9/003 2012

  49. [49]

    Research in Astronomy and Astrophysics , year = 2012, month = jul, volume =

    LAMOST spectral survey An overview. Research in Astronomy and Astrophysics , year = 2012, month = jul, volume =. doi:10.1088/1674-4527/12/7/002 , adsurl =

    work page doi:10.1088/1674-4527/12/7/002 2012

  50. [50]

    Detection of the gravitational redshift in the orbit of the star S2 near the Galactic centre massive black hole

    Detection of the gravitational redshift in the orbit of the star S2 near the Galactic centre massive black hole. , keywords =. doi:10.1051/0004-6361/201833718 , archivePrefix =. 1807.09409 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201833718

  51. [51]

    Vertical waves in the solar neighbourhood in Gaia DR2

    Vertical waves in the solar neighbourhood in Gaia DR2. , keywords =. doi:10.1093/mnras/sty2813 , archivePrefix =. 1809.03507 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2813

  52. [52]

    The mass distribution and gravitational potential of the Milky Way

    The mass distribution and gravitational potential of the Milky Way. , keywords =. doi:10.1093/mnras/stw2759 , archivePrefix =. 1608.00971 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2759

  53. [53]

    2010, Monthly Notices of the Royal Astronomical Society, 408, 1181, doi: 10.1111/j.1365-2966.2010.17197.x

    Local kinematics and the local standard of rest. , keywords =. doi:10.1111/j.1365-2966.2010.16253.x , archivePrefix =. 0912.3693 , primaryClass =

    work page doi:10.1111/j.1365-2966.2010.16253.x 2010

  54. [54]

    AGAMA: Action-based galaxy modelling architecture

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

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/sty2672

  55. [55]

    Understanding Deep Neural Networks with Rectified Linear Units

    Understanding Deep Neural Networks with Rectified Linear Units. arXiv e-prints , keywords =. doi:10.48550/arXiv.1611.01491 , archivePrefix =. 1611.01491 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1611.01491

  56. [56]

    , keywords =

    Exploring the Sagittarius stream with RR Lyrae stars from Gaia Data Release 3. , keywords =. doi:10.1051/0004-6361/202555670 , archivePrefix =. 2505.20165 , primaryClass =

    work page doi:10.1051/0004-6361/202555670

  57. [57]

    arXiv e-prints , keywords =

    Reconstructing the whole 6D properties of the Sagittarius stream with N-body simulations. arXiv e-prints , keywords =. doi:10.48550/arXiv.2204.08542 , archivePrefix =. 2204.08542 , primaryClass =

    work page doi:10.48550/arxiv.2204.08542

  58. [58]

    Detection of a population gradient in the Sagittarius Stream

    Detection of a population gradient in the Sagittarius stream. , keywords =. doi:10.1051/0004-6361:20066002 , archivePrefix =. astro-ph/0608513 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20066002

  59. [59]

    A 2MASS All-Sky View of the Sagittarius Dwarf Galaxy. V. Variation of the Metallicity Distribution Function along the Sagittarius Stream. , keywords =. doi:10.1086/522483 , archivePrefix =. astro-ph/0605101 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/522483

  60. [60]

    High-resolution spectroscopy of RGB stars in the Sagittarius streams. I. Radial velocities and chemical abundances. , keywords =. doi:10.1051/0004-6361:20066228 , archivePrefix =. astro-ph/0611070 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361:20066228

  61. [61]

    Kinematics and Chemistry of Stars Along the Sagittarius Trailing Tidal Tail and Constraints on the Milky Way Mass Distribution

    Kinematics and Chemistry of Stars along the Sagittarius Trailing Tidal Tail and Constraints on the Milky Way Mass Distribution. , keywords =. doi:10.1088/0004-637X/744/1/25 , archivePrefix =. 1111.0014 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/744/1/25

  62. [62]

    Discovery of a Dynamical Cold Point in the Heart of the Sagittarius dSph Galaxy with Observations from the APOGEE Project

    Discovery of a Dynamical Cold Point in the Heart of the Sagittarius dSph Galaxy with Observations from the APOGEE Project. , keywords =. doi:10.1088/2041-8205/777/1/L13 , archivePrefix =. 1309.5535 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/2041-8205/777/1/l13 2041

  63. [63]

    Chemical abundances in the nucleus of the Sagittarius dwarf spheroidal galaxy

    Chemical abundances in the nucleus of the Sagittarius dwarf spheroidal galaxy. , keywords =. doi:10.1051/0004-6361/201730707 , archivePrefix =. 1705.03251 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201730707

  64. [64]

    A photometric metallicity analysis of the Sagittarius dwarf spheroidal galaxy

    The Pristine Inner Galaxy Survey (PIGS) - IV. A photometric metallicity analysis of the Sagittarius dwarf spheroidal galaxy. , keywords =. doi:10.1093/mnras/stac2869 , archivePrefix =. 2204.12140 , primaryClass =

    work page doi:10.1093/mnras/stac2869

  65. [65]

    , keywords =

    Chemical Cartography of the Sagittarius Stream with Gaia. , keywords =. doi:10.3847/1538-4357/ad187b , archivePrefix =. 2307.08730 , primaryClass =

    work page doi:10.3847/1538-4357/ad187b

  66. [66]

    , keywords =

    Full 5D characterisation of the Sagittarius stream with Gaia DR2 RR Lyrae. , keywords =. doi:10.1051/0004-6361/202037819 , archivePrefix =. 2002.11142 , primaryClass =

    work page doi:10.1051/0004-6361/202037819 2002

  67. [67]

    , keywords =

    Tracing Kinematic and Chemical Properties of Sagittarius Stream by K-Giants, M-Giants, and BHB stars. , keywords =. doi:10.3847/1538-4357/ab48e2 , archivePrefix =. 1909.12558 , primaryClass =

    work page doi:10.3847/1538-4357/ab48e2 1909

  68. [68]

    , keywords =

    Revisiting a Disky Origin for the Faint Branch of the Sagittarius Stellar Stream. , keywords =. doi:10.3847/2041-8213/ac738c , archivePrefix =. 2205.14902 , primaryClass =

    work page doi:10.3847/2041-8213/ac738c 2041

  69. [69]

    , keywords =

    A Pristine-UNIONS view on the Galaxy: Kinematics of the distant spur feature of the Sagittarius stream traced by blue horizontal branch stars. , keywords =. doi:10.1051/0004-6361/202554131 , archivePrefix =. 2502.17319 , primaryClass =

    work page doi:10.1051/0004-6361/202554131

  70. [70]

    , keywords =

    Mapping the Stellar Halo with the H3 Spectroscopic Survey. , keywords =. doi:10.3847/1538-4357/ab38b8 , archivePrefix =. 1907.07684 , primaryClass =

    work page doi:10.3847/1538-4357/ab38b8 1907

  71. [71]

    SEGUE: A Spectroscopic Survey of 240,000 stars with g=14-20

    SEGUE: A Spectroscopic Survey of 240,000 Stars with g = 14-20. , keywords =. doi:10.1088/0004-6256/137/5/4377 , archivePrefix =. 0902.1781 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-6256/137/5/4377

  72. [72]

    Tracing Sagittarius Structure with SDSS and SEGUE Imaging and Spectroscopy

    Tracing Sagittarius Structure with SDSS and SEGUE Imaging and Spectroscopy. , keywords =. doi:10.1088/0004-637X/700/2/1282 , archivePrefix =. 0905.4502 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/700/2/1282

  73. [73]

    The GALAH Survey: Scientific Motivation

    The GALAH survey: scientific motivation. , keywords =. doi:10.1093/mnras/stv327 , archivePrefix =. 1502.04767 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stv327

  74. [74]

    The GALAH Survey: Observational Overview and Gaia DR1 companion

    The GALAH survey: observational overview and Gaia DR1 companion. , keywords =. doi:10.1093/mnras/stw2835 , archivePrefix =. 1609.02822 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stw2835

  75. [75]

    , keywords =

    The Seventeenth Data Release of the Sloan Digital Sky Surveys: Complete Release of MaNGA, MaStar, and APOGEE-2 Data. , keywords =. doi:10.3847/1538-4365/ac4414 , archivePrefix =. 2112.02026 , primaryClass =

    work page doi:10.3847/1538-4365/ac4414

  76. [76]

    The Sixth Data Release of the Radial Velocity Experiment (RAVE). II. Stellar Atmospheric Parameters, Chemical Abundances, and Distances. , keywords =. doi:10.3847/1538-3881/ab9ab8 , archivePrefix =. 2002.04512 , primaryClass =

    work page doi:10.3847/1538-3881/ab9ab8 2002

  77. [77]

    The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data from SDSS-III

    The Eleventh and Twelfth Data Releases of the Sloan Digital Sky Survey: Final Data from SDSS-III. , keywords =. doi:10.1088/0067-0049/219/1/12 , archivePrefix =. 1501.00963 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0067-0049/219/1/12

  78. [78]

    Galactic Archaeology: Near-Field Cosmology and the Formation of the Milky Way , year = 2012, editor =

    Evolution of the Milky Way: Some Open Issues for Gaia. Galactic Archaeology: Near-Field Cosmology and the Formation of the Milky Way , year = 2012, editor =

    work page 2012

  79. [79]

    , keywords =

    The Gaia-ESO Public Spectroscopic Survey: Implementation, data products, open cluster survey, science, and legacy. , keywords =. doi:10.1051/0004-6361/202243141 , archivePrefix =. 2206.02901 , primaryClass =

    work page doi:10.1051/0004-6361/202243141

  80. [80]

    , keywords =

    Accurate distances to Galactic globular clusters through a combination of Gaia EDR3, HST, and literature data. , keywords =. doi:10.1093/mnras/stab1474 , archivePrefix =. 2105.09526 , primaryClass =

    work page doi:10.1093/mnras/stab1474

Showing first 80 references.