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ARGOS IV: The Kinematics of the Milky Way Bulge

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Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
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M. Ness, K. Freeman, E. Athanassoula, E. Wylie-de-Boer, J. Bland-Hawthorn, M. Asplund, G.F Lewis, D. Yong
show 3 more authors
R.R. Lane, L.L Kiss, R. Ibata

Astrophysics of Galaxies · Submitted 26 Mar 2013

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We do not exclude an underlying merger generated bulge component but our results favour bulge formation from instabilities in the early thin disk.

how it is stated · hedged possibility 0.92 read the record →

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arXiv ID1303.6656 (version 1)
Pith IDNSFMPDSM, Pith's permanent record of this paper and its review
CitationD. Yong, E. Athanassoula, E. Wylie-de-Boer, G.F Lewis, J. Bland-Hawthorn, K. Freeman, L.L Kiss, M. Asplund, M. Ness, R. Ibata, R.R. Lane. "ARGOS IV: The Kinematics of the Milky Way Bulge." arXiv:1303.6656 (2013). https://pith.science/paper/NSFMPDSM
Claim paper

The compiled record

The paper's own sentences, arranged. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Open the compiled record

Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 7,191 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.80 · human participants 0.02 · controlled comparison 0.10 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.51 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; .

We present the kinematic results from our ARGOS spectroscopic survey of the Galactic bulge of the Milky Way. Our aim is to understand the formation of the Galactic bulge. We examine the kinematics of about 17,400 stars in the bulge located within 3.5 kpc of the Galactic centre, identified from the 28,000 star ARGOS survey. We aim to determine if the formation of the bulge has been internally driven from disk instabilities as suggested by its boxy shape, or if mergers have played a significant role as expected from Lambda CDM simulations. From our velocity measurements across latitudes b = -5 deg, -7.5 deg and -10 deg we find the bulge to be a cylindrically rotating system that transitions smoothly out into the disk. Within the bulge, we find a kinematically distinct metal-poor population ([Fe/H] < -1.0) that is not rotating cylindrically. The 5% of our stars with [Fe/H] < -1.0 are a slowly rotating spheroidal population, which we believe are stars of the metal weak thick disk and halo which presently lie in the inner Galaxy. The kinematics of the two bulge components that we identified in ARGOS paper III (mean [Fe/H] = -0.25 and [Fe/H] = +0.15, respectively) demonstrate that they are likely to share a common formation origin and are distinct from the more metal poor populations of the thick disk and halo which are colocated inside the bulge. We do not exclude an underlying merger generated bulge component but our results favour bulge formation from instabilities in the early thin disk.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#sentencerolethe authors' own workstates the main conclusionstrength
s0 We present the kinematic results from our ARGOS spectroscopic survey of the Galactic bulge of the Milky Way. contribution 1.00 0.94 0.03 asserted 0.96
s1 Our aim is to understand the formation of the Galactic bulge. background 0.65 0.16 0.02 asserted 0.63
s2 We examine the kinematics of about 17,400 stars in the bulge located within 3.5 kpc of the Galactic centre, identified from the 28,000 star ARGOS survey. contribution 0.62 0.91 0.03 asserted 0.96
s3 We aim to determine if the formation of the bulge has been internally driven from disk instabilities as suggested by its boxy shape, or if mergers have played a significant role as expected from Lambda CDM simulations. background 0.45 0.11 0.03 hedged possibility 0.82
s4 From our velocity measurements across latitudes b = -5 deg, -7.5 deg and -10 deg we find the bulge to be a cylindrically rotating system that transitions smoothly out into the disk. result 1.00 0.98 0.38 asserted 1.00
s5 Within the bulge, we find a kinematically distinct metal-poor population ([Fe/H] < -1.0) that is not rotating cylindrically. result 1.00 0.97 0.11 asserted 1.00
s6 The 5% of our stars with [Fe/H] < -1.0 are a slowly rotating spheroidal population, which we believe are stars of the metal weak thick disk and halo which presently lie in the inner Galaxy. interpretation 0.76 0.89 0.09 hedged possibility 0.57
s7 The kinematics of the two bulge components that we identified in ARGOS paper III (mean [Fe/H] = -0.25 and [Fe/H] = +0.15, respectively) demonstrate that they are likely to share a common formation origin and are distinct from the more metal poor populations of the thick disk and halo which are colocated inside the bulge. interpretation 0.78 0.90 0.23 hedged possibility 0.84
s8 We do not exclude an underlying merger generated bulge component but our results favour bulge formation from instabilities in the early thin disk. interpretation 0.99 0.77 0.58 hedged possibility 0.92

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.85.

What was examined, and what was not

sources read
  • arXiv listing abstract v1
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
levels run
  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
  • R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper
Original abstract

We present the kinematic results from our ARGOS spectroscopic survey of the Galactic bulge of the Milky Way. Our aim is to understand the formation of the Galactic bulge. We examine the kinematics of about 17,400 stars in the bulge located within 3.5 kpc of the Galactic centre, identified from the 28,000 star ARGOS survey. We aim to determine if the formation of the bulge has been internally driven from disk instabilities as suggested by its boxy shape, or if mergers have played a significant role as expected from Lambda CDM simulations. From our velocity measurements across latitudes b = -5 deg, -7.5 deg and -10 deg we find the bulge to be a cylindrically rotating system that transitions smoothly out into the disk. Within the bulge, we find a kinematically distinct metal-poor population ([Fe/H] < -1.0) that is not rotating cylindrically. The 5% of our stars with [Fe/H] < -1.0 are a slowly rotating spheroidal population, which we believe are stars of the metal weak thick disk and halo which presently lie in the inner Galaxy. The kinematics of the two bulge components that we identified in ARGOS paper III (mean [Fe/H] = -0.25 and [Fe/H] = +0.15, respectively) demonstrate that they are likely to share a common formation origin and are distinct from the more metal poor populations of the thick disk and halo which are colocated inside the bulge. We do not exclude an underlying merger generated bulge component but our results favour bulge formation from instabilities in the early thin disk.

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References
How later papers used it

45 later papers cite it

Evidence: substantial. 33 of the citing papers share no author with it, and 12 of those carry a confident label from Pith's citation classifier.

Pith read 13 of the 100 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

Uses its method or tool 1 of 3 papers with this label · 1 by the same authors

By the same authors

Uses its data or values 1 of 8 papers with this label · 1 by the same authors

By the same authors

Compares with it 1 of 7 papers with this label · 1 by the same authors

By the same authors

  • Found that bin A stars give the main mass support to the bar, although this paper found bin B to be the most populated metallicity bin in the data.

    Chemodynamical Modelling of the Galactic Bulge and Bar (2017) (same authors) · 0.84 · paraphrased: the licence does not allow quoting

How the literature uses it

What this paper does with the arXiv papers it cites

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

What it cites · 1 sentence without a confident label

Uses the method or tool of 1 paper
  • The stellar parameters were derived from a $χ^2$ comparison with synthetic spectra generated in the 1D Local Thermal Equilibrium (LTE) stellar synthesis program MOOG [ref] using the Castelli/Kurucz model atmospheres [ref] .

    New Grids of ATLAS9 Model Atmospheres · Observations and Strategy · 1.00

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