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Heavy Element Dispersion in the Metal-Poor Globular Cluster M92

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Ian U. Roederer (Carnegie Observatories), Christopher Sneden (University of Texas)

Solar and Stellar Astrophysics · Submitted 27 Apr 2011

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

The authors' main claim We present detection of r-process dispersion relative to Fe in 19 red giants of the metal-poor GC M92.

how it is stated · asserted 1.00 read the record →

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arXiv ID1104.5055 (version 2)
Pith IDLHWAOWXE, Pith's permanent record of this paper and its review
CitationChristopher Sneden (University of Texas), Ian U. Roederer (Carnegie Observatories). "Heavy Element Dispersion in the Metal-Poor Globular Cluster M92." arXiv:1104.5055 (2011). https://pith.science/paper/LHWAOWXE
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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.

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Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,281 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.07 · states limitation 0.88 · human participants 0.02 · controlled comparison 0.22 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.95 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v2. Results and the main claim are underlined; .

Dispersion among the light elements is common in globular clusters (GCs), while dispersion among heavier elements is less common. We present detection of r-process dispersion relative to Fe in 19 red giants of the metal-poor GC M92. Using spectra obtained with the Hydra multi-object spectrograph on the WIYN Telescope at Kitt Peak National Observatory, we derive differential abundances for 21 species of 19 elements. The Fe-group elements, plus Y and Zr, are homogeneous at a level of 0.07-0.16 dex. The heavy elements La, Eu, and Ho exhibit clear star-to-star dispersion spanning 0.5-0.8 dex. The abundances of these elements are correlated with one another, and we demonstrate that they were produced by r-process nucleosynthesis. This r-process dispersion is not correlated with the dispersion in C, N, or Na in M92, indicating that r-process inhomogeneities were present in the gas throughout star formation. The r-process dispersion is similar to that previously observed in the metal-poor GC M15, but its origin in M15 or M92 is unknown at present.

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 Dispersion among the light elements is common in globular clusters (GCs), while dispersion among heavier elements is less common. background 1.00 0.04 0.04 asserted 1.00
s1 We present detection of r-process dispersion relative to Fe in 19 red giants of the metal-poor GC M92. result 0.51 0.97 0.56 asserted 1.00
s2 Using spectra obtained with the Hydra multi-object spectrograph on the WIYN Telescope at Kitt Peak National Observatory, we derive differential abundances for 21 species of 19 elements. method 1.00 0.97 0.03 asserted 1.00
s3 The Fe-group elements, plus Y and Zr, are homogeneous at a level of 0.07-0.16 dex. result 1.00 0.92 0.05 asserted 1.00
s4 The heavy elements La, Eu, and Ho exhibit clear star-to-star dispersion spanning 0.5-0.8 dex. result 1.00 0.94 0.52 asserted 1.00
s5 The abundances of these elements are correlated with one another, and we demonstrate that they were produced by r-process nucleosynthesis. interpretation 0.62 0.94 0.29 asserted 1.00
s6 This r-process dispersion is not correlated with the dispersion in C, N, or Na in M92, indicating that r-process inhomogeneities were present in the gas throughout star formation. interpretation 0.85 0.92 0.25 hedged possibility 0.58
s7 The r-process dispersion is similar to that previously observed in the metal-poor GC M15, but its origin in M15 or M92 is unknown at present. limitation 0.37 0.38 0.08 asserted 0.81

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.99.

What was examined, and what was not

sources read
  • arXiv listing abstract v2
not examined
  • full text
  • figures and tables
  • references and citing sentences
  • relations to other papers
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  • P abstract
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  • 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

Dispersion among the light elements is common in globular clusters (GCs), while dispersion among heavier elements is less common. We present detection of r-process dispersion relative to Fe in 19 red giants of the metal-poor GC M92. Using spectra obtained with the Hydra multi-object spectrograph on the WIYN Telescope at Kitt Peak National Observatory, we derive differential abundances for 21 species of 19 elements. The Fe-group elements, plus Y and Zr, are homogeneous at a level of 0.07-0.16 dex. The heavy elements La, Eu, and Ho exhibit clear star-to-star dispersion spanning 0.5-0.8 dex. The abundances of these elements are correlated with one another, and we demonstrate that they were produced by r-process nucleosynthesis. This r-process dispersion is not correlated with the dispersion in C, N, or Na in M92, indicating that r-process inhomogeneities were present in the gas throughout star formation. The r-process dispersion is similar to that previously observed in the metal-poor GC M15, but its origin in M15 or M92 is unknown at present.

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References
How the literature uses it

2 arXiv papers cite this in 6 sentences

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

Papers whose main result relates to this one's

Found among the papers closest to this one by title and main claim. Pith's classifier compared each pair's main results and a second model family confirmed the relation; checked against two further families, shown conflicts agreed 118 times in 120 and shown same results 218 times in 239. The quoted sentence is the other paper's main claim.

States a conflicting result 1 paper
  • Although there have been recent claims that there is a large dispersion in the abundances of the heavy neutron capture elements in the old Galactic globular cluster M92, we show that the measured dispersion for the absolute abundances of four of the rare earth elements within a sample of 12 luminous red giants in M92 (less than or equal to 0.07 dex) does not exceed the relevant sources of uncertainty.

    No Heavy Element Dispersion in the Globular Cluster M92 · 0.97

Papers citing it · 4 sentences without a confident label

Uses its data or values 1 paper
  • lccccc Correlations among Abundance Ratios 0pt Cluster (References) 5cRatio Pair 2-6 [La/Fe] $+$ [Eu/Fe] [La/Fe] $+$ [Na/Fe] [Eu/Fe] $+$ [Na/Fe] M3 [ref] (0.64, 20, 0.00024) ($-$0.20, 20, 0.39) (0.12, 22, 0.60) M3 [ref] (0.35, 7, 0.45) ($-$0.21, 7, 0.65) ($-$0.24, 8, 0.57) M5 [ref] (0.43, 25, 0.034) ($-$0.25, 25, 0.22) ($-$0.16, 25, 0.45) M5 [ref] (0.80, 17, 0.00010) (0.10, 17, 0.70) (0.16, 17, 0.55) M12 [ref] (-0.31, 21, 0.17) ($-$0.37, 11, 0.26) (0.41, 11, 0.21) M13 [ref] (0.72, 18, 0.00066) ($-$0.51, 18, 0.029) ($-$0.40, 18, 0.099) M13 [ref] (0.07, 11, 0.83) ($-$0.23, 12, 0.47) (0.43, 12, 0.16) M15 [ref] (0.97, 6, 0.0011) M15 [ref] (0.89, 9, 0.0012) (0.02, 9, 0.95) ($-$0.12, 9, 0.77) M22 [ref] a ($-$0.07, 21, 0.75) ($-$0.13, 21, 0.56) (0.21, 21, 0.36) M80 [ref] (0.37, 8, 0.37) (0.23, 10, 0.52)b (0.66, 8, 0.075)b M92 [ref] (0.49, 16, 0.052) ($-$0.02, 13, 0.95) ($-$0.24, 12, 0.45) NGC 1

    Primordial r-process Dispersion in Metal-Poor Globular Clusters · Literature Data · 0.98

Cites it as support 1 paper

What it cites · 1 sentence without a confident label

Cites as background 1 paper
  • While the heaviest elements in most metal-poor GCs have been produced primarily by rapid ($r$) nucleosynthesis, some GCs have been enriched by a significant amount of material produced in the slow ($s$) process (M4, [ref] , [ref] ; M22, [ref] ; , [ref] , [ref] , [ref] , [ref] ; $ω$ Centauri, e.g., [ref] , [ref] ).

    The two metallicity groups of the globular cluster M22: a chemical perspective · Introduction · 0.83

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