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The Oxygen Abundance of HE 1327-2326

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Anna Frebel, Norbert Christlieb, John E. Norris, Wako Aoki, Martin Asplund

Astrophysics · Submitted 21 Dec 2005

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

The authors' main claim Using a correction of -1.0 dex to account for 3D effects on OH line formation, the abundances are lowered to [O/Fe] = 2.8 and [O/Fe] = 2.5, respectively, which we adopt.

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arXiv IDastro-ph/0512543 (version 1)
Pith IDMFVDJXSZ, Pith's permanent record of this paper and its review
CitationAnna Frebel, John E. Norris, Martin Asplund, Norbert Christlieb, Wako Aoki. "The Oxygen Abundance of HE 1327-2326." arXiv:astro-ph/0512543 (2005). https://pith.science/paper/MFVDJXSZ
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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.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,449 input tokens.

What the abstract itself states, as probabilities: claims first 0.14 · states limitation 0.90 · human participants 0.01 · controlled comparison 0.10 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.94 · mentions code or data availability 0.02.

The abstract, sentence by sentence

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

From a newly obtained VLT/UVES spectrum we have determined the oxygen abundance of HE 1327-2326, the most iron-poor star known to date. UV-OH lines yield a 1D LTE abundance of [O/Fe]_OH = 3.7 (subgiant case) and [O/Fe]_OH = 3.4 (dwarf case). Using a correction of -1.0 dex to account for 3D effects on OH line formation, the abundances are lowered to [O/Fe] = 2.8 and [O/Fe] = 2.5, respectively, which we adopt. Without 3D corrections, the UV-OH based abundance would be in disagreement with the upper limits derived from the OI triplet lines: [O/Fe]_trip < 2.8 (subgiant) and [O/Fe]_trip < 3.0 (dwarf). We also correct the previously determined carbon and nitrogen abundances for 3D effects. Knowledge of the O abundance of HE 1327-2326 has implications for the interpretation of its abundance pattern. A large O abundance is in accordance with HE 1327-2326 being an early Population II star which formed from material chemically enriched by a first generation supernova. Our derived abundances, however, do not exclude other possibilities such as a Population III scenario.

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 From a newly obtained VLT/UVES spectrum we have determined the oxygen abundance of HE 1327-2326, the most iron-poor star known to date. contribution 0.91 0.97 0.20 asserted 1.00
s1 UV-OH lines yield a 1D LTE abundance of [O/Fe]_OH = 3.7 (subgiant case) and [O/Fe]_OH = 3.4 (dwarf case). result 1.00 0.92 0.11 asserted 1.00
s2 Using a correction of -1.0 dex to account for 3D effects on OH line formation, the abundances are lowered to [O/Fe] = 2.8 and [O/Fe] = 2.5, respectively, which we adopt. result 0.88 0.92 0.48 asserted 1.00
s3 Without 3D corrections, the UV-OH based abundance would be in disagreement with the upper limits derived from the OI triplet lines: [O/Fe]_trip < 2.8 (subgiant) and [O/Fe]_trip < 3.0 (dwarf). result 0.47 0.81 0.09 asserted 0.94
s4 We also correct the previously determined carbon and nitrogen abundances for 3D effects. contribution 0.69 0.92 0.03 asserted 0.99
s5 Knowledge of the O abundance of HE 1327-2326 has implications for the interpretation of its abundance pattern. interpretation 0.90 0.16 0.07 asserted 0.84
s6 A large O abundance is in accordance with HE 1327-2326 being an early Population II star which formed from material chemically enriched by a first generation supernova. interpretation 1.00 0.14 0.16 hedged possibility 0.85
s7 Our derived abundances, however, do not exclude other possibilities such as a Population III scenario. interpretation 0.67 0.61 0.12 hedged possibility 0.82

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

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not examined
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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

From a newly obtained VLT/UVES spectrum we have determined the oxygen abundance of HE 1327-2326, the most iron-poor star known to date. UV-OH lines yield a 1D LTE abundance of [O/Fe]_OH = 3.7 (subgiant case) and [O/Fe]_OH = 3.4 (dwarf case). Using a correction of -1.0 dex to account for 3D effects on OH line formation, the abundances are lowered to [O/Fe] = 2.8 and [O/Fe] = 2.5, respectively, which we adopt. Without 3D corrections, the UV-OH based abundance would be in disagreement with the upper limits derived from the OI triplet lines: [O/Fe]_trip < 2.8 (subgiant) and [O/Fe]_trip < 3.0 (dwarf). We also correct the previously determined carbon and nitrogen abundances for 3D effects. Knowledge of the O abundance of HE 1327-2326 has implications for the interpretation of its abundance pattern. A large O abundance is in accordance with HE 1327-2326 being an early Population II star which formed from material chemically enriched by a first generation supernova. Our derived abundances, however, do not exclude other possibilities such as a Population III scenario.

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