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Fe K Emission Lines in Low-luminosity AGNs

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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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Yuichi Terashima (1, 2), Naoko Iyomoto (1), Luis C. Ho (3), Andrew F. Ptak (4) ((1) ISAS, (2) Univ. of Maryland, (3) Carnegie Observatories, (4) Johns Hopkins Univ.)

Astrophysics · Submitted 28 Feb 2002

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

The authors' main claim The weakness of the Fe line is consistent with the absence of an optically thick disk in the vicinity of a central black hole.

how it is stated · hedged possibility 0.94 read the record →

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arXiv IDastro-ph/0202511 (version 1)
Pith IDJBRTRU47, Pith's permanent record of this paper and its review
Citation2), (2) Univ. of Maryland, (3) Carnegie Observatories, (4) Johns Hopkins Univ.), Andrew F. Ptak (4) ((1) ISAS, Luis C. Ho (3), Naoko Iyomoto (1), Yuichi Terashima (1. "Fe K Emission Lines in Low-luminosity AGNs." arXiv:astro-ph/0202511 (2002). https://pith.science/paper/JBRTRU47
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.

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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,236 input tokens.

What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.68 · human participants 0.01 · controlled comparison 0.74 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.93 · 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 results of a systematic analysis of Fe K emission lines in low-luminosity AGNs (LLAGNs) observed with ASCA. We used a sample of LLAGNs with small intrinsic absorption to compare with luminous AGNs and accretion models. Some objects show an Fe line at 6.4 keV or 6.7 keV, and the rest of the objects show no significant Fe K emission line. We made a composite spectrum of sources without detected Fe emission lines to search for weak lines and obtained an upper limit on the equivalent width (EW) of a narrow line at 6.4 keV of 145 eV, which is marginally consistent with EWs seen in Seyfert 1s. Even in those objects with detected Fe lines, a skewed broad component, typically observed in Seyfert 1s, is not seen. The weakness of the Fe line is consistent with the absence of an optically thick disk in the vicinity of a central black hole. Alternatively, it might be due to the ionization of a standard disk. The lack of big blue bump favors the former.

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 results of a systematic analysis of Fe K emission lines in low-luminosity AGNs (LLAGNs) observed with ASCA. contribution 1.00 0.96 0.05 asserted 0.95
s1 We used a sample of LLAGNs with small intrinsic absorption to compare with luminous AGNs and accretion models. method 0.93 0.85 0.03 asserted 0.97
s2 Some objects show an Fe line at 6.4 keV or 6.7 keV, and the rest of the objects show no significant Fe K emission line. result 1.00 0.91 0.12 asserted 1.00
s3 We made a composite spectrum of sources without detected Fe emission lines to search for weak lines and obtained an upper limit on the equivalent width (EW) of a narrow line at 6.4 keV of 145 eV, which is marginally consistent with EWs seen in Seyfert 1s. result 0.95 0.97 0.12 asserted 0.58
s4 Even in those objects with detected Fe lines, a skewed broad component, typically observed in Seyfert 1s, is not seen. result 1.00 0.89 0.13 asserted 1.00
s5 The weakness of the Fe line is consistent with the absence of an optically thick disk in the vicinity of a central black hole. interpretation 1.00 0.55 0.52 hedged possibility 0.94
s6 Alternatively, it might be due to the ionization of a standard disk. interpretation 1.00 0.11 0.06 speculative 0.96
s7 The lack of big blue bump favors the former. interpretation 0.97 0.54 0.20 asserted 0.64

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from analysis of existing data 0.95.

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 results of a systematic analysis of Fe K emission lines in low-luminosity AGNs (LLAGNs) observed with ASCA. We used a sample of LLAGNs with small intrinsic absorption to compare with luminous AGNs and accretion models. Some objects show an Fe line at 6.4 keV or 6.7 keV, and the rest of the objects show no significant Fe K emission line. We made a composite spectrum of sources without detected Fe emission lines to search for weak lines and obtained an upper limit on the equivalent width (EW) of a narrow line at 6.4 keV of 145 eV, which is marginally consistent with EWs seen in Seyfert 1s. Even in those objects with detected Fe lines, a skewed broad component, typically observed in Seyfert 1s, is not seen. The weakness of the Fe line is consistent with the absence of an optically thick disk in the vicinity of a central black hole. Alternatively, it might be due to the ionization of a standard disk. The lack of big blue bump favors the former.

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