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RXTE Observations of an Outburst of Recurrent X-ray Nova GS 1354-644

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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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Mikhail G. Revnivtsev (1, 2), Konstantin N. Borozdin (2, 1), William C. Priedhorsky(2), Alexey Vikhlinin(3) ((1)-Space Research Institute, Moscow, Russia; (2)-LANL
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Los Alamos, NM, USA; (3)-Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA)

Astrophysics · Submitted 28 May 1999

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

The authors' main claim We note a qualitative difference in the shape of the dependence of fractional variability on energy, when we compare systems with black holes and with neutron stars.

how it is stated · asserted 0.99 read the record →

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arXiv IDastro-ph/9905380 (version 3)
Pith IDOBTVLNIR, Pith's permanent record of this paper and its review
Citation1), 2), Alexey Vikhlinin(3) ((1)-Space Research Institute, Cambridge, Konstantin N. Borozdin (2, Los Alamos, MA, Mikhail G. Revnivtsev (1, Moscow, NM, Russia; (2)-LANL, USA), USA; (3)-Harvard-Smithsonian Center for Astrophysics, William C. Priedhorsky(2). "RXTE Observations of an Outburst of Recurrent X-ray Nova GS 1354-644." arXiv:astro-ph/9905380 (1999). https://pith.science/paper/OBTVLNIR
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, 10,729 input tokens, $0.0005 reported.

What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.48 · human participants 0.01 · controlled comparison 0.19 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.95 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v3. Results and the main claim are underlined; .

We present the results of Rossi X-ray Timing Explorer observations of GS 1354-644 during a modest outburst in 1997-1998. The source is one of a handful of black hole X-ray transients that are confirmed to be recurrent in X-rays. A 1987 outburst of the same source observed by Ginga was much brighter, and showed a high/soft spectral state. In contrast the 1997-1998 outburst showed a low/hard spectral state. Both states are typical for black hole binaries. The RXTE All Sky Monitor observed an outburst duration of 150 to 200 days. PCA and HEXTE observations covered ~70 days near the maximum of the light curve and during the flux decline. Throughout the observations, the spectrum can be approximated by Compton upscattering of soft photons by energetic electrons. The hot electron cloud has a temperature kT ~30 keV and optical depth tau~4--5. To fit the data well an additional iron fluorescent line and reflection component are required, which indicates the presence of optically thick cool material, most probably in the outer part of the accretion disk. Dramatic fast variability was observed, and has been analyzed in the context of a shot noise model. The spectrum appeared to be softest at the peaks of the shot-noise variability. The shape of the power spectrum was typical for black hole systems in a low/hard state. We note a qualitative difference in the shape of the dependence of fractional variability on energy, when we compare systems with black holes and with neutron stars. Since it is difficult to discriminate these systems on spectral grounds, at least in their low/hard states, this new difference might be important.

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 Rossi X-ray Timing Explorer observations of GS 1354-644 during a modest outburst in 1997-1998. contribution 0.99 0.95 0.05 asserted 0.98
s1 The source is one of a handful of black hole X-ray transients that are confirmed to be recurrent in X-rays. background 0.99 0.11 0.05 asserted 1.00
s2 A 1987 outburst of the same source observed by Ginga was much brighter, and showed a high/soft spectral state. background 0.96 0.09 0.04 asserted 1.00
s3 In contrast the 1997-1998 outburst showed a low/hard spectral state. result 1.00 0.85 0.10 asserted 1.00
s4 Both states are typical for black hole binaries. background 0.52 0.13 0.06 asserted 1.00
s5 The RXTE All Sky Monitor observed an outburst duration of 150 to 200 days. result 0.89 0.83 0.03 asserted 1.00
s6 PCA and HEXTE observations covered ~70 days near the maximum of the light curve and during the flux decline. method 0.98 0.88 0.02 asserted 1.00
s7 Throughout the observations, the spectrum can be approximated by Compton upscattering of soft photons by energetic electrons. result 0.92 0.90 0.14 asserted 0.92
s8 The hot electron cloud has a temperature kT ~30 keV and optical depth tau~4--5. result 0.99 0.90 0.07 asserted 1.00
s9 To fit the data well an additional iron fluorescent line and reflection component are required, which indicates the presence of optically thick cool material, most probably in the outer part of the accretion disk. interpretation 0.77 0.92 0.16 hedged possibility 0.97
s10 Dramatic fast variability was observed, and has been analyzed in the context of a shot noise model. result 0.95 0.94 0.07 asserted 0.99
s11 The spectrum appeared to be softest at the peaks of the shot-noise variability. result 1.00 0.91 0.07 asserted 0.95
s12 The shape of the power spectrum was typical for black hole systems in a low/hard state. result 0.97 0.88 0.09 asserted 1.00
s13 We note a qualitative difference in the shape of the dependence of fractional variability on energy, when we compare systems with black holes and with neutron stars. result 0.84 0.78 0.27 asserted 0.99
s14 Since it is difficult to discriminate these systems on spectral grounds, at least in their low/hard states, this new difference might be important. interpretation 1.00 0.47 0.24 speculative 0.94

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.87.

What was examined, and what was not

sources read
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not examined
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  • references and citing sentences
  • relations to other papers
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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

We present the results of Rossi X-ray Timing Explorer observations of GS 1354-644 during a modest outburst in 1997-1998. The source is one of a handful of black hole X-ray transients that are confirmed to be recurrent in X-rays. A 1987 outburst of the same source observed by Ginga was much brighter, and showed a high/soft spectral state. In contrast the 1997-1998 outburst showed a low/hard spectral state. Both states are typical for black hole binaries. The RXTE All Sky Monitor observed an outburst duration of 150 to 200 days. PCA and HEXTE observations covered ~70 days near the maximum of the light curve and during the flux decline. Throughout the observations, the spectrum can be approximated by Compton upscattering of soft photons by energetic electrons. The hot electron cloud has a temperature kT ~30 keV and optical depth tau~4--5. To fit the data well an additional iron fluorescent line and reflection component are required, which indicates the presence of optically thick cool material, most probably in the outer part of the accretion disk. Dramatic fast variability was observed, and has been analyzed in the context of a shot noise model. The spectrum appeared to be softest at the peaks of the shot-noise variability. The shape of the power spectrum was typical for black hole systems in a low/hard state. We note a qualitative difference in the shape of the dependence of fractional variability on energy, when we compare systems with black holes and with neutron stars. Since it is difficult to discriminate these systems on spectral grounds, at least in their low/hard states, this new difference might be important.

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