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ISO SWS/LWS observations of SN 1987A

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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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P. Lundqvist, J. Sollerman, C. Kozma, B. Larsson, J. Spyromilio, A.P.S. Crotts, J. Danziger, D. Kunze

Astrophysics · Submitted 29 May 1999

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

The authors' main claim Assessing various uncertainties of the model, we obtain an upper limit of 1.5\EE{-4} solar masses.

how it is stated · asserted 0.98 read the record →

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arXiv IDastro-ph/9905389 (version 1)
Pith IDGLMLLSTL, Pith's permanent record of this paper and its review
CitationA.P.S. Crotts, B. Larsson, C. Kozma, D. Kunze, J. Danziger, J. Sollerman, J. Spyromilio, P. Lundqvist. "ISO SWS/LWS observations of SN 1987A." arXiv:astro-ph/9905389 (1999). https://pith.science/paper/GLMLLSTL
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, 6,890 input tokens, $0.0003 reported.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.83 · human participants 0.01 · controlled comparison 0.03 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.14 · mentions code or data availability 0.02.

The abstract, sentence by sentence

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

We report on observations of SN 1987A with ISO SWS/LWS made 9 - 11 years after the explosion. No emission from the supernova was seen. In particular, the upper limits on the fluxes of [Fe I] 24.05 microns and [Fe II] 25.99 microns on day 3999 are roughly 1.1 Jy and 1.4 Jy, respectively. Assuming a homogeneous distribution of Ti-44 inside 2000 km/s, we have made theoretical models to estimate the mass of ejected Ti-44. Assessing various uncertainties of the model, we obtain an upper limit of 1.5\EE{-4} solar masses. The implications of this are discussed. The LWS data display continuum emission as well as nebular lines of [O I], [C II] and [O III] from neighboring photoexcited regions in the LMC. The [O III] lines indicate an electron density of 120 +/- 75 cm^{-3}, and the continuum can be explained by dust with a temperature of roughly 37 K. A second dust component with approximately 10 K may also be 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 We report on observations of SN 1987A with ISO SWS/LWS made 9 - 11 years after the explosion. contribution 0.91 0.94 0.04 asserted 0.99
s1 No emission from the supernova was seen. result 1.00 0.93 0.40 asserted 1.00
s2 In particular, the upper limits on the fluxes of [Fe I] 24.05 microns and [Fe II] 25.99 microns on day 3999 are roughly 1.1 Jy and 1.4 Jy, respectively. result 1.00 0.93 0.10 asserted 0.98
s3 Assuming a homogeneous distribution of Ti-44 inside 2000 km/s, we have made theoretical models to estimate the mass of ejected Ti-44. method 0.98 0.95 0.04 asserted 0.99
s4 Assessing various uncertainties of the model, we obtain an upper limit of 1.5\EE{-4} solar masses. result 1.00 0.95 0.62 asserted 0.98
s5 The implications of this are discussed. interpretation 1.00 0.29 0.04 unclear 0.92
s6 The LWS data display continuum emission as well as nebular lines of [O I], [C II] and [O III] from neighboring photoexcited regions in the LMC. result 0.99 0.93 0.05 asserted 1.00
s7 The [O III] lines indicate an electron density of 120 +/- 75 cm^{-3}, and the continuum can be explained by dust with a temperature of roughly 37 K. result 0.80 0.89 0.05 asserted 0.68
s8 A second dust component with approximately 10 K may also be present. result 0.94 0.80 0.03 hedged possibility 1.00

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.97.

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 report on observations of SN 1987A with ISO SWS/LWS made 9 - 11 years after the explosion. No emission from the supernova was seen. In particular, the upper limits on the fluxes of [Fe I] 24.05 microns and [Fe II] 25.99 microns on day 3999 are roughly 1.1 Jy and 1.4 Jy, respectively. Assuming a homogeneous distribution of Ti-44 inside 2000 km/s, we have made theoretical models to estimate the mass of ejected Ti-44. Assessing various uncertainties of the model, we obtain an upper limit of 1.5\EE{-4} solar masses. The implications of this are discussed. The LWS data display continuum emission as well as nebular lines of [O I], [C II] and [O III] from neighboring photoexcited regions in the LMC. The [O III] lines indicate an electron density of 120 +/- 75 cm^{-3}, and the continuum can be explained by dust with a temperature of roughly 37 K. A second dust component with approximately 10 K may also be present.

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