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Mid-infrared imaging and spectrophotometry of N 66 in the SMC with ISOCAM

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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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A. Contursi (IPAC/CalTech), J. Lequeux (DEMIRM, Observatory of Paris), C. Cesarsky (IAS/University of Paris 11, MPE) et al

Astrophysics · Submitted 13 Jun 2000

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

The authors' main claim We interpret this behavior as due to the destruction of both AIBs carriers and VSGs in a very high ISRF.

how it is stated · hedged possibility 0.38 read the record →

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arXiv IDastro-ph/0006185 (version 1)
Pith ID65Y5CEF2, Pith's permanent record of this paper and its review
CitationA. Contursi (IPAC/CalTech), C. Cesarsky (IAS/University of Paris 11, J. Lequeux (DEMIRM, MPE) et al, Observatory of Paris). "Mid-infrared imaging and spectrophotometry of N 66 in the SMC with ISOCAM." arXiv:astro-ph/0006185 (2000). https://pith.science/paper/65Y5CEF2
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-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 10,229 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.22 · human participants 0.01 · controlled comparison 0.30 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.83 · 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 observations with the mid-infrared camera ISOCAM on board ISO of the major star-forming region N66 in the Small Magellanic Cloud and of its surroundings. These observations were performed with broad filters and the CVF giving a spectral resolution of about 40. In addition, CO(2-1) data are presented, allowing us to identify and study how hot dust relates with the different phases of the Interstellar Medium present in N66. The spectra are dominated by the strong emission of fine structure line. Monochromatic maps have been made in the [NeIII] 15.6 microns and [SIV] 10.5 microns line. There are significant differences between their distributions, due to the effects of density and of shocks. Aromatic Infrared Bands are seen at various places in the field but they are generally faint. They exhibit a variety of shapes and relative intensities, suggesting that a diversity of carbonaceous materials are present. Silicate emission is also clearly visible in the central condensation and in a few others and emission from hot small grains longward of 10 microns is present in the whole region. All these dust components are heated by the very strong far UV radiation of the many young, massive stars contained in the region. The interstellar radiation field (ISRF) at 1600 A is >= 10^5 times the ISRF of the solar neighborhood in the peaks of MIR emission. The relative contributions of the dust components to the MIR spectra seem to depend on the intensity and the hardness of the far UV field. In general the 15/6.75 microns intensity ratio is higher than in relatively quiescent galactic regions but it is not as high as expected for a linear increase with ISRF. We interpret this behavior as due to the destruction of both AIBs carriers and VSGs in a very high ISRF.

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 observations with the mid-infrared camera ISOCAM on board ISO of the major star-forming region N66 in the Small Magellanic Cloud and of its surroundings. contribution 0.98 0.96 0.04 asserted 0.98
s1 These observations were performed with broad filters and the CVF giving a spectral resolution of about 40. method 1.00 0.94 0.02 asserted 1.00
s2 In addition, CO(2-1) data are presented, allowing us to identify and study how hot dust relates with the different phases of the Interstellar Medium present in N66. method 0.60 0.87 0.06 asserted 0.99
s3 The spectra are dominated by the strong emission of fine structure line. result 1.00 0.88 0.04 asserted 1.00
s4 Monochromatic maps have been made in the [NeIII] 15.6 microns and [SIV] 10.5 microns line. method 0.36 0.95 0.04 asserted 1.00
s5 There are significant differences between their distributions, due to the effects of density and of shocks. result 0.75 0.90 0.07 asserted 1.00
s6 Aromatic Infrared Bands are seen at various places in the field but they are generally faint. result 1.00 0.93 0.03 asserted 1.00
s7 They exhibit a variety of shapes and relative intensities, suggesting that a diversity of carbonaceous materials are present. result 0.63 0.89 0.06 hedged possibility 0.97
s8 Silicate emission is also clearly visible in the central condensation and in a few others and emission from hot small grains longward of 10 microns is present in the whole region. result 1.00 0.94 0.06 asserted 1.00
s9 All these dust components are heated by the very strong far UV radiation of the many young, massive stars contained in the region. interpretation 0.89 0.68 0.13 asserted 1.00
s10 The interstellar radiation field (ISRF) at 1600 A is >= 10^5 times the ISRF of the solar neighborhood in the peaks of MIR emission. result 1.00 0.84 0.09 asserted 1.00
s11 The relative contributions of the dust components to the MIR spectra seem to depend on the intensity and the hardness of the far UV field. result 0.84 0.83 0.20 hedged possibility 0.81
s12 In general the 15/6.75 microns intensity ratio is higher than in relatively quiescent galactic regions but it is not as high as expected for a linear increase with ISRF. result 1.00 0.89 0.16 asserted 0.95
s13 We interpret this behavior as due to the destruction of both AIBs carriers and VSGs in a very high ISRF. interpretation 1.00 0.61 0.54 hedged possibility 0.38

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

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 observations with the mid-infrared camera ISOCAM on board ISO of the major star-forming region N66 in the Small Magellanic Cloud and of its surroundings. These observations were performed with broad filters and the CVF giving a spectral resolution of about 40. In addition, CO(2-1) data are presented, allowing us to identify and study how hot dust relates with the different phases of the Interstellar Medium present in N66. The spectra are dominated by the strong emission of fine structure line. Monochromatic maps have been made in the [NeIII] 15.6 microns and [SIV] 10.5 microns line. There are significant differences between their distributions, due to the effects of density and of shocks. Aromatic Infrared Bands are seen at various places in the field but they are generally faint. They exhibit a variety of shapes and relative intensities, suggesting that a diversity of carbonaceous materials are present. Silicate emission is also clearly visible in the central condensation and in a few others and emission from hot small grains longward of 10 microns is present in the whole region. All these dust components are heated by the very strong far UV radiation of the many young, massive stars contained in the region. The interstellar radiation field (ISRF) at 1600 A is >= 10^5 times the ISRF of the solar neighborhood in the peaks of MIR emission. The relative contributions of the dust components to the MIR spectra seem to depend on the intensity and the hardness of the far UV field. In general the 15/6.75 microns intensity ratio is higher than in relatively quiescent galactic regions but it is not as high as expected for a linear increase with ISRF. We interpret this behavior as due to the destruction of both AIBs carriers and VSGs in a very high ISRF.

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