Pith. Sign in

RECORD

The Interstellar Medium of Star-forming Irregular Galaxies: The View with ISO

PaperPDF from arXiv

data files

Paper breakdownThe authors' claims, conditions and measurements, as JSON Signed receiptProof this review has not been altered
X Bluesky LinkedIn Reddit Hacker News
D. Hunter (1), M. Kaufman (2), D. Hollenbach (3), R. Rubin (3), S. Malhotra (4), D. Dale (5), J. Brauher (5), N. Silbermann (5)
show 7 more authors
G. Helou (5), A. Contursi (5), S. Lord (5) ((1) Lowell Observatory, (2) San Jose State University, (3) NASA/Ames Research Center, (4) Johns Hopkins University, (5) IPAC)

Astrophysics · Submitted 15 Dec 2000

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

The authors' main claim These data are combined with PDR and HII region models to deduce properties of the interstellar medium of these galaxies.

how it is stated · asserted 1.00 read the record →

Comment (0) Read on arXiv ↗
Cite ▾
arXiv IDastro-ph/0012354 (version 1)
Pith IDRBFZ7R6R, Pith's permanent record of this paper and its review
Citation(2) San Jose State University, (3) NASA/Ames Research Center, (4) Johns Hopkins University, (5) IPAC), A. Contursi (5), D. Dale (5), D. Hollenbach (3), D. Hunter (1), G. Helou (5), J. Brauher (5), M. Kaufman (2), N. Silbermann (5), R. Rubin (3), S. Lord (5) ((1) Lowell Observatory, S. Malhotra (4). "The Interstellar Medium of Star-forming Irregular Galaxies: The View with ISO." arXiv:astro-ph/0012354 (2000). https://pith.science/paper/RBFZ7R6R
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, 5,095 input tokens.

What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.08 · human participants 0.01 · controlled comparison 0.03 · randomized assignment 0.01 · states quantitative result 0.49 · compares with prior results 0.06 · 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 mid-infrared imaging and far-infrared (FIR) spectroscopy of 5 IBm galaxies observed by ISO as part of our larger study of the inter- stellar medium of galaxies. Most of the irregulars in our sample are very actively forming stars. The mid-infrared imaging was in a band centered at 6.75 microns that is dominated by polycyclic aromatic hydrocarbons (PAHs) and in a band centered at 15 microns that is dominated by small dust grains. The spectroscopy of 3 of the galaxies includes [CII]158 microns and [OI]63 microns, important coolants of photodissociation regions (PDRs), and [OIII]88 microns and [NII]122 microns, which come from ionized gas. [OI]145 microns and [OIII]52 microns were measured in one galaxy as well. These data are combined with PDR and HII region models to deduce properties of the interstellar medium of these galaxies.

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 mid-infrared imaging and far-infrared (FIR) spectroscopy of 5 IBm galaxies observed by ISO as part of our larger study of the inter- stellar medium of galaxies. contribution 0.90 0.95 0.04 asserted 1.00
s1 Most of the irregulars in our sample are very actively forming stars. result 0.72 0.75 0.06 asserted 1.00
s2 The mid-infrared imaging was in a band centered at 6.75 microns that is dominated by polycyclic aromatic hydrocarbons (PAHs) and in a band centered at 15 microns that is dominated by small dust grains. method 0.99 0.87 0.03 asserted 1.00
s3 The spectroscopy of 3 of the galaxies includes [CII]158 microns and [OI]63 microns, important coolants of photodissociation regions (PDRs), and [OIII]88 microns and [NII]122 microns, which come from ionized gas. method 0.82 0.90 0.03 asserted 1.00
s4 [OI]145 microns and [OIII]52 microns were measured in one galaxy as well. method 0.50 0.93 0.03 asserted 1.00
s5 These data are combined with PDR and HII region models to deduce properties of the interstellar medium of these galaxies. method 0.91 0.90 0.19 asserted 1.00

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.91.

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 mid-infrared imaging and far-infrared (FIR) spectroscopy of 5 IBm galaxies observed by ISO as part of our larger study of the inter- stellar medium of galaxies. Most of the irregulars in our sample are very actively forming stars. The mid-infrared imaging was in a band centered at 6.75 microns that is dominated by polycyclic aromatic hydrocarbons (PAHs) and in a band centered at 15 microns that is dominated by small dust grains. The spectroscopy of 3 of the galaxies includes [CII]158 microns and [OI]63 microns, important coolants of photodissociation regions (PDRs), and [OIII]88 microns and [NII]122 microns, which come from ionized gas. [OI]145 microns and [OIII]52 microns were measured in one galaxy as well. These data are combined with PDR and HII region models to deduce properties of the interstellar medium of these galaxies.

Human review

How Pith checks papers → · Full audit of this paper →

Discussion

Know something about this paper? Leave a comment, or highlight any passage above to comment on it.