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Star formation history and X-ray binary populations: the case of the Small Magellanic Cloud

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Vallia Antoniou (1, 2, 3), Andreas Zezas (1, 4), Despina Hatzidimitriou (4, 5), Vicky Kalogera (6) ((1) Harvard-Smithsonian Center for Astrophysics
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(2) Physics Department, University of Crete, Greece, (3) Iowa State University, (4) IESL/FORTH, (5) Physics Department, University of Athens, (6) Northwestern University)

High Energy Astrophysical Phenomena · Submitted 11 Jun 2010

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

The authors' main claim The similarity of this age with the age of maximum occurrence of the Be phenomenon (~40 Myr) indicates that the presence of a circumstellar decretion disk plays a significant role in the number of observed XRBs in the 10-100 Myr age range.

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

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arXiv ID1006.2381 (version 1)
Pith IDBUL3PN6E, Pith's permanent record of this paper and its review
Citation2, (2) Physics Department, 3), (3) Iowa State University, 4), (4) IESL/FORTH, 5), (5) Physics Department, (6) Northwestern University), Andreas Zezas (1, Despina Hatzidimitriou (4, Greece, University of Athens, University of Crete, Vallia Antoniou (1, Vicky Kalogera (6) ((1) Harvard-Smithsonian Center for Astrophysics. "Star formation history and X-ray binary populations: the case of the Small Magellanic Cloud." arXiv:1006.2381 (2010). https://pith.science/paper/BUL3PN6E
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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-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 5,115 input tokens, $0.0002 reported.

What the abstract itself states, as probabilities: claims first 0.02 · states limitation 0.21 · human participants 0.01 · controlled comparison 0.13 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.30 · mentions code or data availability 0.02.

The abstract, sentence by sentence

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

Using Chandra, XMM-Newton, and optical photometric catalogs we study the young X-ray binary (XRB) populations of the Small Magellanic Cloud. We find that the Be/X-ray binaries (Be-XRBs) are observed in regions with star formation rate bursts ~25-60 Myr ago. The similarity of this age with the age of maximum occurrence of the Be phenomenon (~40 Myr) indicates that the presence of a circumstellar decretion disk plays a significant role in the number of observed XRBs in the 10-100 Myr age range. We also find that regions with strong but more recent star formation (e.g., the Wing) are deficient in Be-XRBs. By correlating the number of observed Be-XRBs with the formation rate of their parent populations, we measure a Be-XRB production rate of ~1 system per 3 x 10^(-3) M$_{\odot}$/yr. Finally, we use the strong localization of the Be-XRB systems in order to set limits on the kicks imparted on the neutron star during the supernova explosion.

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 Using Chandra, XMM-Newton, and optical photometric catalogs we study the young X-ray binary (XRB) populations of the Small Magellanic Cloud. contribution 0.71 0.93 0.03 asserted 0.80
s1 We find that the Be/X-ray binaries (Be-XRBs) are observed in regions with star formation rate bursts ~25-60 Myr ago. result 1.00 0.96 0.31 asserted 1.00
s2 The similarity of this age with the age of maximum occurrence of the Be phenomenon (~40 Myr) indicates that the presence of a circumstellar decretion disk plays a significant role in the number of observed XRBs in the 10-100 Myr age range. interpretation 1.00 0.62 0.38 hedged possibility 0.94
s3 We also find that regions with strong but more recent star formation (e.g., the Wing) are deficient in Be-XRBs. result 1.00 0.96 0.09 asserted 1.00
s4 By correlating the number of observed Be-XRBs with the formation rate of their parent populations, we measure a Be-XRB production rate of ~1 system per 3 x 10^(-3) M$_{\odot}$/yr. result 1.00 0.97 0.17 asserted 1.00
s5 Finally, we use the strong localization of the Be-XRB systems in order to set limits on the kicks imparted on the neutron star during the supernova explosion. result 0.81 0.95 0.12 asserted 0.97

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from analysis of existing data 0.78.

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
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  • P abstract
not run
  • S sections
  • T body sentences
  • C citations
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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

Using Chandra, XMM-Newton, and optical photometric catalogs we study the young X-ray binary (XRB) populations of the Small Magellanic Cloud. We find that the Be/X-ray binaries (Be-XRBs) are observed in regions with star formation rate bursts ~25-60 Myr ago. The similarity of this age with the age of maximum occurrence of the Be phenomenon (~40 Myr) indicates that the presence of a circumstellar decretion disk plays a significant role in the number of observed XRBs in the 10-100 Myr age range. We also find that regions with strong but more recent star formation (e.g., the Wing) are deficient in Be-XRBs. By correlating the number of observed Be-XRBs with the formation rate of their parent populations, we measure a Be-XRB production rate of ~1 system per 3 x 10^(-3) M$_{\odot}$/yr. Finally, we use the strong localization of the Be-XRB systems in order to set limits on the kicks imparted on the neutron star during the supernova explosion.

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