INTEGRAL and Swift observations of EXO 2030+375 during a giant outburst

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https://www.aanda.org/articles/aa/abs/2007/12/aa6801-06/aa6801-06.html

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https://doi.org/10.1051/0004-6361:20066801
 http://hdl.handle.net/11603/30017

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UMBC Center for Space Sciences and Technology (CSST) / Center for Research and Exploration in Space Sciences & Technology II (CRSST II)
UMBC Physics Department

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Author/Creator ORCID

https://orcid.org/0000-0002-4656-6881

Date

2007-01-29

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journal articles
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Citation of Original Publication

Klochkov, D., D. Horns, A. Santangelo, R. Staubert, A. Segreto, C. Ferrigno, P. Kretschmar, et al. “INTEGRAL and Swift Observations of EXO 2030+375 during a Giant Outburst.” Astronomy & Astrophysics 464, no. 3 (March 1, 2007): L45–48. https://doi.org/10.1051/0004-6361:20066801.

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Abstract

Aims.We investigate the X-ray spectral and timing properties of the high mass X-ray binary EXO 2030+375 observed during its June–September 2006 giant (type II) outburst. Methods.The data analyzed in this work are from partly simultaneous observations with INTEGRAL and Swift. The pulse period P and its temporal derivative P are measured. X-ray pulse profiles in different energy ranges and time intervals are constructed. Pulse averaged X-ray spectra for different time intervals are studied. Results.We report a strong spin-up of the source during the outburst, comparable to that observed in 1985 during the previous giant outburst when the source was discovered. The value of P is found to be linearly related to the X-ray luminosity of the source during the outburst. For the first time the hard X-ray (>25 keV) characteristics of the source during a type II outburst are studied. The X-ray pulse profiles apparently change with luminosity. The X-ray spectral continuum in the 3–120 keV energy range is modeled with an absorbed power law with an exponential cutoff around E ~ 26 keV. An iron emission line at ~6–7 keV is observed. The spectrum reveals some features between 10 and 20 keV which can be modeled either by a broad emission line at ~13–15 keV (a “bump”) or by two absorption lines at ~10 and ~20 keV.