Torres, M. A. P., Jonker, P. G., Steeghs, D., Roelofs, Gijs H. A., Bloom, Joshua S., Casares, J., Falco, E. E., Garcia, M. R., Marsh, T. R., Mendez, M. M., Miller, J. M., Nelemans, G. and Rodriguez-Gil, P. (2008) Observations of the 599 Hz accreting X-ray pulsar IGR J00291+5934 during the 2004 outburst and in quiescence. Astrophysical Journal, Vol.672 (No.2). pp. 1079-1090. doi:10.1086/523831 ISSN 0004-637X.

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Abstract

We report on optical and near-infrared observations obtained during and after the 2004 December discovery outburst of the X-ray transient and accretion-powered millisecond pulsar IGR J00291+5934. Our observations monitored the evolution of the brightness and the spectral properties of IGR J00291+5934 during the outburst decay toward quiescence. We also present optical, near-infrared, and Chandra observations obtained during true quiescence. Photometry of the field during outburst reveals an optical and near-infrared counterpart that brightened from R similar or equal to 23 to R similar or equal to 17 and from K = 19 to K similar or equal to 16. Spectral analysis of the RIJHK broadband photometry shows excess in the near-infrared bands that may be due to synchrotron emission. The H alpha emission line profile suggests the orbital inclination is similar or equal to 22 degrees-32 degrees. The preferred range for the reddening toward the source is 0.7 <= E(B - V) <= 0: 9, which is equivalent to 4.06 x 10(21) cm(-2) <= N-H <= 5.22 x 10(21) cm(-2). The Chandra observations of the pulsar in its quiescent state gave an unabsorbed 0.5-10 keV flux for the best-fitting power-law model to the source spectrum of (7.0 +/- 0.9)x10(-14) ergs cm(-2) s(-1) (adopting a hydrogen column of 4.6x10(21) cm(-2)). The fit resulted in a power-law photon index of 2.4(-0.4)(+0.5). The (R - K)(0) color observed during quiescence supports an irradiated donor star and accretion disk. We estimate a distance of 2-4 kpc toward IGR J00291+ 5934 by using the outburst X-ray light curve and the estimated critical X-ray luminosity necessary to keep the outer parts of the accretion disk ionized. Using the quiescent X-ray luminosity and the spin period, we constrain the magnetic field of the neutron star to be <3x10(8) G.

Item Type:	Journal Article
Subjects:	Q Science > QB Astronomy
Divisions:	Faculty of Science, Engineering and Medicine > Science > Physics
Library of Congress Subject Headings (LCSH):	Pulsars
Journal or Publication Title:	Astrophysical Journal
Publisher:	IOP Publishing
ISSN:	0004-637X
Official Date:	10 January 2008
Dates:	Date Event 10 January 2008 Published
Volume:	Vol.672
Number:	No.2
Number of Pages:	12
Page Range:	pp. 1079-1090
DOI:	10.1086/523831
Status:	Peer Reviewed
Publication Status:	Published
Access rights to Published version:	Restricted or Subscription Access
Date of first compliant deposit:	14 December 2015
Date of first compliant Open Access:	14 December 2015
Funder:	Smithsonian Astrophysical Observatory, United States. National Aeronautics and Space Administration (NASA), Alfred P. Sloan Foundation, Harvard University, University of California, Berkeley, Particle Physics and Astronomy Research Council (Great Britain) (PPARC)
Grant number:	NAG5-10889 (NASA), NAS8-39073 (NASA)

Data sourced from Thomson Reuters' Web of Knowledge

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