M. A. P. Torres et al. 2008 ApJ 672 1079 doi:10.1086/523831
Observations of the 599 Hz Accreting X-Ray Pulsar IGR J00291+5934 during the 2004 Outburst and in Quiescence
FREE ISSUEM. A. P. Torres1, P. G. Jonker1,2,3, D. Steeghs1, G. H. A. Roelofs4, J. S. Bloom5, J. Casares6, E. E. Falco1, M. R. Garcia1, T. R. Marsh7, M. Mendez2,3,8, J. M. Miller1,9, G. Nelemans4 and P. Rodríguez-Gil6
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23 to R 17 and from K = 19 to K 16. Spectral analysis of the RIJHK broadband photometry shows excess in the near-infrared bands that may be due to synchrotron emission. The Hα emission line profile suggests the orbital inclination is 22°-32°. The preferred range for the reddening toward the source is 0.7 ≤ E(B − V) ≤ 0.9, which is equivalent to 4.06 × 1021 cm −2 ≤ NH ≤ 5.22 × 1021 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) × 10−14 ergs cm−2 s−1 (adopting a hydrogen column of 4.6 × 1021 cm−2). The fit resulted in a power-law photon index of 2.4+ 0.5−0.4. 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 <3 × 108 G.
- Subject headings
accretion, accretion disks; binaries: close; stars: individual (IGR J00291+5934); X-rays: stars
- Dates
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Issue 2 (2008 January 10)
Received 2007 January 4, accepted for publication 2007 August 16
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Observations of the 599 Hz Accreting X-Ray Pulsar IGR J00291+5934 during the 2004 Outburst and in Quiescence
M. A. P. Torres et al. 2008 ApJ 672 1079
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