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IGR J17252-3616: an accreting pulsar observed by INTEGRAL and XMM-Newton

J. A. Zurita Heras·G. De Cesare·R. Walter·A. Bodaghee·G. Belanger·T. Courvoisier·S. E. Shaw·J. B. Stephen
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Abstract

The discovery of the X-ray source IGR J17252-3616 by INTEGRAL was reported on 9 February 2004. Regular monitoring by INTEGRAL shows that IGR J17252-3616 is a persistent hard X-ray source with an average count rate of 0.96 counts/s (~6.4 mCrab) in the 20-60 keV energy band. A follow-up observation with XMM-Newton, which was performed on 21 March 21 2004, showed that the source is located at R.A.(2000.0)=17h25m11.4 and Dec.=-36degr16'58.6" with an uncertainty of 4". The only infra-red counterpart to be found within the XMM-Newton error circle was 2MASS J17251139-3616575, which has a Ks-band magnitude of 10.7 and is located 1" away from the XMM-Newton position. The analysis of the combined INTEGRAL and XMM-Newton observations shows that the source is a binary X-ray pulsar with a spin period of 413.7 s and an orbital period of 9.72 days. The spectrum can be fitted with a flat power law plus an energy cut off (Gamma~0.02,Ecut~8.2 keV) or a Comptonized model (kTe~5.5 keV, tau~7.8). The spectrum also indicates a large hydrogen column density of Nh~15x1e22 atoms/cm-2 suggesting an intrinsic absorption. The Fe Kalpha line at 6.4 keV is clearly detected. Phase-resolved spectroscopy does not show any variation in the continuum except the total emitted flux. The absorption is constant along the pulse phase. This source can be associated with EXO 1722-363 as both systems show common timing and spectral features. The observations suggest that the source is a wind-fed accreting pulsar accompanied by a supergiant star.

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J. A. Zurita Heras, G. De Cesare, R. Walter, A. Bodaghee, G. Belanger, T. Courvoisier, S. E. Shaw, J. B. Stephen. 2005-11-03. IGR J17252-3616: an accreting pulsar observed by INTEGRAL and XMM-Newton. https://doi.org/10.1051/0004-6361%3A20053876

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