An XMM-Newton Spectral and Timing Study of IGR J16207-5129: An Obscured and Non-Pulsating HMXB

TL;DR

This study presents a detailed X-ray analysis of IGR J16207-5129, revealing it as an obscured, non-pulsating high-mass X-ray binary with high variability and spectral features similar to neutron star systems.

Contribution

First detailed soft X-ray spectral and timing analysis of IGR J16207-5129, identifying its obscured nature and non-pulsating behavior, expanding understanding of similar HMXBs.

Findings

Spectrum dominated by absorbed power-law with soft excess and iron line.

High variability with 64% rms noise in 0.0001-0.05 Hz.

No pulsations detected within 0.0001-88 Hz.

Abstract

We report on a 12 hr XMM-Newton observation of the supergiant High-Mass X-ray Binary IGR J16207-5129. This is only the second soft X-ray (0.4-15 keV, in this case) study of the source since it was discovered by the INTEGRAL satellite. The average energy spectrum is very similar to those of neutron star HMXBs, being dominated by a highly absorbed power-law component with a photon index of 1.15. The spectrum also exhibits a soft excess below 2 keV and an iron Kalpha emission line at 6.39+/-0.03 keV. For the primary power-law component, the column density is 1.19E23 cm^-2, indicating local absorption, likely from the stellar wind, and placing IGR J16207-5129 in the category of obscured IGR HMXBs. The source exhibits a very high level of variability with an rms noise level of 64%+/-21% in the 0.0001 to 0.05 Hz frequency range. Although the energy spectrum suggests that the system may harbor a neutron star, no pulsations are detected with a 90% confidence upper limit of 2% in a frequency range from 0.0001 to 88 Hz. We discuss similarities between IGR J16207-5129 and other apparently non-pulsating HMXBs, including other IGR HMXBs as well as 4U 2206+54 (but see arXiv:0812.2365) and 4U 1700-377.