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Chandra X-ray Observations of the Young Stellar Cluster NGC 6193 in the Ara OB1 Association

S. L. Skinner·S. A. Zhekov·F. Palla·C. L. D. R Barbosa
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Abstract

A 90 ks Chandra HETG observation of the young stellar cluster NGC 6193 in the southern Ara OB1 association detected 43 X-ray sources in a 2' x 2' core region centered on the young O stars HD 150135 (O6.5V) and HD 150136 (O3+O6V). The cluster is dominated by exceptionally bright X-ray emission from the two O stars, which are separated by only 10 arcsecs. The X-ray luminosity of HD 150136 is log Lx = 33.39 (ergs/s), making it one of the most luminous O-star X-ray sources known. All of the fainter X-ray sources in the core region have near-IR counterparts, but JHK photometry provides little evidence for near-IR excesses. These core sources have typical mean photon energies of 2 keV and about one-third are variable. It is likely that some are young low-mass stars in the cluster, but cluster membership remains to be determined. Grating spectra show that the X-ray properties of HD 150135 and HD 150136 are similar, but not identical. Both have moderately broadened unshifted emission lines and their emission is dominated by cool plasma, pointing to a wind shock origin. However, the emission of HD 150136 is slightly hotter and 4 times more luminous than its optical twin HD 150135. We discuss the possibility that a radiative colliding wind shock contributes to the prodigious X-ray output of the short-period (2.66 d) binary HD 150136. A surprising result is that the X-ray emission of HD 150136 is slowly variable on a timescale of less than one day. The origin of the variability is not yet known, but the observed behavior suggests that it is an occultation effect.

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S. L. Skinner, S. A. Zhekov, F. Palla, C. L. D. R Barbosa. 2005-04-25. Chandra X-ray Observations of the Young Stellar Cluster NGC 6193 in the Ara OB1 Association. https://doi.org/10.1111/j.1365-2966.2005.09154.x

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