VLT-SINFONI time-resolved spectroscopy of the central, luminous, H-rich WN stars of R136Report as inadecuate



 VLT-SINFONI time-resolved spectroscopy of the central, luminous, H-rich WN stars of R136


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Using the Very Large Telescopes Spectrograph for INtegral Field Observation in the Near-Infrared VLT-SINFONI, we have obtained repeated AO-assisted, NIR spectroscopy of the six central luminous, Wolf-Rayet WR stars in the core of the very young ~1 Myr, massive and dense cluster R136, in the Large Magellanic Cloud LMC. We also de-archived available images that were obtained with the Hubble Space Telescopes Space Telescope Imaging Spectrograph HST-STIS, and extracted high-quality, differential photometry of our target stars to check for any variability related to binary motion. Previous studies, relying on spatially unresolved, integrated, optical spectroscopy, had reported that one of these stars was likely to be a 4.377-day binary. Our study set out to identify the culprit and any other short-period system among our targets. However, none displays significant photometric variability, and only one star, BAT99-112 R136c, located on the outer fringe of R136, displays a marginal variability in its radial velocities; we tentatively report an 8.2-day period. The binary status of BAT99-112 is supported by the fact that it is one of the brightest X-ray sources among all known WR stars in the LMC, consistent with it being a colliding-wind system. Follow-up observations have been proposed to confirm the orbital period of this potentially very massive system.



Author: O. Schnurr; A. -N. Chene; J. Casoli; A. F. J. Moffat; N. St-Louis

Source: https://archive.org/







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