The XMM-Newton view of the yellow hypergiant IRC + 10420 and its surroundings |
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| Institution: | 1. China Center for Energy Economics Research, School of Economics, Xiamen University, Xiamen, Fujian 361005, China;2. School of Economics and Finance, Xi''an Jiaotong University, Xi''an, Shaanxi 710061, China;1. University of Zürich, Department of Geography, Switzerland;2. Eawag: Swiss Federal Institute of Aquatic Science and Technology, Dübendorf, Switzerland;3. University of Fribourg, Department of Geosciences, Switzerland;4. WSL: Institute for Snow and Avalanche Research SLF, Davos Dorf, Switzerland;5. Climate Change, Extremes, and Natural Hazards in Alpine Regions Research Center CERC, Davos Dorf, Switzerland;1. State Key Laboratory of Protein and Plant Gene Research, School of Life Sciences and Peking-Tsinghua Center for Life Sciences, Peking University, Beijing 100871, China;2. Academy for Advanced Interdisciplinary Studies, Peking University, Beijing 100871, China;3. School of Life Sciences, Tsinghua University, Beijing 100084, China |
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| Abstract: | Among evolved massive stars likely in transition to the Wolf–Rayet phase, IRC + 10420 is probably one of the most enigmatic. It belongs to the category of yellow hypergiants and it is characterized by quite high mass loss episodes. Even though IRC + 10420 benefited of many observations in several wavelength domains, it has never been a target for an X-ray observatory. We report here on the very first dedicated observation of IRC + 10420 in X-rays, using the XMM-Newton satellite. Even though the target is not detected, we derive X-ray flux upper limits of the order of 1–3 × 10?14 erg cm?2 s?1 (between 0.3 and 10.0 keV), and we discuss the case of IRC + 10420 in the framework of emission models likely to be adequate for such an object. Using the Optical/UV Monitor on board XMM-Newton, we present the very first upper limits of the flux density of IRC + 10420 in the UV domain (between 1800 and 2250 Å and between 2050 and 2450 Å). Finally, we also report on the detection in this field of 10 X-ray and 7 UV point sources, and we briefly discuss their properties and potential counterparts at longer wavelengths. |
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| Keywords: | Stars: early-type X-rays: stars |
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