The nature of the soft X-ray source in DG Tau

Abstract

The classical T Tauri star DG Tau shows all typical signatures of X-ray activity and, in particular, harbors a resolved X-ray jet. We demonstrate that its soft and hard X-ray components are separated spatially by approximately 0.2 arcsec by deriving the spatial offset between both components from the event centroids of the soft and hard photons utilizing the intrinsic energy-resolution of the Chandra ACIS-S detector. We also demonstrate that this offset is physical and cannot be attributed to an instrumental origin or to low counting statistics. Furthermore, the location of the derived soft X-ray emission peak coincides with emission peaks observed for optical emission lines, suggesting that both, soft X-rays and optical emission, have the same physical origin.

arXiv comment5 pages, 3 figures, accepted for publication as A&A Letter

References in corpus (9)

• X-ray emitting young stars in the Orion Nebula
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• HST/STIS spectroscopy of the optical outflow from DG Tau: structure and kinematics on sub-arcsecond scales
• Locating the Launching Region of T Tauri Winds: The Case of DG Tau
• Chandra/ACIS Subpixel Event Repositioning. II. Further Refinements and Comparison between Backside and Front-side Illuminated X-ray CCDs
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• X-rays from jet-driving protostars and T Tauri stars
• HeI 1.083 micron emission and absorption in DG Tau: line excitation in jet, hot wind, and accretion flow
• Hubble Space Telescope Images of the Subarcsecond Jet in DG Tau

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