(DOI: will be inserted by hand later) XMM-Newton Detection of Hot Gas in the Eskimo Nebula: Shocked Stellar Wind or Collimated Outflows? ⋆

• Main Authors: M. A. Guerrero, Y. -h. Chu, R. A. Gruendl, M. Meixner
• Other Authors: The Pennsylvania State University CiteSeerX Archives
• Format: Text
• Language: English
• Published: 2004
• Subjects: eskimo*
• Online Access: http://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.317.9100; http://arxiv.org/pdf/astro-ph/0412540v1.pdf

Abstract. The Eskimo Nebula (NGC 2392) is a double-shell planetary nebula (PN) known for the exceptionally large expansion velocity of its inner shell,∼90 km s −1, and the existence of a fast bipolar outflow with a line-of-sight expansion velocity approaching 200 km s −1. We have obtained XMM-Newton observations of the Eskimo and detected diffuse X-ray emission within its inner shell. The X-ray spectra suggest thin plasma emission with a temperature of ∼ 2×10 6 K and an X-ray luminosity of LX = (2.6±1.0)×10 31 (d/1150 pc) 2 ergs s −1, where d is the distance in parsecs. The diffuse X-ray emission shows noticeably different spatial distributions between the 0.2–0.65 keV and 0.65–2.0 keV bands. High-resolution X-ray images of the Eskimo are needed to determine whether its diffuse X-ray emission originates from shocked fast wind or bipolar outflows.