EDP Sciences
Free access
Volume 430, Number 3, February II 2005
Page(s) L69 - L72
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:200400131

A&A 430, L69-L72 (2005)
DOI: 10.1051/0004-6361:200400131


XMM-Newton detection of hot gas in the Eskimo Nebula: Shocked stellar wind or collimated outflows?

M. A. Guerrero1, Y.-H. Chu2, R. A. Gruendl2 and M. Meixner3

1  Instituto de Astrofísica de Andalucía, CSIC, Apartado Correos 3004, 18080, Granada, Spain
    e-mail: mar@iaa.es
2  Astronomy Department, University of Illinois, 1002 W. Green Street, Urbana, IL 61801, USA
    e-mail: [chu;gruendl]@astro.uiuc.edu
3  Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
    e-mail: meixner@stsci.edu

(Received 1 December 2004 / Accepted 19 December 2004 )

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  $\times$ 10 6 K and an X-ray luminosity of $L_{\rm X} =
(2.6\pm1.0)$   $\times$ $10^{31} (d/1150~{\rm pc})^2$ erg 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.

Key words: ISM: planetary nebulae: general -- ISM: planetary nebulae: individual: NGC 2392 -- stars: winds, outflows

SIMBAD Objects

© ESO 2005