Chandra observations of the planetary nebula IC 4593

Abstract

The ACIS-S camera on board the Chandra X-ray Observatory has been used to discover a hot bubble in the planetary nebula (PN) IC4593, the most distant PN detected by Chandra so far. The data are used to study the distribution of the X-ray-emitting gas in IC 4593 and to estimate its physical properties. The hot bubble has a radius of ~2${}^{\prime \prime }$ and is found to be confined inside the optically-bright innermost cavity of IC 4593. The X-ray emission is mostly consistent with that of an optically-thin plasma with temperature $kT\approx 0.15$ keV (or $T_{\mathrm{X}}\approx 1.7\times 10^6$ K), electron density $n_{\mathrm{e}}\approx 15$ cm${}^{-3}$, and intrinsic X-ray luminosity in the 0.3-1.5 keV energy range $L_{\mathrm{X}}=3.4\times 10^{30}$ erg s${}^{-1}$. A careful analysis of the distribution of hard ($E>$0.8 keV) photons in IC 4593 suggests the presence of X-ray emission from a point source likely associated with its central star (CSPN). If this were the case, its estimated X-ray luminosity would be $L_{\mathrm{X},\mathrm{CSPN}}=7\times 10^{29}$ erg s${}^{-1}$, fulfilling the log$(L_{\mathrm{X},\mathrm{CSPN}}/L_{\mathrm{bol}})\approx -7$ relation for self-shocking winds in hot stars. The X-ray detection of the CSPN helps explain the presence of high-ionisation species detected in the UV spectra as predicted by stellar atmosphere models.

arXiv comment6 pages, 4 figures; Accepted to MNRAS

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