The Twisting X-Ray Isophotes of the Elliptical Galaxy NGC 720

We present spatial analysis of the deep (57ks) ROSAT HRI X-ray image of the E4 galaxy NGC 720. The orientation of the HRI surface brightness is consistent with the optical position angle $(PA)$ interior to semi-major axis $asim 60arcsec$ (optical $R_esim 50arcsec$). For larger $a$ the isophotes twist and eventually $(agtrsim 100arcsec)$ orient along a direction consistent with the $PA$ measured with the PSPC data (Buote & Canizares 1994) -- the $sim 30arcdeg$ twist is significant at an estimated 99% confidence level. We argue that this twist is not the result of projected foreground and background sources, ram pressure effects, or tidal distortions. If spheroidal symmetry and a nearly isothermal hot gas are assumed, then the azimuthally averaged radial profile displays features which, when combined with the observed $PA$ twist, are inconsistent with the simple assumptions that the X-ray emission is due either entirely to hot gas or to the combined emission from hot gas and discrete sources. We discuss possible origins of the $PA$ twist and radial profile features (e.g., triaxiality).Comment: 17 pages (3 figures), AASTeX manuscript with PostScript figures, to appear in ApJ September 10, 1996. Only a few minor cosmetic changes in this versio