Wind fluctuations in [WC 8-9]-type central stars of planetary nebulae have been detected. Moving features seen on the top of the C III lambda 5696 and C IV lambda lambda 5801/12 emission lines of HD 826 (NGC 40) and BD +30^o3639 are interpreted as outflowing clumps which are radially accelerated in the Wolf-Rayet winds. Kinematic parameters of the

Chandra observations on Jan 16, 2002 surveyed M31 with a series of 5 short (1ks) HRC images. Preliminary analysis yields the following info on new transients and highly variable sources: A new source CXOU J004307.0+411809 (RA=00h43m07s.099, DEC=+41o18'09".95, +/- 1", J2000) is discovered at a luminosity of 2.7 x 1037 ergs/sec (emitted over 0.3-7.0

The recent history of star formation in VII Zw 403 is analyzed taking into account the dynamics of the starburst blown superbubble and the restrictions that follow from X-ray observations, and from our H alpha data. Our results show that the starburst energizing VII Zw 403 is not coeval, but rather the star forming phase has lasted for more than 30

The PN M2-48 is formed by three main structures, namely, a bipolar central region (CR), a set of knots tracing a semicircular shell surrounding CR, and two symmetric bow-shocks. CR shows a kinematic structure corresponding to a bipolar shell, with an expansion velocity of =~ 50kms-1. The semicircular shell appears to be expanding at =~ 20kms-1

We present the first results on the identifications of a medium sensitivity survey (X-ray flux limit 2x 10-14 erg cm-2 s-1 in the 0.5-4.5 keV band) at high galactic latitude ({mid}b{mid}>20deg) carried out with the XMM-Newton X-ray observatory within the AXIS observing programme. This study is being conducted as part of the XMM-Newton Survey

We compute photoionization models for the giant extragalactic H II region NGC 5461, and compare their predictions to several observational constraints. The models are constrained to reproduce the observed density profile, and our analysis takes into consideration the bias introduced by the shapes and sizes of the slits used by different observers.