We have carried out a survey searching for Hα emitting galaxies at z~0.24 using a narrow band filter tuned with the redshifted line. The total sky area covered was 0.19 square degrees within the redshift range 0.228 to 0.255 in a set of four fields in the ELAIS-N1 zone. This corresponds to a volume of 9.8x103Mpc3 and a look-back time of 3.6Gyr when

The capabilities of Eddington for the detection and analysis of extrasolar planets are outlined. The primary goal of the PF (Planet finding) part of the mission is the detection of planets that are Earth like - which limits their size to less then 3 Earth radii - and which are potentially habitable - which limits their temperature or their orbital

Not Available

We present Doppler images of the more intense emission lines in the spectrum of the Black Hole X-ray Nova XTE J1118+480 during the 2000 outburst and near quiescence. Use of MOLLY, DOPPLER and TRAILER routines developed largely by T. R. Marsh is acknowledged.

We report the detection of modulated circular polarization in V795 Her. The degree of polarization increases with wavelength and is modulated with a period of 19.54 min, which is very close to the reported optical QPO period. The modulation has a peak-to-peak amplitude of 0.12% in the U-band. The estimated magnetic field intensity is in the range 2

A ground based transit survey of M and K-dwarf stars near the galactic plane should be able to determine the abundance of the lower end of the planetary radius function, i.e., extrasolar planets smaller than Neptune. We have shown (Doyle et al. 2000), that the ground-based detection of planets as small as 2.5 Earth-radii within the M-star