Measurements on the local seeing have been carried out during two and a half yea rs (March 29, 1992 to October 7, 1994), over a total of 378 nights. The Site Tes ting Telescope (STT) from the Steward Observatory yields a median seeing of 0.61 arcsec and a first quartile of 0.50 arcsec. Additional measurements with the Carnegie Monitor (CM), many of

We present new optical observations of the nearby barred spiral galaxy Dwingeloo 1 (Dw1) obtained with the Isaac Newton, William Herschel and Wise telescopes. Dw1 lies at Galactic coordinates (l=138.˚52, b=-0.˚11) and it is heavily obscured by dust and gas in the Milky Way. We infer that Dw1 is of morphological type SBb or SBc (T=4), has an

We are continuing to study the observational characteristics of Holoea. This young stellar object, associated with IRAS 05327+3404, appears to be undergoing the quick transition from embedded (Class I) to exposed (Class II) T Tauri star. We have obtained new observations of this source, particularly pertaining to the outflow and the characteristics

We have carried out quantitative observations of the vector magnetic field during the emergence of three small bipolar active regions in June, 1992, July 1993, and September 1994 using the Advanced Stokes Polarimeter (ASP). The region of horizontal magnetic field at the actual site of emergence is always characterized by low magnetic field strength

Spectroscopic observations for the full sample of Hα emission-line galaxy candidates (ELGs) from the Universidad Complutense de Madrid objective-prism survey Lists 1 and 2 have been obtained in order to investigate fully the properties of the survey constituents as well as the selection characteristics and completeness limits of the survey itself

We have obtained for the first time 2.10 - 2.45 micron infrared spectra of soft X-ray transient V404 Cygni. We determine a 95 percent confidence upper limit to the fraction of light arising from the accretion disc of 14 percent. The effect this has on the mass of the compact object, determined from modelling the infrared ellipsoidal variations, is