Following our optical monitoring of the halo black-hole candidate XTE J1118+480 (ATELs #383, #402, #424), we have obtained time-resolved R-band photometry with the ESA 1-m OGS telescope at the Spanish Observatorio del Teide and with the FLWO 1.2m telescope on Mt. Hopkins. Our observations show that the source has settled into a near-quiescence

We have observed the cosmic microwave background (CMB) temperature fluctuations in eight fields covering three separated areas of sky with the Very Small Array at 34GHz. A total area of 101 square degrees has been imaged, with sensitivity on angular scales of 3.6{deg}-0.4{deg} (equivalent to angular multipoles l=150-900). (2 data files).

We present the first results of a photometric survey of poorly studied nova remnants in the Northern Hemisphere. The main results are as follows: DM Gem shows a modulation at 0.123 d (probably linked to the orbit) and rapid variations at ˜ 22 min. A moderate resolution spectrum taken at the time of the photometric observations shows intense He II

In the framework of our narrow-band survey of Local Group galaxies, we present the results of the search for planetary nebulae (PNe) in three spheroidal companions to the Andromeda galaxy. We find 9 candidate PNe in NGC 147, 5 in NGC 185, and 75 in the ˜0.4 square degree area searched around NGC 205, increasing the number of PNe known in these

We present an analysis of the integrated Hα emission line profiles for the H SHAPE Ii region population of the spiral galaxies NGC 1530, NGC 6951 and NGC 3359. We show that ˜70% of the line profiles show two or three Gaussian components. The relations between the luminosity (log LHα) and non-thermal line width (log σnt) for the H SHAPE Ii regions

An attractive diagnostic tool for investigating the magnetism of the solar chromosphere is the observation and theoretical modeling of the Hanle and Zeeman effects in spicules, as shown in this Letter for the first time. Here we report on spectropolarimetric observations of solar chromospheric spicules in the He I λ10830 multiplet and on their