We study the morphology and masses of extremely red galaxies (EROs) within the GOYA survey (Galaxy Origins and Young Assembly), by combining optical data (UBVI) with near-infrared data (JKs). The initial K-band selected catalogue contains some 2500 sources over 4.5 arcmin2, of which 113 sources have F814W-Ks>=4 and are classified as EROs. In order

We describe the status of our long-term radial velocity (RV) survey of a sample of 1000 GK-giants with the 9.2-m Hobby-Eberly Telescope and its High Resolution Spectrograph, in search for planetary-mass companions. The survey uses the I2 cell calibration method to achieve a 4-6 m s-1 precision of RV measurements, which is quite sufficient, given

We analyse V- and H-band surface photometry of a sample of 18 Sb-Sd galaxies. Combining high-resolution Hubble Space Telescope (HST) images with ground-based near-infrared observations, we extract photometric profiles, which cover the whole disc and provide the highest possible resolution. This is the first photometric study of late-type spirals

We examine the nature of MHD kink waves. This is done by determining the frequency, the damping rate and the eigenfunctions of MHD kink waves for three widely different MHD waves cases: a compressible pressure-less plasma, an incompressible plasma and a compressible plasma with non-zero plasma pressure which allows for MHD radiation. The overall

Context: HH 223 is a knotty, undulating nebular emission of ˜30 arcsec length found in the L723 star-forming region. It lies projected onto the largest blueshifted lobe of the quadrupolar CO outflow powered by a low-mass YSO system embedded in the core of L723. Aims: We analysed the physical conditions and kinematics along HH 223 with the aim of

We present time-resolved spectroscopy and circular spectropolarimetry of the SW Sex star RXJ1643.7+3402. We find significant polarization levels exhibiting a variability at a period of 19.38 +/- 0.39 min. In addition, emission-line flaring is found predominantly at twice the polarimetric period. These two findings are strong evidences in favour of