We present a comparison between the observed galaxy stellar mass function and the one predicted from the De Lucia & Blaizot semi-analytic model applied to the Millennium Simulation, for cluster satellites and galaxies in the field (meant as a wide portion of the sky, including all environments), in the local universe (z ~ 0.06), and at intermediate

The results of O/H abundances derived from PNe in M31 (accompanying poster by Hensley et al.) have extended the radius coverage of our previous gradient studies out to projected disk distances of 100 kpc. The PNe are drawn from the peak of the [OIII] PNLF which suggests that their progenitor stars are more massive than about 1.5 M_sun with

More than about 20 central stars of planetary nebulae (CSPNs) have been observed spectropolarimetrically, yet no clear, unambiguous signal of the presence of a magnetic field in these objects has been found. We perform a statistical (Bayesian) analysis of all the available spectropolarimetric observations of CSPN to constrain the magnetic fields in

Context. Determining the magnetic field vector in quiescent solar prominences is possible by interpreting the Hanle and Zeeman effects in spectral lines. However, observational measurements are scarce and lack high spatial resolution. Aims: We determine the magnetic field vector configuration along a quiescent solar prominence by interpreting

JEM-EUSO (Extreme Universe Space Observatory on Japanese Experiment Module) is an advanced observatory that will be on-board the International Space Station (ISS) and use the Earth׳s atmosphere as a huge calorimeter detector. However, the atmospheric clouds introduce uncertainties in the signals measured by JEM-EUSO. Therefore, it is extremely

Context. The search for planets orbiting metal-poor stars is of utmost importance for our understanding of planet formation models. However, no dedicated searches have been conducted so far for very low mass planets orbiting such objects. Only a few cases of low-mass planets orbiting metal-poor stars are thus known. Amongst these, HD 41248 is a