The transiting planet CoRoT-1b is thought to belong to the pM-class of planets, in which the thermal emission dominates in the optical wavelengths. We present a detection of its secondary eclipse in the CoRoT white channel data, whose response function goes from ~400 to ~1000 nm. We used two different filtering approaches, and several methods to

We obtain the probability distribution for the volume of excursion sets in a three-dimensional Gaussian field, in order to develop the approximation to the cosmic mass function that follows directly from the assumption that the spherical collapse criteria may be applied to field points. We also use this distribution to develop an analytical

We present the evolution of the luminosity-size and stellar mass-size relations of luminous (LV>~3.4×1010 h-270 Lsolar) and massive (M*>~3×1010 h-270 Msolar) galaxies in the last ~11 Gyr. We use very deep near-infrared images of the Hubble Deep Field-South and the MS 1054-03 field in the Js, H, and Ks bands from FIRES to retrieve the sizes in the

Genuine spectral energy distributions (SED) of the central few parsec region of the nearest and brightest active galaxies in the southern hemisphere are presented. These are compiled from very high-spatial resolution data taken from radio (VLBA), IR adaptive optics and interferometry, and optical (HST) observations. The new SEDs are characterized

The distribution of stars in the Hertzsprung-Russell diagram narrates their evolutionary history and directly assesses their properties. Placing stars in this diagram however requires the knowledge of their distances and interstellar extinctions, which are often poorly known for Galactic stars. The spectroscopic Hertzsprung-Russell diagram (sHRD)

We estimate the typical spectrum of spatial fluctuations of intensity due to the penumbral filaments. High angular resolution continuum images are used (cut-off frequencies equivalent to 0.28" wavelength of about 5257 Å). The amplitude of the observed spectra follows the modulation transfer function of our optical system. In other words, the