We present a strong case for a transiting hot Jupiter planet identified during a single-field transit survey toward the Lupus Galactic plane. The object, Lupus-TR-3b, transits a V=17.4 K1 V host star every 3.91405 days. Spectroscopy and stellar colors indicate a host star with effective temperature 5000 +/- 150 K, with a stellar mass and radius of

Se ha desarrollado un algoritmo de selección de cuásares de Tipo 1, que hemos denominado AAL, basado en la fotometría óptica. El algoritmo AAL obtuvo resultados aceptables sobre la muestra de entrenamiento que se utilizó para su desarrollo, consiguiendo una eficiencia del 49\% y una completitud relativa del 82\%. La primera aplicación real de AAL

We present preliminary results of Hα near-infrared spectroscopy of six galaxies with redshifts z˜1 drawn from the DEEP2 Galaxy Redshift Survey. The spectra have been taken with the multi-object mode of LIRIS (Long-slit Intermediate Resolution Infrared Spectrograph) installed at the 4.2-m William Herschel Telescope. This is a pilot study for a

Context: The study of symbiotic stars is essential to understand important aspects of stellar evolution in interacting binaries. Their observed population in the Galaxy is however poorly known, and is one to three orders of magnitudes smaller than the predicted population size. Aims: IPHAS, the INT Photometric Hα survey of the Northern Galactic

This work focuses on the properties of dusty tori in active galactic nuclei (AGN) derived from the comparison of SDSS type 1 quasars with mid-Infrared (MIR) counterparts and a new, detailed torus model. The infrared data were taken by the Spitzer Wide-area InfraRed Extragalactic (SWIRE) Survey. Basic model parameters are constraint, such as the

We present evidence of Fe fluorescent emission in the Chandra HETGS spectrum of the single G-type giant HR 9024 during a large flare. In analogy to solar X-ray observations, we interpret the observed Fe Kα line as being produced by illumination of the photosphere by ionizing coronal X-rays, in which case, for a given Fe photospheric abundance, its