The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra program that has imaged the central 0.9 deg2 of the COSMOS field down to limiting depths of 1.9 × 10-16 erg cm-2 s-1 in the soft (0.5-2 keV) band, 7.3 × 10-16 erg cm-2 s-1 in the hard (2-10 keV) band, and 5.7 × 10-16 erg cm-2 s-1 in the full (0.5-10 keV) band. In this paper we report

Commissioning observations with the Apache Point Observatory Galactic Evolution Experiment (APOGEE), part of the Sloan Digital Sky Survey III, have produced radial velocities (RVs) for ~4700 K/M-giant stars in the Milky Way (MW) bulge. These high-resolution (R ~ 22, 500), high-S/N (>100 per resolution element), near-infrared (NIR; 1.51-1.70 μm)

We present the star formation history (SFH) as a function of galactocentric radius for a sample of isolated dwarf galaxies from the Local Cosmology from the Isolated Dwarfs (LCID) project. The results show a decrease of the star formation with radius for stars with ages ≤ 9 Gyr. Star formation for ages ≥ 10 Gyr is present regardless of distance to

We have fully characterized the NGSL stellar spectral library, which allows us to open the UV stellar spectral range for stellar population studies. We have performed the necessary steps to prepare this library for its implementation in models synthesizing SEDs of stellar cluster and galaxy spectra. We have determined and homogenized the

We present new spectroscopic identifications of 12 X-shaped radio galaxies and use the spectral data to derive starburst histories and masses of the nuclear supermassive black holes in these galaxies. The observations were done with the 2.1-m telescope of the Observatorio Astronómico Nacional at San Pedro Mártir, México. The new spectroscopic

A sample of ~150 compact Galactic PNe has been observed with the Spitzer/IRS spectrograph to characterize their dust properties. These PNe are likely to be at the onset of the PN evolutionary phase, and are therefore ideal for probing dust evolution. The molecular emission features in these Galactic PN spectra are similar to those found in our