In its three years of operation, the Sloan Digital Sky Survey Apache Point Observatory Galactic Evolution Experiment (APOGEE-1) observed >14,000 stars with enough epochs over a sufficient temporal baseline for the fitting of Keplerian orbits. We present the custom orbit-fitting pipeline used to create this catalog, which includes novel quality

We investigate the properties of circumgalactic gas in the halo of quasar (QSO) host galaxies from C IV absorption-line systems. We use the optical spectroscopy of closely aligned pairs of quasars (projected distance ≤ 200 kpc) obtained at the Gran Telescopio Canarias to investigate the distribution of the absorbing gas for a sample of 18 quasars

Aims: During the last ~50 years, the population of black hole candidates in X-ray binaries has increased considerably, with 59 Galactic objects being detected in transient low-mass X-ray binaries, as well as a few in persistent systems (including ~5 extragalactic binaries). Methods: We collect near-infrared, optical, and X-ray information spread

We present the stellar kinematics across the Galactic bulge and into the disk at positive longitudes from the SDSS-III APOGEE spectroscopic survey of the Milky Way. APOGEE includes extensive coverage of the stellar populations of the bulge along the midplane and near-plane regions. From these data, we have produced kinematic maps of 10,000 stars

Ultra-diffuse galaxies (UDGs) have the sizes of giants but the luminosities of dwarfs. A key to understanding their origins comes from their total masses, but their low surface brightnesses (μ (V) ≥slant 25.0) generally prohibit dynamical studies. Here, we report the first such measurements for a UDG (VCC 1287 in the Virgo cluster), based on its

The iron carbonyl complexes with C60 and C70 fullerenes were synthesized in high yield by photochemical irradiation of solutions of C60 and C70 in presence of Fe(CO)5. The resulting complexes were studied by FT-IR, Raman and electronic absorption spectroscopy. All the data are consistent with the structures [Fe(CO)4(η2C60)] and [Fe(CO)4(η2C70)]