We triggered a Chandra ToO observation of the ongoing outburst of a transient source in the globular cluster Terzan 5 (ATel #2919, #2920, #2922, #2924, #2929, #2932, #2933, #2937, #2939, #2940, #2946, #2952, #2958). The 9.9 ks observation was taken with the ACIS S3 chip in imaging mode and began on 2010-10-24 at 19:30:29 UTC. Inspection of the new

The Chandra Multiwavelength Plane (ChaMPlane) Survey is a project to identify a large sample of serendipitous X-ray sources in the galactic plane, including cataclysmic variables, quiescent low mass X-ray binaries (qLMXBs: in both black hole and neutron star systems), Be X-ray binaries and stellar coronal sources (see Grindlay et al 2000, BAAS, 196

Chandra observations of two quiecent black-hole x-ray nova (BHXN), A0620-00 and GS2000+25 emphasize the reality of the difference in the x-ray luminosity swings of these systems and their neutron-star containing analogs. For A0620-00, the slope of the x-ray spectrum is much more accurately determined than had previously been possible, and is

NGC 2420 is a ∼2 Gyr old well-populated open cluster that lies about 2 kpc beyond the solar circle, in the general direction of the Galactic anti-center. Most previous abundance studies have found this cluster to be mildly metal-poor, but with a large scatter in the obtained metallicities. Detailed chemical abundance distributions are derived for

Aims: To understand the formation and evolution of the different stellar populations within our Galaxy it is essential to combine detailed kinematical and chemical information for large samples of stars. The aim of this work is to explore the chemical abundances of neutron capture elements which are a product of different nucleosynthesis processes

Aims: We aim to derive the chemical behavior of a significant sample of PNe and HII regions in the irregular galaxy NGC 6822. The selected objects are distributed in different zones of the galaxy. Our purpose is to obtain the chemical abundances of the present interstellar medium (ISM), represented by H ii regions, and the corresponding values at