The paper analyzes white-light images of solar granulation taken outside active regions, at regular intervals along the polar axis and the equator, in order to study its center-to-limb variation and possible changes with the solar latitude. The 2D spatial power spectra of the brightness distribution are calculated and corrected for the distortions

We present the results from a short (10 ks) Chandra GO1 observation of the nearby (z=0.051) radio source 3C371. The source is known to exhibit a 4.5arcsec-long radio synchrotron jet which was detected at optical wavelengths with ground-based observations and in our HST data. The jet is clearly detected in our Chandra exposure (which was optimized

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