The present work is based on the multi-wavelength catalog of IRAC 3.6+4.5um selected galaxies in the EGS (RA=14h14m, DEC=+53°30') presented in Paper I (Barro et al. 2011, Cat. J/ApJS/193/13). We cross-correlated our IRAC-selected catalog with the X-ray (Chandra) and radio (VLA/20cm) catalogs of Laird et al. (2009, Cat. J/ApJS/180/102) and Ivison et

The MASTER auto-detection system at Tunka (Baykal Lake) detected a new transient source at the position (R.A., Dec) = 17h 29m 00.07s , +75d 18m 42s.5, (J2000) with a typical uncertainty of 0.5" at 2011-05-12 18:24:47.725 (UT). The OT is seen at 2 images. There is no minor planet and any object brighter 21 mag in DSS at this place. The unfiltered (0

We present the results of a comprehensive study of the gamma-ray burst 080928 and of its afterglow. GRB 080928 was a long burst detected by Swift/BAT and Fermi/GBM. It is one of the exceptional cases where optical emission had already been detected when the GRB itself was still radiating in the gamma-ray band. For nearly 100 s simultaneous optical

We have identified the optical counterpart of the ULX source P13 in the nearby spiral galaxy NGC 7793. The object is a V ˜ 20.5 mag star, ten times brighter than any other established counterpart of a ULX in nearby galaxies. Medium resolution optical spectroscopy carried out in 2008 and 2009 with the ESO-VLT reveals the presence of narrow high

We present the most exhaustive and accurate inferences of the internal solar rotation rate and its evolution during solar cycle 23. A full solar cycle of MDI observations have been analyzed using our state of the art fitting methodology. Time series of various lengths have been fitted, from a single 4608-day long epoch (64 times 72 day or 12.6 yr)

We identify SDSS J010657.39-100003.3 (hereafter J0106-1000) as the shortest period detached binary white dwarf (WD) system currently known. We targeted J0106-1000 as part of our radial velocity programme to search for companions around known extremely low-mass (ELM; ˜0.2 M&sun;) WDs using the 6.5-m Multiple Mirror Telescope. We detect peak-to-peak