The San Fernando automatic meridian circle (CMASF) is a meridian telescope built by Grubb-Parsons in 1948 fully automated between 1987 and 1995. In 1996 was moved from the Real Instituto y Observatorio de la Armada (ROA) in San Fernando to the Carlos U. Cesco (CUC) mountain observatory in San Juan (Argentine). The CUC is owned by the Observatorio

CCD UBV photometry of 2279 stars in Sextans A is presented. Differences with the photometric scales of Sandage and Carlson (1985) and Hoessel et al. (1983) are discussed; recalibration of the Sandage and Carlson data for Cepheids in Sextans A results in a smaller value for the distance modulus, μ = 25.6. A similar value for the distance modulus is

R-band photometric and isophotal parameters for 171 late-type dwarf galaxies. For each galaxy the date of observation, seeing, adopted distance, equatorial coordinates, apparent magnitudes, central surface brightnesses, isophotal diameters and fractional light radii are given. For 46 galaxies, photometric and isophotal parameters derived from B

ABSTRACT: B, V, R, and I CCD frames were obtained for the Southern Galaxies NGC 5757, and IC 1091. The frames were analysed to derive standard photometric and geometric parameters such as integrated magnitudes and colors, dimensions and inclination. Radial luminosity profiles along several directions were calculated and combined to give one mean

Based on a 5ks Chandra ACIS-I observation of M31 on Nov 11 2009, we report a dramatic brightening of CXOM31 J004321.1+411751, [aka r3-7 (Kong et al. 2002 ApJ 577, 738), source 437 (Pietsch, Freyberg, and Haberl 2005 A&A 434, 483), RX J0043.3+4117 (Supper et al. 2001 A&A 373, 63)]. The spectrum on Nov 11 can be well fit with a power law with photon

M31 has been monitored by the HRC and ACIS detectors aboard Chandra from 1999 to 2002. We report here a summary of properties of X-ray sources in M31 with a focus on an ongoing Chandra/HST program to monitor X-ray transients in M31. By comparing individual X-ray images, more than 100 sources were found to be variable (half the total number observed