Broad-band optical observations of the extraordinarily bright optical afterglow of the intense gamma-ray burst GRB 991208 started ~2.1 days after the event and continued until 4 Apr. 2000. The flux decay constant of the optical afterglow in the R-band is -2.30 +/- 0.07 up to ~5 days, which is very likely due to the jet effect, and it is followed by

In this poster we present the results from the multi-wavelength study of the dynamical and photometric evolution of the Blue Compact Dwarf galaxy Mrk 86. We have obtained BVRJHK, Hα , and [Oiii]λ 5007 Å imaging, long-slit optical spectroscopy, and Hα Fabry-Perot interferometry for this galaxy. These observations will be complemented in a near

An analytical model has been developed to empirically study the effects of stellar spots and faculae on the observed equivalent widths of Li i 6708, Na i 5896 and K i 7699 Å lines (and abundances in the case of lithium) in late-type stars, taking into account the changes in the observed magnitudes and colors. Solar spectra corresponding to

The Downing Planetarium is the first facility in a new Central California Science Center planned for the California State University, Fresno campus. Construction of this 1.7 million project was primarily funded through a 1.1 million donation from Dr. F. Harold Downing. At the successful completion of construction, Dr. Downing also established a $1

We report results of a spectrophotometric study of SBS 1150+599A and discuss the nature of this object based upon our data. Our study shows that SBS 1150+599A is most probably a planetary nebula located in the Galactic halo and not a cataclysmic variable as originally proposed by the authors of the Second Byurakan Survey from low resolution

We present the first radial velocity measurement of the stellar component of the Local Group dwarf galaxy Phoenix, using the FORS1 instrument at the VLT's Unit Telescope 1 (Antu). From the spectra of 31 red giant branch stars, we derive a heliocentric optical radial velocity for Phoenix of Vsolar=-52+/-6 km s-1. On the basis of this velocity, and