Here, we discussed our recent results of elemental abundance survey of Galactic disk based on 181 F- and G-type dwarfs (published by Reddy et al. 2003, MNRAS, 340, 304). Using high-resolution and high signal-to-noise spectra we obtained quantitative abundances for 27 elements: C, N, O, Na, Mg, Al, Si, S, K, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Cu, Zn, Sr

Using a high resolution spectrum of the secondary star in the Low Mass X-ray Binary (LMXB) A0620-00 we have derived the stellar parameters and the veiling caused by the accretion disk in a consistent way. We have used a χ 2 minimization procedure to explore a grid of 600000 synthetic spectra computed for a plausible range of both stellar and

We investigate the presence of possible blends in the spectral region of the Li resonance line at 6708Å in solar-type metal-rich stars using high resolution and high S/N spectroscopic observations. Our analysis does not confirm the identification of a weak absorption feature at 6708.025Å with the low excitation Ti I line proposed recently by Reddy

The black hole binary, Cyg X-1, is generally observed in one of two long duration X-ray states: a low flux, hard spectrum state (most common) and a high flux, soft spectrum state (rare). Models predict that the high/ soft state corresponds to a high mass transfer phase in the binary, and since the X-ray source is fueled by accretion from the

We report the detection of the first two microlensing candidates from the Wendelstein Calar Alto Pixellensing Project (WeCAPP). Both are detected with a high signal-to-noise ratio and were filtered out from 4.5 million pixel light curves using a variety of selection criteria. Here we only consider well-sampled events with timescales of 1 day

We present the evolution of the rest-frame optical luminosity density jrestλ, the integrated rest-frame optical color, and the stellar mass density, ρ*, for a sample of Ks band-selected galaxies in the Hubble Deep Field-South (HDF-S). We derived jrestλ in the rest-frame U, B, and V bands and found that jrestλ increases by a factor of 1.9+/-0.4, 2.9