We discuss several lines of evidence indicating that gas is flowing into the solar neighborhood and go on to offer a theoretical framework to explain this phenomenon, which is important for any model of the chemical and dynamical evolution of the Galaxy. We derive a theoretical age distribution for the G dwarf stars in the solar neighborhood that

The GRB010222 optical and near-infrared (NIR) afterglow was monitored at the TNG and other Italian telescopes starting ~ 1 day after the high-energy prompt event. The BVR light curves, which are the best sampled, are continuously steepening and can be described by two power laws, f(t) ~ t-alpha , of indices alpha1 ~ 0.7 and alpha2 ~ 1.3 before and

Several proof corrections were not carried faithfully to the published version of this article. In particular, a central sentence of the abstract should readThis can be achieved by varying the relative bulge-to-disk stellar density while maintaining the same effective bulge-to-disk size ratio.In Astron. J. 121, 820 (2001), there is an erroneous

Hen 3-1475 (IRAS 17423-1755) has recently been identified via ground-based and HST optical images as a bipolar proto-planetary nebula displaying a remarkable highly--collimated optical jet and a spectacular S-shaped string of knots along its bipolar axis, associated to extremely high velocities which decrease with the distance to the central star

The COMPTEL observations of the diffuse galactic 1.809 MeV emission attributed to the radioactive decay of 26 Al have confirmed the diffuse nature of this interstellar emission line. One of the most significant features of the reconstructed intensity pattern is a flux enhancement in the direction of the Cygnus region. This region is fairly young

We report the detection at X-rays of the radio/optical jet of 3C 371 from a short (10 ks) Chandra exposure in 2000 March. We also present a new MERLIN observation at 1.4 GHz together with a reanalysis of the archival Hubble Space Telescope Wide Field Planetary Camera 2 F555W image. Despite the limited signal-to-noise ratio of the Chandra data, the