Since the beginning of this century we have attended a blooming of the gravity-mode research thanks to the unprecedented quality of the data available, either from space with SoHO, or from the ground-based networks as BiSON or GONG. From the first upper limit of the gravity-mode amplitudes fixed at 10 mm/s at 200 μHz given by Appourchaux et al.

In this Letter we present clear evidence that Mrk 573 is an obscured narrow-line Seyfert 1 (NLSy1) galaxy and not an archetypal Seyfert 2, as it has been classified until now. Only three galaxies have been proposed as members of this class, prior to this work. Here we report near-infrared spectroscopic data taken with LIRIS on the 4.2 m William

Since September 2007 we have been monitoring the optical counterpart (V, R and i-bands) of the black hole X-ray binary GX 339-4 with the Faulkes Telescope South situated at Siding Spring in Australia. The source has continued to decline from its 2006-7 outburst (ATel #968) until May 2008, in which a period of strong variability began. At its

Two extremely compact Hα-emitting sources have been discovered in our deep images of the Abell 539 and Abell 634 clusters of galaxies. Follow-up spectroscopy of these two unresolved sources have revealed that they are active starburst members of their respective clusters. The Hα luminosities and extreme Hα equivalent widths (of ≃ 430 Å and 1010 Å

We express in linearized form the five classical coupled equations representing the rotating gas disk of a standard disk galaxy. We solve them in three limiting cases for the gas disk: 1) infinite thickness and uniform rotation, 2) finite thickness and uniform rotation, and 3) infinite thickness and shearing box approximating differential rotation

In this proceedings paper we make use of the two-dimensional stellar kinematics of a representative sample of E and S0 galaxies obtained with the SAURON integral-field spectrograph to reveal that early-type galaxies appear in two broad flavors, depending on whether they exhibit clear large-scale rotation or not. We measure the level of rotation via