We present UV data of a small sample of shell galaxies. For the majority of them (namely, NGC 2865 and NGC 7135), the NUV matches the optical emission, while the FUV is present in the innermost regions alone.

The application of tomography to the study of gas flows in interacting binaries has led to fascinating images of the Cataclysmic Variables and Algol-type binaries. Such detailed images are currently unachievable using direct-imaging techniques. Numerous images of accretion flows have now been derived from optical and ultraviolet spectra and they have been used to identify multiple emission sources including the gas stream, accretion disk, accretion annulus, shock regions, and the chromosphere of the mass loser. It was difficult to distinguish between the separate sources of emission since these sources have overlapping velocities in the Doppler tomogram. However, with the aid of a new spectral synthesis code, we can now systematically extract the individual emission sources to sequentially isolate the images of the disk and gas stream. With these new tools, we have begun to extract the critical properties of the disk and gas stream more accurately than previously possible.

The central ≈ 80×200 pc of the barred spiral galaxy M83 (NGC 5236) has been observed with the GEMINI-S+CIRPASS configuration which produced 490 spectra with a spectral resolving power of 3200, centered at 1.3 microns, oriented NW-SE. We determine the kinematics of this region with 0.36″ sampling and sub-arcsec resolution. Disk-like motions have been detected in Paβ at parsec scales around: a) the optical nucleus, b) the center of the external K-band isophotes coincident with that of the CO velocity map both also tracing the center of the bulge, and c) a hidden condensation located at (R,θ)=(158pc, 301o). The present resolution allows to detect other minor whirls, not discussed here. The disk around (a) has a radius of ∼8 pc and the two around (b) and (c) can be traced approximately up to 50–60 pc from their kinematical centers.

The rotation curves have been fitted by Satoh like spheroids+disk indicating masses of ≈4× 106M⊙, 60– 70× 106M⊙ and 30– 40× 106M⊙ respectively. Limit to the masses of central BHs can be set by supposing that the central unresolved line broadening inside each condensations is dominated by the BH as far as allowed by the central error bars. The BH +Satoh models were smoothed with a 9 pc Gaussian. The upper mass limit derived for the BH is for (a) ∼ 106 / sin(i)M⊙, and for (b) and (c) 0.2–1.0× 106 / sin(i)M⊙. Many questions arise from this interesting nucleus: are we witnessing a unique phenomenon or simply a barred galaxy with ongoing strong SF in our backyard? Does each one of the condensations host a BH indeed? or is there only one at the bulge center? Which is the fate of this complex scenario?

Stationary axisymmetric magnetic fields are expelled from outer horizons of black holes as they become extremal. Extreme black holes exhibit Meissner effect also within exact Einstein–Maxwell theory and in string theories in higher dimensions. Since maximally rotating black holes are expected to be astrophysically most important, the expulsion of the magnetic flux from their horizons represents a potential threat to an electromagnetic mechanism launching the jets at the account of black-hole rotation.

H I 21cm-line self-absorption (HISA) reveals the shape and distribution of cold atomic clouds in the Galactic disk. Many of these clouds lack corresponding CO emission, despite being colder than purely atomic gas in equilibrium models. HISA requires background line emission at the same velocity, hence mechanisms that can produce such backgrounds. Weak, small-scale, and widespread absorption is likely to arise from turbulent eddies, while strong, large-scale absorption appears organized in cloud complexes along spiral arm shocks. In the latter, the gas may be evolving from an atomic to a molecular state prior to star formation, which would account for the incomplete HISA-CO agreement.

We present XMM-Newton observations of the galaxy cluster Abell 514. This cluster shows a very complex X-ray morphology. Radio observations show that there are six radio sources located inside the cluster. This makes it possible to determine the magnetic field strength using the Faraday rotation method. This cluster is an example for the hierarchical growth of structure and a very interesting object for studying the correlation between magnetic field strength and X-ray properties.

A high-accuracy method for the removal of point sources from maps of the cosmic microwave background

ASTRONET is an ERA-NET led by a group of European funding agencies, including ESO and ESA. Its aim is to establish a comprehensive, long-term planning process for all of European astronomy – at all wavelengths, from the ground and from space, and for all of Europe. By addressing both long-term scientific goals, infrastructure needs, and resource management procedures, ASTRONET seeks to consolidate the continued development of European astronomy as a front-line player in the field.

The European initiative for an Extremely Large Telescope is presented. During the past year the transition from the 100 m OWL concept to a 30 m to 42 m diameter telescope has been made. The history and the current status of this development is described.

TV cameras equipped with image intensifiers are suitable and often used instruments for observing faint meteors. Our regular double-station observations with image intensifiers Dedal (type Dedal 41) started in 1998. Since 2006 we perform observations using new Mullard XX1332 intensifiers. In this paper we present an overview of the eight years of Dedal era. The amount of observing hours, number of meteors, statistics how many meteors were recognized using the automatic system MetRec or found manually, etc. are presented for each year. We also briefly overview the science results from these observations.

Clumpy galaxies are prominent in the early Universe. We present morphological and photometric properties of a wide range of galaxy types and their star-forming clumps in the Hubble Ultra Deep Field. Sizes, scale lengths, and scale heights suggest that galaxies grow by a factor of 2 from z = 4 to the present, and that thick disks are present in the early Universe. The largest clumps of star formation are 107–109M⊙ in different galaxies, much more massive than large star-forming complexes in local galaxies. Dissolved clumps may account for both the exponential disks and the early thick disks of spirals and proto-spiral galaxies.

We discuss the selection of star-forming galaxies at z≃6 through the Lyman-break technique. Spitzer imaging implies many of these contain older stellar populations (>200Myr) which produce detectable Balmer breaks. The ages and stellar masses (∼1010M⊙) imply that the star formation rate density at earlier epochs may have been significantly higher than at z≃6, and might have played a key role in re-ionizing the universe.

The molecular cloud associated with the Sh 254-258 group of 5 small H II regions appears to be forming a (late)-OB association. We have mapped the associated molecular cloud in the J=2-1 line of the CO molecule over 0.75o × 1o, and the CO J=3-2 line toward the 2 main peaks, with the University of Arizona Heinrich Hertz Submm Telescope (HHT). We propose a scenario for sequential formation of the stars exciting the H II regions, triggered by the compression/heating of the molecular gas.

The SuperMACHO project has discovered light echoes from 3 ancient SNe in the LMC. These SNRs are three of the six youngest in the LMC, and are classified as likely SN Ia based on X-ray data.

We present the first results of a targeted survey carried out with the 305m Arecibo radiotelescope to detect HI-line emission from disk galaxies at redshift z > 0.16. We are using this sample to study the evolution of the zero point of the Tully-Fisher relation (TFR) for galaxies at intermediate redshifts. Compared to optical widths, HI measurements sample a larger fraction of the disks, where the rotation curves are typically flat, and are not affected by slit smearing and misalignment or by aperture effects. Thus, in contrast to studies based on optical spectroscopy, this dataset allows for a direct comparison with the local TFR that is technique independent.

We discuss an accurate harmonic development of Lunar ephemeris LE-405/406

The improvement of the dynamical models of solar system bodies’ motions will be very useful for the future space astrometry mission Gaia for a fast identification of objects, to discriminate between the well-known objects and the new ones. ‘Observations in the Past’ with plate archives allow realising it.

We report on new results of our multiplicity study and present our follow-up observations of the recently detected faint companion HD 3651 B, the first directly–imaged T dwarf companion of an exoplanet host star.

The Virtual Observatory effort has undergone a substantial evolution over the last four years. In the talk we will discuss the directions of the current effort, and consider the direction along which the Virtual Observatory might evolve along with various other large astronomy projects. We will also discuss similar efforts in other disciplines and the relation of the VO to Grid Computing.

Astronomical education is entering a new stage of development which is closely connected with the development of new technologies for communication, computing and data visualization. We discuss this evolution in the context of astronomy education in Armenia. As students spend only a short time in Byurakan Observatory for training in observations, they are not able to carry out systematic astronomical observations. Hence their training places emphasis on the use of astronomical archives and analysis of observational data obtained previously with the Byurakan telescopes and other ground-based and space telescopes. Thus, one of the aims of the Armenian Virtual Observatory is to support the training of students in this modern context.