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We have selected a sample of nearby ( < 0.2) BL Lacs, in order to extend the current knowledge on radio loud AGN to low redshift, weak objects and to test the unified scheme in the low luminosity range. Hubble Space Telescope observations have been previously presented [2], as well as radio observations of a few well known objects. After collecting the main results from the literature, we have obtained new observations, resulting in a complete set of parsec and kiloparsec scale images of all the objects in the sample. From the analysis of these data, we obtain the following main results [1]:

The formation of powerful extragalactic jets is not well understood at present as well as the associated key question:“What makes an AGN radio loud?”. Here we discuss how the combination of VLBI and X-ray spectroscopic observations allows the inter-relation between the accretion flow and the formation of relativistic jets in AGN to be explored.

Very Long Baseline Interferometry at millimetre wavelengths (mm-VLBI) allows to image compact galactic and extragalactic radio sources with microarcsecond resolution, unreachable by other astronomical observing techniques. Future global VLBI at millimetre wavelengths therefore should allow to map,with a spatial resolution of only a few to a few ten gravitational radii, the direct vicinity of the Super Massive Black Holes (SMBH) located in the centres of nearby galaxies. With the reduced intrinsic self-absorption at short wavelengths, mm- VLBI opens a direct view onto the often jet-producing “central engine”.

In order to explain the complex broad lines of AGNs, we apply the twocomponent model assuming that the line wings originated in a very broad line region (VBLR) and line core in an intermediate line region (ILR). The VBLR is assumed to be an accretion disk and ILR a spherical region. Such a model can very well fit complex broad lines of AGNs

The study of massive star formation is crucial for the understanding of the development of galaxies, as well as the Chemical Evolution of our galaxy. This study is at an early stage. The Atacama Large Millimeter Array (ALMA) will provide complete, high sensitivity, high angular resolution images of quasi-thermal dust and molecular line emission in protostellar objects. The data will have unprecedented quality, far exceeding what is now possible.

The potential of current and future infrared and millimeter facilities to provide an inventory of the gases and solids during star- and planet formation is discussed, and the evolutionary pathways to complex, possibly prebiotic, species are described.

GAIA will provide a multi-colour photometric and astrometric census of some one billion compact sources, complete to 20th magnitude. In addition, spectra for radial velocities will be obtained for about 30 million stars brighter than = 17. The high spatial resolution and astrometric precision, 0.1 arcsec and 10 microarcsec to = 15, will not only quantify the distribution of mass and the stellar populations in the Galaxy, but make major advances in fundamental physics, cosmology and solar system science. GAIA is an ESA mission, scheduled for launch in mid-2010. A full description of the GAIA project and science case, fairly crediting the hundreds of contributors, is available in the project ‘Red Book’ [1]. A brief overview is provided by Perryman, de Boer, Gilmore, et al. [2]. The www site is .

The Arecibo 305 m antenna is the largest filled–aperture radio telescope in the world. As such, it has extraordinary potential for high–sensitivity surveys. A new 7–element, 1225–1525 MHz, dual–polarization focal plane array receiver was installed in April 2004. The Arecibo L–band Focal Plane Array (ALFA) increases mapping speeds and so enables large-scale surveys for galactic astronomy, including HI and recombination lines and continuum, extragalactic astronomy using HI, and pulsars. We discuss some key characteristics of the new systems and the surveys that are being proposed. Additional information on ALFA and associated scientific consortia is available at .

The Submillimeter Array (SMA) is nearing completion on the summit of Mauna Kea and has begun science operations. The completed instrument will consist of eight 6-m diameter elements in recon.gurable arrays providing baselines from 7 to 500 m and resolutions of about 0.1 to 5 arcseconds. The full array will cover the atmospheric windows around 230, 345, 460, 650 and 850 GHz (1.3 to 0.3 millimeter wavelength) with a total bandwidth of 2GHz in each of 2 sidebands and high spectral resolution. The dedication took place in November 2003, and internal science proposals have been accepted for the 230 GHz and 345 GHz receivers since that time. We will report on exciting results that are becoming available as data using the 230 GHz and 345 GHz receivers during the commissioning phase of operations are reduced. The science topics explored with these early observations range from star formation and evolved stars in our Galaxy to imaging starburst regions in nearby galaxies and attempting to perform high precision astrometry on extremely high redshift submillimeter galaxies. In addition, phase closure at 682 GHz and 691 GHz was achieved in late 2002 using 3 antennas, and further test observations at these frequencies are ongoing.

The UV range supplies a richness of experimental data which is unmatched by any other spectral domain for the study of astrophysical plasmas since (1) almost all the resonance lines of all elements, covering plasmas from the coolest regimes (10- 1000K) up to hot (some 10K) temperatures are observed in this range, (2)the electronic transitions of the most abundant molecules, such as H, are in the ultraviolet which is also the most sensitive to the presence of large molecules such as the PAHs and (3)the strong forbidden coronal lines produced at temperatures from 10K to 10K are also observed in this range. Amazingly enough, no firm plans exist for the future to maintain an Ultraviolet observing capability for Astrophysics. Only concerted efforts by the community will supply the information required to have the space agencies decide to release the funding needed for the support of these important Astrophysical study capabilities. For this purpose, the Network for UltraViolet Astrophysics (NUVA, ) has been established within the OPTical Infrared COordination network for Astronomy (OPTICON). NUVA will assess the future needs and develop a perspective for the future on a European scale.