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In May 1997 a consistent part of the services and structures committed to the industry had already been released to the commissioning group. The telescope itself was, with the exception of the Nasmyth derotators, motors and all the optics groups, basically ready in its mechanical parts to accept the integration of all services and control equipment. Also the verification of the cabling (interlocks, data-nets, power and controls) already mounted was started in the same period. Starting from June 1998 (telescope first-light date) the telescope went gradually in use, several nights per week, in order to test and tune the tracking and pointing system, the optics and the first derotator system (Nasmyth A station). At the end of the commissioning period and with the first scientific instruments mounted (April 1999) also the first routinely observations started. In this moment the telescope is doing astronomy 80% of time and the complete first-light instrumentation is mounted., Comment: 14 pages

This work concerns the development of a 3D measuring system able to realize noncontact surface topography with millimetric depth-range and micrometric resolutions both in the spatial and depth axes. The optical concept is based on the well known low coherence interferometry (LCI) technique. The most widespread set-up of such technique is that of measuring only a point at a time with a 2D scanning system that permits the measure on an area. The novel concept of our instrument is based on the use of a 2D sensor (CMOS), where every single pixel measures a point on the object and this permits a fast analysis on square centimeters areas without the need for any precise (and expensive) scanning system. We present here accurate depth calibration which shows the potentiality of this instrument., Comment: Pg. 376-379 ISBN: 9780955308260

The effect of the AlOx barrier thickness on magnetic and morphological properties of Ta/Co/(AlOx)/Alq3/Si hybrid structures was systematically studied by means of atomic force microscopy, SQUID magnetometry and nuclear magnetic resonance (NMR). All used techniques pointed out that the barrier thickness of 2 nm is required to obtain a magnetically good cobalt layer on top of Alq3. 59Co NMR measurements revealed that the AlOx barrier gives rise to the formation of an interface layer with "defective" cobalt favouring growth of "bulk" cobalt with good magnetic properties., Comment: 4 pages, Accepted for publication in Applied Physics Letters

We present the first results of an asteroid photo--polarimetry program started at Asiago--Cima Ekar Observatory. The aim of our survey is to estimate diversity in polarimetric properties of asteroids belonging to different taxonomic and dynamical classes. The data were obtained with the polarization analyser placed inside the Faint Object Spectrographic Camera (AFOSC) of the 1.8m telescope. This instrument allows simultaneous measurements of the two first Stokes parameters without any lambda/2 retarding plate. Our survey began in 2002, and up to now we have obtained data on a sample of 36 asteroids; most of them are being investigated with the polarimetric technique for the first time. Combining our data with those already available in literature, we present an estimate of the inversion angle for 7 asteroids in this paper. Furthermore, we present the polarimetric measurements of the rare asteroid classes belonging to the A and D types and a detailed VRI observations at extremely small phase angles of the low albedo asteroid 1021 Flammario, Comment: 8 pages, paper accepted for pubblication on A&A

The SRT (Sardinia Radio Telescope) is a general purpose, fully steerable, active surface equipped, 64 meters antenna, which is in an advanced construction state near Cagliari (Sardinia - Italy). It will be an antenna which could improve a lot the performances of the EVN network, particularly at frequencies higher than 22 GHz. The main antenna geometry consist of a shaped reflector system pair, based on the classical parabola-ellipse Gregorian configuration. It is designed to be able to operate with a good efficiency in a frequency range from 300 MHz up to 100 GHz. This frequency range, is divided in two parts which define also two antenna operational modes, one up to 22 GHz with a minimal amount of accessory instrumentation, and the other up to 100 GHz with a full complement of instrumentation. The goal is to make it possible to build a telescope operable up to 22 GHz, and then upgrade it at a future date to operate at frequencies up to 100 GHz. In order to get these goals, the SRT Metrology group is studying and developing different types of strategies, instrumentation, and techniques for measuring and reducing the various components of pointing and efficiency errors, taking advantage also from experiences developed in other radio telescopes, like GBT (Green Bank Telescope, USA), LMT (Large Millimiter Telescope, MEX), and IRAM (Institut de Radio Astronomie Millimetrique, Fr). Many of those system will be installed and tested at the 32 meters radio-telescope in Medicina (Bologna), before of their implementation on SRT., Comment: 2 pages. no figures. Proceedings of the 7th European VLBI Network Symposium held in Toledo, Spain on October 12-15, 2004. Editors: R. Bachiller, F. Colomer, J.-F. Desmurs, P. de Vicente (Observatorio Astronomico Nacional), p. 293-294. Needs evn2004.cls

We have tested the experimental prerequisites for a Space-to-Ground quantum communication link between satellites and an optical ground station. The feasibility of our ideas is being assessed using the facilities of the ASI Matera Laser Ranging Observatory (MLRO). Specific emphasis is put on the necessary technological modifications of the existing infrastructure to achieve single photon reception from an orbiting satellite., Comment: 8 pages 5 figures, SPIE proceedings Quantum Communications and Quantum Imaging II conference in Denver, July 2004

We present the results of our polarimetric and spectropolarimetric monitoring of V838 Monocerotis, performed at Asiago and Crimean observatories during and after the multiple outbursts that occurred in January-March 2002. The polarization of the object is mainly due to interstellar polarization (P=2.48%). Intrinsic polarization up to 0.7% at 5000 A is present during the second maximum of the object (February 2002). This intrinsic component increases toward shorter wavelengths but our limited spectral coverage (5000-7500 A) does not allow conclusive inferences about its origin. A strong depolarization across the Halpha profile is observed. The interstellar polarization gives a lower limit to the reddening of E(B-V)>0.28, with E(B-V)=0.5 being the most probable value. A normal ratio of total to selective absorption (R_V=3.22+-0.17) was derived from the wavelength of maximum interstellar polarization. This suggests a low (if any) contribution by circumstellar material with peculiar dust to gas ratio. A polarimetric map of a portion of the light echo shows a complex polarization distribution reaching P_max=45%., Comment: 10 pages, 8 figures, A&A, in press

We propose a new technique, the use of FBGs (fiber Bragg gratings), for accurate, easy and low cost wavelength calibration of GAIA, RAVE and follow-ups spectra at local Observatories. FBGs mark the spectra with absorption lines, freely defined in number and position during the fibers manufacturing. The process goes in parallel with the science exposure and through the same optical train and path, thus ensuring the maximum return in wavelength calibration accuracy. Plans to manufacture and test FBGs for the CaII/Paschen region are underway at the Astronomical Observatory of Padova., Comment: in "GAIA Spectroscopy, Science and Technology", U.Munari ed., ASP Conf. Series, in press

We report on a spectro-polarimetric analysis of four southern Ultra-Luminous Infrared Galaxies (ULIRGs), aimed at constraining the presence of hidden broad AGN lines. For IRAS 19254--7245 ({\sl The Superantennae}) we find evidence for a significant level of polarized light in the H$\alpha$ line with FWHM$>$2300 km/s. Some degree of polarization is also detected in IRAS 20551-4250, though with lower significance. In the two other sources (IRAS 20100--4156 and IRAS 22491--1808) no polarized signals are detected. Although it is unclear from the present data if the origin of polarization is due to reflected light from an AGN or more simply to dichroic transmission by a dust slab, we find interesting correlation between the presence of polarized components in the optical spectra and independent evidence for AGN emissions in hard X-rays and the far-IR., Comment: 5 pages, 4 figures, accepted for publications on MNRAS Letters