TAILIEUCHUNG - The vatly radio telescope

A small radio telescope (SRT) has been installed on the roof of the Hanoi astrophysics laboratory VATLY. It is equipped with a m diameter mobile parabolic dish remotely controlled in elevation and azimuth and with super-heterodyne detection around the 21 cm hydrogen line. First results of observations of the Sun and of the centre of the Milky Way are presented. They demonstrate the high quality of the telescope performance and are used to evaluate lobe size, signal to noise ratios, anthropogenic interferences and measurement accuracies. Particular attention is given to the measurement of the pointing accuracy. The rich measurement programme that is now at hand is briefly sketched. | Communications in Physics, Vol. 22, No. 4 (2012), pp. 365-374 THE VATLY RADIO TELESCOPE NGUYEN VAN HIEP, PHAM TUAN ANH, PHAM NGOC DIEP, PHAM NGOC DONG, DO THI HOAI, PHAM THI TUYET NHUNG, NGUYEN THI THAO, AND PIERRE DARRIULAT VATLY, Institute for Nuclear Science and Technology Abstract. A small radio telescope (SRT) has been installed on the roof of the Hanoi astrophysics laboratory VATLY. It is equipped with a m diameter mobile parabolic dish remotely controlled in elevation and azimuth and with super-heterodyne detection around the 21 cm hydrogen line. First results of observations of the Sun and of the centre of the Milky Way are presented. They demonstrate the high quality of the telescope performance and are used to evaluate lobe size, signal to noise ratios, anthropogenic interferences and measurement accuracies. Particular attention is given to the measurement of the pointing accuracy. The rich measurement programme that is now at hand is briefly sketched. I. THE VATLY RADIO TELESCOPE A small radio telescope (SRT) has been installed on the roof of the VATLY astrophysics laboratory [1], commissioned and run-in. It is now routinely taking data. The present note presents its main features, illustrates its performance and provides evidence for excellent measuring conditions on both the continuum and the 21 cm hydrogen line. The telescope is equipped with a mobile parabolic dish, m in diameter, remotely adjustable in elevation and azimuth (Fig. 1). The reflected power is collected at the focus, where it is locally preamplified, shifted to lower frequency using standard superheterodyne, amplified and digitized. Standard data collection consists in a sequence of successive measurements of ∼ s duration each, digitized in the form of a frequency histogram covering ∼ MHz in 156 bins of ∼ kHz each. Such a typical distribution is shown in Figure 2 (left). The 21 cm hydrogen line is clearly seen above a slowly varying continuum. The hydrogen line .

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