Observation of the galactic Sample Clauses

Observation of the galactic radio background‌ The antenna test bench at the site of the Nanc¸ay Radio Observatory is dedicated to the comparison and improvement of antennas used in radio astronomy. Owing to its radio quietness, the Nanc¸ay site features similar observing conditions as the site of the Xxxxxx Xxxxx Observatory. The three antennas under consideration (cf. section 2) were installed in the test bench for simultaneous observation of the radio background intensity with their read out dipole axes pointing in east-west direction. Besides different coaxial cables, all antennas were read out with the same chain of analog electronics. Frequency spectra from 22 to 82 MHz were recorded from the different antennas in consecutive sweeps with the same spectrum analyzer. We measure one spectrum every ~ 4 seconds per antenna. Within the measured bandwidth the continuous noise floor of the readout chain is more than 10 dB lower than the average signal power delivered by the Salla antenna, which provides the lowest signal power of the three antennas. In figure 17 the dynamic spectra derived from 105 spectrum sweeps for each antenna are displayed. The readings of the spectrum analyzer are normalized to the resolution bandwidth of the device to yield the recorded power spectral density. 2012 In the dynamic spectra, FM band transmitters appear as horizontal lines at the highest frequen- cies. At the lowest frequencies, short wave transmitters are visible with varying amplitude due to the changing conditions of the ionosphere. In the relevant frequency range from 30 to 80 MHz only a few transmitters are present, some of them only appearing for short periods of time. Vertical glitches are indicators for a saturation of the antenna over short periods of time. JINST For all three tested antennas, a variation over a wide frequency range with a day-like period- icity is visible. This variation results from the changing position of the galactic disc in the field of view of the antennas and follows sidereal time. The sidereal day is ~ 4 minutes shorter than the Julian day. We have verified the observation of the sidereal period with repeated measurements in the test bench several months apart to rule out man-made interference [19]. We observe that the variation of the visible galactic radio sky is mapped differently by the antennas onto the recorded power spectral density. Especially in the case of the Salla, the amplitude of the variation appears to be less distinct than for the other antennas. In...
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