Mapping of the Decameter Radio Sources of Cassiopeia A Using a 100 km Range Long-Baseline Interferometer: Verification of a New Method of Phase Calibration of Interferometers

Details Mapping of the Decameter Radio Sources of Cassiopeia A Using a 100 km Range Long-Baseline Interferometer: Verification of a New Method of Phase Calibration of Interferometers Mapping of the Decameter Radio Sources of Cassiopeia A Using a 100 km Range Long-Baseline Interferometer: Verification of a New Method of Phase Calibration of Interferometers

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003pasj...55..527o&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.55, No.2, pp. 527-534

Astronomy and Astrophysics

Astronomy

Instrumentation: Interferometers, Ism: Individual (Cassiopeia A), Ism: Supernova Remnants, Techniques: High Angular Resolution, Techniques: Interferometric

Scientific paper

A new method is proposed for detecting the phase difference of cesium frequencystandards facilitated at coupling stations of an interferometer of 100km rangebaselines for observations of decameter wavelength radio waves. In this method, the Earth's rotation is utilized. That is, a time-depending variation of the phase differences of arriving radio waves from a given source forms a so-called fringe function due to the Earth's rotation. By generating a reference fringe function corresponding to the position of a selected radio source, the signals can be detected being selected from widely and continuously distributed radio sources in the sky, when the correlation is analyzed between the generated reference fringe function and the fringe data detected by the interferometer. The feasibility of the proposed method has been verified by applying the method to observations of a 100km range baseline interferometer for decameter wavelength radio waves at Tohoku University selecting the radio-wave sources in the Cassiopeia A supernova remnant as the objective. The results of the analyzed correlation values averaged for the observation data of 30hr, at 22.158MHz, are determined being scattered around average values with a distributionof less than 25& ; this distribution corresponds to a phase determination error of ± 12° for the cesium frequency standards of the interferometer at 10MHz. That is, we can calibrate the phase shift of the cesium frequency standards facilitated at each member station of the interferometer system with an accuracy of ± 12°, which corresponds to an accuracy of ± 1" fordetermining the direction of the radio-source position in the sky in the case of 100km range long baseline interferometer. This accuracy is, however, only possible when an integration time longer than 30hr is applied for analyses of the fringe correlation values.

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