High precision astrometry via very-long-baseline radio interferometry: Estimate of the angular separation between the quasars 1038+528A and B

Details High precision astrometry via very-long-baseline radio interferometry: Estimate of the angular separation between the quasars 1038+528A and B High precision astrometry via very-long-baseline radio interferometry: Estimate of the angular separation between the quasars 1038+528A and B

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983aj.....88.1133m&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 88, Aug. 1983, p. 1133-1137.

Astronomy and Astrophysics

Astronomy

36

Astrometry, Extragalactic Radio Sources, Quasars, Very Long Base Interferometry, Distance, Separation

Scientific paper

Dual-wavelength VLBI observations with the Mark III system of the two radio quasars 1038 + 528A and B yielded the following relative positions for the epoch 17 March 1981 (1950.0 coordinate system): ΔαB-A = 2s.1205009 ± 0s.0000002; ΔδB-A = 27".1429228 ± 0s.000003 (λ3.6 cm); °αB-A = 2.sl204408 ± 0s.0000006; A = 27".1428622 ± 0s.000009 (λ13 cm). The statistical standard errors represent fractional uncertainties of about 1 and 3 parts in l07 for λ3.6 and λ13 cm, respectively. The position of the brightest CLEAN component was chosen as the reference in each source at each wavelength. The difference found in the separations of these points at the two wavelengths, about 0".10008, is statistically very significant and probably represents the effect of wavelength-dependent opacity in the quasar 1038+528A (Marcaide and Shapiro 1983); plasma refraction contributes negligibly. Earlier, lower precision observations of these sources at these two wavelengths yielded relative positions consistent with those from the March 1981 epoch.

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