VLBI observations at 18 and 2.8 CM - 0133 + 47, 0735 + 178, OH 471, OQ 172, 1633 + 38, and NRAO 667 /2147 + 145/

Details VLBI observations at 18 and 2.8 CM - 0133 + 47, 0735 + 178, OH 471, OQ 172, 1633 + 38, and NRAO 667 /2147 + 145/ VLBI observations at 18 and 2.8 CM - 0133 + 47, 0735 + 178, OH 471, OQ 172, 1633 + 38, and NRAO 667 /2147 + 145/

Jun 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980aj.....85..668m&link_type=abstract

Astronomical Journal, vol. 85, June 1980, p. 668-672. NASA-NSF-supported research.

Astronomy and Astrophysics

Astronomy

26

Centimeter Waves, Quasars, Radio Astronomy, Radio Sources (Astronomy), Stellar Structure, Very Long Base Interferometry, Astronomical Models, Heao 1, Heao 2, Spaceborne Astronomy

Scientific paper

We discuss our VLBI observations of the very flat-spectrum radio sources 0133+47 and PKS 0735+178 at 18 and 2.8 cm. The high-redshift QSOs OH 471 and OQ 172, the QSO 1633+38, and the steep-spectrum, low-frequency variable NRAO 667 (2147+145) were observed at 18 cm only. The effective angular resolution is ˜0".005 at 18 cm and ˜0".001 at 2.8 cm. The angular size of 0133+47 varies almost linearly with wavelength, as would occur if its flat spectrum were caused by a single, inhomogeneous, self-absorbed synchrotron component. The orientation of the radio structure also varies with wavelength, as has been found in other compact sources by Readhead et at. (1978). The flat-spectrum BL Lac object PKS 0735+178 is composed of several discrete components. At 18 cm, the sources OH 471 and 1633+38 appear to have a "core-halo" structure. OQ 172 is highly elongated, suggestive of either a jet or an unresolved double, while NRAO 667 is found to contain at least two components plus a more diffuse "halo." The sizes of OH 471 and OQ 172 are consistent with their lack of detection at x-ray energies by HEAO-1. HEAO-2 observations will be able to determine whether relativistic effects are required to reduce the expected Compton fluxes.

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