Positions, Structures and Polarization of 404 Compact Radio Sources

Abstract

Amplitude calibration was based on 3C286, whose fluxes at 4885 and 1465 MHz were assumed to be 7.41 and 14.41 Jy, respectively, in accord with the scale of Baars et al. (1977).

short description of columns, as taken from the publication:

• 1 source name
• 2 alternate name (3C, 4C)
• 3 Right ascension (B1950)
• 4 Declination (B1950)
• 5 Flux at 4885 MHz (mJy)
• 6 Flux at 1464 MHz (mJy)
• 7 Spectral index alpha^20_6, defined by S~(nu)^(-alpha)
• 8 Polarized flux at 4885 MHz (mJy)
• 9 Position angle of polarized flux at 4885 MHz in degrees
• 10 Degree of polarized flux at 4885 MHz, in percent.
• 11 Polarized flux at 1465 MHz (mJy).
• 12 Position angle of polarized flux at 1465 MHz in degrees
• 13 Degree of polarized flux at 1465 MHz, in percent.
• 14 Peak brightness of secondary structure, or upper limit (as percentage of peak), at 6 cm.
• 15 Peak brightness of secondary structure, or upper limit (as percentage of peak), at 20 cm.
• 16 Optical identification
• 17 Visual magnitude of optical ID.
• 18 A plus sign indicates that the optical ID was taken from Hewitt and Burbidge 1980, ApJS 43, 57.
• 19 Note to structure (see other table) for sources marked with an asterisk.

  Important comments concerning Table II follow.

  Column 2. It is often difficult to decide whether a given 4C source is to be identified with a compact source. A conservative approach has been used.

  5 and 6. This is the flux of the core in all cases where this can be determined. Sources where this could not be done have an asterisk in column 14 or 15. The error in the flux is estimated to be less than ~ sqrt [(0.03S)**2 + (0.002)**2] Jy, with S in Jy.

  8, 9, 11, and 12. The listed flux applies to the core only, unless the core cannot be distinguished, in which case the listing applies to the whole source. The error in polarized flux is estimated to be sqrt [4 + (0.4S)**2] mJy, where S is the total flux in Jy. The error in position angle is strongly dependent upon the polarized flux, and is roughly given by 65 sqrt[4 + (0.4S)**2]/m degrees.

  14 and 15. Listed secondaries are generally found within the clean-search window defined earlier. Occasionally, larger windows were searched to find more distant structure. The absence of a listed secondary does not guarantee the source has none -it may lie outside the search window. This is particularly true at 6 cm where the search window was 6.4 arcsec wide. Entries marked by an asterisk indicate the source is slightly resolved, but not enough for a reliable map.

  16-18. These are taken from Hewitt and Burbidge