A Catalogue of Radio Sources

H. Kuehr, U. Nauber, I.I.K. Pauliny-Toth, and A. Witzel

(1.variant scanned/proofed by H.Andernach 10/95)
(2.variant typed by N. Zabavskaja 01/96)

Abstract

The flux densities

Generally only flux densities greater than three times their probable error were included in the list.

For some catalogues giving flux densities at frequencies below 1400 MHz, we found that the flux densities below a certain value became increasingly unreliable. Therefore we did not include these flux densities in Table 2. The limiting flux density value is given in col. 5 of Table 1. In those cases where individual flux density measurements at one frequency in several catalogues agreed within the errors, we generally included only one value in Table 2. Also included in Table 2 are a number of previously unpublished flux densities. These are,in order of frequency: 750 MHz and 1400 MHz flux densities obtained by Kellermann and Pauliny-Toth with the 300 ft telescope of the NRA0 in 1968 and 1969 (code nrs 101, 102), 1410 and 2380 MHz flux densities obtained by Biermann with the Arecibo telescope in 1978 (code nrs 103, 104), 2695 MHz flux densities obtained by Pauliny-Toth, Preuss and Witzel in 1972 with the 100-m telescope (code nr 105), 2695 MHz flux densities obtained by Porcas et al. between 1974 and 1976 with the Jodrell Bank MKII telescope and with the 300 ft telescope of the NRA0 in 1976 (106), and 10695 MHz flux densities obtained by Pauliny-Toth, Preuss and Witzel in 1972 with the 100-m telescope (107). Also under the code nr. 105 the 2695 MHz flux densities from the "S4" paper (Pauliny-Toth et al. 1978) are listed.

The radio spectra

In a first attempt we tried to fit the spectrum with a straight line of the form y = (a + bx), where y = ln S, x = ln freq. If the straight line (S) could not fit the data a function of the type (a + b*x + c*e^+-x ) was tried (CC+, CC-). If such an exponential function could not represent the data a parabolic fit (a + bx + cx^2) was attempted (C+, C-). A reduced chi-square-test was used to decide whether the data could be fitted with either of the above functions. The spectra of those sources which could not be adequately fitted were considered to be complex (CPX).

Content of Table 1

colomns:
• 1 gives the code nr., which is used with the flux densities in Table 2
• 2 denotes the frequency of the flux densities of the catalogue
• 3 gives the reference
• 4 gives the conversion factor used to scale the flux densities to the scale of Baars et al.
• 5 gives the flux density limit, below which no flux density was included in Table 2
• 6 gives the common designation of the catalogue if any

Content of Table 2

In the following lines, flux density data at one or more frequencies are listed as follows: the frequency, the flux density and its error and the code nr. corresponding to col. 1 of Table 1.

Remarks to Table 1

• (i) Unpublished flux densities at several frequencies are listed in Table 2 with code numbers 101 - 107. See page II
• (ii) 178 MHz flux densities from Kellermann et al. 1969 (code nr. 9) were only included in Table 2 if no flux density by Veron 1977 (code nr. 10) was available.
• (iii) 1400 MHz flux densities by Bridle et al. 1972 (code nr. 32) were included in Table 2 if no flux density by Witzel et al. 1971 (code nr. 31) was available.
• (iv) Flux densities measured by Fitch et al. 1969 and Brundage et al. 1971 (code nr. 36) were included in Table 2 for 23 sources for which no flux density was given in Witzel et al. 1971, Bridle et al. 1972, or Witzel et al. 1979.

References: