8035 VIII/35 Radio Sources observed with Culgoora Circular Array O B Slee Australian J. Phys. 48 143-186 1995 1995AuJPh..48..143S Radio sources This is a final, updated and recalibrated list of sources that were observed with the Culgoora Circular Array (CCA) in the interval 1970-1984. The list contains all the sources that were published in the Culgoora-1,2,3 Lists plus additional sources resulting from a survey of 353 Abell clusters of galaxies. The observations were made at 80 MHz and 160 MHz with HPBW in RA of 3.70' and 1.85' respectively. The beamwidth in Dec is wider by sec(30.3 + Dec). This list brings together all CCA measurements of flux density, position, spectral index and angular size, with limiting flux densities of 4 Jy at 80 MHz and 2 Jy at 160 MHz. References to the original Culgoora publications are given for each source. The sources were selected for CCA observations from the Parkes, 4C and Ohio catalogues if an extrapolation of the then existing spectral data indicated that the 80 MHz flux density would be > 5 Jy. In addition, about 300 additional sources were added from lists of special classes of objects such as those discovered at higher frequencies from surveys of the galactic plane, lists of pulsars and supernova remnants, from a list of nearby bright galaxies and finally from a CCA survey of 353 Abell clusters of galaxies. An area of 16'x16' was surveyed about the centres of 3500 fields, resulting in a total survey area of about 0.1 sr at 80 MHz. Nomenclature Notes: Sources from this catalogue are designated "Cul HHMM+DDd" in the literature. Note that the original Cul 1,2,3 lists have only HHMM+DD as a name, but the present names should be preferred.

Cul Source name number=1 the Cul designation contains the B1950 name of the source, using IAU recommended standards. The first four characters are the hours and minutes of right ascension, and the last four the signed declination in tenths of a degree (truncated). The source names in the original Culgoora-1,2,3 Lists contained the signed declination in degrees (truncated). IAU names given to tenths of declination in previous papers (e.g. ref #4 in section 9 below) may differ by one or two in the last digit. The Cul designation is followed by symbols: * An asterisk (*) following the source name denotes that this is the centroid of two or more components, which can be located in the maps and tables of references 3,4 and 5 below. The components are not always parts of the same source. # the flag '#' indicates that the Culgoora position was lost, but the source can confidently be identified with a source whose coordinates are given in the publication listed in the reference column. --- n_Cul Note on Source number=1 the Cul designation contains the B1950 name of the source, using IAU recommended standards. The first four characters are the hours and minutes of right ascension, and the last four the signed declination in tenths of a degree (truncated). The source names in the original Culgoora-1,2,3 Lists contained the signed declination in degrees (truncated). IAU names given to tenths of declination in previous papers (e.g. ref #4 in section 9 below) may differ by one or two in the last digit. The Cul designation is followed by symbols: * An asterisk (*) following the source name denotes that this is the centroid of two or more components, which can be located in the maps and tables of references 3,4 and 5 below. The components are not always parts of the same source. # the flag '#' indicates that the Culgoora position was lost, but the source can confidently be identified with a source whose coordinates are given in the publication listed in the reference column. --- o_S(160) Number of observations at 160 MHz number=2 These columns contain the numbers of independent observations at 160 MHz and 80 MHz respectively. Each observation consists of averaging 10-20 drift scans with the central 8 or 16 beams (spaced in declination) of the CCA. --- o_S(80) Number of observations at 80 MHz number=2 These columns contain the numbers of independent observations at 160 MHz and 80 MHz respectively. Each observation consists of averaging 10-20 drift scans with the central 8 or 16 beams (spaced in declination) of the CCA. --- RAh Right Ascension B1950 (hours) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. h RAm Right Ascension B1950 (minutes) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. min RAs Right Ascension B1950 (seconds) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. s DE- Declination B1950 (sign) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. --- DEd Declination B1950 (degrees) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. deg DEm Declination B1950 (minutes) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. arcmin DEs Declination B1950 (seconds) number=3 The 160 MHz position is given if available, otherwise the 80 MHz position. The positional calibration was obtained by observing at 2-hourly intervals strong unresolved sources with accurate high-frequency positions. Position errors are tabulated for various flux ranges and numbers of observations in the original Culgoora-1,2,3 Lists. The positions of sources with contour maps at 160 MHz (entries in the angular size columns) are the centroids of the brightness distributions. Positions of other sources were found by fitting a one-dimensional Gaussian to the hour angle drift response and another Gaussian across the declination channels. arcsec GLON Galactic longitude deg GLAT Galactic latitude deg l_S(160) Limit flag on S(160). --- S(160) Flux density at 160 MHz number=4 a recalibration of the flux scales was carried out by Slee & Siegman (1988MNRAS.235.1313S). This resulted in our increasing the flux density by an average of 10% at 80 MHz and 12% at 160 MHz. The 160 MHz flux densities of sources with contour maps (entries in the angular size columns) were obtained by integrating the brightness contours. Jy l_S(80) Limit flag on S(80). --- S(80) Flux density at 80 MHz number=4 a recalibration of the flux scales was carried out by Slee & Siegman (1988MNRAS.235.1313S). This resulted in our increasing the flux density by an average of 10% at 80 MHz and 12% at 160 MHz. The 160 MHz flux densities of sources with contour maps (entries in the angular size columns) were obtained by integrating the brightness contours. --- SpIndex Spectral index between 80 and 160 MHz number=5 this column contains the power-law spectral index between 80 and 160 MHz (S(nu) {prop.to} nu^SpIndex^). A negative spectral index implies that flux density is decreasing with frequency. --- l_MajAxis Limit flag on MajAxis --- MajAxis Major axis to 0.10 brightness at 160 MHz number=6 These columns contain the major and minor axes of a 2-dimensional Gaussian ellipse that has been fitted to the 160 MHz contour map together with the position angle of the major axis (from north through east).The axes are given to the 0.10 brightness points (1.82 x half-brightness diameter). Where only the major axis is presented as a lower limit of 1.8 arcmin, the limit was derived (at the 95% confidence level) from one-dimensional Gaussian fits to the drift profiles in RA and Dec. arcmin l_MinAxis Limit flag on MinAxis --- MinAxis Minor axis to 0.10 brightness at 160 MHz number=6 These columns contain the major and minor axes of a 2-dimensional Gaussian ellipse that has been fitted to the 160 MHz contour map together with the position angle of the major axis (from north through east).The axes are given to the 0.10 brightness points (1.82 x half-brightness diameter). Where only the major axis is presented as a lower limit of 1.8 arcmin, the limit was derived (at the 95% confidence level) from one-dimensional Gaussian fits to the drift profiles in RA and Dec. arcmin PA Position angle of major axis (east from north) number=6 These columns contain the major and minor axes of a 2-dimensional Gaussian ellipse that has been fitted to the 160 MHz contour map together with the position angle of the major axis (from north through east).The axes are given to the 0.10 brightness points (1.82 x half-brightness diameter). Where only the major axis is presented as a lower limit of 1.8 arcmin, the limit was derived (at the 95% confidence level) from one-dimensional Gaussian fits to the drift profiles in RA and Dec. deg Refs References number=7 References are 1 =1973AuJPS..27....1S Slee & Higgins 1973 (Culgoora-1 List) 2 =1975AuJPS..36....1S Slee & Higgins 1975 (Culgoora-2 List) 3 =1977AuJPS..43....1S Slee 1977 (Culgoora-3 List) 4 =1983PASAu...5..114S Slee & Siegman, Proc. ASA (Cluster Survey) 5 =1982PASAu...4..278S Slee, Siegman, & Mulhal (Culgoora-3 Analysis) 6 =1979PASAu...3..332S Slee & Quinn, Proc. ASA (Cluster Survey) 7 =1972ApL....12...75S Slee, Astrophys. Lett. (Bright Galaxies at 80 MHz) 8 =1972AuJPh..25..429D Dulk & Slee, Austral. (Supernova Remnants) 9 =1975PASAu...2....1S Slee & Sheridan, Proc.ASA (Cen-A & Pictor-A) 10 =1974Natur.248...33D Dulk & Slee (Sgr-A at 160 MHz) 11 =1991ApJS...75....1B Becker, White & Edwards (0736+016,2330+091,2349+135) 12 =1992ApJS...80..501O Owen, White & Burns (1005+007) 13 =1980BAAS...19.1048D Douglas (Texas Survey) Additional data in these papers include 80 MHz positions, optical identifications and beam broadening from the one-dimensional Gaussian fitting. The Culgoora-1,2,3 papers also contain tables listing the expected errors in flux density and position. References 3 and 4 contain the 160 MHz contour maps for many sources. Reference numbers 11,12,13 do not refer to Culgoora publications, but refer to papers containing sources that can be confidently identified with five sources, whose Culgoora positions have been lost. --- Heinz J. Andernach ESA-IUE 1996Feb19Author's address: O.B Slee, Australia Telescope National Facility, CSIRO, Sydney <bslee@atnf.csiro.au> UNKNOWN UNKNOWN The basic table was formed by electronically scanning the Culgoora-3 list. Each line was later checked by visual comparison with the unscanned list and scanning errors were corrected manually. Additional sources were added manually from other references in <cul_ref>. Angular size information was extracted from references 4 and 5 and added manually to the final table. Positions of five sources for which Culgoora positions had been lost were identified with the help of the EINLINE service (telnet to einline.harvard.edu, login as 'einline' with no password) and H. Andernach (file r132.new). Note that the electronic version differs from the one published in AuJPh.48.143 in that it includes several dozen more upper limits at 160 MHz, taken from the listed references. VIII_35.xml