J/AJ/77/797 J/AJ/77/797 NRAO 5GHz Strong Source Survey I I K Pauliny-Toth K I Kellermann Astron. J. 77 797 1972 1972AJ.....77..797P VIII/38 : The Parkes-MIT-NRAO 4.85GHz (PMN) Surveys (Griffith+ 1993-1996) J/ApJS/90/173 : PMN map catalog of radiosources (Gregory+, 1994) Davies, Paper I. 1971AJ.....76..980D Pauliny-Toth et al., Paper II. 1972AJ.....77..265P (S1,S2 surveys) Radio sources Surveys The 140-ft telescope at the National Radio Astronomy Observatory has been used to extend the 5-GHz strong source (S) survey over an area of 1.14 steradian. Some 240 sources have been detected in this region, of which 135 are above the completeness limit of 0.6f.u. The distribution of spectral indices for sources above the completeness limit is much broader than for samples selected from long-wavelength surveys, owing to an increase in the fraction of compact sources with flat spectra. For about half of the sources selected at 6 cm, the spectral index {alpha}>-0.5. Analysis of the dependence of the spectral index on the flux density shows that, as expected from the 408-MHz number counts and spectral index distribution, at 5 GHz there are fewer flat spectra among the weak sources than among the stronger ones. The spectral index distributions for the identified galaxies and quasars show the familiar forms: the galaxies have a strong concentration near {alpha}=-0.8 with a small tail extending toward flat spectra. The quasars show a much broader distribution of indices, but the fraction (80%) of quasars having flat spectra ({alpha}>-0.5) is much greater than that found in the low-frequency surveys. The number-flux density relation for various groups of sources selected from the 5-GHz survey show that the anomalously steep slope is confined to (a) unidentified sources, (b) sources with steep spectra ({alpha}<-0.5), and (c) sources located in the north galactic hemisphere. Sources identified with radio galaxies or quasars, or which have flat spectra, or which are in the south galactic hemisphere all show a number-flux density slope near -1.5.

S3 Object designation --- RAh Right ascension (1950.0) h RAm Right ascension (1950.0) min RAs Right ascension (1950.0) s DE- Declination sign --- DEd Declination (1950.0) deg DEm Declination (1950.0) arcmin DEs Declination (1950.0) arcsec n_RAh Origin of the position number=1 blank = position measured with the 140-ft telescope at 5 GHz. OPT= optical position from literature. NRI= position measured with the NRAO interferometer at 2.7 GHz (Clark and Hogg, 1966ApJ...145...21C; Hogg, 1969ApJ...155.1099H; Wade, 1970ApJ...162..381W; Wade and Miley, 1971AJ.....76..101W). RRE= position measured with the interferometer of the Royal Radar establishment, Malvern at 2.7 GHz (Adgie, Crowther, and Gent, 1972MNRAS.159..233A). CAM= position measured with the Cambridge 1-mile synthesis instrument at 1.4 GHz (Parker, Elsmore, and Shakeshaft, 1966Natur.210...22P MacDonald, Kenderdine, and Neville, 1968MNRAS.138..259M; Mackay, 1969MNRAS.145...31M; Elsmore and Mackay, 1969MNRAS.146..361E). PKT= Parkes transit measurements at 2.7 GHz (Shimmins, Clarke, and Ekers, 1966AuJPh..19..649S). CT21= position measured with OVRO interferometer at 1.4 GHz (Fomalont and Moffet, 1971AJ.....76....5F). BOL= position from Bologna surveys at 408 MHz (Grueff and Vigotti, 1968ApL.....2..113G; Colla et al., 1970, Cat. <VIII/36>, 1972, Cat. <VIII/36>). 300= position measured with the 300-ft telescope at 1.4 GHz (Pauliny-Toth, Wade, and Heeschen, 1966ApJS...13...65P). --- S5GHz Flux density at 5GHz Jy n_SI > when lower limit --- SI Spectral index below 5GHz number=2 The spectral index is defined here as flux {prop.to} {nu}^{alpha}^ --- e_SI rms uncertainty on SI --- Ident Optical identification number=4 QSS: quasars with spectroscopic or photometric confirmation GAL: galaxy of undetermined type E: elliptical galaxy D: D galaxy DB: dumbbell galaxy SEY: Seyfert galaxy N: N galaxy EF: empty field (no object above plate limit or neutral star) CF: confused field: several galaxies or stellar objects in field --- n_Ident : tentative identification number=3 An asterisk denotes a tentative identification, e.g., a suggested QSS with no photometric or spectroscopic confirmation. Identifications made on the basis of the present work are indicated by a reference to a footnote in column Notes which also gives the origin of the position used others are taken from the literature. Identification are only given for sources above the completeness limit --- Notes Individual notes detailed in file "notes.dat" --- Cat Membership in other catalogs --- NoteID Note number, repeated when several lines are needed. --- Text Text of note --- James Marcout, Patricia Bauer CDS 1998Oct20 UNKNOWN UNKNOWN Prepared via OCR at CDS, and proof-read by Heinz Andernach (heinz@astro.ugto.mx). J_AJ_77_797.xml