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J/MNRAS/204/151       Bright radio sources at 178 MHz (3CRR)       (Laing+ 1983)

Bright radio sources at 178 MHz: flux densities, optical identifications and the cosmological evolution of powerful radio galaxies. Laing R.A., Riley J.M., Longair M.S. <Mon. Not. R. Astron. Soc. 204, 151 (1983)> =1983MNRAS.204..151L
ADC_Keywords: Radio continuum ; Photometry, UBVRI ; Redshifts; Galaxies, radio ; QSOs Abstract: A revised sample of bright radio sources at 178MHz is defined in order to correct the biases introduced into the 3CR catalog by confusion and partial resolution. The sample is shown to be 96 percent complete to a flux-density limit of 10Jy for sources smaller than 10arcmin. The bias of the 3CR catalog against objects of larger angular size is also reduced. Optical identifications are presented for 96 percent of the sources, 71 percent with galaxies and 25 percent with quasars. The radio-galaxy population is found to show strong space-density evolution for luminosities in excess of approximately 1026.5W/Hz/sr at 178MHz (redshifts greater than or approximately equal to 0.2), while the evolutionary properties of galaxies and quasars of the same luminosity and redshift are very similar. Description: The sample is defined as in Jenkins, Pooley & Riley (1977, Cat. VIII/32), by the following rules : S178 ≥ 10Jy on the KPW (Kellerman et al. 1969ApJ...157....1K) scale; δ≥10° and |b|≥10°. A preliminary list of sources satisfying these criteria was prepared from the 3CR (Bennett, 1962, Cat. VIII/1; 1962MNRAS.125...75B), 4C (Pilkington+ 196 and Gower et al. 1967, Cat. VIII/4; Clarke 1965Obs....85...67C, Wills & Parker 1966MNRAS.131..503W) and 4CT (Williams et al. 1968MNRAS.139..289W, Caswell+ 1969MNRAS.145..181C and KPW) catalogues, the 3CR flux densities having been multiplied by 1.08 in order to rbing them on the KPW scale (Bennett, 1962, Cat. VIII/1). In addition, the literature was searched for references to sources with θEW>5arcmin, which would have been partially resolved by the 3CR telescope. Their flux densities at 178MHz have been determined by interpolation or extrapolation. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 146 173 Radio and optical data for the sample (June 1992 update by R. Laing) refs.dat 169 178 References notes.dat 80 27 Individual notes
See also: VIII/14 : 87GB Catalog of radio sources (Gregory et al., 1991) VIII/3 : An Optical Catalogue of Radio Galaxies (Burbidge+ 1979) VIII/32 : Extragalactic sources at 5GHz (Jenkins+ 1977) VII/49 : Galaxies and Clusters of Galaxies (CGCG) (Zwicky, 1968) VIII/4 : Fourth Cambridge Survey (4C) (Pilkington+ 1965; Gower+ 1967) VIII/1 : The 3C and 3CR Catalogues (Edge+ 1959-1962) J/AZh/77/3 : Studies of Bright Steep-Spectrum Radio Sources (Lipovka+, 2000) J/ApJS/13/65 : Radio source flux densities at 750+1400MHz (Pauliny-Toth+ 1966) : 3CRR Atlas home page : The online 3CRR catalogue Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 8 A8 --- IAU IAU name (HHMM+DDd; B1950) 9 A1 --- n_IAU [n] n : Note in notes.dat file 11- 18 A8 --- Name Common name if any 19- 24 F6.1 Jy S178 Flux at 178MHz (KPW scale) 27 I1 --- r_S178 [1/6] Source for S178 (1) 29- 32 F4.1 --- alpha Radio spectral index α, generally between 178 and 750MHz (2) 35- 36 A2 --- FR [I II C T] Radio morphology (3) 37 A1 --- f_FR [*] flag not explained in the paper 39- 40 A2 --- Core [C? ] C: compact radio core detected 42- 43 A2 --- OT [GQU? *] Optical type (4) 45- 46 A2 --- SpT Spectral classification (5) 48- 53 F6.4 --- z ? Redshift 54 A1 --- f_z [*] *: redshift estimated from the apparent magnitude (section 4) 55- 59 F5.2 mag Bmag ? B (blue) magnitude 60 A1 --- u_Bmag [*] Uncertain Bmag (6) 61- 65 F5.2 mag Vmag ? V (visual) magnitude 66 A1 --- u_Vmag [*] Uncertain Vmag (6) 67- 71 F5.2 mag Rmag ? R (red) magnitude 72 A1 --- u_Rmag [*] Uncertain Rmag (6) 73- 77 F5.2 mag rmag ? r magnitude 78 A1 --- u_rmag [*] Uncertain rmag (6) 79- 80 I2 h RAh Right ascension (B1950.0) 81- 82 I2 min RAm Right ascension (B1950.0) 83- 88 F6.3 s RAs Right ascension (B1950.0) 89 A1 --- f_RAs [*] * : pos. from 87GB (Cat. VIII/14) 90- 93 F4.3 s e_RAs ? rms uncertainty on right ascension 94 A1 --- DE- Declination sign (B1950.0) 95- 96 I2 deg DEd Declination (B1950.0) 97- 98 I2 arcmin DEm Declination (B1950.0) 99-103 F5.2 arcsec DEs Declination (B1950.0) 104 A1 --- n_DEs [*] * : position from 87GB (Cat. VIII/14) 105-108 F4.2 arcsec e_DEs ? rms uncertainty on declination 110-146 A37 --- Ref References for the radio structure, optical position, magnitude and spectrum, in refs.dat file
Note (1): Reference for 178MHz flux as follows: 1 = 4CT, Williams et al., 1968MNRAS.139..289W; Caswell & Crowther, 1969MNRAS.145..181C KPW, Kellerman et al., 1969ApJ...157....1K 2 = 4C, Clarke, 1965Obs....85...67C; Wills & Parker, 1966MNRAS.131..503W 3 = 4C, Pilkington & Scott, 1965, Cat. VIII/4 Gower, Scott & Wilss, 1967, Cat. VIII/4 4 = 3CR, Bennett, 1962, Cat. VIII/1 5 = 3CR, corrected for confusion by Veron (1977A&AS...30..131V) 6 = interpolation or extrapolation Note (2): Radio spectral index, α(S∝ν), generally between 178 and 750MHz (col. 4, Pauliny-Toth et al. 1966, Cat. J/ApJS/13/65; KPW (Kellermann et al., 1969ApJ...157....1K)). α has sometimes been determined from other published flux densities in the frequency range 151-2700MHz. All flux densities have been scaled by the factors listed in Laing & Peacock (1980MNRAS.190..903L) before evaluating spectral indices, so as to ensure consistency with the absolute scale of Baars et al. (1977A&A....61...99B). Thus the 178MHz flux densities used in evaluating the spectral indices are higher than those listed in col. "S178" by a factor of 1.09. Note (3): Radio morphology. Type as follows: I = The brightness distribution is peaked around the optical identification. II = The emission is brightest at the ends of the radio lobes (hotspots) furthest from the optical identification. This calculation is due to Fanaroff & Riley, 1974MNRAS.167P..31F) C = The brightness distribution for ν≳1GHz is dominated by an unresolved component with θ<1arcsec, possibly with weaker, extended emission. T = C in the original table Note (4): Optical type as follows: G = galaxy, confirmed spectroscopically and/or with an extended image. G* = probable galaxy, but with an image too faint for any extension to be measured. No spectroscopy has been attempted; the colours, if known, are those of an elliptical galaxy at high redshift. G? = doubtful identification with a galaxy, because (i) the image is very faint (ii) the field is obscured by a star (iii) the object is displaced from the centre of the source. Q = spectroscopically-confirmed quasar Q* = probable quasar or N-galaxy, with a stellar image but no spectral information U = unidentified Note (5): Spectral classification as follows: SE = strong emission lines such as [OII] λ 3727, [OIII] λ 5007 and [NeIII] λ 3869 are present in the spectrum (equivalent to Class A of Hine & Longair, 1979MNRAS.188..111H). Quasars are included in this group. E = weak emission lines, notably [OII] lλ 3727, are present. A = the spectrum contains absorption features only. ? = there is no published spectral information. The distinction between E- and A-type spectra (which together make up Class B of Hine & Longair, 1979MNRAS.189..111H) is very dependent on the sensitivity and spatial resolution of the detector used, but is retained because of its importance in the assessment of the reliability of the identifications. References are listed by Burbidge & Crowne (1979, Cat. VIII/3), Hine & Longair (1979MNRAS.189..111H) and Smith & Spinrad (1980PASP...92..553S); Note (6): * = denotes an approximate magnitude estimated from a photographic plate and uncertain by 0.5-1.0mag.
Byte-by-byte Description of file: refs.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Ref Reference code 10- 28 A19 --- BibCode BibCode 31- 53 A23 --- Aut Author's name 55-169 A115 --- Com Comments
Byte-by-byte Description of file: notes.dat
Bytes Format Units Label Explanations
1- 8 A8 --- IAU IAU name 10- 80 A71 --- Note Text of the note
Acknowledgements: From Heinz A. Andernach (A062 in his list)
(End) Patricia Bauer [CDS] 27-Nov-2003
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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