CDROM/APJS/V95/P345 Second Caltech-Jodrell Bank VLBI Survey. I. (Taylor+ 1994) ================================================================================ The Second Caltech-Jodrell Bank VLBI Survey. I. Observations of 91 of 193 Sources G. B. Taylor, R. C. Vermeulen, T. J. Pearson, A. C. S. Readhead, D. R. Henstock, I. W. A. Browne, & P. N. Wilkinson <1994, ApJS, 95, 345> =1994ApJS...95..345T ================================================================================ Abstract: We define the sample for the second Caltech-Jodrell Bank VLBI survey. This is a sample of 193 flat- or gigahertz-peaked-spectrum sources selected at 4850 MHz. This paper presents images of 91 sources with a resolution of ~1 mas, obtained using VLBI observations at 4992 MHz with a global array. The remaining images and the integrated radio spectra will be presented in a forthcoming paper by Henstock et al. Keywords: galaxies: structure -- quasars: general -- radio continuum: galaxies -- surveys -- techniques: interferometric File Summary: -------------------------------------------------------------------------------- File Name Lrecl Records Explanations -------------------------------------------------------------------------------- table1.dat 84 193 The CJ2 sample table3.dat 66 91 Map parameters table4.dat 64 208 Gaussian models figure2 . . Directory of FITS images corresponding to the maps in Figure 2 of the printed paper -------------------------------------------------------------------------------- Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Source B1950 source name according to IAU convention 9-11 I3 h RAh *Right ascension, J2000 12-14 I3 min RAm R.A. 15-23 F9.5 s RAs R.A. 24 A1 --- DE- Declination sign, always blank 25-26 I2 deg DEd Declination, J2000 27-29 I3 arcmin DEm Dec. 30-37 F8.4 arcsec DEs Dec. 38-43 F6.3 --- S80cm *[]? Total flux density at 80 cm 44-49 F6.3 --- S20cm *[]? Total flux density at 20 cm 50-55 F6.3 --- S6cm *Total flux density at 6 cm 56-61 F6.3 --- S3.6cm *Total flux density at 3.6 cm 62 1X --- --- Blank 63-64 A2 --- ID *Optical identification 65-69 F5.1 mag R *[]? Apparent R magnitude 70 A1 --- f_z [f] Indicates a featureless spectrum 71-75 F5.3 --- z *[]? Redshift 76 1X --- --- Blank 77-84 A8 --- Date Date of VLBI observations -------------------------------------------------------------------------------- Notes for file: table1.dat -------------------------------------------------------------------------------- RAh: The position for one source 0256+424 was off in Patnaik et al. (1992, MNRAS, 254, 655) and as reproduced in the text. In this table the correct position is reported. Accuracy is ~12 mas, except for 0256+424 for which the accuracy is ~100 mas. S80cm: Total flux density at 80cm from J. Douglas, private communication. S20cm: Total flux density at 20cm from White & Becker (1992, ApJS, 79, 331). S6cm: Total flux density at 6cm from Gregory & Condon (1991, ApJS, 75, 1011). S3.6cm: Total flux density at 3.6cm from Kuhr et al (1981, AJ, 86, 854) or JVAS (Patnaik et al 1992, MNRAS, 254, 655). ID: Optical identification from automated scanning of the POSS plates or by eye. Key to identifications: Q - Quasar; G - Galaxy; BL - BL Lac object; EF - Empty Field; BS - Blue stellar object; BO - Blue object; RS - Red stellar object; RO - Red object; NS - Neutral stellar object; NO - Neutral object. R: Apparent R magnitude of the object obtained by automated scanning of the POSS E plates. The rms error is 0.3 down to magnitude 19.5 and increases to 0.5 by magnitude 20.0. z: Redshifts primarily from Veron-Cetty and Veron 1993, ESO Scientific Report No. 13 -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Source B1950 source name according to IAU convention 9 1X --- --- Blank 10-17 A8 --- Date Date of VLBI observation 18-20 I3 min Dur Duration on source of VLBI observation 21-25 F5.2 mas a FWHM of major axis of the restoring beam 26-30 F5.2 mas b FWHM of minor axis of the restoring beam 31-34 I4 deg PA Position angle of major axis, north thru east 35-39 I5 mJy/beam Snat Peak flux density, naturally weighted map 40-45 F6.2 mJy/beam Snat_rms Off source rms, naturally weighted map 46-50 F5.2 % Snat_cnt First contour, percent of peak flux density 51-55 I5 mJy/beam Stap []? Peak flux density, tapered map 56-61 F6.2 mJy/beam Stap_rms []? Off source rms, tapered map 62-66 F5.2 % Stap_cnt []? First contour, % of peak flux density -------------------------------------------------------------------------------- Byte-by-byte Description of file: table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Source *B1950 source name according to IAU convention 9-14 F6.3 Jy S Flux density of component 15-21 F7.2 mas r *Radius of component 22-28 F7.1 deg Theta *Angle to component 29-34 F6.2 mas a FWHM of major axis of component 35-39 F5.2 --- ba Axial ratio of major to minor axis, b/a 40-46 F7.1 deg Phi Position angle of major axis, north thru east 47-52 F6.3 --- Amp []? Amplitude agreement factor 53-58 F6.3 --- Phase []? Closure phase agreement factor 59-64 F6.3 --- Total []? Total agreement factor -------------------------------------------------------------------------------- Notes for file: table4.dat -------------------------------------------------------------------------------- Source: If this field is blank, the other fields are continuations of the previous record. r: Radius of component, measured from position of first component. Theta: Angle to component, measured north thru east from the position of the first component. -------------------------------------------------------------------------------- ================================================================================ (End) Lee Brotzman [ADS] 07-May-95