Table 2: Results from the observations. "Tapered'' 6 cm flux densities were measured using images tapered and restored with the 18 cm beam size. The MERLIN 18 cm and 6 cm positions differ by 35 mas because the coordinates used at the correlator were changed in an unknown way and the resulting offset could not be removed accurately. We have precessed the MERLIN B1950 coordinates to J2000 using NRAO's scheduling software SCHED. Positions are absolute for observations that were phase-referenced and the phase-referencing worked; such positions are given in h, m, s (for RA) and $^{\circ }$, $^{\prime }$, $^{\prime \prime }$ (for Dec). Otherwise the positions are given in mas relative to the strongest component. The flux density error estimates represent $1~\sigma$.
  Int. flux density Peak flux density Peak position (J2000) rms Beam size $\alpha^{18}_6$
  (mJy) (mJy/beam) RA                  Dec (mJy/beam) (mas) ( $S\propto\nu^{\alpha}$)
       NGC 5506      
global VLBI, 6 cm, 28 Feb. 1994            
B0 $45.7\pm5.9$ $33.9\pm4.3$ 0.0  0.0 0.9 12.6 $\times $ 6.0  
B1 $30.0\pm4.2$ $12.2\pm2.1$ 28.0 mas  7.3 mas      
B2 $10.6\pm2.5$ $4.9\pm1.4$ 41.6 mas  -8.3 mas      
VLBA 1997, 18 cm, Feb. 5, 1997            
B0 $27.9\pm3.1$ $24.0\pm2.7$ 0.0  0.0 0.26 $18.4\times11.4$  
B1 $24.4\pm2.9$ $15.9\pm1.9$ 29.7 mas  9.7 mas      
B2 $6.8\pm1.3$ $4.0\pm0.7$ 37.1 mas  -10.5 mas      
VLBA 1997, 6 cm, Feb. 5, 1997            
B0 $41.6\pm4.9$ $29.6\pm3.3$ 0.0  0.0 0.30 $5.7\times3.7$  
B1 $24.4\pm3.0$ $4.3\pm0.7$ 28.9 mas  9.1 mas      
VLBA 1997, 3.6 cm, Feb. 5, 1997            
B0 $27.0\pm3.4$ $21.5\pm2.6$ 0.0  0.0 0.46 $6.5\times3.0$  
EVN, 18 cm, Nov. 11, 1999            
B0 $32.9\pm4.1$ $31.0\pm3.5$ 0.0  0.0 0.43 26.2 $\times $ 14.1 0.06
B1 $25.6\pm3.3$ $22.1\pm2.6$ 26.2 mas  9.3 mas     -0.73
B2 $ 6.1\pm1.4$ $5.4\pm1.0$ 37.9 mas  -15.2 mas     -0.30
MERLIN, 18 cm, Nov. 11, 1999            
  $113.2\pm10.3$ $86.6\pm6.7$ 0.0  0.0 2.41 259.1 $\times $ 150.9 -0.33
EVN, 6 cm, Feb. 28, 2000            
B0 $35.9\pm4.1$ $36.1\pm4.2$ 14 13 14.87720  -03 12 27.6460 0.20 8.8 $\times $ 6.8  
(tapered) $32.0\pm3.7$          
B1 $11.0\pm1.4$ $6.8\pm1.2$ 14 13 14.87916  -03 12 27.6365      
(tapered) $10.8\pm1.4$          
B2 $1.9\pm0.5$ $1.3\pm0.4$ 14 13 14.87982  -03 12 27.6583      
(tapered) $4.4\pm0.7$          
MERLIN, 6 cm, Feb. 28, 2000            
B0+B1+B2 $85.8\pm6.4$ $66.8\pm3.8$ 0.0  0.0 0.43 78.6 $\times $ 62.4  
(tapered) $78.8\pm5.9$          
VLBA 2000, 18 cm, May 31, 2000            
B0 $49.0\pm5.8$ $46.0\pm5.1$ 0.0  0.0 0.45 18.6 $\times $ 11.3  
B1 $35.8\pm4.4$ $24.7\pm2.9$ 29.7 mas  10.1 mas      
B2 $4.6\pm1.1$          
             
VLBA 2000, 6 cm, May 31, 2000            
B0 $48.1\pm5.2$ $42.2\pm4.6$ 0.0  0.0 0.42 $7.4\times4.3$  
B1 $15.3\pm2.7$ $6.6\pm1.1$ 29.1 mas  9.6 mas      
B2 $2.3\pm0.8$ $2.7\pm0.7$ 45.2 mas  -8.5 mas      

     NGC 7674      
EVN, 18 cm, Apr. 13, 1985            
SE $31.4\pm3.9$ $31.4\pm3.9$ 0.0  0.0 0.46 $39.3\times24.2$  
NW $4.1\pm1.1$ $5.1\pm0.97$ -453.1 mas  230.8 mas      
EVN, 18 cm, Nov. 11, 1999            
SE $37.6\pm4.5$ $23.9\pm2.8$ 23 27 56.71054  +08 46 44.1310 0.40 32.5 $\times $ 9.8 -1.78
NW $11.0\pm2.1$ $5.6\pm1.0$ 23 27 56.67984  +08 46 44.3641      
MERLIN, 18 cm, Nov. 11, 1999            
SE $111.5\pm8.6$ $74.9\pm4.6$ 23 27 56.71730  +08 46 44.0104 0.82 276 $\times $ 110 -1.45
NW $45.6\pm4.0$ $29.2\pm2.3$ 23 27 56.68608  +08 46 44.2195     -1.58
EVN, 6 cm, Feb. 28, 2000            
SE $6.2\pm1.2$ $5.0\pm0.7$ 23 27 56.71201  +08 46 44.1368 0.24 8.2 $\times $ 4.6  
(tapered) $5.2\pm1.0$          
MERLIN, 6 cm, Feb. 28, 2000            
SE $18.0\pm2.3$ $16.2\pm1.1$ 0.0  0.0 0.31 82.2 $\times $ 36.8  
(tapered) $18.7\pm2.4$          
NW $3.8\pm0.7$ $3.9\pm0.5$ -452.5 mas  229.5 mas      
(tapered) $6.9\pm1.1$          
       NGC 2110      
EVN, 18 cm, Nov. 11, 1999            
Core $15.5\pm1.1$ $13.9\pm1.7$ 05 52 11.37378  -07 27 22.7071 0.32 26.2 $\times $ 14.6 0.12
MERLIN, 18 cm, Nov. 11, 1999            
(tapered)            
Core $29.4\pm2.9$ $31.4\pm2.5$ 05 52 11.38263  -07 27 22.5310 0.89 318.0 $\times $ 193.4 0.20
North $11.4\pm2.1$ $12.8\pm2.2$ 05 52 11.39579  -07 27 20.8662      
South $9.1\pm1.9$ $10.8\pm2.0$ 05 52 11.37443  -07 27 24.1280      
EVN, 6 cm, Feb. 28, 2000            
Core $20.3\pm2.7$ $20.0\pm2.5$ 0.0  0.0 0.48 7.9 $\times $ 6.4  
(tapered) $17.6\pm2.4$          
MERLIN, 6 cm, Feb. 28, 2000            
Core $36.6\pm2.9$ $38.9\pm2.3$ 0.0  0.0 0.33 90.0 $\times $ 67.7  
       Mrk 1210      
VLBA, 18 cm, Aug. 6, 1998            
(natural weighting)            
NW $37.4\pm3.8$ $21.6\pm2.5$ 08 04 05.85528  +05 06 49.8530 0.16 18.6 $\times $ 14.2  
SE $11.8\pm1.9$ $10.9\pm1.8$ 08 04 05.85690  +05 06 49.8292      
(uniform weighting) NW $36.0\pm3.8$ $12.8\pm1.6$ 08 04 05.85514  +05 06 49.8532 0.19 12.2 $\times $ 8.6 -1.26
SE $12.1\pm1.9$ $8.5\pm1.5$ 08 04 05.85701  +05 06 49.8291     -0.78
VLBA, 6 cm, Aug. 6, 1998            
(tapered)            
NW $9.1\pm1.1$ $6.3\pm1.2$ 08 04 05.85529  +05 06 49.8552 0.31 12.3 $\times $ 8.4  
SE $5.0\pm1.1$ $4.5\pm1.0$ 08 04 05.85694  +05 06 49.8304      
(full resolution)            
NW1 $1.0\pm0.2$ $1.1\pm0.1$ 08 04 05.85566  +05 06 49.8570 0.12 $3.2\times1.5$  
NW2 $2.1\pm0.4$ $1.7\pm0.2$ 08 04 05.85538  +05 06 49.8554      
NW31) $1.1\pm0.2$ $0.9\pm0.1$ 08 04 05.85511  +05 06 49.8553      
NW41) $1.2\pm0.3$ $1.0\pm0.1$ 08 04 05.85500  +05 06 49.8557      
SE $3.9\pm0.6$ $2.6\pm0.3$ 08 04 05.85696  +05 06 49.8298      
             
EVN, 18 cm, Nov. 11, 1999            
NW $36.6\pm4.3$ $19.8\pm2.3$ 08 04 05.85520  +05 06 49.8545 0.33 24.6 $\times $ 11.3 -1.19
SE $13.0\pm2.3$ $8.0\pm1.1$ 08 04 05.85666  +05 06 49.8301      
MERLIN, 18 cm, Nov. 11, 1999            
  $121.3\pm9.0$ $99.3\pm5.5$ 08 04 05.86024  +05 06 49.8985 0.50 240.7 $\times $ 136.5 -1.01
EVN, 6 cm, Feb. 28, 2000            
  $9.8\pm2.1$ $7.7\pm1.4$ 0.0  0.0 0.63 38.4 $\times $ 28.0  
MERLIN, 6 cm, Feb. 28, 2000            
  $33.1\pm2.5$ $24.1\pm1.4$ 0.0  0.0 0.21 72.7 $\times $ 47.6  
(tapered) $39.4\pm3.0$          

1) Positions and flux densities measured by fitting Gaussians to the image, instead of fitting a quadratic surface and integrating over the component region.

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