Alma Mater Studiorum Universit`a degli Studi di Bologna ... - Inaf

138 Data reduction and imaging of lobed radio galaxies
Table 6: Resolutions and noise levels for the images used in this work. Col.1 source name; Col.2
angular resolution; Col.3 observing frequency; Col.4 VLA configurations; Col.5 imaging method;
Col.6 off-source noise level on the I image (σ I ) and the average of the noise levels for Q and
U (σ P ). Col.7 approximate maximum scale of structure imaged reliably (Ulvestad, Perley &
Chandler 2009). Col.8 corrected single-dish flux densities put in the standard scale of Baars et al.
(1977), as used at the VLA. Col.9 references.
Source FWHM Freq Config. Method rms noise level Max I int /Jy Ref.
[arcsec] [GHz] I QU [µJy beam −1 ] scale Image SD
σ I σ P [arcsec]
0206+35 1.20 4860.1 BC MR MR 12 12 300 0.90±0.02 0.98±0.12 1
1.20 1464.9 AB MR MR 21 22 300 2.12±0.04 2.13 3
1.20 1385.1 AB MR MR 21 23 300 2.12±0.04 2.22 3
1.20 1425.0 AB MR − 19 − 300 2.12±0.04 2.18 4
4.50 4860.1 BC MR − 18 − 300 0.90±0.02 0.98±0.12 1
4.50 1425.0 AB MR − 38 − 300 2.13±0.04 2.18 4
0755+37 1.30 4860.1 BCD MR MR 7.8 7.9 300 1.26±0.03 1.27±0.02 2
1.30 1464.9 ABC MR MR 28 28 300 2.60±0.05 2.53±0.09 2
1.30 1385.1 ABC MR MR 27 26 300 2.74±0.05 2.62±0.09 2
1.30 1425.0 ABC MR − 20 − 300 2.64±0.05 2.57±0.09 2
4.00 4860.1 BCD MR MR 14 12 300 1.25±0.03 1.27±0.02 2
4.00 1464.9 ABC MR MR 44 42 300 2.59±0.05 2.53±0.09 2
4.00 1385.1 ABC MR MR 46 36 300 2.73±0.05 2.62±0.09 2
4.00 1425.0 ABC MR MR 32 − 300 2.65±0.05 2.57±0.09 2
M 84 1.65 4860.1 a ABC MR MR 15 11 300 2.94±0.06 2.88±0.08 3
1.65 1413.0 AB MR MR 140 140 120 6.03±0.12 6.44±0.24 3
4.5 4860.1 a C MR MR 23 20 300 2.98±0.06 2.88±0.08 3
4.5 1464.9 B MR MR 120 70 120 6.14±0.12 6.32±0.24 3
4.5 1413.0 AB MR MR 210 150 120 5.99±0.12 6.44±0.24 3
4.5 1385.1 B MR MR 130 69 120 6.46±0.13 6.51±0.24 3
References: 1 Gregory & Condon (1991); 2 Kühr et al. (1981); 3 Laing & Peacock (1981); 4 White & Becker (1992).
a Although the 1980 and 1981 observations have a centre frequency of 4885.1 MHz, the weighted mean for the combined dataset is
still close to 4860.1 MHz.
flux densities using the AIPS verbTVSTAT. We estimate that the errors are dominated by a residual
scale error of≈2%. All of the results are in excellent agreement with single-dish measurements
(Table 6).
The configurations, resolutions, deconvolution algorithms and noise levels for the final images
are listed in Table 6. The noise levels were measured before correction for the primary beam, and
are appropriate for the centre of the field.
.2 Images
Our conventions are as follows:
1. images of total intensity are show as grey-scales, over a range indicated by the labelled
wedges.
138