Table 3: Results corresponding to the VLA data. Given are the source name, the frequency of the observation, the rms noise of the image, the integrated flux density and the source size.
Source $\nu$ $\sigma$ Integ. $S_{\nu}$ Size
  (GHz) (mJy/beam) (Jy) ( $\hbox{$^{\prime\prime}$ }$)
IRAS 01045+6505 8.4 0.29 242 4.7
IRAS 18032-2032 8.4 1.24 461, 71, 66$^\ddagger$ $19\times10,4,1^\natural$
IRAS 18479-0005 8.4 1.30 2588$^\star$ $4.8,1.5^\rhd$
IRAS 19442+2427 8.4 0.19 80$^\dagger$ $1,12\times7^\Diamond$
IRAS 19598+3324 8.4 2.57 3380 6
DR21 8.4 2.75 561, 864$^\lhd$ $4.4\times3, 6\times3.2^\triangle$
IRAS 23133+6050 8.4 0.74 737 9
$^\dagger$ Respective flux densities of components B, C and D. $^\natural$ Respective sizes of components B, C and D. $^\star$ The two main conponents A and B have flux densities of approximately 1315 and 571 mJy, respectively. $^\rhd$ Respective sizes of components A and B. $^\dagger$ The compact core has a flux density of 32 mJy. $^\Diamond$ Sizes of the compact and diffuse components, respectively. $^\lhd$ Flux densities of components A and B, respectively. $^\triangle$ Sizes of components A and B, respectively.

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