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Home All issues Volume 502 / No 2 (August I 2009) A&A, 502 2 (2009) 549-558 Full HTML
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Table 2:

Flux measurements at 92 cm (unless otherwise noted) for detections and nondetections of GCRT J1745-3009 at $\alpha $ = ${\rm 17h45m5.15s}$,$\delta $ = $-30\degr09\hbox{$^\prime$ }52.7\hbox{$^{\prime\prime}$ }$ (Kaplan et al. 2008). Corrections for primary beam attenuation and bandwidth smearing have been applied where appropiate.
No. Date Telescope Peak flux density Error on fit rms noise Resolution
  (yymmdd) (+conf.) (mJy/beam) (mJy/beam) (mJy/beam) ( $\hbox{$^{\prime\prime}$ }\times \hbox{$^{\prime\prime}$ }$)
1 860329 VLA A -49 27 18 $10\times 4$
2 860805 VLA B -19 20 100 $^{{\rm 1}}$ $44\times 33$
3 861226 VLA C -26 29 100 $^{{\rm 1}}$ $105\times 54$
4 881203 VLA A -18 15 15 $12\times 6$
5 890318 VLA B 41 19 8 $27\times 14$
6 020930 VLA CnB 110 $^{{\rm 2}}$ 8 $^{{\rm 2}}$ 8 $^{{\rm 3}}$ $44\times 36$
7 050324 WSRT 5 4 4 $148\times 27$
8 050514 WSRT (21 cm) -0.3 0.2 0.2 $68\times 9$
$^{{\rm 1}}$ The formal rms noise levels in these two maps are 19 mJy  ${\rm beam^{-1}}$ and 69 mJy  ${\rm beam^{-1}}$ for the 1986 August 5 and December 26 observations respectively, (much) lower than the indicated value of 100 mJy  ${\rm beam^{-1}}$. However, many bright compact sources that should be detectable in these maps, are not due to the very poor uv coverage of this observation. We accounted for this by replacing the rms noise by a higher number, in this way giving a very crude representation of these missing sources.
$^{{\rm 2}}$ Here we did not tie the clean beam fit to the position from Kaplan et al. (2008), but set the AIPS task ``IMFIT'' to solve for peak flux density as well as position in the residual image.
$^{{\rm 3}}$ This is the average noise in the residual image.

Source LaTeX | All tables | In the text

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