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Home All issues Volume 502 / No 2 (August I 2009) A&A, 502 2 (2009) 529-540 Full HTML
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Table 1:

Southern samplea.
Sourceb V-range rms $L_{\rm {H_{2}O}}^c$ Epoch Teld
  ( $\rm {km \ s^{-1}}$) ($\rm {mJy}$) ($L_{\odot}$)    
NGC 0055 -592, 752 10 <0.001 25-Jan.-2005 T
NGC 0134 891, 2236 5 <0.08 09-Sep.-2007 T
NGC 0300 -518, 827 9 <0.001 24-Apr.-2005 T
        30-Apr.-2005  
  -547, 797 5 <0.001 17-Sep.-2007  
        18-Sep.-2007  
NGC 1097   15 <0.30 13-Aug.-2003  
NGC 1313 -262, 1083 4 <0.005 02-Jan.-2005 T
NGC 1365   12 <0.39 09-Jun.-2003  
NGC 1559 596, 1941 5 <0.05 09-Apr.-2005 T
        10-Apr.-2005  
NGC 1672   19 <0.41 27-Jun.-2004  
NGC 1792 478, 1823 5 <0.05 24-Apr.-2005 T
        30-Apr.-2005  
NGC 1808   15 <0.18 05-May-2003  
NGC 2997 353, 1697 7 <0.05 17-Apr.-2005 T
        19-Apr.-2005  
        24-Apr.-2005  
NGC 3256e see Table 2       T
          A
NGC 3620e see Table 2       T
          A
NGC 3621 35, 1380 5 <0.02 26-Mar.-2005 T
        02-Apr.-2005  
NGC 4945     160 20-Sep.-1978  
        22-Sep.-1978  
NGC 5128f -50, 1200 - - 10-Apr.-2005 T
        17-Apr.-2005  
        24-Apr.-2005  
  407, 668 2 <0.02 29-Jun.-2006 A
NGC 6744   15 <0.13 17-May-2002  
NGC 7552   13 <0.41 19-Jun.-2004  
NGC 7582   13 <0.40 27-Jun.-2004  
NGC 7793 -445, 899 7 <0.002 26-Aug.-2007 T
        31-Aug.-2005  
a For coordinates, systemic velocities, 100 $\rm {\mu m}$ flux densities, and references see the Table containing the entire sample of FIR bright galaxies.
b Bold-faced source names refer to sources observed in this study; source names in italics refer to previously measured targets. For NGC 4945, see Dos Santos & Lèpine (1979), Batchelor et al. (1982), Greenhill et al. (1997). For the other sources in italics, see Kondrakto et al. (2006).
c Upper limits to maser luminosities are derived from $L_{\rm {H_{2}O}}/[\hbox{$L_{\odot}$ }]=0.023 \times S/[\rm {Jy}] \times \Delta \textit{v}/[\rm {km \ s^{-1}}] \times \textit{D}^{2}/[\rm {Mpc^{2}}]$, where S is 3 times the rms, in Col. 4, and $\Delta v$ is the channel width, $\rm {0.5 \ km\ s^{-1}}$ and $\rm {1.7 \ km \ s^{-1}}$ in our Tidbinbilla and ATCA observations (NGC 5128/Cen A only), respectively.
d Telescope: T = Tidbinbilla; A = ATCA.
e Newly detected maser.
f Observed with ATCA, because the 22 GHz continuum was too strong to obtain single-dish spectra with high baseline quality.

Source LaTeX | All tables | In the text

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