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Table 3:

A comparison between the H I halo cloud samples observed with different telescopes.
  |z| d $N_{\rm HI}$ $ \Delta \upsilon_{1/2}$ s D $\langle n \rangle$ $M_{H {\sc i}}$
  kpc  kpc $10^{19}{\rm cm^{-2}}$ km s-1 $^\prime$ pc ${\rm cm^{-3}}$ $M_{\odot}$
Effelsberg 0.9-5.4 3-11 0.4-7.4 2-21.1 9-27 8-70 0.07-1.2 3-770
WSRT     1.2-3.2 2.5-4.0 0.9-2.1 2-6 1.3-3.1 1-24
VLA     2.9-7.6 2.8-5.8 0.9-2.1 2-6 2.2-5.7 7-32
Lockman (2002) 0.6-1.2   0.7-6.3 5.4-26.3   19-35 0.1-0.9 12-290
Stanimirovic et al. (2006) 0.06-0.9 0.2-3 1-3 3-7.6 6-12 0.6-8   0.03-7
Ford et al. (2008) 0.3-1.7   0.4-6.6 5.8-26.2   46-100   120-4850
Stil et al. (2006) 0.01-0.16 4.2-7.7 8-39 3.4-16.5 1.8-29.4 3.4-36.7 3-24 9-2500

Notes. The table gives the range of values of the clouds for the following properties: |z| which is the absolute height above the plane (defined in the inner part of the disk) in kpc. d the distance in kpc. $N_{\rm HI}$ is the column density of H I gas in $10^{19}{\rm cm^{-2}}$. $ \Delta \upsilon_{1/2}$ is the line width in km s-1. s is the observed angular size in $^\prime$. D is the diameter in pc. $\langle n \rangle$ is the average volume density in ${\rm cm^{-3}}$. $M_{H {\sc i}}$ is the visible H I mass in $M_{\odot}$.


Source LaTeX | All tables | In the text

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