Table 3: Total column densities, radial velocities, intrinsic line widths b, and origin of the detected H2 towards each star in the sample.
Name log N(H2) (a) $v_{\rm rad}$ (H2) (b) b Origin Ref. Inclination Ref.
    (km s-1) (km s-1) of H2   of the disk ($^\circ$) (c)  
$\beta $ Pictoris $\leq$17.41 - - - (1) $\sim $0 (6)
HD 135344 $\leq$17 - - - (1) 79 $\pm $ 2 (7)
HD 100453 $\leq$16 - - - (1) $\sim $65 (8)
HD 36112 $\leq$17.85 -- - - (1) 53-57 (9)
HD 104237 $\rm 18.68_{-0.61}^{+0.39}$ $\rm 1.4_{-1.0}^{+0.9}$ $\rm 5.3_{-0.7}^{+0.6}$ CS (1) 78 (10)
HD 163296 $\rm 18.16_{-0.40}^{+0.27}$ 0 $\pm $ 2 $\rm 2.2_{-0.7}^{+0.5}$ CS (2), (1) 60 $\pm $ 5 (11)
NX Pup $\leq$19.30 - - - (1) ?  
AB Aur $\rm 20.03_{-0.19}^{+0.15}$ 2 $\pm $ 3 $\rm 6.8_{-2.2}^{+2.8}$ IS/CS? (1),(4) 55-63 (13)
HD 141569 $\rm 20.32_{-0.22}^{+0.20}$ 20 $\rm 5.3_{-0.5}^{+0.3}$ IS (1) 51 $\pm $ 3 (14)
HD 100546 $\rm 16.46_{-0.14}^{+0.24}$ 0 $\pm $ 2 $\rm 3.4_{-0.5}^{+0.8}$ CS (2), (1) 51 $\pm $ 3 (15)
HD 109573 $\leq$15.40 - - - (1) 20.5 $\pm $ 3 (12)
HD 176386 $\rm 20.80_{-0.26}^{+0.18}$ $\sim $-7.0   CS (1) n  
HD 250550 $\rm 19.26_{-0.40}^{+0.17}$ $\rm -1.0_{-2.0}^{+1.7}$ $\rm 5.6_{-0.8}^{+0.7}$ CS (3) n  
HD 85567 $\rm 19.33_{-0.17}^{+0.20}$ $\rm 4.5_{-0.2}^{+0.3}$ $\rm 6.0_{-0.9}^{+0.7}$ CS (1) n  
HD 259431 $\rm 20.64_{-0.19}^{+0.11}$ $\rm 13.0_{-1.8}^{+2.2}$ $\rm 4.5_{-0.5}^{+0.3}$ CS (3) n  
HD 38087 $\rm 20.43_{-0.08}^{+0.15}$ $\rm 2.36_{-2.1}^{+1.2 }$ $\rm 3.7_{-0.2}^{+0.3}$ CS (1) n  
HD 76534 $\rm 20.64_{-0.16}^{+0.16}$ $\rm0.0_{-1.3}^{+0.3}$ $\rm 5.0_{-0.3}^{+0.4}$ CS (5) n  
(a) Upper limits on the column densities have been obtained with b=1 km s-1.
(b) Radial velocities are in the stars' rest frames.
(c) The inclination angles for the disks are given with respect to the line of sight (i=0: edge-on). ``n'' indicates stars with no evidence of disk.
References in Col. 6 concern the results given in Cols. 2 to 5, and references in Col. 8 are for the inclination angles of the disks. References: (1) this work; (2) Lecavelier des Etangs et al. (2003); (3) Bouret et al. (2003); (4) Roberge et al. (2001); (5) Martin et al. (2004); (6) Smith & Terrile (1984); (7) Dent et al. (2005); (8) Dominik et al. (2003); (9) Eisner et al. (2004); (10) Grady et al. (2004); (11) Grady et al. (2000); (12) Augereau et al. (1999); (13) Eisner et al. (2003); (14) Weinberger et al. (1999); (15) Augereau et al. (2001).


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