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Table 3:

Results of the H2 S(1) line analysis.

Star 		$\lambda _{\rm obs}$(a) Integrated flux(b) Intensity(b) $N({\rm H}_2)$ upper limits(b)   H2 mass upper limits(b, c)
HD ($\mu $m) (erg s-1 cm-2) (erg s-1 cm-2 sr-1) (cm-2)   ( $M_{\rm Jup}$)
        150 K 300 K 1000 K   150 K 300 K 1000 K
142527 17.0351 $<1.0\times 10^{-14}$ <2.5 $\times$ 10-3 9.4 $\times$ 1022 6.1 $\times$ 1021 1.4 $\times$ 1021   1.9 $\times$ 10-1 1.2 $\times$ 10-2 3.3 $\times$ 10-3
169142 17.0343 <1.8 $\times$ 10-14 <4.2 $\times$ 10-3 1.6 $\times$ 1023 1.0 $\times$ 1022 2.4 $\times$ 1021   3.5 $\times$ 10-1 2.1 $\times$ 10-2 6.1 $\times$ 10-3
150193A 17.0349 <2.1 $\times$ 10-14 <5.0 $\times$ 10-3 1.9 $\times$ 1023 1.2 $\times$ 1022 2.8 $\times$ 1021   4.5 $\times$ 10-1 2.7 $\times$ 10-2 7.7 $\times$ 10-3
163296 17.0345 <2.8 $\times$ 10-14 <6.7 $\times$ 10-3 2.5 $\times$ 1023 1.6 $\times$ 1022 3.8 $\times$ 1021   3.9 $\times$ 10-1 2.4 $\times$ 10-2 6.9 $\times$ 10-3
100546 17.0363 <1.4 $\times$ 10-13 <3.3 $\times$ 10-2 1.2 $\times$ 1024 7.9 $\times$ 1022 1.9 $\times$ 1022   1.4 8.4 $\times$ 10-2 2.4 $\times$ 10-2

Notes. (a) expected position of the line in the observed spectra by correcting the radial velocity of the star for the epoch of observation. (b) 3$\sigma $ upper confidence limits. (c) masses of H2 are calculated assuming the distances quoted in Table 1.


Source LaTeX | All tables | In the text

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