Table 4: p- ${\rm D}_{2}{\rm H}^{+}$ column density upper limits.
Source $\Delta {v}_{\rm res}$ $T_{\rm sys}$ $t_{\rm int}$ $T_{\rm rms}$a $T_{\rm R}$ $\eta_{\rm b}$ $T_{\rm ex}$b N(p- ${\rm D}_{2}{\rm H}^{+}$) p/oc
Name ( ${\rm km~s}^{-1}$) (K) (min) (K) (K)   (K) (1013 cm-2)  
B 1 0.083 3950 251 0.068 <0.20 0.4 11.9 <0.9 <1.0
NGC 1333- ${\rm DCO}^+$ 0.083 3300 91 0.068 <0.20 0.4 12.6 <0.9 <2.6
NGC 2264G-VLA2 0.021 1436 93 0.045 <0.14 0.4 14.4 <0.2 <0.7
L 183 0.042 1770 42 0.084 <0.25 0.4 6.9 <7.9 <3.2
16293Ed 0.10 ... 103 0.19 0.85 0.60 10.7 1.2 $\pm$ 0.5 1.0
L 1544e 0.021 ... 230 0.18 <0.54 0.4 7.6 <2.5 <0.8
a In radiation temperature units; b excitation temperature assuming a critical density of 105  ${{\rm cm}}^{-3}$ for the observed ${\rm D}_{2}{\rm H}^{+}$ transition; c p/o $\equiv $ N(para- ${\rm D}_{2}{\rm H}^{+}$)/N(ortho- ${\rm H}_{2}{\rm D}^{+}$); d data from Vastel et al. (2004). The column density has been estimated using the method described in the text; e data from Vastel et al. (2006a). The column density has been estimated using the method described in the text, with the parameters listed in Table 3.

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