First detection of ND in the solar-mass protostar IRAS16293-2422

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Table 2:

Parameters given by the HFS fit of each ND and NH transition.
Molecule	$\tau(J_{\nu}(T_{\rm ex}) - J_\nu(T_{\rm bg})-T_{c})$	$\Delta \varv$	$\tau$	$T_{\rm ex}$	N
& transition	K	km s^-1		K	cm^-2
ND (0₁-1₂)	-2.57 $\pm$ 0.33	0.74 $\pm$ 0.14	28.8 $\pm$ 3.9	4.6	$(1.7 \pm 0.6) \times 10^{14}$
ND (0₁-1₁)	-1.18 $\pm$ 0.13	0.82 $\pm$ 0.14	7.9 $\pm$ 2.1	4.5	$(0.9 \pm 0.4) \times 10^{14}$
NH (0₁-1₀)	-3.78 $\pm$ 0.58	0.60 $\pm$ 0.08	8.4 $\pm$ 2.1	9.5	$(2.0 \pm 0.8) \times 10^{14}$
NH (0₁-1₂)	-27.3 $\pm$ 0.27	0.64 $\pm$ 0.08	34.9 $\pm$ 4.8	7.7	$(1.8 \pm 0.4) \times 10^{14}$
NH (0₁-1₁)	-18.6 $\pm$ 0.75	0.63 $\pm$ 0.08	25.1 $\pm$ 1.6	8.8	$(2.2 \pm 0.4) \times 10^{14}$

Notes. $\tau$ is the total optical depth, $T_{\rm ex}$ the excitation temperature, $J_{\nu}(T_{\rm ex})$ the radiation temperature at the frequency of the transition, $J_{\nu}(T_{\rm bg})$ the radiation temperature of the cosmological background at $T_{\rm bg}=2.7$ K, $T_{\rm c}$ the brightness temperature of the continuum, $\Delta \varv$ the linewidth (full width at half maximum), and N the total measured column density in the given species. $T_{\rm ex}$ was deduced from Col. (2). Because of uncertainties in some stages of the data reduction process, we estimate that the linewidths are not known to better than about 0.25 MHz. It is this uncertainty that we quote here in Col. (3).

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