Nitrogen chemistry and depletion in starless cores

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Table 2:

Properties of the average profiles and average fractional abundance towards the observed cores (main beam temperature scale).
Source	$\aver{\tmb}$	$\aver{W}$	$\aver{v_0}$	FWHM	$\aver{N(\hcfifn)}$	$\aver{N(\hh)}_{20\hbox{$^{\prime\prime}$ }}$ ^b	$\aver{N}/\aver{2N(\hh)}$ ^c
	mK	m			10	22	$\times\dix{-12}$
L 183	125 $\pm$ 15	47 $\pm$ 4	2.49	0.35 $\pm$ 0.04	8.9 $\pm$ 0.8	5.6	0.8
L 1544^a	170 $\pm$ 12	85 $\pm$ 5	7.20	0.48 $\pm$ 0.05	16.1 $\pm$ 1.0	4.3	1.9
Oph D	102 $\pm$ 15	47 $\pm$ 6	3.44	0.43 $\pm$ 0.08	8.9 $\pm$ 1.1	5.6	0.8
L 1517B	82 $\pm$ 15	29 $\pm$ 3	5.69	0.33 $\pm$ 0.04	5.5 $\pm$ 0.6	2.0	1.4
L 310	20 $\pm$ 10	21 $\pm$ 3	6.69	0.98 $\pm$ 0.16	4.0 $\pm$ 0.6	0.8	2.5

Notes. ^(a) Using a two-component Gaussian fit. The FWHM is taken to be the equivalent linewidth, in this case; v₀=7.2 is adopted from Hily-Blant et al. (2008). ^(b) Column density of derived from the dust emission smoothed to 20 $^{\prime \prime }$ , assuming $\tdust=8$ K (see Table 1). The total (statistical and systematic) uncertainty is 30%. ^(c) The uncertainty is typically 40%.

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