Nitrogen chemistry and depletion in starless cores

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Table 1:

The sample of cores observed. Note that $\rho$ Oph D is also known as L 1696A.
Source	$\alpha_{2000}$	$\delta_{2000}$	$\Delta \alpha,\Delta \delta$ ^a	$\vlsr$ ^b	$n(\hh)$ ^c	$S_{1.2~\rm mm}$	$N(\hh)$ ^d	$\tkin$ ^e	References
			$^{\prime \prime }$		$\dix{5}$		22	K
L 183	15:54:08.80	-02:52:44.0	(0,0)	2.37	20	18.3	7.2	7.0	(1)
L 1544	05:04:16.90	+25:10:47.0	(0,0)	7.20	14	17.2	6.7	7.0	(2)
Oph D	16:28:30.40	-24:18:29.0	(0,0)	3.35	8.5	14.6	5.7	6.0	(3)
L 1517B	04:55:18.80	+30:38:03.8	(-10,-20)	5.87	2.2	7.1	2.8	10.0	(4)
L 310	18:07:11.90	-18:21:35.0	( 30, 80)	6.70	0.9	7.5	2.9	9.0	(5)

Notes. ^(a) Offsets of the continuum peak with respect to the reference position. ^(b) Systemic LSR velocity. ^(c) Peak particle number density. ^(d) Column density computed assuming $\tdust=8$ K and $\kappa_\nu=0.01\rm ~cm^2~g^{-1}$ . The values increase by 25% if $\tdust=7$ K.

^(e) Gas kinetic temperature from the literature.

References. (1) Pagani et al. (2004,2007), (2) Tafalla et al. (2002), Crapsi et al. (2007), (3) Ward-Thompson et al. (1999), Harju et al. (2008) (4) Tafalla et al. (2004) (5) Bacmann et al. (2002).

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