Physical and chemical modeling of the starless core L 1512

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Table 1

Observational parameters.

Species	Transition	Frequency^(a)	δv	Beam Size^(b)	η_MB	T_sys^(c)	rms noise
		(MHz)	(m s⁻¹)	(′′)		(K)	(mK)
IRAM 30-m (Dec. 2013, May 2014, Oct. 2014, Sep. 2017)

N₂H⁺	1–0	93 173.764	31	26	0.85	90–160	32–71
DCO⁺	2–1	144 077.282	41	17	0.80	80–300	28–102
N₂D⁺	2–1	154 217.181	38	16	0.78	90–600	18–33
DCO⁺	3–2	216 112.582	68	11	0.66	360–460	53–94
C¹⁸O	2–1	219 560.358	67	11	0.65	340–400	50–89
N₂H⁺	3–2	279 511.832	42	9	0.56	190–400	29–51

GBT 100-m (Nov. 2014)

DCO⁺	1–0	72 039.303	48	11	0.50	140–160	40–90
N₂D⁺	1–0	77 109.616	44	10	0.50	105–130	29–44

JCMT 15-m (Dec. 2015)

H₂D⁺	1₁₀–1₁₁	372 421.356	49	13	0.70	690	19–71
N₂H⁺	4–3	372 672.526	49	13	0.70	725	26–50

Notes. ^(a) N₂H⁺ and N₂ D⁺ frequencies are taken from Pagani et al. (2009b). The frequencies correspond to the strongest hyperfine component for each transition. ^(b) The beam size is the HPBW. ^(c) T_sys is expressed in the scale (Kutner & Ulich 1981).

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