Dynamic star formation in the massive DR21 filament

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Volume 520 (September-October 2010)

A&A, 520 (2010) A49

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Table 1:

Observing parameters of the molecular line data obtained with the FCRAO and IRAM 30 m telescope.
	$\nu$	HPBW	$\eta_{\rm mb}$	$T_{\rm sys}$	$\Delta v_{\rm res}$	$\Delta T_{\rm rms}$
	[GHz]			[K]	[km s^-1]	[K]
FCRAO
¹³CO $1\to 0$	110.2	45''	0.48	210	0.067	0.48
CS $2\to 1$	98.0	48''	0.48	200	0.075	0.38
N₂H⁺ $1\to 0$	93.2	48''	0.48	200	0.079	0.38
IRAM
¹²CO $2\to 1$	230.8	11''	0.52	601	0.05	0.8
H₂CO 3(1,2)-2(1,1)	225.7	11''	0.55	549	0.05	0.65
¹³CO $2\to 1$	220.4	11''	0.57	580	0.03	0.9
C³⁴S $2\to 1$	96.4	26''	0.77	210	0.025	0.5
N₂H⁺ $1\to 0$	93.2	26''	0.77	158	0.03	0.1
HCO⁺ $1\to 0$	89.2	28''	0.77	138	0.05	0.2
H¹³CO⁺ $1\to 0$	86.8	29''	0.78	114	0.025	0.25

Notes. Column one and two indicate the molecular transition and frequency, followed by the half power beam width (HPBW) in arcsec, $\eta_{\rm mb}$ is the main beam efficiency, $T_{\rm sys}$ the system temperature, $\Delta v_{\rm res}$ denotes the velocity resolution, and $\Delta T_{\rm rms}$ the average rms noise temperature per channel on a $T_{\rm mb}$ scale.

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