Deuteration and evolution in the massive star formation process - The role of surface chemistry

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Volume 575 (March 2015)

A&A, 575 (2015) A87

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Table 2

Observed transitions and technical parameters.

Molecular line	Line rest frequency	HPBW	Δv	T _sys	η _MB
	(GHz)	(′′)	(km s^-1)	(K)


IRAM-30 m Telescope
ortho-NH₂D(1_1,1−1_0,1)	85.9263	~28	0.136	~85–120	0.85
para-NH₂D(1_1,1−1_0,1)	110.1536	~22	0.106	~95–125	0.83
CH₃OH(3 mm-band)	89.11–96.89^a	27^b	~0.62^c	~100–120	0.84
CH₃OH(1 mm-band)	216.0–223.78^a	11^b	~0.26^c	~200–300	0.66


Green Bank Telescope
NH₃(1,1)	23.6945	~32	~ 0.15	~50–100	~ 0.81
NH₃(2,2)	23.7226	~32	~ 0.15	~50–100	~ 0.81

Notes.

^(a)

Total spectral window covered by the FTS correlator. Please see Tables B.1 and B.2 to see the transitions detected in it.

^(b)

Telescope HPBW at the central frequency of the spectral window.

^(c)

Maximum spectral resolution obtained with FTS.

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