Tracing early evolutionary stages of high-mass star formation with molecular lines

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Volume 522 (November 2010)

A&A, 522 (2010) A40

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Table 2

Molecular lines observed.

Species	Transition	Frequency	E_up	HPBW	η_mb	Receiver	δυ^a	T_sys
	J_{K _p, K_o}	(GHz)	(K)	(″)			(m·s^-1)	(K)

HDO	1_1,0 → 1_0,1	80.5783	47	31	0.79	A100	74	140–190
	3_1,2 → 2_2,1	225.8967	168	11	0.54	B230	53	750–1600
HO	3_1,3 → 2_2,0	203.4075	204	12	0.57	A230	59	600–1300
SO₂	12_0,12 → 11_1,11	203.3916	70	12	0.57	A230	59	600–1300
CH₃OH	5_−1,5 → 4_0,4E	84.5212	40	29	0.78	B100	71	140–190

Notes. Columns 2–9 indicate energy level transitions, line emission rest frequencies, half power beam width (HPBW), main beam efficiency η_mb, receiver name, velocity resolution δυ, and system temperature T_sys.

^(a)

Values for the VESPA backend.

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