Evolutionary study of complex organic molecules in high-mass star-forming regions

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Table 2

Spectral windows (first column) observed with the IRAM-30m telescope, with the relative setup used.

Frequency	Receiver	λ₀	Spectrometer	Δν	ΔV_max	HPBW	T_sys
(GHz)		(mm)		(kHz)	(km s⁻¹)	(′′)	(K)
85.3–87.1	E0 (LSB)	3	FTS50	49	0.2	27−29	100−200
85.6–93.4			FTS200	195	0.7
88.6–90.4			FTS50	49	0.2

140.0–141.8	E1 (LSB)	2	FTS50	49	0.1	16−18	100−500
141.1–148.9			FTS200	195	0.4
143.3–145.1			FTS50	49	0.1
151.8–153.6			FTS50	49	0.1

280.9–282.7	E3 (LSB)	0.9	FTS50	49	0.05	9	400−1000
284.2–286.0			FTS50	49	0.05

Notes. In order: EMIR receiver with its wavelength, FTS spectrometer with its frequency and velocity resolutions, HPBW of the beam of the telescope at the observed frequencies, and system temperatures for each waveband.

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