TIMASSS: the IRAS 16293-2422 millimeter and submillimeter spectral survey - I. Observations, calibration, and analysis of the line kinematics

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Table 1

Parameters of the observations at IRAM-30 m and JCMT-15 m telescopes.


Telescope	Frequency	Resolution		Backend¹	rms²	T_sys	HPBW	Beam	σ_cal³	N_cal⁴	P_cal⁵
	(GHz)	(MHz)	(km s^-1)		(mK)	(K)	(arcsec)	efficiency	(%)	lines	(%)


IRAM	80–115.5	0.32	0.81–1.17	VESPA	4–8	90–400	30–21	0.80–0.78	11	28	15
IRAM	129–177	0.32	0.53–0.72	VESPA	5–14	200–1000	19–14	0.76–0.69	17	22	12
IRAM		1.0	1.65–2.25	1 MHz FB					10⁽⁶⁾	84⁽⁶⁾	95⁽⁶⁾
IRAM	197–265	1.0	1.13–1.52	1 MHz FB	7–13	180–1200	12–9	0.65–0.51	17	36	10
IRAM		1.25	1.41–1.90	VESPA
IRAM	265–280	1.25	1.34–1.41	VESPA	9–17	470–4200	9	0.51–0.47
JCMT	328–366	0.625	0.51–0.57	ACSIS	4–9	90–400	14	0.56–0.53	18	26	25

Notes.

⁽¹⁾

In the 2 mm band, each frequency setting is observed twice, i.e. once at each of the two spectral resolutions (0.32 and 1 MHz), while in the 197–265 GHz band, each frequency setting is observed only one time, at a slightly different spectral resolution (1 or 1.25 MHz),

⁽²⁾

rms is given in 1.5 km s^-1 bins,

⁽³⁾

σ_Cal is the calibration uncertainty,

⁽⁴⁾

N_cal is the number of compared lines for calibration purposes,

⁽⁵⁾

P_cal is the percentage of compared spectra for calibration purposes,

⁽⁶⁾

these values refer to the “internal” comparison between VESPA and 1 MHz FB spectra simultaneously observed; the other ones refer to “external” comparisons with published or previously obtained observations.

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