Probing the CO and methanol snow lines in young protostars - Results from the CALYPSO IRAM-PdBI survey

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Volume 591 (July 2016)

A&A, 591 (2016) A3

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Table 2

Synthesized beam sizes and rms noise per channel in the final datacubes for the observed lines and sources.

Source	Line	Synthesized half-power beam width^a	Δν	Noise per channel^b
		major × minor (Pos. Ang.)	(km s^-1)	(mJy/beam)

IRAS4A	C¹⁸O (2–1)	1.05′′× 0.79′′ (199°)	0.10	21.9
	e-CH₃OH (5₁–4₂)	1.10′′× 0.82′′ (201°)	0.20	16.6
	N₂H⁺ (1–0)	1.80′′× 1.32′′ (38°)	0.15	5.8
L1448C	C¹⁸O (2–1)	1.01′′× 0.73′′ (24°)	0.10	18.9
	e-CH₃OH (5₁–4₂)	1.05′′× 0.74′′ (26°)	0.20	13.8
	N₂H⁺ (1–0)	1.75′′× 1.40′′ (64°)	0.15	5.5
L1157	C¹⁸O (2–1)	0.84′′× 0.76′′ (–178°)	0.10	23.5
	e-CH₃OH (5₁–4₂)	0.87′′× 0.77′′ (4°)	0.20	17.7
	N₂H⁺ (1–0)	1.49′′× 1.10′′ (59°)	0.15	6.2
IRAS4B	C¹⁸O (2–1)	1.05′′× 0.81′′ (–160°)	0.10	21.9
	e-CH₃OH (5₁–4₂)	1.10′′× 0.84′′ (–161°)	0.20	16.6
	N₂H⁺ (1–0)	1.77′′× 1.28′′ (38°)	0.15	5.8

Notes.

^(a)

The imaging was performed with natural weighting.

^(b)

The reported value corresponds to the median noise level of all channel maps of the cube, the noise level in each channel being derived from a Gaussian fit to the distribution of intensities within the map of this channel.

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