The HH30 edge-on T Tauri star - A rotating and precessing monopolar outflow scrutinized by ALMA

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Table 1.

Observational set-up of the ALMA-cycle 2 data set.

Spectral window	¹²CO(2–1)	¹³CO(2–1)	Continuum
			1.28 mm	1.38 mm	1.33 mm^a
Frequency	230.538 GHz	220.398 GHz	234.006 GHz^b	217.040 GHz^b	225.204 GHz^b
Bandwidth	117 MHz	117 MHz	2 GHz	2 GHz	4 GHz
Native channel width	122 kHz	122 kHz	15.6 MHz	15.6 MHz	–
Primary beam	25.3″	26.4″	24.9″	24.9″	–
Synthesized beam	0″̣24 × 0″̣19	0″̣25 × 0″̣20	0″̣25 × 0″̣18	0″̣28 × 0″̣19	0″̣26 × 0″̣18
Beam PA	26.8^∘	31.2^∘	27.2^∘	31.2^∘	29.7^∘

Rms noise level^c	2.0 mJy beam⁻¹	2.3 mJy beam⁻¹	30.96 μJy beam⁻¹	29.15 μJy beam⁻¹	21.74 μJy beam⁻¹
Flux^d	15.4 Jy km s⁻¹	0.88 Jy km s⁻¹	24.53 mJy	20.85 mJy	22.30 mJy

Notes.

^(a)

The continuum at 1.33 mm results from the merging of the 1.28 mm and 1.38 mm continuum bands.

^(b)

The mean frequency was calculated assuming a S(ν) ∝ ν^−2.2 emission spectra accurately describes the interstellar medium spectral energy distribution slope in frequency range considered.

^(c)

The noise level of the CO transition lines are given per channel, and the channels have a width of 0.3 km s⁻¹.

^(d)

The continuum and ¹²CO(2–1) fluxes are integrated within the area given by the 5σ level. The ¹³CO(2–1) flux is integrated within the area given by the 3σ level.

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