The complexity of Orion: an ALMA view - I. Data and first results

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Volume 604 (August 2017)

A&A, 604 (2017) A32

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Table 1

Frequency bands and beam parameters.

Band	Window	Block^a	Frequency range^b		Beam shape	Pos. angle	Noise^c	Conversion	Noise^c
(#)	(spw)	(sg)	(MHz)	(MHz)	(arcsec)	(degree)	(mJy/beam)	(K/Jy)	(mK)

1	3^d	1	215 149.592	216 086.673	1.8 × 1.1	86	7.0	13.3	93
2	2^d	1	216 342.044	217 279.136	1.8 × 1.1	84	3.7	13.1	48
3	3	2	217 273.522	218 210.619	2.2 × 1.0	102	3.6	11.7	42
4	2	2	218 203.531	219 140.628	2.2 × 1.0	102	4.6	11.6	53
5	3^d	3	219 126.547	220 063.614	1.9 × 1.0	95	4.5	13.3	60
6	2^d	3	219 783.544	220 720.641	1.8 × 1.0	95	5.1	14.0	71
7	1	1	229 756.971	230 694.089	1.4 × 0.8	80	4.0	20.6	82
8	1	2	230 698.921	231 636.062	2.1 × 0.9	102	3.9	12.1	47
9	1	5	232 238.058	233 175.172	1.6 × 1.0	80	3.5	14.1	49
10	0	1–5	233 469.680	234 421.910	1.6 × 0.8	90	2.3	17.5	40
11	1	3	235 083.689	236 020.787	1.7 × 0.9	95	5.1	14.4	73
12	1	4	236 268.702	237 205.799	1.6 × 0.9	87	3.8	15.2	58
13	3	5	244 833.767	245 770.865	1.6 × 0.9	79	4.6	14.1	65
14	2	5	245 772.781	246 709.895	1.6 × 0.9	79	4.6	14.0	64
15	2	4	250 153.833	251 090.932	1.5 × 0.9	88	8.0	14.4	115
16	3	4	251 078.799	252 015.916	1.3 × 0.8	86	8.4	18.6	156

Notes.

^(a)

Observing block: all frequency windows with the same observing block number have been observed simultaneously

^(b)

the frequency range is given for V_LSR=˜ 9 km s^-1.

^(c)

Noise is not corrected for primary beam coupling and is therefore a lower limit to the actual noise in each source. Corrections run from 1% (IRc7) to 41% (MF10).

^(d)

A last minute change of frequency introduced an error in setting the bands creating a hole from 216 087 MHz to 216 342 MHz and an overlap from 219 784 to 220 064 MHz. The reduced ALMA data cubes are available at the CDS.

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