Exploring molecular complexity with ALMA (EMoCA): Detection of three new hot cores in Sagittarius B2(N)

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Volume 604 (August 2017)

A&A, 604 (2017) A60

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Table B.4

Peak flux densities and H₂ column densities toward Sgr B2(N4).

Freq		rms^ALMA^a	rms^SMA^b	^c	^d
(GHz)	(mJy/beam)		(Jy/beam)	(10²³ cm^-2)

85.0	_	5.3	0.53	<4.38	<5.21
86.5	21.82(60)	4.3	0.51	3.43(9)	<5.26
88.0	_	9.6	0.53	<7.28	<5.28
90.5	_	8.3	0.48	<6.56	<5.41
92.0	_	7.4	0.64	<3.70	<4.79
94.5	_	7.5	0.63	<3.49	<4.82
96.0	35.90(12)	2.7	0.44	4.94(2)	<5.45
97.0	33.06(50)	4.4	0.43	4.43(7)	<5.47
97.5	33.77(50)	2.6	0.42	4.62(7)	<5.50
98.5	28.88(76)	4.3	0.42	3.85(10)	<5.52
99.0	31.10(76)	4.8	0.44	3.90(10)	<5.48
100.0	33.53(64)	5.0	0.41	4.44(8)	<5.62
101.5	34.03(64)	3.7	0.42	4.11(8)	<5.54
102.5	36.90(103)	5.3	0.40	4.67(13)	<5.65
104.0	29.66(104)	5.0	0.54	2.38(8)	<5.03
106.5	38.82(105)	5.0	0.51	3.04(8)	<5.08
108.0	41.37(66)	3.0	0.36	4.96(8)	<5.71
109.5	42.23(13)	2.5	0.35	5.09(2)	<5.77
111.0	44.44(54)	8.2	0.37	4.71(6)	<5.70
113.5	_	7.6	0.35	<4.36	<5.78

Notes. As in Table B.1 but for Sgr B2(N4).

^(a)

Noise level measured in the ALMA continuum map with GO NOISE.

^(b)

Noise level measured in the SMA map inside a polygon defined around Sgr B2(N4)’s position as described in Sect. 3.2.2.

^(c)

Where Sgr B2(N4) is not detected in the ALMA maps, an upper limit to its H₂ column density has been calculated at the 5σ level.

^(d)

The upper limits correspond to 5σ.

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