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.3

H₂ column density upper limits toward Sgr B2(N3).

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

85.0	5.3	0.12	<4.4	<1.9
86.5	4.3	0.19	<3.5	<1.9
88.0	9.6	0.12	<7.2	<2.0
90.5	8.3	0.19	<6.6	<2.1
92.0	7.4	0.23	<3.7	<1.7
94.5	7.5	0.23	<	<1.7
96.0	2.7	0.17	<2.0	<2.1
97.0	4.4	0.17	<3.1	<2.1
97.5	2.6	0.17	<1.9	<2.1
98.5	4.3	0.16	<3.0	<2.1
99.0	4.8	0.17	<3.2	<2.1
100.0	5.0	0.16	<3.5	<2.2
101.5	3.7	0.17	<2.4	<2.1
102.5	5.3	0.16	<3.6	<2.2
104.0	5.0	0.20	<2.1	<1.8
106.5	5.0	0.19	<2.1	<1.9
108.0	3.0	0.15	<1.9	<2.3
109.5	2.5	0.14	<1.6	<2.3
111.0	8.2	0.15	<4.7	<2.3
113.5	7.6	0.14	<4.4	<2.3

Notes. As in Table B.1 but for Sgr B2(N3).

^(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(N3)’s position as described in Sect. 3.2.2.

^(c)

The upper limits correspond to 5σ.

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