The physical and chemical structure of Sagittarius B2 - II. Continuum millimeter emission of Sgr B2(M) and Sgr B2(N) with ALMA

Á. Sánchez-Monge; P. Schilke; A. Schmiedeke; A. Ginsburg; R. Cesaroni; D. C. Lis; S.-L. Qin; H. S. P. Müller; E. Bergin; C. Comito; Th. Möller

doi:10.1051/0004-6361/201730426

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Volume 604 (August 2017)

A&A, 604 (2017) A6

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Table 3

Dust emission, ionized gas, and molecular properties of the ALMA continuum sources in Sgr B2.

	Dust emission			Ionized gas			Molecular content

	M _{d + g}	n _H₂	N _H₂	n _e	M _i	Ṅ _i	lines	L _lines	L_l/L_{c + l}
ID	(M_⊙)	(10⁸ cm^-3)	(10²⁴ cm^-2)	(cm^-3)	(M_⊙)	(s^-1)	per GHz	(0.1L_⊙)	(%)

Sgr B2(N)

AN01	8668–4083	20.94–9.86	130.9–61.6	4.8 × 10⁴	0.13	1.9 × 10⁴⁸	74.8 (6.9)	92.61	22.1
AN02	623–294	7.77–3.66	48.6–22.9	...	...	...	101.6 (6.8)	11.77	33.7
AN03	470–221	4.83–2.27	30.2–14.2	4.4 × 10⁴	0.013	1.7 × 10⁴⁷	92.0 (4.9)	10.81	37.8
AN04	419–198	3.59–1.69	22.4–10.6	...	...	...	100.3 (7.6)	7.98	33.6
AN05	346–163	2.47–1.16	15.4–7.3	...	...	...	99.2 (24.1)	3.12	19.4
AN06	345–163	2.16–1.02	13.5–6.4	...	...	...	100.9 (29.4)	3.60	22.0
AN07	104–49	2.70–1.27	16.8–7.9	...	...	...	52.2 (24.9)	0.48	11.3
AN08	105–49	1.51–0.71	9.5–4.5	...	...	...	65.8 (23.9)	0.90	19.1
AN09	141–66	0.75–0.35	4.7–2.2	...	...	...	10.4 (8.7)	0.02	0.4
AN10	57–27	0.71–0.34	4.5–2.1	7.7 × 10⁴	0.017	4.1 × 10⁴⁷	73.3 (11.6)	1.39	33.7
AN11	80–38	0.57–0.27	3.6–1.7	...	...	...	8.1 (11.1)	0.01	0.3
AN12	140–66	0.60–0.28	3.8–1.8	...	...	...	32.9 (33.2)	0.07	1.4
AN13	353–166	0.44–0.21	2.8–1.3	...	...	...	48.2 (42.3)	0.36	3.0
AN14	167–79	0.39–0.18	2.4–1.1	...	...	...	18.1 (10.6)	0.11	1.9
AN15	50–23	0.40–0.19	2.5–1.2	...	...	...	10.0 (9.9)	0.01	0.4
AN16	159–75	0.32–0.15	2.0–0.94	...	...	...	24.9 (15.4)	0.14	2.7
AN17	26–12	0.47–0.22	2.9–1.4	...	...	...	60.0 (26.2)	0.36	26.8
AN18	122–57	0.34–0.16	2.1–1.0	...	...	...	22.3 (13.0)	0.11	2.7
AN19	40–19	0.30–0.14	1.8–0.87	...	...	...	17.8 (11.9)	0.02	1.5
AN20	12–6	0.31–0.14	1.9–0.90	5.8 × 10⁴	0.0043	7.6 × 10⁴⁶	10.1 (5.5)	0.01	3.5

Sgr B2(M)

AM01	1544–727	23.59–11.11	147.4–69.4	4.4 × 10⁵	0.072	9.8 × 10⁴⁸	66.2 (32.0)	5.90	7.6
AM02	1731–815	21.92–10.32	137.0–64.5	3.0 × 10⁵	0.064	5.9 × 10⁴⁸	69.5 (37.0)	7.01	8.7
AM03	608–286	6.33–2.98	39.5–18.6	...	...	...	75.7 (22.2)	4.21	15.5
AM04	388–183	5.42–2.55	33.9–15.9	9.4 × 10⁴	0.018	5.2 × 10⁴⁷	29.6 (7.3)	1.48	8.8
AM05	406–191	5.87–2.77	36.7–17.3	...	...	...	75.7 (38.9)	2.60	14.6
AM06	318–150	4.60–2.17	28.8–13.5	...	...	...	40.5 (9.1)	2.28	16.0
AM07	268–126	4.92–2.32	30.8–14.5	5.2 × 10⁴	0.0065	1.1 × 10⁴⁷	44.1 (8.4)	1.41	12.1
AM08	99–46	4.15–1.96	26.0–12.2	3.0 × 10⁵	0.011	1.0 × 10⁴⁸	20.7 (10.0)	0.47	8.5
AM09	232–109	3.35–1.58	20.9–9.9	...	...	...	40.4 (10.3)	1.29	13.1
AM10	340–160	1.46–0.69	9.2–4.3	...	...	...	35.3 (8.5)	1.32	9.5
AM11	178–84	2.58–1.21	16.1–7.6	...	...	...	5.6 (5.3)	0.05	0.7
AM12	185–87	1.44–0.68	9.0–4.2	...	...	...	15.6 (8.8)	0.62	8.5
AM13	186–88	1.12–0.53	7.0–3.3	...	...	...	26.2 (10.5)	0.55	7.5
AM14	101–48	1.30–0.61	8.1–3.8	...	...	...	19.4 (7.9)	0.73	16.1
AM15	11–5	0.18–0.08	1.1–0.52	1.6 × 10⁵	0.023	1.1 × 10⁴⁸	10.5 (6.9)	0.18	8.9
AM16	83–39	0.28–0.13	1.7–0.82	6.6 × 10⁴	0.10	2.1 × 10⁴⁸	2.9 (2.9)	0.06	1.1
AM17	95–45	0.31–0.15	1.9–0.91	4.0 × 10⁴	0.067	8.2 × 10⁴⁷	5.4 (4.6)	0.04	1.0
AM18	46–21	0.45–0.21	2.8–1.3	...	...	...	3.3 (3.4)	0.01	0.9
AM19	62–29	0.39–0.19	2.5–1.2	...	...	...	3.0 (4.0)	0.02	0.8
AM20	54–26	0.28–0.13	1.7–0.81	...	...	...	3.5 (2.9)	0.02	1.1
AM21	22–10	0.32–0.15	2.0–0.93	...	...	...	1.9 (2.0)	0.01	0.2
AM22	25–12	0.30–0.14	1.9–0.88	...	...	...	3.7 (3.1)	0.01	0.9
AM23	48–22	0.23–0.11	1.5–0.69	...	...	...	3.4 (4.1)	0.02	1.3
AM24	...	...	...	1.9 × 10⁵	0.0083	4.8 × 10⁴⁷	6.1 (3.6)	0.03	6.2
AM25	18–9	0.25–0.12	1.6–0.75	...	...	...	1.4 (1.6)	0.01	0.8
AM26	39–18	0.22–0.10	1.4–0.65	...	...	...	6.5 (4.0)	0.08	6.4
AM27	16–8	0.22–0.10	1.3–0.63	...	...	...	2.7 (2.5)	0.01	0.9

Notes. The symbol “...” denotes if a source is not associated with VLA 40 GHz emission and therefore the physical parameters of an Hii region cannot be derived. For source AM24 in Sgr B2(M), all the ALMA continuum flux at 242 GHz results seems to be originated by ionized gas, the physical parameters of the dust content cannot be derived.

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