The physical and chemical structure of Sagittarius B2 - I. Three-dimensional thermal dust and free-free continuum modeling on 100 au to 45 pc scales

A. Schmiedeke; P. Schilke; Th. Möller; Á. Sánchez-Monge; E. Bergin; C. Comito; T. Csengeri; D. C. Lis; S. Molinari; S.-L. Qin; R. Rolffs

doi:10.1051/0004-6361/201527311

Free Access

Table B.2

Small scale structure: dust density components in Sgr B2.

ID ¹	Model ²	RA ³	Dec ⁴	dz⁵	r₀ ⁶	n_c ⁷	η ⁸	Star ⁹
		[h:m:s, J2000]	[d:m:s, J2000]	[10⁵ au]	[10³ au]	[10⁷ H₂ cm^-3]

M-SMA-1a	ABCD	17:47:20.197	−28:23:04.36	1.0	20	3.0	5.0	B0
M-SMA-1b	ABCD	17:47:20.170	−28:23:04.60	1.0	35	3.1	5.0	B0.5
M-SMA-1c	ABCD	17:47:20.158	−28:23:05.08	1.0	10	3.6	5.0	B0.5
M-SMA-1d	ABCD	17:47:20.148	−28:23:05.48	1.0	20	3.6	5.0	B0.5
M-SMA-2a	ABCD	17:47:20.152	−28:23:04.18	0.0	19	3.2	5.0	B0.5
M-SMA-2b	ABCD	17:47:20.124	−28:23:04.45	0.0	14	3.3	5.0	B0.5
M-SMA-3	ABCD	17:47:20.100	−28:23:04.04	0.0	14	2.8	5.0	B0.5
M-SMA-4	ABCD	17:47:20.152	−28:23:03.30	0.0	7	3.4	5.0	none
M-SMA-5	ABCD	17:47:20.212	−28:23:04.90	0.0	7	3.2	5.0	B0.5
M-SMA-6	ABCD	17:47:20.175	−28:23:06.08	0.0	35	3.0	5.0	none
M-SMA-7	ABCD	17:47:20.118	−28:23:06.35	0.0	30	2.9	5.0	B0.5
M-SMA-8	ABCD	17:47:20.215	−28:23:06.43	0.0	4	3.6	5.0	none
M-SMA-9	ABCD	17:47:20.250	−28:23:07.10	0.0	9	2.8	5.0	B0.5
M-SMA-10	ABCD	17:47:20.005	−28:23:05.79	0.0	15	3.3	5.0	none
M-SMA-11	ABCD	17:47:20.108	−28:23:03.10	1.0	20	3.2	5.0	B0.5
M-SMA-12	ABCD	17:47:20.136	−28:23:02.24	1.0	50	3.8	5.0	B0
N-SMA-1a	A	17:47:19.912	−28:22:18.25	−5.0	45	9.0	5.0	none
	BCD			−6.95	45	9.0	5.0	none
N-SMA-1b	A	17:47:19.900	−28:22:19.51	−2.0	75	4.0	5.0	none
	BCD			−6.98	75	4.0	5.0	none
N-SMA-2a	A	17:47:19.944	−28:22:13.64	−3.0	10	6.9	5.0	B0.5
	BCD			−6.97	10	6.9	5.0	B0.5
N-SMA-2b	A	17:47:19.880	−28:22:13.80	−30	10	6.8	5.0	B0.5
	BCD			−6.97	10	6.8	5.0	B0.5

Notes.

⁽¹⁾

ID is the identifier used in the model. These identifiers are identical to the ones introduced by Qin et al. (2011). Note: some of these objects identified by Qin et al. (2011) show an elongated intensity structure. We recover these objects with a superposition of several spherical symmetric clumps. We distinguish these components by adding additional lowercase letters to the identifier introduced by Qin et al. (2011).

⁽²⁾

Model refers to one of the four model described in this paper.

⁽³⁾

RA is the right ascension of the density component given in units of hours:minutes:seconds in the equatorial coordinate system.

⁽⁴⁾

Dec is the declination of the density component given in units of degrees:arcminutes:arcseconds in the equatorial coordinate system.

⁽⁵⁾

dz is the displacement along the line of sight with respect to the model center. The z-axis is oriented such that it points towards the observer.

⁽⁶⁾

r₀ is the radius defining the component, as described in Eq. (4).

⁽⁷⁾

n_c is the central density.

⁽⁸⁾

η is the exponent of the dust density profile.

⁽⁹⁾

This column indicates whether an additional heating source had to be included inside the dust component. If this is the case, the spectral type of the star is given.

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