ALMA-IMF - VII. First release of the full spectral line cubes: Core kinematics traced by DCN J = (3−2)

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Volume 678 (October 2023)

A&A, 678 (2023) A194

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Table 3.

Example of the DCN fits towards the first 15 cores of the young protocluster G338.93.

n⁽¹⁾	Core ⁽¹⁾	RA ⁽¹⁾	Dec ⁽¹⁾	F_A⁽¹⁾	F_B⁽¹⁾	PA ⁽¹⁾	T	V_LSR⁽²⁾	Linewidth ⁽²⁾	Spectral ⁽³⁾
	name	[ICRS]	[ICRS]	[″]	[″]	[deg]	[K]	[km s⁻¹]	[km s⁻¹]	type
1	250.1422011-45.6934028	16:40:34.13	−45:41:36.25	0.89	0.79	84	100 ± 50	−57.34 ± 0.08	–	Complex
2	250.1427268-45.6936217	16:40:34.25	−45:41:37.04	0.97	0.73	124	100 ± 50	−58.71 ± 0.08	–	Complex
3	250.1417044-45.7020244	16:40:34.01	−45:42:7.290	0.86	0.79	92	100 ± 50	−62.49 ± 0.03	–	Complex
4	250.1397543-45.6936984	16:40:33.54	−45:41:37.31	0.86	0.82	7	100 ± 50	−60.37 ± 0.04	–	Complex
5	250.1417392-45.7025004	16:40:34.02	−45:42:9.000	0.86	0.79	89	36 ± 7	−64.94 ± 0.02	2.19 ± 0.07	Single
6	250.1419183-45.7022799	16:40:34.06	−45:42:8.210	1.0	0.86	65	35 ± 10	−64.36 ± 0.01	2.98 ± 0.12	Single
7	250.1378537-45.7040233	16:40:33.08	−45:42:14.48	0.81	0.76	56	30 ± 6	–	–	–
8	250.1433977-45.6938542	16:40:34.42	−45:41:37.88	1.42	0.88	119	27 ± 6	−58.93 ± 0.03	1.81 ± 0.12	Single
9	250.1497218-45.6929092	16:40:35.93	−45:41:34.47	0.98	0.74	29	24 ± 5	–	–	–
10	250.1403862-45.7027264	16:40:33.69	−45:42:9.820	1.02	0.88	63	100 ± 50	−63.32 ± 0.07	–	Complex
11	250.1409277-45.6954519	16:40:33.82	−45:41:43.63	0.87	0.74	15	27 ± 6	−59.8 ± 0.05	0.95 ± 0.2	Single
12	250.1444989-45.69665	16:40:34.68	−45:41:47.94	1.99	1.75	16	24 ± 5	–	–	–
13	250.1423231-45.6931039	16:40:34.16	−45:41:35.17	1.06	1.04	129	29 ± 6	−57.29 ± 0.02	2.12 ± 0.09	Single
14	250.1394346-45.6928199	16:40:33.46	−45:41:34.15	0.87	0.7	72	28 ± 6	−59.26 ± 0.06	1.69 ± 0.17	Single
15	250.1461922-45.6894135	16:40:35.09	−45:41:21.89	1.68	1.26	124	24 ± 5	–	–	–

Notes.

⁽¹⁾

The core numbering (n), core name, RA, Dec, position angle (PA), core major (F_A) and core minor (F_B) FWHM and dust temperatures (T) are taken from the smoothed core catalogues in Louvet et al. (2023), where the dust temperatures are those assumed for the core mass estimates presented in this work.

⁽²⁾

The V_LSR and linewidth are taken from the HFS fits. For reference, we include the V_LSR for the complex-type spectra, however, as the spectra are complex, often containing multiple components, we do not use them in the analysis or provide the linewidths.

⁽³⁾

Dashes are given for those cores with no DCN (3–2) detection.

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