Spokes cluster: The search for the quiescent gas | Astronomy & Astrophysics (A&A)

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Volume 555 (July 2013)

A&A, 555 (2013) A106

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Table 1

List of observed sources.

				On-source time
Source	RA	Dec	σ _v ^a	N₂H⁺ (3–2)	N₂D⁺ (3–2)	# YSOs
	(hh:mm:ss)	(dd:mm:ss)	(km s^-1)	(min)	(min)	within APEX beams^b

MM01	06:41:05.8	+09:34:06	0.59	4.0	23.0	1 (7)^c
MM02	06:41:06.3	+09:35:56	0.51	2.3	28.0	1
MM03	06:41:04.2	+09:35:01	0.26	3.3	24.0	1
MM04	06:41:00.3	+09:35:26	0.81	3.3	...	0 (1)^d
MM05	06:40:49.4	+09:34:29	0.42	13.4	24.0	0 (1)^d
MM06	06:40:57.9	+09:36:24	0.55	3.3	...	0 (1)^d
MM07	06:41:11.6	+09:35:32	0.59	3.3	17.0	1
MM08	06:41:02.9	+09:34:31	0.34	3.3	31.0	0
MM09	06:41:07.0	+09:33:31	0.55	3.3	...	1
MM10	06:41:07.7	+09:34:18	0.72	3.3	...	1
MM11	06:40:47.9	+09:34:42	0.30	13.7	33.0	0
MM12	06:40:51.2	+09:35:24	0.38	8.0	79.0	0 (1)^d
MM13	06:41:08.5	+09:35:43	0.89	6.3	...	1
MM15	06:41:04.6	+09:36:19	0.64	13.7	...	2

Notes.

^(a)

Velocity dispersion from Peretto et al. (2006) derived using N₂H⁺ (1–0) fits.

^(b)

Number of protostars located within the APEX HPBW (see Table 2) (Peretto et al. 2006, and references therein), (Teixeira et al. 2006).

^(c)

Targeted SMA observations of this core revealed additional compact millimeter sources undetected in the infrared (Teixeira et al. 2007).

^(d)

The value in parenthesis corresponds to the number of faint 24 μm sources that have no other wavelength counterpart (and therefore we cannot confirm their protostellar nature).

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