Sequential star formation in IRAS 06084-0611 (GGD 12-15) - From intermediate-mass to high-mass stars

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Table 2

Properties of objects located in the SINFONI field of view.


	(J2000)		Available photometric data				Objects properties							cluster
Object #	RA (h m s)	Dec (° ′ ″)	SOFI	2MASS	IRAC	Radio	Sp. Type^a	Lum^a	IR_ex^b	class^c	T_eff^d	A_V^e	R_⊙^f	member

VLA1	6 10 50.50	−6 11 51.4	...	...	1243	VLA1	HII region^†	...	+	...	...	...	...	+
1	6 10 50.40	−6 11 19.3	JK	JHK	1234	...	early-B	V	+	II	27700 ± 5000	21.0 ± 0.16	5.0 ± 0.29	+
2	6 10 50.31	−6 11 57.6	JK	...	1234	VLA 4	Herbig Be^††	...	+	0 / I	...	...	...	+
3	6 10 49.81	−6 11 45.0	JK	JHK	1234	...	G0 - G3	V	+	0 / I	5950 ± 500	10.9 ± 0.17	4.2 ± 0.25	+
4	6 10 49.45	−6 11 42.0	K	HK	1234	VLA 2	...	...	+	0 / I	...	...	...	+
5	6 10 50.50	−6 12 04.4	JK	JK	1	...	K1 - K2	IV	...	...	5000 ± 350	4.7 ± 0.52	3.4 ± 0.21	...
6	6 10 50.68	−6 11 55.1	JK	JK	1	...	K2	IV	+	...	4900 ± 350	12.9 ± 0.25	3.7 ± 0.27	+
7	6 10 49.21	−6 11 30.2	JK	JHK	12	VLA 8	K1	IV	no	...	5100 ± 350	8.2 ± 0.45	2.3 ± 0.14	+
8	6 10 52.52	−6 11 35.0	JK	K	1	...	K0 - K2	IV	+	...	5100 ± 350	12.5 ± 0.80	2.9 ± 0.18	+
9	6 10 48.63	−6 12 00.4	JK	JHK	1234	...	G8 - K0	IV	+	II	5400 ± 350	13.6 ± 0.74	3.0 ± 0.18	+
10	6 10 49.65	−6 11 22.1	JK	K	1	...	K1	IV	...	...	5100 ± 350	7.5 ± 0.45	2.1 ± 0.12	...
11	6 10 50.82	−6 11 39.6	K	HK	123	...	...	...	+	...	...	...	...	+
12	6 10 50.61	−6 11 35.0	K	HK	123	...	...	...	+	...	...	...	...	+
13	6 10 48.18	−6 11 25.7	JK	JHK	1234	...	K1	V	+	II	5100 ± 350	8.3 ± 0.20	1.9 ± 0.11	+
14	6 10 50.39	−6 11 55.3	JK	...	...	...	M4	V	...	...	3350 ± 350	4.9 ± 0.42	2.4 ± 0.15	no
15	6 10 47.74	−6 12 00.9	JK	HK	1234	...	K5	IV	+	II	4350 ± 250	13.7 ± 0.61	2.3 ± 0.13	+
16	6 10 50.28	−6 12 05.6	JK	...	...	...	K5	IV	...	...	4350 ± 250	7.8 ± 0.61	2.3 ± 0.13	...
17	6 10 48.82	−6 11 43.8	JK	JHK	1234	...	K1	IV	+	II	5100 ± 250	7.8 ± 0.45	1.4 ± 0.08	+
18	6 10 48.78	−6 11 32.6	K	K	1234	...	...	...	+	0 / I	...	...	...	+
19	6 10 49.64	−6 11 15.3	JK	JHK	1	...	K1	IV	...	...	5100 ± 350	6.2 ± 0.45	1.2 ± 0.07	+
20	6 10 50.12	−6 11 59.0	JK	...	...	...	...	...	...	...	...	...	...	+
21	6 10 50.76	−6 11 44.9	K	HK	123	...	K3 - K4	IV	+	...	4650 ± 350	23.9 ± 0.24	2.1 ± 0.13	+
22	6 10 49.44	−6 11 20.6	K	K	1234	...	...	...	+	0 / I	...	...	...	+
23	6 10 51.49	−6 11 35.0	K	HK	123	...	...	...	+	...	...	...	...	+
24	6 10 48.02	−6 11 42.8	JK	HK	123	...	...	...	+	...	...	...	...	+
25	6 10 50.16	−6 11 55.0	JK	...	...	...	...	...	...	...	...	...	...	+
26	6 10 48.15	−6 11 06.6	JK	JHK	12	...	...	...	...	...	...	...	...	...
27	6 10 52.01	−6 12 12.3	JK	HK	12	...	...	...	...	...	...	...	...	...
28	6 10 51.10	−6 11 25.3	K	HK	12	...	...	...	...	...	...	...	...	...
29	6 10 51.64	−6 12 07.8	K	K	1234	...	...	...	+	0 / I	...	...	...	+
30	6 10 52.35	−6 11 32.1	K	K	123	VLA 7	...	...	+	...	...	...	...	+
31	6 10 48.43	−6 12 03.9	K	HK	124	...	...	...	...	...	...	...	...	+
32	6 10 51.55	−6 11 26.4	K	K	123	...	...	...	+	...	...	...	...	...
33	6 10 50.75	−6 11 42.0	K	...	4	VLA 6	...	...	...	...	...	...	...	+
34	6 10 52.23	−6 11 25.2	JK	...	...	...	...	...	...	...	...	...	...	...
35	6 10 50.54	−6 11 19.0	K	...	...	...	...	...	...	...	...	...	...	...
36	6 10 50.98	−6 11 38.3	K	...	...	...	...	...	...	...	...	...	...	...
37	6 10 47.90	−6 11 47.9	K	...	123	...	...	...	+	...	...	...	...	+
38	6 10 49.31	−6 11 46.3	K	...	...	...	...	...	...	...	...	...	...	...
39	6 10 51.80	−6 11 16.3	K	...	1234	...	...	...	+	0 / I	...	...	...	+

Notes.

^(a)

Based on spectral comparison with reference spectra from Rayner et al. (2009).

^(b)

IR excess based on 2MASS, SOFI and IRAC photometry compared to Kurucz models (Kurucz 1993) and IRAC color criteria as described in Sect. 3.3.

^(c)

Evolutionary class (Lada 1987) derived from the IRAC colors as defined by Megeath et al. (2004).

^(d)

Temperature from Kenyon & Hartmann (1995), averaged between the spectral type range.

^(e)

A_V derived using intrinsic colors of Koornneef (1983).

^(f)

Result of fitting with Kurucz (Kurucz 1993) model. A distance of 830 ± 50 pc is assumed (Herbst & Racine 1976).

^†

Based on radio continuum flux Gómez et al. (2002) estimate the ionizing object to be of spectral type B0.5.

^††

Based on the infrared luminosity Persi & Tapia (2003) estimate the presence of a very young star somewhat later than B3.

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