2011A&A...527A..32W


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.13CEST05:54:55

2011A&A...527A..32W - Astronomy and Astrophysics, volume 527A, 32-32 (2011/3-1)

Different evolutionary stages in the massive star-forming region S255 complex.

WANG Y., BEUTHER H., BIK A., VASYUNINA T., JIANG Z., PUGA E., LINZ H., RODON J.A., HENNING T. and TAMURA M.

Abstract (from CDS):

Massive stars form in clusters, and they are often found in different evolutionary stages located close to each other. To understand evolutionary and environmental effects during the formation of high-mass stars, we observed three regions of massive star formation at different evolutionary stages, and all are found that in the same natal molecular cloud. The three regions, S255IR, S255N, and S255S, were observed at 1.3 mm with the submillimeter array (SMA), and follow-up short spacing information was obtained with the IRAM 30m telescope. Near infrared (NIR) H+K-band spectra and continuum observations were taken for S255IR with VLT-SINFONI to study the different stellar populations in this region. This combination of millimeter (mm) and near infrared data allow us to characterize different stellar populations within the young forming cluster in detail. While we find multiple mm continuum sources toward all regions, their outflow, disk, and chemical properties vary considerably. The most evolved source S255IR exhibits a collimated bipolar outflow visible in CO and H2 emission, and the outflows from the youngest region S255S are still small and fairly confined in the regions of the mm continuum peaks. Also the chemistry toward S255IR is the most evolved, exhibiting strong emission from complex molecules, while much fewer molecular lines are detected in S255N, and in S255S we detect only CO isotopologues and SO lines. Also, rotational structures are found toward S255N and S255IR. Furthermore, a comparison of the NIR SINFONI and mm data from S255IR clearly reveal two different (proto) stellar populations with an estimated age difference of approximately 1Myr. A multiwavelength spectroscopy and mapping study reveals different evolutionary phases of the star formation regions. We propose the triggered outside-in collapse star formation scenario for the bigger picture and the fragmentation scenario for S255IR.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: jets and outflows - ISM: molecules - stars: early-type - diagrams Hertzsprung-Russell - ISM: individual objects: S255

Nomenclature: Table 1: [WBB2011] S255IR-SMAN (Nos SMA1-SMA3), [WBB2011] S255N-SMAN (Nos SMA1-SMA3), [WBB2011] S255S-SMAN (Nos SMA1-SMA2). Fig. 24, Table 11: [WBB2011] NN (Nos 1-18).

Simbad objects: 44

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Number of rows : 44

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 1336 GiG 03 26 32.199 -35 42 48.86   13.12   11.95   ~ 106 0
2 QSO J0530+13 QSO 05 30 56.41672 +13 31 55.1495     20.0 19.35   ~ 879 1
3 SH 2-257 HII 06 12 44 +17 59.3           ~ 121 1
4 [MBH2005] G192.60-0.05 MM 1 Cld 06 12 52.9 +18 00 27           ~ 7 0
5 [WBB2011] S255N-SMA2 smm 06 12 52.95 +18 00 31.7           ~ 8 0
6 GAL 192.58-00.04 HII 06 12 53 +18 00.4           ~ 23 0
7 2MASS J06125318+1759058 pr* 06 12 53.182 +17 59 05.86           G8/K0 3 0
8 [WBB2011] 16 * 06 12 53.290 +17 59 21.70           K0 1 0
9 SH 2-255 N HII 06 12 53.3 +18 00 42           ~ 25 0
10 [MBH2005] G192.60-0.05 MM 2 Cld 06 12 53.4 +17 59 23           ~ 5 0
11 [WBB2011] 5 * 06 12 53.600 +17 59 28.18           K4 1 0
12 [WBB2011] S255N-SMA3 smm 06 12 53.65 +18 00 18.3           ~ 5 0
13 [WBB2011] S255N-SMA1 smm 06 12 53.71 +18 00 27.3           ~ 6 0
14 [WBB2011] S255IR-SMA2 mm 06 12 53.77 +17 59 26.1           ~ 8 0
15 NAME S255-2 IR 06 12 53.8 +17 59 22           ~ 38 0
16 2MASS J06125385+1759242 X 06 12 53.85 +17 59 24.2           ~ 11 0
17 [WBB2011] S255IR-SMA3 mm 06 12 53.88 +17 59 23.7           ~ 5 0
18 NAME SH 2-255 IRS 1 Y*O 06 12 54.0060 +17 59 22.958           ~ 317 0
19 [WBB2011] 8 * 06 12 54.130 +17 59 29.18           K2 1 0
20 [WBB2011] 18 * 06 12 54.150 +17 59 34.19           ~ 1 0
21 [WBB2011] 17 * 06 12 54.180 +17 59 47.58           ~ 1 0
22 2MASS J06125445+1759365 * 06 12 54.454 +17 59 36.57           K3 2 0
23 2MASS J06125452+1759029 pr* 06 12 54.524 +17 59 02.90           K1 2 0
24 2MASS J06125458+1759173 pr* 06 12 54.587 +17 59 17.33           K3 2 0
25 [WBB2011] 3 * 06 12 54.680 +17 59 32.82           B8-A3 1 0
26 [WBB2011] 4 * 06 12 54.8164338776 +17 59 12.889594614           M1.5 2 0
27 [WBB2011] 14 pr* 06 12 54.900 +17 59 40.96           G8/K0 1 0
28 [WBB2011] 1 * 06 12 54.9138830270 +17 59 20.907744608           B3-B7 2 0
29 [WBB2011] 2 * 06 12 55.060 +17 59 28.93           B8-A3 1 0
30 [WBB2011] 13 pr* 06 12 55.060 +17 59 31.09           G7 1 0
31 [WBB2011] 11 pr* 06 12 55.100 +17 59 21.34           K1 1 0
32 [WBB2011] 6 pr* 06 12 55.310 +17 59 15.90           K3 1 0
33 SH 2-255 S HII 06 12 56.1 +17 58 42           ~ 7 0
34 2MASS J06125638+1759326 pr* 06 12 56.382 +17 59 32.64           K2 2 0
35 [WBB2011] S255S-SMA1 mm 06 12 56.65 +17 58 41.2           ~ 1 0
36 [MBH2005] G192.60-0.05 MM 3 Cld 06 12 56.8 +17 58 03           ~ 3 0
37 [WBB2011] S255S-SMA2 mm 06 12 56.85 +17 58 35.0           ~ 1 0
38 IC 2162 HII 06 13 04.1 +17 58 44           ~ 338 2
39 HD 47632 * 06 40 03.6059983985 +12 22 30.244590796   7.89 7.90     B9 7 0
40 HD 49339 * 06 42 25.8451126282 -68 16 06.877640763   8.81 8.93     B5V 6 0
41 HD 84971 * 09 48 44.4862105776 -02 42 48.970456826 7.76 8.48 8.64     B3II 62 0
42 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5320 1
43 HD 115106 PM* 13 15 13.3854885114 -19 12 17.774315738   9.17 8.53     G2V 13 0
44 3C 454.3 QSO 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2506 2

    Equat.    Gal    SGal    Ecl

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2020.07.13-05:54:55

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