2010ApJ...713..883B


Query : 2010ApJ...713..883B

2010ApJ...713..883B - Astrophys. J., 713, 883-899 (2010/April-3)

Sequential star formation in RCW 34: a spectroscopic census of the stellar content of high-mass star-forming regions.

BIK A., PUGA E., WATERS L.B.F.M., HORROBIN M., HENNING Th., VASYUNINA T., BEUTHER H., LINZ H., KAPER L., VAN DEN ANCKER M., LENORZER A., CHURCHWELL E., KURTZ S., KOUWENHOVEN M.B.N., STOLTE A., DE KOTER A., THI W.F., COMERON F. and WAELKENS C.

Abstract (from CDS):

In this paper, we present VLT/SINFONI integral field spectroscopy of RCW 34 along with Spitzer/IRAC photometry of the surroundings. RCW 34 consists of three different regions. A large bubble has been detected in the IRAC images in which a cluster of intermediate- and low-mass class II objects is found. At the northern edge of this bubble, an H II region is located, ionized by 3 OB stars, of which the most massive star has spectral type O8.5V. Intermediate-mass stars (2-3 M) are detected of G- and K-spectral type. These stars are still in the pre-main-sequence (PMS) phase. North of the H II region, a photon-dominated region is present, marking the edge of a dense molecular cloud traced by H2emission. Several class 0/I objects are associated with this cloud, indicating that star formation is still taking place. The distance to RCW 34 is revised to 2.5±0.2 kpc and an age estimate of 2±1 Myr is derived from the properties of the PMS stars inside the H II region. Between the class II sources in the bubble and the PMS stars in the H II region, no age difference could be detected with the present data. The presence of the class 0/I sources in the molecular cloud, however, suggests that the objects inside the molecular cloud are significantly younger. The most likely scenario for the formation of the three regions is that star formation propagated from south to north. First the bubble is formed, produced by intermediate- and low-mass stars only, after that, the H II region is formed from a dense core at the edge of the molecular cloud, resulting in the expansion similar to a champagne flow. More recently, star formation occurred in the rest of the molecular cloud. Two different formation scenarios are possible. (1) The bubble with the cluster of low- and intermediate-mass stars triggered the formation of the O star at the edge of the molecular cloud, which in its turn induces the current star formation in the molecular cloud. (2) An external triggering is responsible for the star formation propagating from south to north.

Abstract Copyright:

Journal keyword(s): H II regions - infrared: stars - photon-dominated region: PDR - stars: early-type - stars: formation - stars: pre-main sequence

Nomenclature: Fig. 10, Table 6: [BPW2010] NN (Nos 1-29).

CDS comments: Gum 29 is a misprint for Gum 19.

Simbad objects: 40

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Number of rows : 40
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4015 0
2 HD 69929 * 08 17 41.2975586760 -39 06 10.724214636   8.71 8.70     B3V 12 0
3 NAME VELA MOL RIDGE MoC 08 53 -45.0           ~ 141 0
4 [BPW2010] 20 Y*O 08 56 24.6 -43 06 01           K1-3 1 0
5 [BPW2010] 15 * 08 56 26.7159691824 -43 06 26.654120964           G7-9V 1 0
6 VdBH 25a C * 08 56 26.7967340856 -43 05 34.958082048     15.00     G5.5-7.5V 2 0
7 VdBH 25q * 08 56 26.8 -43 05 41           K2V 2 0
8 [BPW2010] 19 * 08 56 27.80 -43 06 07.5           K1-3V 1 0
9 [BPW2010] 13 * 08 56 27.8039964456 -43 06 21.119192568           G5.5-7.5V 1 0
10 [BPW2010] 29 * 08 56 28.00 -43 05 53.7           ~ 1 0
11 2MASS J08562804-4306127 Y*O 08 56 28.0493029320 -43 06 12.870955080           G7-9V 1 0
12 V* V391 Vel B Y*O 08 56 28.0767790920 -43 05 56.815393668           ~ 1 0
13 RCW 34 HII 08 56 28.1 -43 05 58   10.5 11.21     ~ 94 0
14 V* V391 Vel A * 08 56 28.1094275184 -43 05 55.300855128           ~ 1 0
15 V* V391 Vel Or* 08 56 28.109952 -43 05 55.40028 12.61 12.71 11.73 11.50   O8/8.5V 81 1
16 [BPW2010] 5 Y*O 08 56 28.1738112288 -43 05 58.107998508           K8-9 1 0
17 [BPW2010] 24 * 08 56 28.40 -43 05 34.9           K 2 0
18 [BPW2010] 27 * 08 56 29.00 -43 05 54.0           ~ 1 0
19 [BPW2010] 12 Y*O 08 56 29.1 -43 06 19           K0-4V 1 0
20 [BPW2010] 25 * 08 56 29.1 -43 06 19           K 1 0
21 [BPW2010] 6 Y*O 08 56 29.10 -43 05 31.6           K0-4V 1 0
22 [BPW2010] 16 Y*O 08 56 29.20 -43 05 32.5           K0-2 1 0
23 [BPW2010] 18 * 08 56 29.40 -43 06 00.3           K0-2V 1 0
24 [BPW2010] 7 * 08 56 29.60 -43 05 51.9           G0-4V 1 0
25 [BPW2010] 21 * 08 56 29.6 -43 05 34           ~ 1 0
26 [BPW2010] 9 Y*O 08 56 29.70 -43 06 03.2           G1-3V 1 0
27 2MASS J08562970-4306240 Y*O 08 56 29.7027621216 -43 06 23.994669492           G7-9 1 0
28 VdBH 25a B * 08 56 29.8057964424 -43 05 59.146789524     15.00     ~ 2 0
29 [BPW2010] 22 * 08 56 30.7 -43 05 35           ~ 1 0
30 [BPW2010] 8 * 08 56 31.0 -43 05 32           G5.5-7.5V 1 0
31 2MASS J08563166-4305560 Y*O 08 56 31.6551122808 -43 05 56.067864072           G7-9 1 0
32 2MASS J08563191-4306015 Y*O 08 56 31.9341735888 -43 06 01.235018916           G3-5V 1 0
33 [BPW2010] 28 * 08 56 32.5 -43 05 35           ~ 1 0
34 RCW 38 SFR 08 59 05.50 -47 30 39.4           ~ 294 2
35 NAME Vela R2 As* 09 00 -43.0           ~ 25 0
36 HD 79149 * 09 11 31.2015118776 -28 25 39.907180128   7.80 7.83     B9III 10 0
37 HD 86085 bC* 09 55 18.6835570752 -38 45 46.317244068 8 8.83 8.91     B1Vn 26 0
38 HD 92552 * 10 39 55.8552768552 -56 16 40.215223272   7.94 8.00     B3/5V 20 0
39 M 8 HII 18 03 37 -24 23.2           ~ 589 1
40 SH 2-88 B HII 19 46 47.32920 +25 12 45.6230           ~ 156 2

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2022.10.03-00:56:28

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