2011A&A...535A...2B


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.24CET22:06:51

2011A&A...535A...2B - Astronomy and Astrophysics, volume 535A, 2-2 (2011/11-1)

Will the starless cores in Chamaeleon I and III turn prestellar?

BELLOCHE A., PARISE B., SCHULLER F., ANDRE P., BONTEMPS S. and MENTEN K.M.

Abstract (from CDS):

The nearby Chamaeleon molecular cloud complex is a good laboratory for studying the process of low-mass star formation because it consists of three clouds with very different properties. Chamaeleon III does not show any sign of star formation, while star formation has been very active in Chamaeleon I and may already be finishing. Our goal is to determine whether star formation can proceed in Cha III by searching for prestellar cores, and to compare the results to our recent survey of Cha I. We used the Large APEX Bolometer Array (LABOCA) to map Cha III in dust continuum emission at 870µm. The map is compared with a 2MASS extinction map and decomposed with a multiresolution algorithm. The extracted sources are analyzed by carefully taking into account the spatial filtering inherent in the data reduction process. Twenty-nine sources are extracted from the 870µm map, all of them starless. The estimated 90% completeness limit is 0.18M . The starless cores are found down to a visual extinction of 1.9mag, in marked contrast with other molecular clouds, including Cha I. Apart from this difference, the Cha III starless cores share very similar properties with those found in Cha I. They are less dense than those detected in continuum emission in other clouds by a factor of a few. At most two sources (<7%) have a mass larger than the critical Bonnor-Ebert mass, which suggests that the fraction of prestellar cores is very low, even lower than in Cha I (<17%). Only the most massive sources are candidate prestellar cores, in agreement with the correlation found earlier in the Pipe nebula. The mass distribution of the 85 starless cores of Cha I and III that are not candidate prestellar cores is consistent with a single power law down to the 90% completeness limit, with an exponent close to the Salpeter value. A fraction of the starless cores detected with LABOCA in Cha I and III may still grow in mass and become gravitationally unstable. Based on predictions of numerical simulations of turbulent molecular clouds, we estimate that at most 50% and 20% of the starless cores of Cha I and III, respectively, may form stars. The LABOCA survey reveals that Cha III, and Cha I to some extent too, is a prime target to study the formation of prestellar cores, and thus the onset of star formation. Obtaining observational constraints on the duration of the core-building phase prior to gravitational collapse will be necessary to make further progress.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: individual objects: Chamaleon III - ISM: structure - evolution - dust, extinction - stars: protostars

VizieR on-line data: <Available at CDS (J/A+A/535/A2): cha3_870.fit>

Nomenclature: Fig. 3, Tables 2-3: [BPR2011] Cha3-CNN (Nos C1-C29).

CDS comments: Paragraph 2.2 IRAS 13134-6264 is a probable misprint for IRAS 13134-6242. Footnote 9 MMS1 not in Simbad.

Simbad objects: 53

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Number of rows : 53

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * alf UMi cC* 02 31 49.09456 +89 15 50.7923 3.00 2.62 2.02 1.53 1.22 F8Ib 619 2
2 NAME Per Region reg 03 37 00.0 +31 15 00           ~ 234 0
3 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3637 0
4 NAME Ori A MoC 05 38 -07.1           ~ 2733 0
5 NGC 2071 RNe 05 47 10 +00 18.0           ~ 612 1
6 * eta Car Em* 10 45 03.5455050 -59 41 03.951060 6.37 7.034 6.21 4.90 4.41 OBepec 2253 0
7 QSO B1057-797 BLL 10 58 43.30977041 -80 03 54.1597166   19.08   17.31   ~ 161 0
8 NAME Polaris Flare MoC 11 00 14.8 +86 10 52           ~ 168 1
9 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1009 1
10 NAME Chamaeleon Region SFR 11 55 -78.0           ~ 708 0
11 [BPR2011] Cha3-C28 cor 12 29 06.05 -80 10 53.3           ~ 1 0
12 [BPR2011] Cha3-C23 cor 12 35 44.30 -80 25 21.6           ~ 1 0
13 [BPR2011] Cha3-C24 cor 12 36 13.68 -80 34 09.3           ~ 1 0
14 [BPR2011] Cha3-C14 cor 12 36 46.21 -80 34 53.5           ~ 1 0
15 IRAS 12340-7958 * 12 37 39.7466355997 -80 15 13.713429632   16.11 14.39 13.63 9.81 ~ 101 0
16 NAME Cha III MoC 12 37.8 -80 15           ~ 131 2
17 [BPR2011] Cha3-C27 cor 12 38 10.69 -80 19 35.8           ~ 1 0
18 [BPR2011] Cha3-C22 cor 12 39 36.53 -80 22 24.5           ~ 1 0
19 [BPR2011] Cha3-C16 cor 12 40 45.58 -80 19 17.0           ~ 1 0
20 [BPR2011] Cha3-C5 cor 12 42 03.29 -80 16 06.6           ~ 1 0
21 [BPR2011] Cha3-C13 cor 12 42 48.27 -80 12 36.8           ~ 1 0
22 [BPR2011] Cha3-C4 cor 12 43 35.51 -80 11 11.7           ~ 1 0
23 [BPR2011] Cha3-C3 cor 12 44 24.79 -80 08 50.2           ~ 1 0
24 [BPR2011] Cha3-C6 cor 12 47 38.53 -80 07 23.2           ~ 1 0
25 [BPR2011] Cha3-C25 cor 12 48 31.42 -79 38 46.7           ~ 1 0
26 [BPR2011] Cha3-C29 cor 12 51 36.11 -79 31 17.1           ~ 1 0
27 [BPR2011] Cha3-C21 cor 12 51 39.85 -79 23 29.5           ~ 1 0
28 [BPR2011] Cha3-C11 cor 12 52 12.93 -79 22 45.4           ~ 1 0
29 [BPR2011] Cha3-C7 cor 12 52 17.60 -79 25 42.1           ~ 1 0
30 [BPR2011] Cha3-C17 cor 12 52 49.09 -79 33 06.9           ~ 1 0
31 [BPR2011] Cha3-C12 cor 12 52 56.46 -79 39 49.4           ~ 1 0
32 NAME Cha II MoC 12 54 -77.2           ~ 304 0
33 [BPR2011] Cha3-C9 cor 12 53 40.41 -78 59 34.7           ~ 1 0
34 [BPR2011] Cha3-C10 cor 12 54 08.10 -78 53 51.0           ~ 1 0
35 [BPR2011] Cha3-C8 cor 12 54 20.65 -79 30 08.0           ~ 1 0
36 [BPR2011] Cha3-C2 cor 12 54 23.02 -78 51 58.0           ~ 1 0
37 [BPR2011] Cha3-C18 cor 12 54 37.43 -78 53 03.5           ~ 1 0
38 [BPR2011] Cha3-C19 cor 12 54 40.89 -79 29 03.3           ~ 1 0
39 [BPR2011] Cha3-C20 cor 12 54 47.60 -78 53 39.6           ~ 1 0
40 [BPR2011] Cha3-C1 cor 12 54 53.58 -78 52 24.2           ~ 1 0
41 [BPR2011] Cha3-C15 cor 12 55 53.07 -79 03 51.3           ~ 1 0
42 [BPR2011] Cha3-C26 cor 12 56 07.33 -79 03 22.2           ~ 1 0
43 IRAS 13134-6242 mul 13 16 42.9 -62 58 45           ~ 29 0
44 [WBH98] 13134-6242 HII 13 16 46.3 -62 58 35           ~ 23 0
45 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3129 1
46 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 349 1
47 GAL 005.88-00.41 HII 18 00 30.388 -24 04 00.20           ~ 303 0
48 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 952 2
49 NAME Aql Rift DNe 18 32 -01.0           ~ 253 1
50 OH 34.26 +0.15 SFR 18 53 18.54 +01 14 57.9           ~ 471 0
51 SH 2-140 OpC 22 19 07.8 +63 17 07           ~ 636 2
52 IRAS 22176+6303 Y*O 22 19 17.978 +63 18 52.92           ~ 590 0
53 NAME Aql Region reg ~ ~           ~ 320 0

    Equat.    Gal    SGal    Ecl

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2021.02.24-22:06:51

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