2016A&A...586A..68P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.06CEST19:11:02

2016A&A...586A..68P - Astronomy and Astrophysics, volume 586A, 68-68 (2016/2-1)

Observational constraints on star cluster formation theory. I. The mass-radius relation.

PFALZNER S., KIRK H., SILLS A., URQUHART J.S., KAUFFMANN J., KUHN M.A., BHANDARE A. and MENTEN K.M.

Abstract (from CDS):

Stars form predominantly in groups usually denoted as clusters or associations. The observed stellar groups display a broad spectrum of masses, sizes, and other properties, so it is often assumed that there is no underlying structure in this diversity. Here we show that the assumption of an unstructured multitude of cluster or association types might be misleading. Current data compilations of clusters in the solar neighbourhood show correlations among cluster mass, size, age, maximum stellar mass, etc. In this first paper we take a closer look at the correlation of cluster mass and radius. We use literature data to explore relations in cluster and molecular core properties in the solar neighbourhood. We show that for embedded clusters in the solar neighbourhood a clear correlation exists between cluster mass and half-mass radius of the form Mc=C*Rcγ with γ=1.7±0.2. This correlation holds for infrared K-band data, as well as for X-ray sources and clusters containing a hundred stars up to those consisting of a few tens of thousands of stars. The correlation is difficult to verify for clusters containing fewer than 30 stars owing to low-number statistics. Dense clumps of gas are the progenitors of the embedded clusters. We find almost the same slope for the mass-size relation of dense, massive clumps as for the embedded star clusters. This might point to a direct translation from gas to stellar mass: however, it is difficult to relate size measurements for clusters (stars) to those for gas profiles. Taking multiple paths for clump mass into cluster mass into account, we obtain an average star-formation efficiency of 18%+9.3–5.7 for the embedded clusters in the solar neighbourhood. The derived mass-radius relation gives constraints for the theory of clustered star formation. Analytical models and simulations of clustered star formation have to reproduce this relation in order to be realistic.

Abstract Copyright:

Journal keyword(s): stars: formation - open clusters and associations: general - ISM: clouds - solar neighborhood

CDS comments: Paragraph 2.2 Cha I 1 may be ISO-ChaI 1 in SIMBAD.

Simbad objects: 39

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Number of rows : 39

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 IC 1805 OpC 02 32 42 +61 27.0   7.03 6.5     ~ 473 2
2 IC 348 1 * 03 43 24.7881401834 +32 17 38.548410923   14.33 12.78     K0III 7 0
3 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3478 0
4 NGC 1893 OpC 05 22 44 +33 24.7   7.90 7.5     ~ 231 0
5 Ass Ori OB 1b As* 05 34.0 -01 30           ~ 235 0
6 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1977 1
7 M 42 HII 05 35 17.3 -05 23 28           ~ 3724 0
8 NAME Ori A MoC 05 38 -07.1           ~ 2675 0
9 NAME Flame Nebula HII 05 41 42.7 -01 54 44           ~ 692 1
10 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1164 0
11 NAME Mon R2 HII 06 07 46.6 -06 22 59           ~ 650 2
12 IRAS 06061+2151 SFR 06 09 07.8 +21 50 39           ~ 81 0
13 NAME Rosette Nebula HII 06 31 40 +04 57.8           ~ 443 1
14 NGC 2244 OpC 06 31 55 +04 56.5   5.26 4.8     ~ 563 4
15 NGC 2264 OpC 06 40 58 +09 53.7     3.9     ~ 1587 1
16 NGC 2362 OpC 07 18 41 -24 57.3     4.1     ~ 361 0
17 RCW 36 HII 08 59 00.9 -43 44 10     15.20     ~ 125 0
18 RCW 38 SFR 08 59 05.50 -47 30 39.4           ~ 268 2
19 Cl Westerlund 2 OpC 10 23 58.1 -57 45 49   11.59 10.5     ~ 277 0
20 Cl Trumpler 14 OpC 10 43 56 -59 33.0   5.70 5.5     ~ 425 0
21 NGC 3372 HII 10 44 19.0 -59 53 21           ~ 888 2
22 Sz 4 TT* 10 57 42.1008128649 -76 59 35.640039635   14.1 14.80   12.17 M4Ve 41 0
23 V* TW Cha Or* 10 59 01.0608276980 -77 22 40.946475900     13.40   11.68 K8Ve 115 0
24 ISO-ChaI 1 * 11 02 16.1871472955 -77 46 33.111440109           F 6 0
25 NGC 3603 OpC 11 15 18.6 -61 15 26           ~ 940 1
26 Cl Westerlund 1 OpC 16 47 04.00 -45 51 04.9           ~ 463 0
27 NGC 6334 HII 17 20 51 -36 06.9           ~ 585 0
28 NGC 6357 HII 17 26.5 -34 12           ~ 250 0
29 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11533 0
30 NAME Arches Cluster Cl* 17 45 50.5 -28 49 28           ~ 629 0
31 M 20 OpC 18 02 42 -22 58.3           ~ 393 1
32 M 8 HII 18 03 37 -24 23.2           ~ 552 1
33 M 16 OpC 18 18 48 -13 48.4   6.58 6.0     ~ 935 2
34 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1484 0
35 LBN 028.77+03.43 HII 18 31 26.5 -02 04 22           ~ 187 2
36 Ass Cyg OB 2 As* 20 33.2 +41 19           ~ 790 0
37 GRS G081.70 +00.50 SFR 20 39 01.6 +42 19 38           O4.5 944 0
38 IRAS 20406+4555 IR 20 42 21.77 +46 05 53.3           ~ 15 0
39 NGC 7380 OpC 22 47 21 +58 07.9   7.62 7.2     ~ 172 0

    Equat.    Gal    SGal    Ecl

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2020.07.06-19:11:02

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