2017A&A...600A.141K


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.28CET22:16:23

2017A&A...600A.141K - Astronomy and Astrophysics, volume 600A, 141-141 (2017/4-1)

Resolving the fragmentation of high line-mass filaments with ALMA: the integral shaped filament in Orion A.

KAINULAINEN J., STUTZ A.M., STANKE T., ABREU-VICENTE J., BEUTHER H., HENNING T., JOHNSTON K.G. and MEGEATH S.T.

Abstract (from CDS):

We study the fragmentation of the nearest high line-mass filament, the integral shaped filament (ISF, line-mass ∼400M/pc) in the Orion A molecular cloud. We have observed a 1.6pc long section of the ISF with the Atacama Large Millimetre/submillimeter Array (ALMA) at 3mm continuum emission, at a resolution of ∼3'' (1200AU). We identify from the region 43 dense cores with masses about a solar mass. 60% of the ALMA cores are protostellar and 40% are starless. The nearest neighbour separations of the cores do not show a preferred fragmentation scale; the frequency of short separations increases down to 1200AU. We apply a two-point correlation analysis on the dense core separations and show that the ALMA cores are significantly grouped at separations below ∼17000AU and strongly grouped below ∼6000AU. The protostellar and starless cores are grouped differently: only the starless cores group strongly below ∼6000AU. In addition, the spatial distribution of the cores indicates periodic grouping of the cores into groups of ∼30000AU in size, separated by ∼50000AU. The groups coincide with dust column density peaks detected by Herschel. These results show hierarchical, two-mode fragmentation in which the maternal filament periodically fragments into groups of dense cores. Critically, our results indicate that the fragmentation models for lower line-mass filaments (∼16M/pc) fail to capture the observed properties of the ISF. We also find that the protostars identified with Spitzer and Herschel in the ISF are grouped at separations below ∼17000AU. In contrast, young stars with disks do not show significant grouping. This suggests that the grouping of dense cores is partially retained over the protostar lifetime, but not over the lifetime of stars with disks. This is in agreement with a scenario where protostars are ejected from the maternal filament by the slingshot mechanism, a model recently proposed for the ISF. The separation distributions of the dense cores and protostars may also provide an evolutionary tracer of filament fragmentation.

Abstract Copyright: © ESO, 2017

Journal keyword(s): ISM: clouds - ISM: structure - stars: formation - ISM: individual objects: OMC-2 - radio continuum: ISM - radio continuum: ISM

VizieR on-line data: <Available at CDS (J/A+A/600/A141): list.dat isf-3mm.fits>

Nomenclature: Fig. 4, Table 2: [KSS2017] NN (Nos 1-43).

CDS comments: Paragraph 3.1 source FIR 6e not in SIMBAD.

Simbad objects: 70

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Number of rows : 70

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 NAME Chandra Deep Field-South reg 03 32 28.0 -27 48 30           ~ 1844 1
2 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1071 3
3 ICRF J051728.1-052040 QSO 05 17 28.1096179909 -05 20 40.837164387           ~ 17 0
4 [EC2006] MM12 HII 05 35 13.41015 -05 24 11.1770           ~ 47 1
5 [MWZ90] OMC-1 FIR 3 IR 05 35 13.8 -05 23 53           ~ 5 0
6 [FW2011] J053514.431-052233.457 IR 05 35 14.431 -05 22 33.46           ~ 13 0
7 NAME OMC 1N PoC 05 35 14.5 -05 22 07           ~ 16 1
8 [MSB86] CS 1 IR 05 35 15.26 -05 22 05.1           ~ 10 0
9 V* V2327 Ori Or* 05 35 18.22776 -05 13 06.8124   20.135 18.098   14.686 M0e 32 0
10 V* V2331 Ori Or* 05 35 18.5237648857 -05 13 38.322116674   18.794 17.244   13.333 M2e 33 0
11 [KSS2017] 43 cor 05 35 19.413 -05 15 37.98           ~ 1 0
12 HOPS 56 Y*O 05 35 19.4586 -05 15 32.779           ~ 12 0
13 V* V2359 Ori Or* 05 35 19.8322266766 -05 15 08.937340600         17.381 ~ 22 0
14 OMC 3 MoC 05 35 20.0 -05 01 00           ~ 225 1
15 [KSS2017] 36 cor 05 35 20.138 -05 13 15.40           ~ 1 0
16 V* V2364 Ori Or* 05 35 20.1521915741 -05 13 15.688010752   20.263 18.348   12.859 K5-M0e 47 0
17 2MASS J05352076-0513225 Y*O 05 35 20.762 -05 13 22.56           ~ 6 0
18 [KSS2017] 37 cor 05 35 21.348 -05 13 17.54           ~ 1 0
19 HOY J053521.34-051319.5 cor 05 35 21.4 -05 13 14           ~ 25 0
20 V* V2377 Ori Or* 05 35 21.5757535214 -05 09 38.822354154   15.1     15.509 K5 39 0
21 [KSS2017] 35 cor 05 35 21.705 -05 13 13.08           ~ 1 0
22 V* V415 Ori Or* 05 35 21.8787923529 -05 07 01.839578555     14.49   12.64 ~ 44 0
23 JW 703 Y*O 05 35 22.4056752156 -05 08 05.132895734     17.26   13.95 M0e 29 0
24 [MWZ90] OMC-2 FIR 6 IR 05 35 22.6 -05 12 37           ~ 18 0
25 [KSS2017] 32 cor 05 35 22.745 -05 12 26.47           ~ 2 0
26 [KSS2017] 33 cor 05 35 22.939 -05 12 40.70           ~ 2 0
27 ISOY J053523.33-051203.4 Y*O 05 35 23.3258 -05 12 03.477           ~ 5 0
28 2MASS J05352332-0507096 Y*O 05 35 23.326 -05 07 09.66           ~ 16 0
29 [TSO2008] 34 IR 05 35 23.4 -05 12 36           ~ 11 0
30 [TSO2008] 23 IR 05 35 23.4 -05 07 32           ~ 14 0
31 2MASS J05352341-0512023 Y*O 05 35 23.417 -05 12 02.34           ~ 23 0
32 [KSS2017] 10 cor 05 35 23.507 -05 07 09.79           ~ 1 0
33 HOPS 394 Y*O 05 35 23.9685 -05 07 52.913           ~ 16 0
34 [KSS2017] 15 cor 05 35 24.009 -05 08 27.65           ~ 1 0
35 [KSS2017] 11 cor 05 35 24.188 -05 07 52.75           ~ 1 0
36 [SMD2014] 083.8513-05.1419 Y*O 05 35 24.2999 -05 08 30.686           ~ 49 0
37 2MASS J05352477-0510296 Y*O 05 35 24.777 -05 10 29.61           ~ 42 1
38 [KSS2017] 12 cor 05 35 24.847 -05 07 53.72           ~ 1 0
39 2MASS J05352486-0506216 Y*O 05 35 24.87 -05 06 21.6           ~ 10 0
40 V* V2434 Ori Or* 05 35 25.2271676753 -05 15 35.730003683 17.433 17.401 16.302   13.355 M2.5e 45 0
41 JW 774 Y*O 05 35 25.646 -05 07 57.31     15.13   13.02 M3.5 31 0
42 [MGM2012] 2369 Y*O 05 35 25.82 -05 05 43.6           ~ 7 0
43 NAME OMC 2 IRS 3 HII 05 35 26.00 -05 10 16.6           ~ 61 0
44 [TSO2008] 18 mm 05 35 26.0 -05 05 42           ~ 38 1
45 [MGM2012] 2366 Y*O 05 35 26.16 -05 05 47.3           ~ 3 0
46 [KSS2017] 29 cor 05 35 26.325 -05 10 25.13           ~ 1 0
47 [KSS2017] 28 cor 05 35 26.396 -05 10 15.20           ~ 1 0
48 [KSS2017] 27 cor 05 35 26.455 -05 10 05.10           ~ 1 0
49 JCMTSF J053526.4-050521 mm 05 35 26.5 -05 05 17           ~ 23 1
50 HOPS 75 Y*O 05 35 26.6455 -05 06 10.404           ~ 9 0
51 IRAS 05329-0505 Y*O 05 35 26.746 -05 03 55.08           ~ 72 0
52 [KSS2017] 26 cor 05 35 26.797 -05 10 04.81           ~ 1 0
53 V* V2455 Ori Or* 05 35 26.83584 -05 09 24.4728           ~ 32 1
54 V* V2457 Ori Or* 05 35 26.97000 -05 09 54.4644         18.858 ~ 117 0
55 [KSS2017] 22 cor 05 35 26.992 -05 09 48.62           ~ 1 0
56 OMC 2 MoC 05 35 27 -05 10.1           ~ 394 1
57 [MGM2012] 2289 Y*O 05 35 27.07 -05 10 00.4           ~ 10 0
58 [KSS2017] 18 cor 05 35 27.197 -05 09 26.10           ~ 1 0
59 [KSS2017] 19 cor 05 35 27.512 -05 09 29.54           ~ 1 0
60 [KSS2017] 23 cor 05 35 27.528 -05 09 50.64           ~ 1 0
61 2MASS J05352762-0509337 Y*O 05 35 27.622 -05 09 33.78           ~ 72 0
62 HOPS 73 Y*O 05 35 27.70 -05 07 03.5           ~ 7 0
63 2MASS J05352787-0504597 Y*O 05 35 27.872 -05 04 59.72           ~ 8 0
64 TKK 870 Y*O 05 35 28.19 -05 03 41.2           ~ 34 0
65 [CRW97] OMC-3 MMS 10 cor 05 35 31.91 -05 05 51.1           ~ 28 0
66 NAME OMC-2/3 reg 05 35 33.0 -05 00 32           ~ 56 0
67 NAME Ori A MoC 05 38 -07.1           ~ 2705 0
68 QSO B0539-057 QSO 05 41 38.08338 -05 41 49.4284     20.4 20.70   ~ 211 2
69 QSO B0605-0834 BLL 06 07 59.69923743 -08 34 49.9781718     18.5 17.70   ~ 399 1
70 LDN 1262 MoC 23 25 47 +74 17.6           ~ 130 0

    Equat.    Gal    SGal    Ecl

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2020.11.28-22:16:23

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