2018A&A...610A..77H


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.19CET07:47:19

2018A&A...610A..77H - Astronomy and Astrophysics, volume 610A, 77-77 (2018/2-1)

An ALMA study of the Orion Integral Filament. I. Evidence for narrow fibers in a massive cloud.

HACAR A., TAFALLA M., FORBRICH J., ALVES J., MEINGAST S., GROSSSCHEDL J. and TEIXEIRA P.S.

Abstract (from CDS):

Aim. We have investigated the gas organization within the paradigmatic Integral Shape Filament (ISF) in Orion in order to decipher whether or not all filaments are bundles of fibers.
Methods. We combined two new ALMA Cycle 3 mosaics with previous IRAM 30m observations to produce a high-dynamic range N2H+ (1-0) emission map of the ISF tracing its high-density material and velocity structure down to scales of 0.009pc (or ∼2000AU).
Results. From the analysis of the gas kinematics, we identify a total of 55 dense fibers in the central region of the ISF. Independently of their location in the cloud, these fibers are characterized by transonic internal motions, lengths of ∼0.15pc, and masses per unit length close to those expected in hydrostatic equilibrium. The ISF fibers are spatially organized forming a dense bundle with multiple hub-like associations likely shaped by the local gravitational potential. Within this complex network, the ISF fibers show a compact radial emission profile with a median FWHM of 0.035pc systematically narrower than the previously proposed universal 0.1pc filament width.
Conclusions. Our ALMA observations reveal complex bundles of fibers in the ISF, suggesting strong similarities between the internal substructure of this massive filament and previously studied lower-mass objects. The fibers show identical dynamic properties in both low- and high-mass regions, and their widespread detection in nearby clouds suggests a preferred organizational mechanism of gas in which the physical fiber dimensions (width and length) are self-regulated depending on their intrinsic gas density. Combining these results with previous works in Musca, Taurus, and Perseus, we identify a systematic increase of the surface density of fibers as a function of the total mass per-unit-length in filamentary clouds. Based on this empirical correlation, we propose a unified star-formation scenario where the observed differences between low- and high-mass clouds, and the origin of clusters, emerge naturally from the initial concentration of fibers.

Abstract Copyright: © ESO 2018

Journal keyword(s): ISM: clouds - ISM: kinematics and dynamics - ISM: structure - stars: formation - submillimeter: ISM

VizieR on-line data: <Available at CDS (J/A+A/610/A77): list.dat fits/*>

Simbad objects: 45

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Number of rows : 45

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 * alf UMi cC* 02 31 49.09456 +89 15 50.7923 3.00 2.62 2.02 1.53 1.22 F8Ib 602 2
2 NGC 1333 SFR 03 28 55 +31 22.2   10.9       ~ 1182 1
3 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1010 0
4 LDN 1495 DNe 04 18.1 +27 37           ~ 276 1
5 Barnard 213 DNe 04 20 51 +27 16.3           ~ 145 0
6 QSO B0420-0127 QSO 04 23 15.80072776 -01 20 33.0654034   17.50 17.00 16.28   ~ 1020 2
7 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3322 0
8 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1327 0
9 LDN 1517 DNe 04 55 45 +30 33.0           ~ 93 0
10 NAME f-Shaped Filament in Orion Cld 05 35.0 -05 30           ~ 57 0
11 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 1907 1
12 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 991 2
13 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 1945 1
14 NAME OMC 1N PoC 05 35 14.5 -05 22 07           ~ 14 1
15 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1433 1
16 OMC 3 MoC 05 35 20.0 -05 01 00           ~ 213 1
17 [MWZ90] OMC-2 FIR 6 IR 05 35 22.6 -05 12 37           ~ 16 0
18 [SMD2014] 083.8513-05.1419 Y*O 05 35 24.2999 -05 08 30.686           ~ 42 0
19 [TSO2008] 24 Y*? 05 35 24.6 -05 07 53           ~ 23 0
20 NAME OMC 2 IRS 3 HII 05 35 26.00 -05 10 16.6           ~ 58 0
21 [TSO2008] 18 mm 05 35 26.0 -05 05 42           ~ 35 1
22 JCMTSF J053526.4-050521 mm 05 35 26.5 -05 05 17           ~ 22 1
23 V* V2457 Ori Or* 05 35 26.97 -05 09 54.5         18.858 ~ 104 0
24 OMC 2 MoC 05 35 27 -05 10.1           ~ 374 1
25 2MASS J05352762-0509337 Y*O 05 35 27.622 -05 09 33.78           ~ 67 0
26 M 43 HII 05 35 31 -05 16.2           ~ 155 0
27 HD 37061 Or* 05 35 31.3653515656 -05 16 02.586154009 6.44 7.09 6.83     O9V 312 0
28 [CRW97] OMC-3 MMS 10 cor 05 35 31.91 -05 05 51.1           ~ 27 0
29 NAME OMC-2/3 reg 05 35 33.0 -05 00 32           ~ 46 0
30 NAME Ori A MoC 05 38 -07.1           ~ 2615 0
31 QSO B0539-057 QSO 05 41 38.08338 -05 41 49.4284     20.4 20.70   ~ 195 2
32 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 812 1
33 NAME Musca Filament PoC 10 54 -74.0           ~ 20 0
34 NAME Musca Cld 12 23 -71.3           ~ 152 0
35 * rho Oph ** 16 25 35.11766 -23 26 49.8150 4.30 4.85 4.63 4.27 3.96 B2IV+B2V 593 2
36 NAME Nessie Nebula DNe 16 43 -46.7           ~ 20 0
37 LDN 1746 DNe 17 11.3 -27 22           ~ 104 0
38 NGC 6334 HII 17 20 51 -36 06.9           ~ 560 0
39 [CCE98b] 011.11-0.12 Cld 18 10.5 -19 23           ~ 83 1
40 SDC G14.225-0.506 DNe 18 18 11.49 -16 49 29.6           ~ 16 0
41 NAME IRDC 18223-3 Y*O 18 25 08.4002 -12 45 15.466           ~ 59 0
42 NAME Serpens Cloud SFR 18 29 49 +01 14.8           ~ 885 2
43 MSXDC G035.39-0.33 MoC 18 57 09.0 +02 07 46           ~ 74 0
44 IC 5146 SFR 21 53 24 +47 16.0   7.82 7.2     ~ 375 2
45 NAME Gould Belt PoG ~ ~           ~ 685 1

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2019.11.19-07:47:20

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