2021A&A...651A..36S


Query : 2021A&A...651A..36S

2021A&A...651A..36S - Astronomy and Astrophysics, volume 651A, 36-36 (2021/7-1)

Probing the structure of a massive filament: ArTeMiS 350 and 450 µm mapping of the integral-shaped filament in Orion A.

SCHULLER F., ANDRE P., SHIMAJIRI Y., ZAVAGNO A., PERETTO N., ARZOUMANIAN D., CSENGERI T., KONYVES V., PALMEIRIM P., PEZZUTO S., RIGBY A., ROUSSEL H., AJEDDIG H., DUMAYE L., GALLAIS P., LE PENNEC J., MARTIGNAC J., MATTERN M., REVERET V., RODRIGUEZ L. and TALVARD M.

Abstract (from CDS):


Context. The Orion molecular cloud is the closest region of high-mass star formation. It is an ideal target for investigating the detailed structure of massive star-forming filaments at high resolution and the relevance of the filament paradigm for the earliest stages of intermediate- to high-mass star formation.
Aims. Within the Orion A molecular cloud, the integral-shaped filament (ISF) is a prominent, degree-long structure of dense gas and dust with clear signs of recent and ongoing high-mass star formation. Our aim is to characterise the structure of this massive filament at moderately high angular resolution (8'' or ∼0.016pc) in order to measure the intrinsic width of the main filament, down to scales well below 0.1pc, which has been identified as the characteristic width of filaments.
Methods. We used the ArTeMiS bolometer camera at APEX to map a ∼0.6x0.2deg2 region covering OMC-1, OMC-2, and OMC-3 at 350 and 450µm. We combined these data with Herschel-SPIRE maps to recover extended emission. The combined Herschel-ArTeMiS maps provide details on the distribution of dense cold material, with a high spatial dynamic range, from our 8'' resolution up to the transverse angular size of the map, ∼10-15'. By combining Herschel and ArTeMiS data at 160, 250, 350, and 450µm, we constructed high-resolution temperature and H2 column density maps. We extracted radial intensity profiles from the column density map in several representative portions of the ISF, which we fitted with Gaussian and Plummer models to derive their intrinsic widths. We also compared the distribution of material traced by ArTeMiS with that seen in the higher-density tracer N2H+(1-0) that was recently observed with the ALMA interferometer.
Results. All the radial profiles that we extracted show a clear deviation from a Gaussian, with evidence for an inner plateau that had not previously been seen clearly using Herschel-only data. We measure intrinsic half-power widths in the range 0.06-0.11pc. This is significantly larger than the Gaussian widths measured for fibres seen in N2H+, which probably only traces the dense innermost regions of the large-scale filament. These half-power widths are within a factor of two of the value of ∼0.1pc found for a large sample of nearby filaments in various low-mass star-forming regions, which tends to indicate that the physical conditions governing the fragmentation of pre-stellar cores within transcritical or supercritical filaments are the same over a large range of masses per unit length.

Abstract Copyright: © F. Schuller et al. 2021

Journal keyword(s): stars: formation - stars: massive - ISM: structure - submillimeter: ISM - ISM: individual objects: Orion A

VizieR on-line data: <Available at CDS (J/A+A/651/A36): list.dat fits/*>

Simbad objects: 23

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Number of rows : 23
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 3192 2
2 Barnard 211 DNe 04 17 35 +27 43.1           ~ 115 0
3 Barnard 213 DNe 04 20 51 +27 16.3           ~ 194 0
4 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4093 0
5 RAFGL 618 pA* 04 42 53.6242032600 +36 06 53.400902220   16.32   12.59   C-rich 987 0
6 NAME Barnard's Loop HII 05 27.5 -03 58           ~ 120 1
7 NAME f-Shaped Filament in Orion Cld 05 35.0 -05 30           ~ 102 0
8 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2206 1
9 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1127 2
10 NAME Orion-KL SFR 05 35 14.16 -05 22 21.5           ~ 2206 1
11 M 42 OpC 05 35 17 -05 23.4           ~ 3970 0
12 NAME Ori Region reg 05 35 17.30 -05 23 28.0           ~ 550 0
13 OMC 3 MoC 05 35 20.0 -05 01 00           ~ 257 1
14 NAME Orion Bright Bar reg 05 35 22.30 -05 24 33.0           ~ 821 0
15 HOPS 87 Y*O 05 35 23.500 -05 01 29.58           ~ 90 0
16 V* V2457 Ori Or* 05 35 26.97000 -05 09 54.4644         18.858 ~ 143 0
17 OMC 2 MoC 05 35 27 -05 10.1           ~ 434 1
18 NAME OMC-2/3 reg 05 35 33.0 -05 00 32           ~ 82 0
19 NAME Ori A MoC 05 38 -07.1           ~ 2896 0
20 NGC 2071 RNe 05 47 10 +00 18.0           ~ 630 1
21 NAME Orion Molecular Cloud MoC 05 56 -01.8           ~ 1024 1
22 NGC 6334 HII 17 20 53 -36 07.9           ~ 654 0
23 NAME Gould Belt PoG ~ ~           ~ 832 1

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2023.01.27-22:31:03

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