2005ApJ...626..959M


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.15CEST07:32:28

2005ApJ...626..959M - Astrophys. J., 626, 959-965 (2005/June-3)

Multiscale magnetic fields in star-forming regions: interferometric polarimetry of the MMS 6 core of OMC-3.

MATTHEWS B.C., LAI S.-P., CRUTCHER R.M. and WILSON C.D.

Abstract (from CDS):

We present the first interferometric observations of linearly polarized emission toward the OMC-3 region of the Orion A cloud. We have observed the MMS 6 protostellar core at 1.3 mm with the Berkeley-Illinois-Maryland Association (BIMA) array, achieving a resolution of 4".3x3".0. We find that the polarization angle measured changes systematically across the core, orienting along a dust extension to the northwest. The polarization angle is oriented similarly to the 850 and 350 µm polarized emission measured by the SCUBA and Hertz polarimeters. A polarization hole is detected, as is typical of polarized emission data toward cores. Since the BIMA data are insensitive to structure on spatial scales of >40", the emission detected is dominated by the core and not the integral-shaped filament in which it is embedded. Observations of CO J=2-1 reveal CO emission potentially associated with the core, but no outflow signature is detected. Utilizing the Chandrasekhar-Fermi method, we have used the dispersion in the polarization vectors to estimate a field strength of 640 µG in the plane of the sky, assuming a corrective Q-factor of 0.5. Applying the recent measurement of the inclination of the field to the line of sight (Houde et al.), a total field strength of 680 µG is derived. Despite highly nonthermal line widths, the kinetic energy density is found to be insufficient to support this core against gravitational collapse. The magnetic energy density, when combined with the predominantly turbulent kinetic energy density, is comparable to the effects of gravity, but its value is highly dependent on the applied Q-factor to a degree that the core may be subcritical or supercritical. The preservation of the field geometry from large to small scales in this core is consistent with observations of a second protostellar core in a filamentary cloud in Orion B.

Abstract Copyright:

Journal keyword(s): ISM: Clouds - ISM: Individual: Alphanumeric: OMC-3 MMS 6 - ISM: Magnetic Fields - ISM: Molecules - Polarization - Stars: Formation

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 - 2021
#notes
1 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 626 1
2 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 470 0
3 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1258 1
4 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 568 0
5 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 276 0
6 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1131 0
7 NAME OMC-1 MoC 05 35 14 -05 22.4           ~ 1051 2
8 M 42 HII 05 35 17.3 -05 23 28           ~ 3787 0
9 [TSO2008] 9 mm 05 35 18.030 -05 00 17.77           ~ 17 0
10 OMC 3 MoC 05 35 20.0 -05 01 00           ~ 234 1
11 [TSO2008] 13 Y*O 05 35 22.4451 -05 01 14.123           ~ 46 1
12 [TSO2008] 14 mm 05 35 23.420 -05 01 30.35           ~ 60 0
13 IRAS 05329-0505 Y*O 05 35 26.746 -05 03 55.08           ~ 73 0
14 OMC 2 MoC 05 35 27 -05 10.1           ~ 404 1
15 NAME Ori A MoC 05 38 -07.1           ~ 2756 0
16 NAME Flame Nebula HII 05 41 42.7 -01 54 44           ~ 693 1
17 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1217 0
18 NGC 2024 Cl* 05 41 43 -01 50.5           ~ 1087 1
19 [MCK88] NGC 2024 FIR 5 cor 05 41 44.6 -01 55 38           ~ 91 0
20 NAME NGC 2071 IR SFR 05 47 04.4 +00 21 49           ~ 62 0
21 3C 279 Bla 12 56 11.1664521013 -05 47 21.531840471   18.01 17.75 15.87   ~ 2765 2
22 W 51 SNR 19 23 50 +14 06.0           ~ 1176 1
23 [MBS2007c] CygX-N44 Rad 20 39 01.01 +42 22 50.2           ~ 365 0

    Equat.    Gal    SGal    Ecl

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2021.04.15-07:32:28

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