2018A&A...618A.163J


Query : 2018A&A...618A.163J

2018A&A...618A.163J - Astronomy and Astrophysics, volume 618A, 163-163 (2018/1-0)

Magnetic fields in Bok globules: multi-wavelength polarimetry as tracer across large spatial scales.

JORQUERA S. and BERTRANG G.H.-M.

Abstract (from CDS):

Context. The role of magnetic fields in the process of star formation is a matter of continuous debate. Clear observational proof of the general influence of magnetic fields on the early phase of cloud collapse is still pending. In an earlier study on Bok globules with simple structures, we find strong indications of dominant magnetic fields across large spatial scales.
Aims. The aim of this study is to test the magnetic field influence across Bok globules with more complex density structures.
Methods. We apply near-infrared polarimetry to trace the magnetic field structure on scales of 104-105au (∼0.05-0.5pc) in selected Bok globules. The combination of these measurements with archival data in the optical and sub-mm wavelength range allows us to characterize the magnetic field on scales of 103-106au (∼0.005-5pc).
Results. We present polarimetric data in the near-infrared wavelength range for the three Bok globules CB34, CB56, and [OMK2002]18, combined with archival polarimetric data in the optical wavelength range for CB34 and CB56, and in the submillimeter wavelength range for CB34 and [OMK2002]18. We find a strong polarization signal (P≥2%) in the near-infrared for all three globules. For CB34, we detect a connection between the structure on scales of 104-105au (∼0.05-0.5pc) to 105-106au (∼0.5-5pc). For CB56, we trace aligned polarization segments in both the near-infrared and optical data, suggesting a connection of the magnetic field structure across the whole globule. In the case of [OMK2002]18, we find ordered polarization structures on scales of 104-105au (∼0.05-0.5pc).
Conclusions. We find strongly aligned polarization segments on large scales which indicate dominant magnetic fields across Bok globules with complex density structures. To reconcile our findings in globules, the lowest mass clouds known, and the results on intermediate (e.g. Taurus) and more massive (e.g. Orion) clouds, we postulate a mass-dependent role of magnetic fields, whereby magnetic fields appear to be dominant on low and high mass but rather subdominant on intermediate mass clouds.

Abstract Copyright: © ESO 2018

Journal keyword(s): magnetic fields - polarization - stars: formation - stars: low-mass - ISM: clouds - instrumentation: polarimeters

VizieR on-line data: <Available at CDS (J/A+A/618/A163): cb34.dat cb56.dat omk.dat>

Status at CDS : All or part of tables of objects will not be ingested in SIMBAD.

Simbad objects: 14

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Number of rows : 14
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 CPD-69 177 WD* 03 10 31.0201840720 -68 36 03.381441176 10.757 11.413 11.394 11.47 11.558 DA3.0 244 0
2 [OMK2002] 18a MoC 04 21 56.9 +15 29 47           ~ 3 0
3 IRAS 04191+1523 Y*O 04 22 00.43944 +15 30 21.2148           ~ 193 0
4 [OMK2002] 18b MoC 04 22 01.1 +15 30 17           ~ 3 0
5 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3790 0
6 NAME f-Shaped Filament in Orion Cld 05 35.0 -05 30           ~ 85 0
7 LDN 1641 MoC 05 39.0 -07 00           ~ 446 0
8 [CB88] 34 MoC 05 47 02.3 +21 00 10           ~ 59 0
9 2MASS J07044736-1056174 * 07 04 47.3576438799 -10 56 17.552334305   13.89 13.31     A0V: 8 0
10 [DB2002b] G237.93-6.46 MoC 07 14 36 -25 08.9           ~ 9 0
11 IRAS 07125-2507 LP? 07 14 37.9075879085 -25 13 02.021018985           ~ 4 0
12 IRAS 07125-2503 * 07 14 42.3239766236 -25 09 16.435002563           ~ 6 0
13 HD 64299 * 07 52 25.5094669434 -23 17 46.749151162   10.27 10.11     A1V 30 0
14 LDN 57 DNe 17 22 38.2 -23 49 34           ~ 290 1

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2021.10.27-06:48:11

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