The OH ground-state masers in W3(OH) - I. Results for 1665 MHz

M. M. Wright; M. D. Gray; P. J. Diamond

doi:10.1111/j.1365-2966.2004.07572.x

The OH ground-state masers in W3(OH) - I. Results for 1665 MHz

M. M. Wright, M. D. Gray, P. J. Diamond

Research output: Contribution to journal › Article › peer-review

Abstract

We present observational data and analysis of the OH masers in the star-forming region W3(OH). The observation was performed with the Very Long Baseline Array in 1996 August. 276 masers have been detected, and from these 83 Zeeman pairs identified, allowing the velocity profile and magnetic field structure of the gas to be determined. The bulk of the masers lies in a north-south distribution that contains a clear velocity gradient and indicates ordered rotation, implying a minimum mass for the central star of ∼8 M ⊙. The proper motions suggest there must be an element of expansion in the rotation - possibly the destruction of a disc is being observed. Deviations from Gaussian line shapes were found to be extremely rare; major deviations exist for just two cases.

Original language	English
Pages (from-to)	1253-1271
Number of pages	18
Journal	Monthly Notices of the Royal Astronomical Society
Volume	350
Issue number	4
DOIs	https://doi.org/10.1111/j.1365-2966.2004.07572.x
Publication status	Published - 1 Jun 2004

Keywords

ISM: molecules
Magnetic fields
Masers
Polarization
Radio lines: ISM
Stars: formation

Access to Document

10.1111/j.1365-2966.2004.07572.x

Cite this

@article{c926117c25374de0845185f6f39806c2,

title = "The OH ground-state masers in W3(OH) - I. Results for 1665 MHz",

abstract = "We present observational data and analysis of the OH masers in the star-forming region W3(OH). The observation was performed with the Very Long Baseline Array in 1996 August. 276 masers have been detected, and from these 83 Zeeman pairs identified, allowing the velocity profile and magnetic field structure of the gas to be determined. The bulk of the masers lies in a north-south distribution that contains a clear velocity gradient and indicates ordered rotation, implying a minimum mass for the central star of ∼8 M ⊙. The proper motions suggest there must be an element of expansion in the rotation - possibly the destruction of a disc is being observed. Deviations from Gaussian line shapes were found to be extremely rare; major deviations exist for just two cases.",

keywords = "ISM: molecules, Magnetic fields, Masers, Polarization, Radio lines: ISM, Stars: formation",

author = "Wright, \{M. M.\} and Gray, \{M. D.\} and Diamond, \{P. J.\}",

year = "2004",

month = jun,

day = "1",

doi = "10.1111/j.1365-2966.2004.07572.x",

language = "English",

volume = "350",

pages = "1253--1271",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "1365-2966",

publisher = "Oxford University Press",

number = "4",

}

TY - JOUR

T1 - The OH ground-state masers in W3(OH) - I. Results for 1665 MHz

AU - Wright, M. M.

AU - Gray, M. D.

AU - Diamond, P. J.

PY - 2004/6/1

Y1 - 2004/6/1

N2 - We present observational data and analysis of the OH masers in the star-forming region W3(OH). The observation was performed with the Very Long Baseline Array in 1996 August. 276 masers have been detected, and from these 83 Zeeman pairs identified, allowing the velocity profile and magnetic field structure of the gas to be determined. The bulk of the masers lies in a north-south distribution that contains a clear velocity gradient and indicates ordered rotation, implying a minimum mass for the central star of ∼8 M ⊙. The proper motions suggest there must be an element of expansion in the rotation - possibly the destruction of a disc is being observed. Deviations from Gaussian line shapes were found to be extremely rare; major deviations exist for just two cases.

AB - We present observational data and analysis of the OH masers in the star-forming region W3(OH). The observation was performed with the Very Long Baseline Array in 1996 August. 276 masers have been detected, and from these 83 Zeeman pairs identified, allowing the velocity profile and magnetic field structure of the gas to be determined. The bulk of the masers lies in a north-south distribution that contains a clear velocity gradient and indicates ordered rotation, implying a minimum mass for the central star of ∼8 M ⊙. The proper motions suggest there must be an element of expansion in the rotation - possibly the destruction of a disc is being observed. Deviations from Gaussian line shapes were found to be extremely rare; major deviations exist for just two cases.

KW - ISM: molecules

KW - Magnetic fields

KW - Masers

KW - Polarization

KW - Radio lines: ISM

KW - Stars: formation

U2 - 10.1111/j.1365-2966.2004.07572.x

DO - 10.1111/j.1365-2966.2004.07572.x

M3 - Article

SN - 1365-2966

VL - 350

SP - 1253

EP - 1271

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

The OH ground-state masers in W3(OH) - I. Results for 1665 MHz

Abstract

Keywords

Access to Document

Fingerprint

Cite this