Tracing the magnetic field and other properties of G351.417+0.645 at subarcsecond scales with the Long Baseline Array

T. Chanapote, K. Asanok, R. Dodson, M. Rioja, J. A. Green, B. Hutawarakorn Kramer

Research output: Contribution to journalArticle

Abstract

We present the results from the Australian Long Baseline Array (LBA) observations of the ground-and excited-state OH masers (1.7- and 6.0-Gllz lines) at high spatial and velocity resolution towards the high-mass star-forming region G351.417+0.645. We obtained accurate spatial gradient magnetic fields from 21 and 23 Zeeman pairs at ground and excited states, respectively, providing magnetic field measurements between -6.4 and +4.4 mG, In addition, we verify the reliability of magnetic field strengths measured from previous lower resolution observations. We found that OH maser features at 1665- and 6035-MHz reveal the same trend of a reversal of magnetic field which we attribute, based on recent infrared observations to cloud fragmentation. In comparison with previous LBA observations 11 yr prior, we identify several matched Zeeman pairs. We found no significant changes of magnetic field strengths, directions, or radial velocities from the matched Zeeman pairs between these two epochs (although there were small internal proper motions). This implies quite stable physical conditions in this region, Moreover, we also analysed the physical conditions from the coincidence of OH maser features from different transitions based on current OH maser models

Original languageEnglish
Pages (from-to)1670-1689
Number of pages20
JournalMonthly Notices of the Royal Astronomical Society
Volume482
Issue number2
DOIs
Publication statusPublished - Jan 2019

Cite this

Chanapote, T. ; Asanok, K. ; Dodson, R. ; Rioja, M. ; Green, J. A. ; Kramer, B. Hutawarakorn. / Tracing the magnetic field and other properties of G351.417+0.645 at subarcsecond scales with the Long Baseline Array. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 482, No. 2. pp. 1670-1689.
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abstract = "We present the results from the Australian Long Baseline Array (LBA) observations of the ground-and excited-state OH masers (1.7- and 6.0-Gllz lines) at high spatial and velocity resolution towards the high-mass star-forming region G351.417+0.645. We obtained accurate spatial gradient magnetic fields from 21 and 23 Zeeman pairs at ground and excited states, respectively, providing magnetic field measurements between -6.4 and +4.4 mG, In addition, we verify the reliability of magnetic field strengths measured from previous lower resolution observations. We found that OH maser features at 1665- and 6035-MHz reveal the same trend of a reversal of magnetic field which we attribute, based on recent infrared observations to cloud fragmentation. In comparison with previous LBA observations 11 yr prior, we identify several matched Zeeman pairs. We found no significant changes of magnetic field strengths, directions, or radial velocities from the matched Zeeman pairs between these two epochs (although there were small internal proper motions). This implies quite stable physical conditions in this region, Moreover, we also analysed the physical conditions from the coincidence of OH maser features from different transitions based on current OH maser models",
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Tracing the magnetic field and other properties of G351.417+0.645 at subarcsecond scales with the Long Baseline Array. / Chanapote, T.; Asanok, K.; Dodson, R.; Rioja, M.; Green, J. A.; Kramer, B. Hutawarakorn.

In: Monthly Notices of the Royal Astronomical Society, Vol. 482, No. 2, 01.2019, p. 1670-1689.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Tracing the magnetic field and other properties of G351.417+0.645 at subarcsecond scales with the Long Baseline Array

AU - Chanapote, T.

AU - Asanok, K.

AU - Dodson, R.

AU - Rioja, M.

AU - Green, J. A.

AU - Kramer, B. Hutawarakorn

PY - 2019/1

Y1 - 2019/1

N2 - We present the results from the Australian Long Baseline Array (LBA) observations of the ground-and excited-state OH masers (1.7- and 6.0-Gllz lines) at high spatial and velocity resolution towards the high-mass star-forming region G351.417+0.645. We obtained accurate spatial gradient magnetic fields from 21 and 23 Zeeman pairs at ground and excited states, respectively, providing magnetic field measurements between -6.4 and +4.4 mG, In addition, we verify the reliability of magnetic field strengths measured from previous lower resolution observations. We found that OH maser features at 1665- and 6035-MHz reveal the same trend of a reversal of magnetic field which we attribute, based on recent infrared observations to cloud fragmentation. In comparison with previous LBA observations 11 yr prior, we identify several matched Zeeman pairs. We found no significant changes of magnetic field strengths, directions, or radial velocities from the matched Zeeman pairs between these two epochs (although there were small internal proper motions). This implies quite stable physical conditions in this region, Moreover, we also analysed the physical conditions from the coincidence of OH maser features from different transitions based on current OH maser models

AB - We present the results from the Australian Long Baseline Array (LBA) observations of the ground-and excited-state OH masers (1.7- and 6.0-Gllz lines) at high spatial and velocity resolution towards the high-mass star-forming region G351.417+0.645. We obtained accurate spatial gradient magnetic fields from 21 and 23 Zeeman pairs at ground and excited states, respectively, providing magnetic field measurements between -6.4 and +4.4 mG, In addition, we verify the reliability of magnetic field strengths measured from previous lower resolution observations. We found that OH maser features at 1665- and 6035-MHz reveal the same trend of a reversal of magnetic field which we attribute, based on recent infrared observations to cloud fragmentation. In comparison with previous LBA observations 11 yr prior, we identify several matched Zeeman pairs. We found no significant changes of magnetic field strengths, directions, or radial velocities from the matched Zeeman pairs between these two epochs (although there were small internal proper motions). This implies quite stable physical conditions in this region, Moreover, we also analysed the physical conditions from the coincidence of OH maser features from different transitions based on current OH maser models

KW - masers

KW - polarization

KW - methods: data analysis

KW - astrometry

KW - ISM: kinematics and dynamics

KW - ISM: magnetic fields

KW - STAR-FORMING-REGIONS

KW - INTERSTELLAR HYDROXYL MASERS

KW - OH MASERS

KW - PHYSICAL CONDITIONS

KW - METHANOL MASERS

KW - POLARIZATION

KW - DIAGNOSTICS

KW - EMISSION

KW - MHZ

KW - 1720-MHZ

U2 - 10.1093/mnras/sty2767

DO - 10.1093/mnras/sty2767

M3 - Article

VL - 482

SP - 1670

EP - 1689

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 2

ER -