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Simultaneous VLBA polarimetric observations of the v=$\{$1,2$\}$ J=1-0 and v=1, J=2-1 SiO maser emission toward VY CMa II: component-level polarization analysis
Solar and Stellar Astrophysics · Submitted 31 May 2016
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Preliminary conclusions based on the current data provide some support for: i) spin-independent solutions for linear polarization; ii) the influence of geometry on the distribution of fractional linear polarization with intensity; and, iii) $\pi/2$ rotations in linear polarization position angle arising from transitions across the Van Vleck angle ($\sin^2{\theta}=2/3$) between the maser line-of-sight and magnetic field.
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This paper presents a component-level comparison of the polarized v=1 J =1-0, v=2 J=1-0 and v=1 J=2-1 SiO maser emission towards the supergiant star VY CMa at milliarcsecond-scale, as observed using the VLBA at $\lambda=7$mm and $\lambda=3$mm. An earlier paper considered overall maser morphology and constraints on SiO maser excitation and pumping derived from these data. The goal of the current paper is to use the measured polarization properties of individual co-spatial components detected across multiple transitions to provide constraints on several competing theories for the transport of polarized maser emission. This approach minimizes the significant effects of spatial blending. We present several diagnostic tests designed to distinguish key features of competing theoretical models for maser polarization. The number of coincident features is limited by sensitivity however, particularly in the v=1 J=2-1 transition at 86 GHz, and deeper observations are needed. Preliminary conclusions based on the current data provide some support for: i) spin-independent solutions for linear polarization; ii) the influence of geometry on the distribution of fractional linear polarization with intensity; and, iii) $\pi/2$ rotations in linear polarization position angle arising from transitions across the Van Vleck angle ($\sin^2{\theta}=2/3$) between the maser line-of-sight and magnetic field. There is weaker evidence for several enumerated non-Zeeman explanations for circular polarization. The expected 2:1 ratio in circular polarization between J=1-0 and J=2-1 predicted by standard Zeeman theory cannot unfortunately be tested conclusively due to insufficient coincident components.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | This paper presents a component-level comparison of the polarized v=1 J =1-0, v=2 J=1-0 and v=1 J=2-1 SiO maser emission towards the supergiant star VY CMa at milliarcsecond-scale, as observed using the VLBA at $\lambda=7$mm and $\lambda=3$mm. | contribution 0.99 | 0.95 | 0.04 | asserted 1.00 |
| s1 | An earlier paper considered overall maser morphology and constraints on SiO maser excitation and pumping derived from these data. | background 1.00 | 0.21 | 0.01 | asserted 0.99 |
| s2 | The goal of the current paper is to use the measured polarization properties of individual co-spatial components detected across multiple transitions to provide constraints on several competing theories for the transport of polarized maser emission. | contribution 0.95 | 0.40 | 0.05 | asserted 0.92 |
| s3 | This approach minimizes the significant effects of spatial blending. | method 0.78 | 0.50 | 0.02 | asserted 1.00 |
| s4 | We present several diagnostic tests designed to distinguish key features of competing theoretical models for maser polarization. | contribution 0.62 | 0.92 | 0.03 | asserted 0.99 |
| s5 | The number of coincident features is limited by sensitivity however, particularly in the v=1 J=2-1 transition at 86 GHz, and deeper observations are needed. | limitation 0.99 | 0.75 | 0.02 | asserted 0.97 |
| s6 | Preliminary conclusions based on the current data provide some support for: i) spin-independent solutions for linear polarization; ii) the influence of geometry on the distribution of fractional linear polarization with intensity; and, iii) $\pi/2$ rotations in linear polarization position angle arising from transitions across the Van Vleck angle ($\sin^2{\theta}=2/3$) between the maser line-of-sight and magnetic field. | interpretation 0.58 | 0.91 | 0.77 | hedged possibility 0.98 |
| s7 | There is weaker evidence for several enumerated non-Zeeman explanations for circular polarization. | result 0.75 | 0.87 | 0.06 | hedged possibility 0.80 |
| s8 | The expected 2:1 ratio in circular polarization between J=1-0 and J=2-1 predicted by standard Zeeman theory cannot unfortunately be tested conclusively due to insufficient coincident components. | limitation 1.00 | 0.62 | 0.06 | asserted 0.77 |
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Original abstract
This paper presents a component-level comparison of the polarized v=1 J =1-0, v=2 J=1-0 and v=1 J=2-1 SiO maser emission towards the supergiant star VY CMa at milliarcsecond-scale, as observed using the VLBA at $\lambda=7$mm and $\lambda=3$mm. An earlier paper considered overall maser morphology and constraints on SiO maser excitation and pumping derived from these data. The goal of the current paper is to use the measured polarization properties of individual co-spatial components detected across multiple transitions to provide constraints on several competing theories for the transport of polarized maser emission. This approach minimizes the significant effects of spatial blending. We present several diagnostic tests designed to distinguish key features of competing theoretical models for maser polarization. The number of coincident features is limited by sensitivity however, particularly in the v=1 J=2-1 transition at 86 GHz, and deeper observations are needed. Preliminary conclusions based on the current data provide some support for: i) spin-independent solutions for linear polarization; ii) the influence of geometry on the distribution of fractional linear polarization with intensity; and, iii) $\pi/2$ rotations in linear polarization position angle arising from transitions across the Van Vleck angle ($\sin^2{\theta}=2/3$) between the maser line-of-sight and magnetic field. There is weaker evidence for several enumerated non-Zeeman explanations for circular polarization. The expected 2:1 ratio in circular polarization between J=1-0 and J=2-1 predicted by standard Zeeman theory cannot unfortunately be tested conclusively due to insufficient coincident components.
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What it cites · 12 sentences without a confident label
Cites as background 2 papers
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The theory of polarized maser emission in this regime has been investigated in series of papers by Elitzur [ref] , and by Watson and collaborators [ref] .
Theory and Extragalactic Masers · SiO maser polarisation theory · 0.99
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Circular polarisation observations of H$_2$O masers have also been used to derive mangetic field estimates in the circumstellar envelopes of late-type evolved stars [ref] , in protoplanetary nebulae [ref] , and in the so-called water-fountain jet sources [ref] .
Hidden bipolarity in red supergiant winds · Introduction · 0.90
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