# Linear polarization of submillimetre masers. Tracing magnetic fields with ALMA

@article{PerezSanchez2013LinearPO,
title={Linear polarization of submillimetre masers. Tracing magnetic fields with ALMA},
author={A. F. P'erez-S'anchez and Wouter H. T. Vlemmings},
journal={Astronomy and Astrophysics},
year={2013},
volume={551}
}
• Published 4 January 2013
• Physics
• Astronomy and Astrophysics
Context. Once ALMA full polarization capabilities are offered, it will become possible to perform detailed studies of polarized maser emission towards star-forming regions and late-type stars, such as ( post-) asymptotic giant branch stars and young planetary nebulae. To derive the magnetic field orientation from maser linear polarization, a number of conditions involving the rate of stimulated emission R, the decay rate of the molecular state Gamma, and the Zeeman frequency g Omega need to be…
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## References

SHOWING 1-10 OF 64 REFERENCES
Full polarization study of SiO masers at 86 GHz
• Physics
• 2006
Aims. We study the polarization of the SiO maser emission in a representative sample of evolved stars in order to derive an estimate of the strength of the magnetic field, and thus determine the
MAGNETIC FIELDS IN EVOLVED STARS: IMAGING THE POLARIZED EMISSION OF HIGH-FREQUENCY SiO MASERS
• Physics, Geology
• 2011
We present Submillimeter Array observations of high-frequency SiO masers around the supergiant VX Sgr and the semi-regular variable star W Hya. The J = 5–4, v = 128SiO and v = 029SiO masers of VX Sgr
Imaging the Magnetic Field in the Atmosphere of TX Camelopardalis
• Physics
• 1997
Recent advances in very long baseline interferometry (VLBI) allow full interferometric imaging, in both linear and circular polarization, of the 43 GHz SiO maser emission in the immediate
MULTI-EPOCH IMAGING POLARIMETRY OF THE SiO MASERS IN THE EXTENDED ATMOSPHERE OF THE MIRA VARIABLE TX CAM
• Physics
• 2009
We present a time series of synoptic images of the linearly polarized v = 1,  J = 1–0 SiO maser emission toward the Mira variable, TX Cam. These data comprise 43 individual epochs at an approximate
The magnetic field around late-type stars revealed by the circumstellar H2O masers
• Physics, Geology
• 2005
Through polarization observations, circumstellar masers are excellent probes of the magnetic field in the envelopes of late-type stars. Whereas observations of the polarization of the SiO masers
Linearly polarized radiation from astrophysical masers due to magnetic fields of intermediate strength
• Physics
• 1990
Previous solutions for polarization of astrophysical maser radiation due to closed-shell molecules in a magnetic field have potentially serious limitations. These solutions are mostly based on the
Observational evidence for the shrinking of bright maser spots
• Physics, Environmental Science
• 2011
Context. The nature of maser emission means that the apparent angular size of an individual maser spot is determined by the local amplification process as well as by the instrinsic size of the
183 GHz H2O MASER EMISSION AROUND THE LOW-MASS PROTOSTAR SERPENS SMM1
• Physics
• 2009
We report the first interferometric detection of 183 GHz water emission in the low-mass protostar Serpens SMM1 using the Submillimeter Array with a resolution of 3″ and rms of ∼7 Jy in a 3 km s−1
The magnetic field in the star-forming region Cepheus A. from H_2O maser polarization observations
• Physics
• 2005
We present linear and circular polarization observations of the H 2 O masers in 4 distinct regions spread over 1 $\times$ 2 arcsec around the HW2 high-mass young stellar object in the Cepheus A
A Non-Zeeman Interpretation for Polarized Maser Radiation and the Magnetic Field at the Atmospheres of Late-Type Giants
• Physics
• 1998
The linear polarization that is observed, together with likely changes in the orientation of the magnetic field along the line of sight and hence of the optical axes of the medium, can lead to the