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Maser Polarization with ALMA

A.F. Pérez-Sánchez ; Wouter Vlemmings (Institutionen för rymd- och geovetenskap, Radioastronomi och astrofysik)
Proceedings of the International Astronomical Union; Cosmic Masers - from OH to Ho (1743-9213). Vol. 8 (2012), S287, p. 64 - 68.
[Konferensbidrag, övrigt]

Once ALMA full polarization capabilities are offered, (sub-)mm polarization studies will enter a new era. It will become possible to perform detailed studies of polarized maser emission towards for example massive star forming regions and late-type stars such as (post-) Asymptotic Giant Branch stars and young Planetary Nebulae. In these environments, SiO, H2O and HCN are molecules that can naturally generate polarized maser emission observable by ALMA. The maser polarization can then be used to derive the strength and morphology of the magnetic field in the masing regions. However, in order to derive, in particular, the magnetic field orientation from maser linear polarization, a number of conditions involving the rate of stimulated emission, molecular state decay and Zeeman splitting need to be satisfied. In this work, we discuss these conditions for the maser transitions in the ALMA frequency range and highlight the optimum transitions to further our understanding of star formation and evolved star magnetic fields.

Nyckelord: masers; polarization; stars: magnetic fields; stars: AGB and post-AGB; stars: formation


Andrés F. Pérez-Sánchez and Wouter Vlemmings (2012). Maser polarization with ALMA. Proceedings of the International Astronomical Union, 8, pp 64-68 doi:10.1017/S1743921312006655



Denna post skapades 2012-10-31. Senast ändrad 2014-09-02.
CPL Pubid: 165337