Probing the Magnetic Field at Sub-Parsec Radii in the Accretion Disk of NGC 4258

Details Probing the Magnetic Field at Sub-Parsec Radii in the Accretion Disk of NGC 4258 Probing the Magnetic Field at Sub-Parsec Radii in the Accretion Disk of NGC 4258

2005-02-11

arxiv.org/abs/astro-ph/0502240v1

Astrophys.J. 626 (2005) 104-119

Astronomy and Astrophysics

Astrophysics

20 pages, including 10 figures and 2 tables. Accepted for publication in the Astrophysical Journal

Scientific paper

10.1086/429559

We present an analysis of polarimetric observations at 22 GHz of the water vapor masers in NGC 4258 obtained with the VLA and the GBT. We do not detect any circular polarization in the spectrum indicative of Zeeman-induced splitting of the maser lines of water, a non-paramagnetic molecule. We have improved the 1-sigma upper limit estimate on the toroidal component of the magnetic field in the circumnuclear disk of NGC 4258 at a radius of 0.2 pc from 300 mG to 90 mG. We have developed a new method for the analysis of spectra with blended features and derive a 1-sigma upper limit of 30 mG on the radial component of the magnetic field at a radius of 0.14 pc. Assuming thermal and magnetic pressure balance, we estimate an upper limit on the mass accretion rate of ~10^(-3.7) M_sun/yr for a total magnetic field of less than 130 mG. We discuss the ramifications of our results on current maser models proposed to explain the observed maser emission structure and the consequences for current accretion theories. We find from our magnetic field limits that the thin-disk model and the jet-disk model are better candidates for accounting for the extremely low-luminosity nature of NGC 4258, than models that include advection-dominated accretion flows.

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