ALMA polarimetry measures magnetically aligned dust grains in the torus of NGC 1068. (arXiv:1905.08802v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Rodriguez_E/0/1/0/all/0/1">Enrique Lopez-Rodriguez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_Herrero_A/0/1/0/all/0/1">Almudena Alonso-Herrero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garcia_Burillo_S/0/1/0/all/0/1">Santiago Garc&#xed;a-Burillo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gordon_M/0/1/0/all/0/1">Michael S. Gordon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ichikawa_K/0/1/0/all/0/1">Kohei Ichikawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Imanishi_M/0/1/0/all/0/1">Masatoshi Imanishi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kameno_S/0/1/0/all/0/1">Seiji Kameno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Levenson_N/0/1/0/all/0/1">Nancy A. Levenson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nikutta_R/0/1/0/all/0/1">Robert Nikutta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Packham_C/0/1/0/all/0/1">Chris Packham</a>

The obscuring structure surrounding active galactic nuclei (AGN) can be
explained as a dust and gas flow cycle that fundamentally connects the AGN with
their host galaxies. This structure is believed to be associated with dusty
winds driven by radiation pressure. However, the role of magnetic fields, which
are invoked in almost all models for accretion onto a supermassive black hole
and outflows, is not thoroughly studied. Here we report the first detection of
polarized thermal emission by means of magnetically aligned dust grains in the
dusty torus of NGC 1068 using ALMA Cycle 4 polarimetric dust continuum
observations ($0.07″$, $4.2$ pc; 348.5 GHz, $860$ $mu$m). The polarized torus
has an asymmetric variation across the equatorial axis with a peak polarization
of $3.7pm0.5$% and position angle of $109pm2^{circ}$ (B-vector) at $sim8$
pc east from the core. We compute synthetic polarimetric observations of
magnetically aligned dust grains assuming a toroidal magnetic field and
homogeneous grain alignment. We conclude that the measured 860 $mu$m continuum
polarization arises from magnetically aligned dust grains in an optically thin
region of the torus. The asymmetric polarization across the equatorial axis of
the torus arises from 1) an inhomogeneous optical depth, and 2) a variation of
the velocity dispersion, i.e. variation of the magnetic field turbulence at
sub-pc scales, from the eastern to the western region of the torus. These
observations and modeling constrain the torus properties beyond spectral energy
distribution results. This study strongly supports that magnetic fields up to a
few pc contribute to the accretion flow onto the active nuclei.

The obscuring structure surrounding active galactic nuclei (AGN) can be
explained as a dust and gas flow cycle that fundamentally connects the AGN with
their host galaxies. This structure is believed to be associated with dusty
winds driven by radiation pressure. However, the role of magnetic fields, which
are invoked in almost all models for accretion onto a supermassive black hole
and outflows, is not thoroughly studied. Here we report the first detection of
polarized thermal emission by means of magnetically aligned dust grains in the
dusty torus of NGC 1068 using ALMA Cycle 4 polarimetric dust continuum
observations ($0.07″$, $4.2$ pc; 348.5 GHz, $860$ $mu$m). The polarized torus
has an asymmetric variation across the equatorial axis with a peak polarization
of $3.7pm0.5$% and position angle of $109pm2^{circ}$ (B-vector) at $sim8$
pc east from the core. We compute synthetic polarimetric observations of
magnetically aligned dust grains assuming a toroidal magnetic field and
homogeneous grain alignment. We conclude that the measured 860 $mu$m continuum
polarization arises from magnetically aligned dust grains in an optically thin
region of the torus. The asymmetric polarization across the equatorial axis of
the torus arises from 1) an inhomogeneous optical depth, and 2) a variation of
the velocity dispersion, i.e. variation of the magnetic field turbulence at
sub-pc scales, from the eastern to the western region of the torus. These
observations and modeling constrain the torus properties beyond spectral energy
distribution results. This study strongly supports that magnetic fields up to a
few pc contribute to the accretion flow onto the active nuclei.

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