Multi-scale Magnetic Fields in the Central Molecular Zone: Inference from the Gradient Technique. (arXiv:2105.03605v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Hu_Y/0/1/0/all/0/1">Yue Hu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lazarian_A/0/1/0/all/0/1">A. Lazarian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Q/0/1/0/all/0/1">Q.Daniel Wang</a>
The central molecular zone (CMZ) plays an essential role in regulating the
nuclear ecosystem of our Galaxy. To get an insight into the magnetic fields of
the CMZ, we employ the Gradient Technique (GT), which is rooted in the
anisotropy of magnetohydrodynamic turbulence. Our analysis is based on the data
of multiple wavelengths, including molecular emission lines, radio 1.4 GHz
continuum image, and Herschel 70 um image, as well as ionized [Ne II] and
Paschen-alpha emissions. The results are compared with the observations of
Planck 353 GHz and High-resolution Airborne Wideband Camera Plus (HWAC+) 53 um
polarized dust emissions. We map the wavelength-dependent magnetic field
orientation across the central molecular zone, including close-ups of the Radio
Arc and Sagittarius A West regions, on multi scales from ~0.1 pc to 10 pc. The
magnetic fields towards the central molecular zone traced by GT are globally
compatible with the polarization measurements, accounting for the contribution
from the galactic foreground and background. This correspondence suggests that
the magnetic field and turbulence are dynamically crucial in the galactic
center. We find that the magnetic fields associated with the Arched filaments
and the thermal components of the Radio Arc are in good agreement with the
HAWC+ polarization. Our measurement towards the non-thermal Radio Arc reveals
the poloidal magnetic field components in the galactic center. For Sagittarius
A West region, we find a great agreement between the GT measurement using [Ne
II] emission and HWAC+ 53 um observation. We use GT to predict the magnetic
fields associated with ionized Paschen-alpha gas down to scales of 0.1 pc.
These results demonstrate the potential power of GT in the high-resolution
mapping of magnetic fields and in decomposing contributions from different
velocity components and/or different gas phases.
The central molecular zone (CMZ) plays an essential role in regulating the
nuclear ecosystem of our Galaxy. To get an insight into the magnetic fields of
the CMZ, we employ the Gradient Technique (GT), which is rooted in the
anisotropy of magnetohydrodynamic turbulence. Our analysis is based on the data
of multiple wavelengths, including molecular emission lines, radio 1.4 GHz
continuum image, and Herschel 70 um image, as well as ionized [Ne II] and
Paschen-alpha emissions. The results are compared with the observations of
Planck 353 GHz and High-resolution Airborne Wideband Camera Plus (HWAC+) 53 um
polarized dust emissions. We map the wavelength-dependent magnetic field
orientation across the central molecular zone, including close-ups of the Radio
Arc and Sagittarius A West regions, on multi scales from ~0.1 pc to 10 pc. The
magnetic fields towards the central molecular zone traced by GT are globally
compatible with the polarization measurements, accounting for the contribution
from the galactic foreground and background. This correspondence suggests that
the magnetic field and turbulence are dynamically crucial in the galactic
center. We find that the magnetic fields associated with the Arched filaments
and the thermal components of the Radio Arc are in good agreement with the
HAWC+ polarization. Our measurement towards the non-thermal Radio Arc reveals
the poloidal magnetic field components in the galactic center. For Sagittarius
A West region, we find a great agreement between the GT measurement using [Ne
II] emission and HWAC+ 53 um observation. We use GT to predict the magnetic
fields associated with ionized Paschen-alpha gas down to scales of 0.1 pc.
These results demonstrate the potential power of GT in the high-resolution
mapping of magnetic fields and in decomposing contributions from different
velocity components and/or different gas phases.
http://arxiv.org/icons/sfx.gif
