Toggle Main Menu Toggle Search

Open Access padlockePrints

High-resolution radio continuum survey of M 33. III Magnetic fields

Lookup NU author(s): Dr Andrew Fletcher


Full text for this publication is not currently held within this repository. Alternative links are provided below where available.


Aims. We study the magnetic field structure, strength, and energy density in the Scd galaxy M 33. Methods. Using the linearly polarized intensity and polarization angle data at 3.6, 6.2 and 20 cm, we determine variations of Faraday rotation and depolarization across M 33. We fit a 3D model of the regular magnetic field to the observed azimuthal distribution of polarization angles. We also analyze the spatial variation of depolarization across the galaxy.Results. Faraday rotation, measured between 3.6 and 6.2 cm at an angular resolution of 3′ (0.7 kpc), shows more variation in the south than in the north of the galaxy. About 10% of the nonthermal emission from M 33 at 3.6 cm is polarized. High degrees of polarization of the synchrotron emission (>20%) and strong regular magnetic fields in the sky plane (≃6.6 μG) exist in-between two northern spiral arms. We estimate the average total and regular magnetic field strengths in M 33 as ≃6.4 and 2.5 μG, respectively. Under the assumption that the disk of M 33 is flat, the regular magnetic field consists of horizontal and vertical components: however the inferred vertical field may be partly due to a galactic warp. The horizontal field is represented by an axisymmetric () mode from 1 to 3 kpc radius and a superposition of axisymmetric and bisymmetric () modes from 3 to 5 kpc radius.Conclusions. An excess of differential Faraday rotation in the southern half together with strong Faraday dispersion in the southern spiral arms seem to be responsible for the north-south asymmetry in the observed wavelength dependent depolarization. The presence of an axisymmetric mode of the regular magnetic field in each ring suggests that a galactic dynamo is operating in M 33. The pitch angles of the spiral regular magnetic field are generally smaller than the pitch angles of the optical spiral arms but are twice as big as simple estimates based on the mean-field dynamo theory and M 33's rotation curve. Generation of interstellar magnetic fields from turbulent gas motion in M 33 is indicated by the equipartition of turbulent and magnetic energy densities. © 2008 ESO.

Publication metadata

Author(s): Tabatabaei FS, Krause M, Fletcher A, Beck R

Publication type: Article

Publication status: Published

Journal: Astronomy and Astrophysics

Year: 2008

Volume: 490

Issue: 3

Pages: 1005-1017

ISSN (print): 0004-6361

ISSN (electronic): 1432-0746

Publisher: EDP Sciences


DOI: 10.1051/0004-6361:200810590


Altmetrics provided by Altmetric


Find at Newcastle University icon    Link to this publication