Faraday tomography of the local interstellar medium with LOFAR: Galactic foregrounds towards IC 342∗
Journal article, 2017
Magnetic fields pervade the interstellar medium (ISM), but are difficult to detect and characterize. The new generation of low-frequency radio telescopes, such as the Low Frequency Array (LOFAR: a Square Kilometre Array-low pathfinder), provides advancements in our capability of probing Galactic magnetism through low-frequency polarimetry. Maps of diffuse polarized radio emission and the associated Faraday rotation can be used to infer properties of, and trace structure in, the magnetic fields in the ISM. However, to date very little of the sky has been probed at high angular and Faraday depth resolution. We observed a 5° by 5° region centred on the nearby galaxy IC 342 (ℓ = 138.2°,b = + 10.6°) using the LOFAR high-band antennae in the frequency range 115-178 MHz. We imaged this region at 4′.5x3′.84.5 × 3.8 resolution and performed Faraday tomography to detect foreground Galactic polarized synchrotron emission separated by Faraday depth (different amounts of Faraday rotation). Our Faraday depth cube shows a rich polarized structure, with up to 30 K of polarized emission at 150 MHz. We clearly detect two polarized features that extend over most of the field, but are clearly separated in Faraday depth. Simulations of the behaviour of the depolarization of Faraday-thick structures at such low frequencies show that such structures would be too strongly depolarized to explain the observations. These structures are therefore rejected as the source of the observed polarized features. Only Faraday thin structures will not be strongly depolarized at low frequencies; producing such structures requires localized variations in the ratio of synchrotron emissivity to Faraday depth per unit distance. Such variations can arise from several physical phenomena, such as a transition between regions of ionized and (mostly) neutral gas. We conclude that the observed polarized emission is Faraday thin, and propose that the emission originates from two mostly neutral clouds in the local ISM. Using maps of the local ISM to estimate distances to these clouds, we have modelled the Faraday rotation for this line of sight and estimated that the strength of the line of sight component of magnetic field of the local ISM for this direction varies between-0.86 and+0.12 μG (where positive is towards the Earth). We propose that this may be a useful method for mapping magnetic fields within the local ISM in all directions towards nearby neutral clouds.
Show more
Polarization
ISM: clouds
Radio continuum: ISM
Local insterstellar matter
ISM: magnetic fields
Author
C.L. Van Eck
Radboud University
M. Haverkorn
Radboud University
M.I.R. Alves
University of Toulouse
R. Beck
Max Planck Society
A. G. de Bruyn
University of Groningen
Netherlands Institute for Radio Astronomy (ASTRON)
T.A. Enßlin
Max Planck Society
Ludwig Maximilian University of Munich (LMU)
J.S. Farnes
Radboud University
K. Ferriere
University of Toulouse
G. Heald
University of Groningen
Commonwealth Scientific and Industrial Research Organisation (CSIRO)
Cathy Horellou
Chalmers, Earth and Space Sciences, Radio Astronomy and Astrophysics
A. Horneffer
Max Planck Society
M. Iacobelli
Netherlands Institute for Radio Astronomy (ASTRON)
V. Jelić
Netherlands Institute for Radio Astronomy (ASTRON)
Ruder Boskovic Institute
Ivan Marti-Vidal
Chalmers, Earth and Space Sciences, Onsala Space Observatory
D.D. Mulcahy
University of Manchester
W. Reich
Max Planck Society
H. Rottgering
Leiden University
A. Scaife
University of Manchester
D.H.F.M. Schnitzeler
Max Planck Society
C. Sobey
Netherlands Institute for Radio Astronomy (ASTRON)
Commonwealth Scientific and Industrial Research Organisation (CSIRO)
Curtin University
S. S. Sridhar
University of Groningen
Netherlands Institute for Radio Astronomy (ASTRON)
Published in
Astronomy and Astrophysics
0004-6361 (ISSN) 1432-0746 (eISSN)
Vol. 597 p. A98- art. no A98Categorizing
Subject Categories (SSIF 2011)
Astronomy, Astrophysics and Cosmology
Infrastructure
Onsala Space Observatory
Identifiers
DOI
10.1051/0004-6361/201629707