# Performance test of QU-fitting in cosmic magnetism study

@article{Miyashita2018PerformanceTO,
title={Performance test of QU-fitting in cosmic magnetism study},
author={Yoshimitsu Miyashita and Shinsuke Ideguchi and Shouta Nakagawa and Takuya Akahori and Keitaro Takahashi},
journal={Monthly Notices of the Royal Astronomical Society},
year={2018}
}
QU-fitting is a standard model-fitting method to reconstruct distribution of magnetic fields and polarized intensity along a line of sight (LOS) from an observed polarization spectrum. In this paper, we examine the performance of QU-fitting by simulating observations of two polarized sources located along the same LOS, varying the widths of the sources and the gap between them in Faraday depth space, systematically. Markov Chain Monte Carlo (MCMC) approach is used to obtain the best-fit…
4 Citations

## Figures and Tables from this paper

Removing non-physical structure in fitted Faraday rotated signals: Non-parametric QU-fitting
• Physics
Publications of the Astronomical Society of Australia
• 2021
Abstract Next-generation spectro-polarimetric broadband surveys will probe cosmic magnetic fields in unprecedented detail, using the magneto-optical effect known as Faraday rotation. However,
Faraday Dispersion Function of Disk Galaxies with Axisymmetric Global Magnetic Fields. I.
• Physics
• 2019
Faraday tomography is a novel method to probe 3-dimensional structure of magnetic fields of polarized radio sources. In this paper, we investigate Faraday dispersion function (FDF) of disk galaxies
A broad-band spectro-polarimetric view of the NVSS rotation measure catalogue – I. Breaking the nπ-ambiguity
• Y. Ma, +5 authors S. Betti
• Physics
Monthly Notices of the Royal Astronomical Society
• 2019
The NRAO VLA Sky Survey (NVSS) Rotation Measure (RM) catalogue is invaluable for the study of cosmic magnetism. However, the RM values reported in it can be affected by n$\pi$-ambiguity, resulting in
An iterative reconstruction algorithm for Faraday tomography
Faraday tomography offers crucial information on the magnetized astronomical objects, such as quasars, galaxies, or galaxy clusters, by observing its magnetoionic media. The observed linear

## References

SHOWING 1-10 OF 39 REFERENCES
Performance test of RM CLEAN and its evaluation with chi-square value
• Physics
• 2016
RM CLEAN is a standard method to reconstruct the distribution of cosmic magnetic fields and polarized sources along the line of sight (LOS) from observed polarization spectrum. This method is similar
Finding a complex polarized signal in wide-band radio data
We present a new algorithm for fitting and classifying polarized radio sources, which is based on the QU fitting method introduced by O'Sullivan et al. and on our analysis of pulsars. Then we test
Fisher Analysis on Wide-Band Polarimetry for Probing the Intergalactic Magnetic Field
• Physics
• 2014
We investigate the capability of ongoing radio telescopes for probing Faraday rotation measure (RM) due to the intergalactic magnetic field (IGMF) in the large-scale structure of the universe which
INTEGRATED POLARIZATION OF SOURCES AT λ ∼ 1 m AND NEW ROTATION MEASURE AMBIGUITIES
• Physics
• 2011
We present an analysis of the polarization of compact radio sources from six pointings of the Westerbork Synthesis Radio Telescope at 350 MHz with 35% coverage in {lambda}{sup 2}. After correcting
• Physics
• 2014
The Faraday dispersion function (FDF), which can be derived from an observed polarization spec- trum by Faraday rotation measure synthesis, is a profile of polarized emissions as a function of
Comparison of Algorithms for Determination of Rotation Measure and Faraday Structure. I. 1100–1400 MHz
Faraday rotation measures (RMs) and more general Faraday structures are key parameters for studying cosmic magnetism and are also sensitive probes of faint ionized thermal gas. A definition of which
WSRT Faraday tomography of the Galactic ISM at λ ∼ 0.86 m. First results for a field at (l, b)~=~(181°,20°)
• Physics
• 2007
Aims. We investigate the distribution and properties of Faraday rotating and synchrotron emitting regions in the Galactic ISM in the direction of the Galactic anti-centre. Methods. We apply Faraday
We present a detailed study of the Faraday depth structure of four bright (>1 Jy), strongly polarized, unresolved radio-loud quasars. The Australia Telescope Compact Array (ATCA) was used to observe
Study of Vertical Magnetic Field in Face-on Galaxies using Faraday Tomography
Faraday tomography allows astronomers to probe the distribution of magnetic field along the line of sight (LOS), but that can be achieved only after Faraday spectrum is interpreted. However, the
WSRT Faraday tomography of the Galactic ISM at λ ~ 0.86 m. I. The GEMINI data set at (l, b) = (181°, 20°)
• Physics
• 2009
Aims. We investigate the properties of the Galactic ISM by applying Faraday tomography to a radio polarization data set in the direction of the Galactic anti-centre. Methods. We address the problem