Faraday Tomography of the SS433 Jet Termination Region

Sakemi, Haruka; Machida, Mami; Ohmura, Takafumi; Ideguchi, Shinsuke; Miyashita, Yoshimitsu; Takahashi, Keitaro; Akahori, Takuya; Akamatsu, Hiroki; Nakanishi, Hiroyuki; Kurahara, Kohei; Farnes, J. S.

doi:10.3390/galaxies6040137

Cited by 5 publications

(2 citation statements)

References 17 publications

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“…SS 433 is a (so far) unique Galactic object consisting of a stellar jet protruding through the SNR W50. Haruka Sakemi obtained ATCA observations at 2.3 − 3.0 GHz of SS 433 and showed that there is a strong polarized filament behind the SS 433 jet head, and weaker filaments behind it possibly indicating a helical magnetic field [41]. Faraday Tomography reveals a complex pattern of Faraday depth components from 0 to ∼ 300 rad m −2 .…”

Section: Magnetic Fields In Galactic Objectsmentioning

confidence: 99%

Workshop Summary “The Power of Faraday Tomography”

2019

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Section: Magnetic Fields In Galactic Objectsmentioning

confidence: 99%

Workshop Summary “The Power of Faraday Tomography”

2019

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“…In addition, while modern radio polarimetry adopts Faraday tomography to estimate RM (e.g., Van Eck et al 2017;Sakemi et al 2018, Cantwell et al 2020), DING's effects on Faraday dispersion function (FDF) is not paid much attention (Kim et al 2016). Clarification of DING's effects is crucial for exploring galactic (Sun et al 2008;Oppermann et al 2012;Akahori et al 2013;Xu & Han 2014a;Hutschenreuter et al 2021) and intergalactic (Akahori & Ryu 2010;Akahori & Ryu 2011;Hammond et al 2012;Vernstrom et al 2019;O'Sullivan et al 2020) magnetic fields with future large surveys.…”

Section: Introductionmentioning

confidence: 99%

Effects of depolarizing intervening galaxies on background radio emission. I. Global disk magnetic field

Omae

Akahori

Machida

2022

Publications of the Astronomical Society of Japan

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External galaxies often intervene in front of background radio sources such as quasars and radio galaxies. Linear polarization of the background emission is depolarized by Faraday rotation of inhomogeneous magnetized plasma of the intervening galaxies. Exploring the depolarizing intervening galaxies (DINGs) can be a powerful tool to investigate the cosmological evolution of the galactic magnetic field. In this paper, we investigate the effects of DINGs on background radio emission using theoretical DING models. We find that complex structures of galaxy result in complicated depolarization features and Faraday dispersion functions (FDFs), but, for the features of depolarizations and FDFs, the global component of magnetic fields is important. We show the simplest results with ring magnetic field in the galactic disk. We find that the degree of depolarization significantly depends on the inclination angle and the impact parameter of the DING. We found that the larger the standard deviation, the more likely it is that depolarization will occur. The FDF represents the rotation measure (RM) structure within the beam. The FDF exhibits multi-components due mainly to the RM structure within the beam and the fraction of the DING that covers the background emission (the filling factor). The peak Faraday depth of the FDF is different from the beam-averaged RM of the DING. The Monte Carlo simulations indicate that a DING’s contribution to the standard deviation of observed RMs follows σRM ∝ 1/(1 + z)k with k ∼ 2.7 and exhibits a steeper redshift dependence than the wavelength squared. DINGs will have a significant impact on RM catalogs created by future survey projects such as the Square Kilometer Array (SKA) and SKA Precursor/Pathfinder.

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Introduction to Faraday tomography and its future prospects

Takahashi

2023

Publications of the Astronomical Society of Japan

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Faraday tomography is a new method of the study of cosmic magnetic fields enabled by broad-band low-frequency radio observations. Using Faraday tomography it is possible to obtain the Faraday dispersion function, which contains information on the line-of-sight distributions of magnetic fields, thermal electron density, and cosmic ray electron density by measuring the polarization spectrum from a source of synchrotron radiation over a wide band. Furthermore, by combining it with two-dimensional imaging, Faraday tomography allows us to explore the three-dimensional structure of polarization sources. Faraday tomography has been active over the last 20 years, since the broad-band observation has become technically feasible, and polarization sources such as interstellar space, supernova remnants, and galaxies have been investigated. However, the Faraday dispersion function is mathematically the Fourier transform of the polarization spectrum. And since the observable band is finite, it is impossible to obtain a complete Faraday dispersion function by performing a Fourier transform. For this purpose, various methods have been developed to accurately estimate the Faraday dispersion function from the observed polarization spectrum. In addition, the Faraday dispersion function does not directly reflect the distribution of magnetic field, thermal electron density, and cosmic ray electron density in the physical space, and its physical interpretation is not straightforward. Despite these two difficult problems, Faraday tomography is attracting much attention because it has great potential as a new method for studying cosmic magnetic fields and magnetized plasmas. In particular, the next-generation radio telescope SKA (Square Kilometre Array) is capable of polarization observation with unprecedented sensitivity and broad bands, and the application of Faraday tomography is expected to make dramatic progress in the field of cosmic magnetic fields. In this review, we explain the basics of Faraday tomography with simple and instructive examples. Representative algorithms to realize Faraday tomography are introduced, and some applications are shown.

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Faraday Tomography of the SS433 Jet Termination Region

Cited by 5 publications

References 17 publications

Workshop Summary “The Power of Faraday Tomography”

Workshop Summary “The Power of Faraday Tomography”

Effects of depolarizing intervening galaxies on background radio emission. I. Global disk magnetic field

Introduction to Faraday tomography and its future prospects

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