Multifrequency study of a new Hybrid Morphology Radio Source

Gasperin, F. de

doi:10.1093/mnras/stx210

Cited by 7 publications

(1 citation statement)

References 35 publications

(39 reference statements)

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“…It was classified as an FRI for this reason in Chiaberge et al (1999). It is an example of a hybrid morphology radio source (HyMoRS Gopal-Krishna & Wiita 2000a;Gawronski et al 2006;de Gasperin 2017).…”

Section: Coma Amentioning

confidence: 99%

The magnetic field strength of the Faraday screen surrounding the radio galaxy Coma A

Knuettel

O’Sullivan

Curiel

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Studying the interaction between AGN jets and lobes and their surrounding environment is important in order to understand how they transfer energy to their environment as well as determining the intrinsic physical properties of the sources themselves. This paper presents broadband VLA polarization and Faraday rotation observations of the radio galaxy Coma A (3C 277.3) from 1 to 4 GHz, including archival VLA observations at 4.9 and 15 GHz. Through broadband polarization model-fitting, we find that an external Faraday screen with a turbulent magnetic field provides an appropriate description to most of the data. By combining the polarization and Faraday rotation results with previous H α observations, we identified the H α-emitting gas as the Faraday screen responsible for the observed Faraday depolarization. We were able to derive the magnetic field strength in the H α-emitting gas, finding typical field strengths of ∼ 1 µG, which is consistent with studies of the intra-group medium local to other radio galaxies. However, we find a highly depolarized region of the southern lobe coincident with a H α filament that has a field strength comparable to the equipartition field strength in the radio lobe (i.e. 36 µG). This implies that the H α filament is internal to the radio emitting plasma. Such clear examples of internal Faraday depolarization are rare, thus providing another key insight into the evolution of radio galaxies and their ability to provide significant feedback on the local gas that would otherwise cool and form stars.

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Section: Coma Amentioning

confidence: 99%

The magnetic field strength of the Faraday screen surrounding the radio galaxy Coma A

Knuettel

O’Sullivan

Curiel

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Search for hybrid morphology radio galaxies from the FIRST survey at 1400 MHz

Kumari

Pal

2022

Monthly Notices of the Royal Astronomical Society

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Hybrid Morphology Radio Sources (HyMoRS) are a very rare subclass of radio galaxies with apparent mixed FR morphology, i.e. these galaxies seem to have an FR-I structure on one side of the core and an FR-II structure on the other side of the core. We systematically searched for HyMoRS using Very Large Array (VLA) Faint Images of the Radio Sky at Twenty-cm (FIRST) survey with 1400 MHz frequency and identified 33 candidate HyMoRS. Our finding significantly increased the known sample size of HyMoRS. HyMoRS may play an essential role in understanding the interaction of jets with the interstellar medium and the much-debated topic of the FR dichotomy. We identified optical counterparts for 29 sources in our catalogue. In our sample of sources, one source (J1106+1355) had quasar-like behaviour. Four sources were BRCLG (Brightest Cluster Galaxies) and six were LRG (Luminous Red Galaxies). We have estimated the spectral index and radio luminosity of HyMoRS in our catalogue, when possible. We found that J1136–0328 was the most luminous source in our sample (log L = 27.01 W Hz−1sr−1). It was also the farthest HyMoRS (with a redshift z = 0.82) in our sample. With the help of a large sample size of discovered sources, various statistical properties of detected galaxies were studied.

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A multiwavelength study of multiple spectral component jets in AGN: testing the IC/CMB model for the large-scale-jet X-ray emission

Breiding

Meyer

Georganopoulos

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Over ∼150 resolved, kpc-scale X-ray jets hosted by active galactic nuclei have been discovered with the Chandra X-ray Observatory. A significant fraction of these jets have an X-ray spectrum either too high in flux or too hard to be consistent with the high-energy extension of the radio-to-optical synchrotron spectrum, a subtype we identify as Multiple Spectral Component (MSC) X-ray jets. A leading hypothesis for the origin of the X-rays is the inverse-Compton scattering of the cosmic microwave background by the same electron population producing the radio-to-optical synchrotron spectrum (known as the IC/CMB model). In this work, we test the IC/CMB model in 45 extragalactic X-ray jets using observations from the Fermi Large Area Telescope to look for the expected high level of gamma-ray emission, utilizing observations from the Atacama Large Millimeter/submillimeter Array (ALMA) and the Hubble Space Telescope (HST) when possible to best constrain the predicted gamma-ray flux. Including this and previous works, we now find the IC/CMB model to be ruled out in a total of 24/45 MSC X-ray jets due to its over-prediction for the observed MeV-to-GeV gamma-ray flux. We present additional evidence against the IC/CMB model, including the relative X-ray-to-radio relativistic beaming in these sources, and the general mismatch between radio and X-ray spectral indexes. Finally, we present upper limits on the large-scale bulk-flow Lorentz factors for all jets based on the Fermi upper limits, which suggest that these jets are at most mildly relativistic.

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Multifrequency study of a new Hybrid Morphology Radio Source

Cited by 7 publications

References 35 publications

The magnetic field strength of the Faraday screen surrounding the radio galaxy Coma A

The magnetic field strength of the Faraday screen surrounding the radio galaxy Coma A

Search for hybrid morphology radio galaxies from the FIRST survey at 1400 MHz

A multiwavelength study of multiple spectral component jets in AGN: testing the IC/CMB model for the large-scale-jet X-ray emission

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