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Radio Properties of High-Redshift Galaxies at \(\boldsymbol{z\geq 1}\)

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Abstract

Study of high-redshift radio galaxies (HzRGs) can shed light on the active galactic nuclei (AGNs) evolution in massive elliptical galaxies. The vast majority of observed high-redshift AGNs are quasars, and there are very few radio galaxies at redshifts \(z>3\). We present the radio properties of 173 sources optically identified with radio galaxies at \(z\geq 1\) with flux densities \(S_{1.4}\geq 20\) mJy. Literature data were collected for compilation of broadband radio spectra, estimation of radio variability, radio luminosity, and radio loudness. Almost 60\(\%\) of the galaxies have steep or ultra-steep radio spectra; 22\(\%\) have flat, inverted, upturn, and complex spectral shapes, and 18\(\%\) have peaked spectra (PS). The majority of the PS sources in the sample (20/31) are megahertz-peaked spectrum source candidates, i.e. possibly very young and compact radio galaxies. The median values of the variability indices at 11 and 5 GHz are \(V_{S_{11}}=0.14\) and \(V_{S_{5}}=0.13\), which generally indicates a weak or moderate character of the long-term variability of the studied galaxies. The typical radio luminosity and radio loudness are \(L_{5}=10^{43}{-}10^{44}\) erg s\({}^{-1}\) and \(\log R=3{-}4\) respectively. We have found less prominent features of the bright compact radio cores in our sample compared to high-redshift quasars at \(z\geq 3\). The variety of the obtained radio properties shows the different conditions for the formation of radio emission sources in galaxies.

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Notes

  1. http://www.askanastronomer.co.uk/brats/

  2. Determined in assumption of the power law relation between the flux density \(S_{\nu}\) at a frequency \(\nu\) and the spectral index \(\alpha\): \(S_{\nu}\sim\nu^{\alpha}\).

  3. Astronomical CATalogs support System (http:// cats.sao.ru).

  4. NASA/IPAC Extragalactic Database (http://ned.ipac. caltech.edu).

  5. http://www.sdss.org

  6. https://vizier.u-strasbg.fr/viz-bin/VizieR

  7. https://astroquery.readthedocs.io

  8. http://www.sdss.org/dr13/data_access/bulk/

  9. The average spectra were approximated by parabolas, and then we calculated the spectral index as a derivative at a given frequency.

  10. http://astrogeo.org

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ACKNOWLEDGMENTS

A part of the observed data was obtained with the RATAN-600 scientific facility. Observations with the SAO RAS telescopes are supported by the Ministry of Science and Higher Education of the Russian Federation. The renovation of telescope equipment is currently provided within the national project ‘‘Science and Universities.’’ This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; the CATS data base, available on the Special Astrophysical Observatory website.

Funding

The work was performed as part of the SAO RAS government contract approved by the Ministry of Science and Higher Education of the Russian Federation.

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Authors and Affiliations

  1. Special Astrophysical Observatory, Russian Academy of Sciences, 369167, Nizhnii Arkhyz, Russia

    M. L. Khabibullina, A. G. Mikhailov, Yu. V. Sotnikova, T. V. Mufakharov, M. G. Mingaliev, A. A. Kudryashova, N. N. Bursov, V. A. Stolyarov & R. Y. Udovitskiy

  2. Kazan (Volga Region) Federal University, 420008, Kazan, Russia

    Yu. V. Sotnikova, T. V. Mufakharov & M. G. Mingaliev

  3. Institute of Applied Astronomy, Russian Academy of Sciences, 191187, St. Petersburg, Russia

    M. G. Mingaliev

  4. Astrophysics Group, Cavendish Laboratory, University of Cambridge, CB3 0HE, Cambridge, UK

    V. A. Stolyarov

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  1. M. L. Khabibullina
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  2. A. G. Mikhailov
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  3. Yu. V. Sotnikova
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Correspondence to M. L. Khabibullina.

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Khabibullina, M.L., Mikhailov, A.G., Sotnikova, Y.V. et al. Radio Properties of High-Redshift Galaxies at \(\boldsymbol{z\geq 1}\). Astrophys. Bull. 78, 443–463 (2023). https://doi.org/10.1134/S1990341323700190

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  • DOI: https://doi.org/10.1134/S1990341323700190

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