Hostname: page-component-586b7cd67f-dsjbd Total loading time: 0 Render date: 2024-11-23T02:01:04.382Z Has data issue: false hasContentIssue false
  • English
  • Français

Radio galaxies with and without emission lines

Published online by Cambridge University Press:  29 March 2021

Grażyna Stasińska Open the ORCID record for Grażyna Stasińska [Opens in a new window] ,
Natalia Vale Asari Open the ORCID record for Natalia Vale Asari [Opens in a new window]  and
Dorota Kozieł-Wierzbowska
Grażyna Stasińska
Affiliation:
LUTH, Observatoire de Paris, PSL, CNRS 92190 Meudon, France email: [email protected]
Natalia Vale Asari
Affiliation:
Departamento de Fsica - CFM - Universidade Federal de Santa Catarina, Florianópolis, SC, Brazil
Dorota Kozieł-Wierzbowska
Affiliation:
Astronomical Observatory, Jagiellonian University, ul. Orla 171, PL-30244 Krakow, Poland
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Using the recent ROGUE I catalogue of galaxies with radio cores (Kozie_l-Wierzbowska et al. 2020) and after selecting the objects which are truly radio active galactic nuclei, AGNs, (which more than doubles the samples available so far), we perform a thorough comparison of the properties of radio galaxies with and without optical emission lines (galaxies where the equivalent width of Hα is smaller than 3Å are placed in the last category). We do not find any strong dichotomy between the two classes as regards the radio luminosities or black hole masses. The same is true when using the common classification into high- and low-excitation radio galaxies (HERGs and LERGs respectively).

Keywords

radio continuum: galaxiesgalaxies: activecatalogs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S359: Galaxy Evolution and Feedback across Different Environments , March 2019 , pp. 396 - 401
Copyright
© The Author(s), 2021. Published by Cambridge University Press on behalf of International Astronomical Union

References

Abazajian, K. N., et al. 2009, ApJS, 182, 543 CrossRefGoogle Scholar
Becker, R. H., White, R. L., Helfand, D. J., et al. 1995, ApJ, 450, 559 CrossRefGoogle Scholar
Best, P. N. & Heckman, T. M. 2012, MNRAS, 421, 1569 10.1111/j.1365-2966.2012.20414.xCrossRefGoogle Scholar
Buttiglione, S., Capetti, A., Celotti, A., et al. 2010, A&A, 509, A6 Google Scholar
Cid Fernandes, R., Mateus, A., Sodré, L., et al. 2005, MNRAS, 358, 363 CrossRefGoogle Scholar
Cid Fernandes, R., Stasińska, G., Mateus, A., et al. 2011, MNRAS, 413, 1687 CrossRefGoogle Scholar
Heckman, T. M. & Best, P. N. 2014, ARAA, 52, 589 CrossRefGoogle Scholar
Hine, R. G. & Longair, M. S. 1979, MNRAS, 188, 111 CrossRefGoogle Scholar
Kozieł-Wierzbowska, D., Goyal, A., & Żywucka, N. 2020, ApJS, 247, 53 CrossRefGoogle Scholar
Laing, R. A., Jenkins, C. R., Wall, J. V., et al. 1994, ASPC, 54, 201 Google Scholar
Padovani, P., et al. 2017, AARv, 25, 2 Google Scholar
Pracy, M. B., Ching, J. H. Y., Sadler, E. M., et al. 2016, MNRAS, 460, 2 CrossRefGoogle Scholar
York, D. G., et al. 2000, AJ, 120, 1579 CrossRefGoogle Scholar