The relationship between radio power at 22 and 43 GHz and black hole properties of AGN in elliptical galaxies

Songyoun Park, Bong Won Sohn, Sukyoung K. Yi

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9 Citations (Scopus)

Abstract

We investigate the relationship between radio power and properties related to active galactic nuclei (AGNs). Radio power at 1.4 or 5 GHz, which has been used in many studies, can be affected by synchrotron self-absorption and free-free absorption in a dense region. On the other hand, these absorption effects get smaller at higher frequencies. Thus, we performed simultaneous observations at 22 and 43 GHz using the Korean VLBI Network (KVN) radio telescope based on a sample of 305 AGN candidates residing in elliptical galaxies from the overlap between the Sloan Digital Sky Survey (SDSS) Data Release 7 and Faint Images of the Radio Sky at Twenty-Centimeters (FIRST). About 37% and 22% of the galaxies are detected at 22 and 43 GHz, respectively. Assuming no flux variability between the FIRST and KVN observations, spectral indices were derived from FIRST and KVN data and we found that over 70% of the detected galaxies have flat or inverted spectra, implying the presence of optically thick compact regions near the centres of the galaxies. Core radio power does not show a clear dependence on black hole mass at either low (1.4 GHz) or high (22 and 43 GHz) frequencies. However, we found that the luminosity of the [OIII] λ5007 emission line and the Eddington ratio correlate with radio power more closely at high frequencies than at low frequencies. This suggests that radio observation at high frequencies can be an appropriate tool for unveiling the innermost region. In addition, the luminosity of the [OIII] λ5007 emission line and the Eddington ratio can be used as a tracer of AGN activity. Our study suggests a causal connection between high frequency radio power and optical properties of AGNs.

Original languageEnglish
Article numberA80
JournalAstronomy and Astrophysics
Volume560
DOIs
Publication statusPublished - 2013 Dec

Bibliographical note

Funding Information:
We thank the anonymous referee for helpful comments and suggestions. This paper is a result of the collaborative project between Yonsei University and Korea Astronomy and Space Science Institute through DRC program of Korea Research Council of Fundamental Science and Technology (FY 2012). We also acknowledge support from the National Research Foundation of Korea through Doyak Grant (No. 20090078756), the Center for Galaxy Evolution Research Grant (No. 2010-0027910), and S.Y.P. is grateful for support by the International Research & Development Program of the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (MEST) of Korea (Grant number: 2012049606, FY2012). S.K.Y. and B.W.S. both acted as corresponding authors.

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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