Nuclear Luminosities and Radio Loudness of Seyfert Nuclei

By Luis C. Ho, C. Peng. 2001

190 citations recorded by the source corpus.

Historically, Seyfert nuclei have been considered to be radio-quiet active galactic nuclei (AGNs). We question this widely held assumption by showing that the distribution of the radio-to-optical luminosity ratio, R ≡ Lν(6 cm)/Lν(B), when properly measured for the nuclear component, places the majority of type 1 Seyfert nuclei in the category of radio-loud AGNs, defined here as objects with R ≥ 10. This result is further strengthened by strong correlations found between radio power and optical continuum and emission-line luminosities, as has been established previously for more powerful AGNs. We also present a new calibration of the relation between optical continuum and Balmer emission-line luminosities valid in the regime of low-luminosity AGNs.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8f24488b0baae1c0ab9a184e7c14042506298b28

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Citations in the corpus

A Hubble Space Telescope Survey of Extended [O III] λ5007 Å Emission in a Far-Infrared-Selected Sample of Seyfert Galaxies: Results (2003, background): “…nuclear continuum luminosity, as indicated by the correlations between emission line and continuum strength found by several authors (Yee 1980; Shuder 1981; Cid Fernandes et al. 2001; Ho & Peng 2001), one gets that our sample spans about 3 decades in nuclear luminosity (39.2≤ log L([OIII])≤42.2).”
Nuclear Activity in Nearby Galaxies (2008, methodology): “While stellar contamination is certainly a concern, one can take necessary precautions to try to isolate the nuclear emission as much as possible, either through high-resolution imaging (e.g., Ho & Peng 2001; Ravindranath et al. 2001; Peng et al. 2002) or spectral decomposition.”
A New Sample of Low-Mass Black Holes in Active Galaxies (2007, result): “They are roughly consistent with the relation measured for Seyfert galaxies (Ho & Peng 2001), but they are systematically higher than the fiducial relation.”
Accretion states and radio loudness in active galactic nuclei: analogies with X-ray binaries (2006, methodology): “But already Ho & Peng (2001) have shown that the average low-luminosity Seyfert galaxy is more radio-loud than the average ‘radio-loud’ PG quasar if only the nuclear luminosity is considered (i.e. removing the contribution of starlight).”
On the X-ray, optical emission line and black hole mass properties of local Seyfert galaxies ! (2006, background): “On the other hand, some LLAGN show properties which are common to luminous AGN, such as the observed correlations between optical emission lines and ionizing continuum (Ho & Peng 2001) or X-ray emission (Ward et al. 1988; Terashima et al. 2000; Ho et al. 2001).”
Radio Loudness of Active Galactic Nuclei: Observational Facts and Theoretical Implications (2006, methodology): “Therefore, to minimize the related uncertainties, for sources overlapped by samples from Ho & Peng (2001) and Ho (2002), we adopted nuclear luminosities obtained in Ho& Peng from the direct optical measurements and corrected by subtracting the starlight.”
Detailed Structural Decomposition of Galaxy Images (2002, background): “Yet, quantitative investigations of these central sources have often been hampered by the difficulties encountered in separating the faint nucleus from the surrounding bright bulge (see, e.g., Ho 1999; Ho & Peng 2001; Sarzi et al. 2001).”
A Fundamental plane of black hole activity (2003, background): “A link between the disc accretion rate and the generation of relativistic radio jets has been suggested by Willott et al.(1999) for radio galaxies and by Ho & Peng (2001) for Seyfert 1 nuclei, on the basis of the strong observed correlations between radio and optical powers.”
On the Relationship between Radio Emission and Black Hole Mass in Galactic Nuclei (2001, methodology): “M Bfor all the quasars (Schmidt & Green 1983) and for a number of the Seyfert 1 nuclei (Ho & Peng 2001) ; for the bright, variable Seyfert nuclei studied with reverberation mapping, it can be ascertained quite reliably from the published spectrophotometry.”