LeMMINGs III. The e-MERLIN legacy survey of the Palomar sample: exploring the origin of nuclear radio emission in active and inactive galaxies through the [O III] - radio connection - Archive ouverte HAL Access content directly
Journal Articles Monthly Notices of the Royal Astronomical Society Year : 2021

LeMMINGs III. The e-MERLIN legacy survey of the Palomar sample: exploring the origin of nuclear radio emission in active and inactive galaxies through the [O III] - radio connection

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R. D. Baldi
  • Function : Author
D. R. A. Williams
  • Function : Author
R. J. Beswick
  • Function : Author
I. Mchardy
  • Function : Author
B. T. Dullo
  • Function : Author
J. H. Knapen
  • Function : Author
L. Zanisi
  • Function : Author
M. K. Argo
  • Function : Author
S. Aalto
  • Function : Author
A. Alberdi
  • Function : Author
W. A. Baan
  • Function : Author
G. J. Bendo
  • Function : Author
D. M. Fenech
  • Function : Author
D. A. Green
  • Function : Author
H. -R. Klöckner
  • Function : Author
E. Körding
  • Function : Author
T. J. Maccarone
  • Function : Author
J. M. Marcaide
  • Function : Author
I. Mutie
  • Function : Author
F. Panessa
  • Function : Author
M. A. Pérez-Torres
  • Function : Author
C. Romero-Cañizales
  • Function : Author
D. J. Saikia
  • Function : Author
P. Saikia
  • Function : Author
F. Shankar
R. E. Spencer
  • Function : Author
I. R. Stevens
  • Function : Author
P. Uttley
  • Function : Author
E. Brinks
  • Function : Author
I. Martí-Vidal
  • Function : Author
C. G. Mundell
  • Function : Author
M. Pahari
  • Function : Author
M. J. Ward
  • Function : Author

Abstract

What determines the nuclear radio emission in local galaxies? To address this question, we combine optical [O III] line emission, robust black hole (BH) mass estimates, and high-resolution e-MERLIN 1.5-GHz data, from the LeMMINGs survey, of a statistically complete sample of 280 nearby optically active (LINER and Seyfert) and inactive [H II and absorption line galaxies (ALGs)] galaxies. Using [O III] luminosity ($L_{\rm [O\, \small {III}]}$) as a proxy for the accretion power, local galaxies follow distinct sequences in the optical-radio planes of BH activity, which suggest different origins of the nuclear radio emission for the optical classes. The 1.5-GHz radio luminosity of their parsec-scale cores (Lcore) is found to scale with BH mass (MBH) and [O III] luminosity. Below MBH ~ 106.5 M, stellar processes from non-jetted H II galaxies dominate with $L_{\rm core} \propto M_{\rm BH}^{0.61\pm 0.33}$ and $L_{\rm core} \propto L_{\rm [O\, \small {III}]}^{0.79\pm 0.30}$. Above MBH ~ 106.5 M, accretion-driven processes dominate with $L_{\rm core} \propto M_{\rm BH}^{1.5-1.65}$ and $L_{\rm core} \propto L_{\rm [O\, \small {III}]}^{0.99-1.31}$ for active galaxies: radio-quiet/loud LINERs, Seyferts, and jetted H II galaxies always display (although low) signatures of radio-emitting BH activity, with $L_{\rm 1.5\, GHz}rsim 10^{19.8}$ W Hz-1 and MBH ≳ 107 M, on a broad range of Eddington-scaled accretion rates ($\dot{m}$). Radio-quiet and radio-loud LINERs are powered by low-$\dot{m}$ discs launching sub-relativistic and relativistic jets, respectively. Low-power slow jets and disc/corona winds from moderately high to high-$\dot{m}$ discs account for the compact and edge-brightened jets of Seyferts, respectively. Jetted H II galaxies may host weakly active BHs. Fuel-starved BHs and recurrent activity account for ALG properties. In conclusion, specific accretion-ejection states of active BHs determine the radio production and the optical classification of local active galaxies.
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Dates and versions

insu-03642350 , version 1 (15-04-2022)

Licence

Attribution - CC BY 4.0

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R. D. Baldi, D. R. A. Williams, R. J. Beswick, I. Mchardy, B. T. Dullo, et al.. LeMMINGs III. The e-MERLIN legacy survey of the Palomar sample: exploring the origin of nuclear radio emission in active and inactive galaxies through the [O III] - radio connection. Monthly Notices of the Royal Astronomical Society, 2021, 508, pp.2019-2038. ⟨10.1093/mnras/stab2613⟩. ⟨insu-03642350⟩
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