What Distinguishes the Host Galaxies of Radio-loud and Radio-quiet AGNs?

Kozieł-Wierzbowska, D.; Asari, N. Vale; Stasińska, G.; Sikora, Marek; Goettems, E. I.; Wójtowicz, Anna

doi:10.3847/1538-4357/aa8326

Cited by 14 publications

(15 citation statements)

References 76 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In these galaxies the contribution from H II regions can be neglected. The results for the cleaned samples (see Kozieł-Wierzbowska et al, 2017) confirm our findings for the whole RL and mRQ samples concerning morphological properties. From the comparison of CI and of the b/a ratio we see that there is a difference in morphology between RL and mRQ galaxies.…”

Section: Resultssupporting

confidence: 86%

See 2 more Smart Citations

Pair-Matching of Radio-Loud and Radio-Quiet AGNs

Kozieł-Wierzbowska

Stasińska

Asari

et al. 2017

Front. Astron. Space Sci.

View full text Add to dashboard Cite

Active galactic nuclei (AGNs) are known to cover an extremely broad range of radio luminosities and the spread of their radio-loudness is very large at any value of the Eddington ratio. This implies very diverse jet production efficiencies which can result from the spread of the black hole spins and magnetic fluxes. Magnetic fluxes can be developed stochastically in the innermost zones of accretion discs, or can be advected to the central regions prior to the AGN phase. In the latter case there could be systematic differences between the properties of galaxies hosting radio-loud (RL) and radio-quiet (RQ) AGNs. In the former case the differences should be negligible for objects having the same Eddington ratio. To study the problem we decided to conduct a comparison study of host galaxy properties of RL and RQ AGNs. In this study we selected type II AGNs from SDSS spectroscopic catalogs. Our RL AGN sample consists of the AGNs appearing in the Best and Heckman (2012) catalog of radio galaxies. To compare RL and RQ galaxies that have the same AGN parameters we matched the galaxies in black hole mass, Eddington ratio and redshift. We compared several properties of the host galaxies in these two groups of objects like galaxy mass, color, concentration index, line widths, morphological type and interaction signatures. We found that in the studied group RL AGNs are preferentially hosted by elliptical galaxies while RQ ones are hosted by galaxies of later type. We also found that the fraction of interacting galaxies is the same in both groups of AGNs. These results suggest that the magnetic flux in RL AGNs is advected to the nucleus prior to the AGN phase.

show abstract

Section: Resultssupporting

confidence: 86%

“…The histograms of plotted parameters for RL and RQ galaxies are also shown. Updated version published inKozieł-Wierzbowska et al (2017).…”

mentioning

confidence: 99%

See 1 more Smart Citation

Pair-Matching of Radio-Loud and Radio-Quiet AGNs

Kozieł-Wierzbowska

Stasińska

Asari

et al. 2017

Front. Astron. Space Sci.

View full text Add to dashboard Cite

show abstract

“…We note that this is not what is typically expected, as RQ AGN (at least the ones found at bright > 1 mJy radio fluxes, e.g. see Kozieł-Wierzbowska et al 2017) and SFGs are generally found in lower-mass host galaxies than RL AGN. However, perhaps because of our joint selection based on radio detection and SFR IR estimate, particularly in the higher-redshift bins where most of our sample lies the range of SFRs and thus of stellar masses probed by our sample is limited and biased towards higher values, making it difficult to distinguish different populations.…”

Section: Sfr Vs Stellar Masscontrasting

confidence: 68%

The evolution of the low-frequency radio AGN population to z ≃ 1.5 in the ELAIS N1 field

Ocran

Taylor

Vaccari

et al. 2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We study the cosmic evolution of radio sources out to z ≃ 1.5 using a GMRT 610 MHz survey covering ∼1.86 deg2 of the ELAIS N1 field with a minimum/median rms noise 7.1/19.5 μJy / beam and an angular resolution of 6 arcsec. We classify sources as star forming galaxies (SFGs), radio-quiet (RQ) and radio-loud (RL) Active Galactic Nuclei (AGN) using a combination of multi-wavelength diagnostics and find evidence in support of the radio emission in SFGs and RQ AGN arising from star formation, rather than AGN-related processes. At high luminosities, however, both SFGs and RQ AGN display a radio excess when comparing radio and infrared star formation rates. The vast majority of our sample lie along the $\rm {SFR - M_{\star }}$ ”main sequence” at all redshifts when using infrared star formation rates. We derive the 610 MHz radio luminosity function for the total AGN population, constraining its evolution via continuous models of pure density and pure luminosity evolution with $\rm {\Phi ^{\star }\, \propto \, (\, 1+\, z)^{(2.25\pm 0.38)-(0.63\pm 0.35)z}}$ and $\rm {L_{610\, MHz}\, \propto \, (\, 1+\, z)^{(3.45\pm 0.53)-(0.55\pm 0.29)z}}$ respectively. For our RQ and RL AGN, we find a fairly mild evolution with redshift best fitted by pure luminosity evolution with $\rm {L_{610\, MHz}\, \propto \, (\, 1+\, z)^{(2.81\pm 0.43)-(0.57\pm 0.30)z}}$ for RQ AGN and $\rm {L_{610\, MHz}\, \propto \, (\, 1+\, z)^{(3.58\pm 0.54)-(0.56\pm 0.29)z}}$ for RL AGN. The 610 MHz radio AGN population thus comprises two differently evolving populations whose radio emission is mostly SF-driven or AGN-driven respectively.

show abstract

“…It is widely accepted that the broad range in radio powers (up to 4 decades), sizes (up to Mpc scales), and radio morphologies of jet-ted active galactic nuclei (AGNs) stems from the complex interplay between the jet production efficiency (linked to the properties of accretion flow around the supermassive black hole (SMBH) located at the centers of galaxies), interaction of jets with the host galaxy, and the large scale environment they reside in (see, for a recent review, Padovani et al 2017;Blandford et al 2019). While accretion onto the SMBH has been unequivocally accepted as the main source of AGN activity, it is not clear what fraction of it is channeled as kinetic energy of a jet as the majority of the optically selected galaxies and their high luminosity counterparts, quasars, do not show significant radio activity (see Baloković et al 2012;Kozie l-Wierzbowska et al 2017, and references therein). Moreover, the energy exchange between the evolving radio source and the interstellar/intergalactic medium on small as well as large scales forms an important part of the feedback that governs the co-evolution of galaxies, central SMBH, and galaxy groups/clusters over cosmological timescales (see, for a review, McNamara & Nulsen 2007;Fabian 2012).…”

Section: Introductionmentioning

confidence: 99%

Radio Sources Associated with Optical Galaxies and Having Unresolved or Extended Morphologies (ROGUE). I. A Catalog of SDSS Galaxies with FIRST Core Identifications

Kozieł-Wierzbowska

Goyal

Żywucka

2020

ApJS

Self Cite

View full text Add to dashboard Cite

We present the catalog of Radio sources associated with Optical Galaxies and having Unresolved or Extended morphologies I (ROGUE I), consisting of 32,616 spectroscopically selected galaxies. It is the largest handmade catalog of this kind, obtained by cross-matching galaxies from the Sloan Digital Sky Survey (SDSS) Data Release 7 and radio sources from both the First Images of Radio Sky at Twenty Centimetre (FIRST) survey and the NRAO VLA Sky Survey without imposing a limit to the radio flux densities. The catalog provides a visual classification of radio and optical morphologies of galaxies presenting a FIRST core within 3 of the optical position. The radio morphological classification is performed by examining the radio-optical overlays of linear sizes equal to 1 Mpc at the source distance, while the 120 image snapshots from the SDSS database are used for optical classification. The results of our search are: (i) singlecomponent unresolved and elongated, radio sources constitute the major group in the ROGUE I catalog (∼90%), and ∼8% exhibiting extended morphologies, (ii) samples of 269, 730, and 115 Fanaroff-Riley (FR) type I, II, and hybrid galaxies, respectively, are presented (iii) we report 55 newly discovered giant/possible giant, 16 double-double, 9 X-shaped, and 25 Z-shaped radio sources, (iv) on the optical front, most galaxies have elliptical morphologies (∼62%) while spirals form the second major category (∼17%) followed by distorted (∼ 12%) and lenticular (∼7%) morphologies, (v) division between the FR I and the FR II sources in the radio-optical luminosity plane is blurred, in tune with recent studies.

show abstract

What Distinguishes the Host Galaxies of Radio-loud and Radio-quiet AGNs?

Cited by 14 publications

References 76 publications

Pair-Matching of Radio-Loud and Radio-Quiet AGNs

Pair-Matching of Radio-Loud and Radio-Quiet AGNs

The evolution of the low-frequency radio AGN population to z ≃ 1.5 in the ELAIS N1 field

Radio Sources Associated with Optical Galaxies and Having Unresolved or Extended Morphologies (ROGUE). I. A Catalog of SDSS Galaxies with FIRST Core Identifications

Contact Info

Product

Resources

About