Cosmic evolution of radio-excess active galactic nuclei in quiescent and star-forming galaxies across 0 &lt; <i>z</i> &lt; 4

Wang, Yijun; Wang, Tao; Liu, Daizhong; Sargent, Mark T.; Gao, Fangyou; Alexander, David M.; Rujopakarn, Wiphu; Zhou, Luwenjia; Daddi, Emanuele; Xu, Ke; Kohno, Kotaro; Jin, Shuowen

doi:10.1051/0004-6361/202347787

Cited by 3 publications

(1 citation statement)

References 129 publications

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“…A wellestablished correlation, spanning up to 5 orders of magnitude, exists between far-infrared and radio emission from galaxies (e.g., Helou et al 1985;Condon et al 1991aCondon et al , 1991bAppleton et al 2004;Gim et al 2019). The intense radio emission, deviating significantly from this correlation, is attributed to the influence of AGN activities (e.g., Yun et al 2001;Calistro Rivera et al 2017;Wang et al 2024). However, recent studies have shown that radio excess can only collect the most radioloud AGNs (e.g., Morić et al 2010;Solarz et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Very Long Baseline Interferometry Detection of an Active Radio Source Potentially Driving 100 kpc Scale Emission in the Ultraluminous Infrared Galaxy IRAS F01004–2237

Hayashi,

Hagiwara,

Imanishi

2024

ApJ

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The nearby ultraluminous infrared galaxy (ULIRG) IRAS F01004−2237 exhibits 100 kpc scale continuum emission at radio wavelengths. The absence of extended X-ray emission in IRAS F01004−2237 has suggested an active galactic nucleus (AGN) origin for the extended radio emission, whose properties and role in merging systems still need to be better understood. We present the results of multifrequency observations of IRAS F01004−2237 conducted by the Very Long Baseline Array at 2.3 and 8.4 GHz. Compact 8.4 GHz continuum emission was detected on a 1 pc scale in the nuclear region with an intrinsic brightness temperature of 108.1 K suggesting that the radio source originated from an AGN, potentially driving the extended emission. In contrast, no significant emission was observed at 2.3 GHz, indicating the presence of low-frequency absorption. This absorption cannot be attributed solely to synchrotron self-absorption; alternatively, free–free absorption due to thermal plasma is mainly at work in the spectrum. From combined perspectives, including mid-infrared and X-ray data, the AGN is obscured in a dense environment. The kinetic power of the nonthermal jet, as inferred from the extended emission, can play a more important role in dispersing the surrounding medium than the thermal outflow in IRAS F01004−2237. These findings hint that jet activities in ULIRGs may contribute to AGN feedback during galaxy evolution induced by merger events.

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Section: Introductionmentioning

confidence: 99%

Very Long Baseline Interferometry Detection of an Active Radio Source Potentially Driving 100 kpc Scale Emission in the Ultraluminous Infrared Galaxy IRAS F01004–2237

Hayashi,

Hagiwara,

Imanishi

2024

ApJ

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The fundamental plane of black hole activity for low-luminosity radio active galactic nuclei across 0 < z < 4

Wang,

et al. 2024

A&A

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The fundamental plane of black hole activity describes the correlation between radio luminosity ($L_ R $), X-ray luminosity ($L_ X $), and black hole mass ($M_ BH $). It reflects a connection between the accretion disc and the jet. However, the dependence of the fundamental plane on various physical properties of active galactic nuclei (AGNs) and host galaxies remains unclear, especially for low-luminosity AGNs, which is important for understanding the accretion physics in AGNs. Here, we explore the dependence of the fundamental plane on the radio loudness, Eddington-ratio ($ Edd $), redshift, and galaxy star formation properties (star-forming galaxies and quiescent galaxies) across $0.1 < z 4$ for radio AGNs. Based on current deep and large surveys, our studies can extend to lower luminosities and higher redshifts. From the deep and large multi-wavelength surveys in the GOODS-N, GOODS-S, and COSMOS/UltraVISTA fields, we constructed a large and homogeneous radio AGN sample consisting of 208 objects with available estimates for $L_ R $ and $L_ X $. Then we divided the radio AGN sample into 141 radio-quiet AGNs and 67 radio-loud AGNs according to the radio loudness defined by the ratio of $L_ R $ to $L_ X $, and explored the dependence of the fundamental plane on different physical properties of the two populations, separately. The ratio of $L_ R $ to $L_ X $ shows a bimodal distribution that is well described by two single Gaussian models. The cross point between these two Gaussian components corresponds to a radio-loudness threshold of $ R /L_ X ) = -2.73$. The radio-quiet AGNs have a significantly larger Eddington ratio than the radio-loud AGNs. Our radio-quiet and radio-loud AGNs show a significantly different fundamental plane, which indicates a significant dependence of the fundamental plane on the radio loudness. For both radio-quiet and radio-loud AGNs, the fundamental plane shows a significant dependence on $ Edd $, but no dependence on redshift. The fundamental plane shows a significant dependence on the galaxy star formation properties for radio-quiet AGNs, while for radio-loud AGNs this dependence disappears. The fundamental plane sheds important light on the accretion physics and X-ray emission origins of central engines. X-ray emission of radio-quiet AGNs at $0.01 < Edd < 0.1$ are produced by a combination of advection-dominated accretion flow (ADAF) and synchrotron radiation from the jet, while at $0.1 < Edd < 1$ they mainly follow the synchrotron jet model. The origins of X-ray emission of radio-loud AGNs are consistent with a combination of ADAF and the synchrotron jet model at $ Edd < 0.01$, agree with the synchrotron jet model at $0.01 < Edd < 0.1$, and follow a combination of the standard thin disc and a jet model at $ Edd

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Radio-AGN activity across the galaxy population: dependence on stellar mass, star formation rate, and redshift

Kondapally,

Best,

Duncan

et al. 2024

Monthly Notices of the Royal Astronomical Society

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We characterise the co-evolution of radio-loud AGN and their galaxies by mapping the dependence of radio-loud AGN activity on stellar mass and star-formation rate (SFR) across cosmic time (out to z ∼ 1.5). Deep LOFAR radio observations are combined with large galaxy samples to study the incidence of radio-loud AGN across the galaxy population; the AGN are further split into low-excitation radio galaxies (LERGs) and high-excitation radio galaxies (HERGs). We find that LERG activity occurs over a wide range of SFRs, whereas HERGs are typically found in galaxies with ongoing star formation. The LERGs are then split based on their SFRs relative to the main sequence, across redshift. Within quiescent galaxies, LERG activity shows a steep stellar mass dependence with the same normalisation across the past ∼ 10 Gyr; this indicates that hot gas fuels LERGs in quiescent galaxies across cosmic time. In massive galaxies ($\log _{10}(M/\rm {{\rm M}_{\odot }}) \gtrsim 11$), the incidence of LERGs is roughly constant across the galaxy population, suggesting that LERGs in massive galaxies may be fuelled by hot gas regardless of the star-formation activity. At lower masses, however, LERG activity is significantly more enhanced (by a factor of up to 10) in star-forming galaxies compared to quiescent galaxies; this suggests that an additional fuelling mechanism, likely associated with cold gas, may fuel the LERGs in galaxies with higher SFRs. We find that HERGs typically accrete above 1percnt of the Eddington-scaled accretion rate, and the LERGs typically accrete below this level.

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Cosmic evolution of radio-excess active galactic nuclei in quiescent and star-forming galaxies across 0 < z < 4

Cited by 3 publications

References 129 publications

Very Long Baseline Interferometry Detection of an Active Radio Source Potentially Driving 100 kpc Scale Emission in the Ultraluminous Infrared Galaxy IRAS F01004–2237

Very Long Baseline Interferometry Detection of an Active Radio Source Potentially Driving 100 kpc Scale Emission in the Ultraluminous Infrared Galaxy IRAS F01004–2237

The fundamental plane of black hole activity for low-luminosity radio active galactic nuclei across 0 < z < 4

Radio-AGN activity across the galaxy population: dependence on stellar mass, star formation rate, and redshift

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