The fundamental plane of black hole activity for quiescent sources

Dong, Ai‐Jun; Ge, Kang; Liu, Xiang; Zhi, Qi‐Jun

doi:10.1002/asna.202113903

Cited by 3 publications

(7 citation statements)

References 30 publications

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“…In addition, most ETG and AGN (∼83%, or 87% if we include radio upper limits) show a radio-to-X-ray radio loudness R X −3.5, classifying these objects as RQ AGN (Terashima & Wilson 2003;Lambrides et al 2020). We found that ETG (most of which have L X < 10 42 erg s −1 and z < 0.5) follow a relation log(L R ) = a log(L X ) + b with a slope a ∼ 0.6, in agreement with fundamental plane studies of low luminosity AGN (slope 0.5 − 0.7, Merloni et al 2003;Dong et al 2021). This slope is commonly interpreted as a signature of inefficient accretion processes, in contrast with what is found for luminous (L X 10 43 erg s −1 ) X-ray-selected local Seyfert galaxies, for which Panessa et al (2015) found a steeper relation (a∼1.1) that is interpreted as a signature of efficiently accreting systems.…”

Section: Discussionsupporting

confidence: 87%

“…Results are reported in columns 5 and 6 of Table 5. We note that the slope of the ETG correlation (a = 0.58 ± 0.15) is well in the range of the slopes found for low luminosity AGN in the fundamental plane (∼0.5 − 0.7, Merloni et al 2003, see also Dong et al 2021). Such slope values are commonly interpreted as a signature of radiatively inefficient accretion processes (see, e.g., Narayan & Yi 1994;Dong et al 2014, see also Sec.…”

Section: Radio/x-ray Luminosity Correlationssupporting

confidence: 74%

“…The X-ray and radio emission are generally found to follow a (logarithmic) linear correlation with slope distributed around ∼1 (Canosa et al 1999;Brinkmann et al 2000;Panessa et al 2007;Fan & Bai 2016). In particular, for low-luminosity AGN a standard value of 0.5-0.7 is found (Merloni et al 2003;Dong et al 2021), similarly to the typical slope of X-ray binaries (Narayan & Yi 1994). This has been interpreted as a signature of radiatively inefficient accretion mechanisms (Gallo et al 2003;Merloni et al 2003), such asadvection-dominated accretion flows (Narayan & Yi 1994;Heckman & Best 2014).…”

Section: Introductionmentioning

confidence: 95%

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A deep 1.4 GHz survey of the J1030 equatorial field: A new window on radio source populations across cosmic time

D’Amato

Prandoni

Gilli

et al. 2022

A&A

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We present deep L-Band observations of the equatorial field centered on the z = 6.3 Sloan digital sky survey (SDSS) quasar (QSO). This field is rich of multiwavelength photometry and spectroscopy data, making it an ideal laboratory for galaxy evolution studies. Our observations reach a 1σ sensitivity of ∼2.5 µJy at the center of the field. We extracted a catalog of 1489 radio sources down to a flux density of ∼12.5 µJy (5σ) over a field of view of ∼ 30 diameter. We derived the source counts accounting for catalog reliability and completeness, and compared them with others available in the literature. Our source counts are among the deepest available so far, and, overall, are consistent with recent counts' determinations and models. They show a slight excess at flux densities ∼ 50 µJy, possibly associated with the presence of known overdensities in the field. We detected for the first time in the radio band the SDSS J1030+0524 QSO (26 ± 5 µJy, 8σ significance level). For this object, we derived an optical radio loudness R O = 0.62 ± 0.12, which makes it the most radio quiet among active galactic nuclei (AGN) discovered so far at z 6 and detected at radio wavelengths. We unveiled extended diffuse radio emission associated with the lobes of a bright Fanaroff-Riley type II (FRII) radio galaxy located close to the center of the J1030 field, which is likely to become the future brightest cluster galaxy of a protocluster at z = 1.7. The lobes' complex morphology, coupled with the presence of X-ray diffuse emission detected around the FRII galaxy lobes, may point toward an interaction between the radio jets and the external medium. We also investigated the relation between radio and X-ray luminosity for a sample of 243 X-ray-selected objects obtained from 500 ks Chandra observations of the same field, and spanning a wide redshift range (0 z 3). Focused on sources with a spectroscopic redshift and classification, we found that sources hosted by early-type galaxies and AGN follow log(L R )/ log(L X ) linear correlations with slopes of ∼0.6 and ∼0.8, respectively. This is interpreted as a likely signature of different efficiency in the accretion process. Finally, we found that most of these sources ( 87%) show a radio-to-X-ray radio loudness R X −3.5, classifying these objects as radio quiet.

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Section: Discussionsupporting

confidence: 87%

Section: Radio/x-ray Luminosity Correlationssupporting

confidence: 74%

Section: Introductionmentioning

confidence: 95%

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A deep 1.4 GHz survey of the J1030 equatorial field: A new window on radio source populations across cosmic time

D’Amato

Prandoni

Gilli

et al. 2022

A&A

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“…The slope will become much steeper with

b\sim 1.27

than radiatively inefficient accretion mode when the x‐ray emissions are dominated by relativistic jet flow (Yuan & Cui 2005). The results of Yuan et al (2009) and Dong, Ge, et al (2021) support the prediction based on the fundamental plane of quiescent sources and radio loud sources. Similar results are also presented by Z.‐Y.…”

Section: Conclusion and Discussionsupporting

confidence: 59%

“…Our main results are summarized as: (1) The Eddington‐scaled Xxray luminosity of our samples covers in the range of

{L}_{\mathrm{X}}/{L}_{\mathrm{Edd}}\sim {10}^{-7}-{10}^{-1}

, which roughly corresponds to a quiescent state, low/hard state, and bright hard state of black hole sources; (2) Blazars and FR Is track a similar and steeper radio–x‐ray correlation

{F}_{5\kern0.3em \mathrm{GHz}}\propto {F}_{2-10\kern0.3em \mathrm{keV}}^{\sim 1.10}

; (3) Blazars and FR Is track a steeper fundamental plane of black hole activity

{\xi}_{\mathrm{X}}\sim 1.24

. Our results are similar to that of Dong, Ge, et al (2021); Dong & Wu (2015), implying that the x‐ray emissions of strong radio black hole sources are from the jet‐dominated flow.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

The fundamental plane of black hole activity for strong radio black hole sources

Dong

Liu

et al. 2023

Astron Nachr

Self Cite

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It is still controversial whether the x‐ray emissions of strong radio black hole sources (e.g., blazars and FR Is) are from a jet‐dominated flow or from an accretion disc. Previous studies have suggested that the radio–x‐ray correlation is clearly different when the x‐ray luminosity is higher or lower than a critical value, LnormalX,crit∼10−3LEdd$$ {L}_{\mathrm{X},\mathrm{crit}}\sim {10}^{-3}{L}_{\mathrm{Edd}} $$, where LEdd∼1.28×1038normalerg0.3ems−1$$ {L}_{\mathrm{Edd}}\sim 1.28\times {10}^{38}\mathrm{erg}\kern0.3em {\mathrm{s}}^{-1} $$ is the Eddington luminosity. When the black hole transient sources stay in quiescent state (LnormalX,crit≤10−6LEdd$$ {L}_{\mathrm{X},\mathrm{crit}}\le {10}^{-6}{L}_{\mathrm{Edd}} $$), the radio–x‐ray correlation presented a steeper slope (LR∝LXb,b∼1.23$$ {L}_{\mathrm{R}}\propto {L}_{\mathrm{X}}^b,b\sim 1.23 $$). In this work, we constructed a strong radio sample, including blazars and FR Is with a wide x‐ray luminosity distribution (LX∼10−7−10−1LEdd$$ {L}_{\mathrm{X}}\sim {10}^{-7}-{10}^{-1}{L}_{\mathrm{Edd}} $$) to re‐explore this issue. An obvious change in radio–x‐ray correlations is not found when the x‐ray luminosity LnormalX,crit∼10−3LEdd$$ {L}_{\mathrm{X},\mathrm{crit}}\sim {10}^{-3}{L}_{\mathrm{Edd}} $$ and LnormalX,crit∼10−6LEdd$$ {L}_{\mathrm{X},\mathrm{crit}}\sim {10}^{-6}{L}_{\mathrm{Edd}} $$. And the radio–x‐ray correlation and the fundamental plane of black hole activity for strong radio sources follow a slope with ξX=1.24±0.03$$ {\xi}_{\mathrm{X}}=1.24\pm 0.03 $$. These results imply x‐ray emissions of strong radio black hole sources have similar physics and can be well explained by a jet‐dominated flow.

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Heavily obscured AGN detection: A radio versus X-ray challenge

Mazzolari,

Gilli,

Brusa

et al. 2024

A&A

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In the supermassive black hole (SMBH)-galaxy coevolution scenario, heavily obscured active galactic nuclei (AGN) represent a fundamental phase of SMBH growth during which most of the BH mass is accreted and the scaling relations with the host galaxy are set. Obscured nuclei are thought to constitute a major fraction of the whole AGN population, but their statistics and evolution across cosmic time are still highly uncertain. Therefore, it is pivotal to identify new ways to detect this vast and hidden population of growing SMBHs. A promising way to select heavily obscured AGN is through radio emission, which is largely unaffected by obscuration and can be used as a proxy for nuclear activity. In this work, we study the AGN radio detection effectiveness in the major deep extragalactic surveys, considering different AGN obscuration levels, redshift, and AGN bolometric luminosities. We particularly focus on comparing their radio and X-ray detectability, making predictions for present and future radio surveys. We extrapolated the predictions of the AGN population synthesis model of the cosmic X-ray background (CXB) to the radio band, by deriving the 1.4 GHz luminosity functions of unobscured (i.e., with hydrogen column densities $ H <22$), obscured ($22< H <24$), and Compton-thick (CTK, $ H >24$) AGN. We then used these functions to forecast the number of detectable AGN based on the area, flux limit, and completeness of a given radio survey and compare it with the AGN number resulting from X-ray predictions. When applied to deep extragalactic fields covered both by radio and X-ray observations, we show that, while X-ray selection is generally more effective in detecting unobscured AGN, the surface density of CTK AGN radio detected is on average ten times larger than the X-ray one, and even greater at high redshifts, considering the current surveys and facilities. Our results suggest that thousands of CTK AGN are already present in current radio catalogs, but most of them escaped any detection in the corresponding X-ray observations. We also present expectations for the number of AGN to be detected by the Square Kilometer Array Observatory (SKAO) in its future deep and wide radio continuum surveys, finding that it will be able to detect more than 2000 AGN at $z>6$ and tens of them at $z>10$, more than half of which are expected to be CTK.

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The fundamental plane of black hole activity for quiescent sources

Cited by 3 publications

References 30 publications

A deep 1.4 GHz survey of the J1030 equatorial field: A new window on radio source populations across cosmic time

A deep 1.4 GHz survey of the J1030 equatorial field: A new window on radio source populations across cosmic time

The fundamental plane of black hole activity for strong radio black hole sources

Heavily obscured AGN detection: A radio versus X-ray challenge

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