Cosmological evolution of supermassive black holes in galactic centers unveiled by hard X-ray observations

Ueda, Yoshihiro

doi:10.2183/pjab.91.175

Cited by 7 publications

(8 citation statements)

References 101 publications

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“…44.8 =6.2×10 44 erg s −1 ; using a relation between dynamical and black hole masses (Bothwell et al 2013) and between X ray luminosity and black hole mass (Alexander et al 2005a,b), one estimates a black hole mass of 10 8.2 =1.6×10 8 solar masses while, on average (McLure & Dunlop 2004;Ueda 2015), black hole masses increase from 10 8 solar masses at z ∼ 0.2 to 10 9 solar masses at z ∼ 2 and between 10 9 and 10 10 solar masses for z>6 (Wang et al 2010).…”

Section: As 10mentioning

confidence: 99%

On the dust and gas components of the $z$ = 2.8 gravitationally lensed quasar host RX J0911.4+0551

Tuan-Anh¹,

Hoai²,

Nhung³

et al. 2017

Mon. Not. R. Astron. Soc.

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Observations by the Atacama Large Millimetre/sub-millimetre Array of the 358 GHz continuum emission of the gravitationally lensed quasar host RX J0911.4+0551 have been analysed. They complement earlier Plateau de Bure Interferometer observations of the CO(7-6) emission. The good knowledge of the lensing potential obtained from Hubble Space Telescope observations of the quasar makes a joint analysis of the three emissions possible. It gives evidence for the quasar source to be concentric with the continuum source within 0.31 kpc and with the CO(7-6) source within 1.10 kpc. It also provides a measurement of the size of the continuum source, 0.76 ± 0.04 kpc FWHM, making RX J0911.4+0551 one of the few high redshift galaxies for which the dust and gas components are resolved with dimensions being measured. Both are found to be very compact, the former being smaller than the latter by a factor of ∼3.4±0.4. Moreover, new measurements of the CO ladder − CO(10-9) and CO(11-10) − are presented that confirm the extreme narrowness of the CO line width (107±20 km s −1 on average). Their mere detection implies higher temperature and/or density than for typical quasar hosts at this redshift and suggests a possible contribution of the central AGN to gas and dust heating. The results are interpreted in terms of current understanding of galaxy evolution at the peak of star formation. They suggest that RX J0911.4+0551 is a young galaxy in an early stage of its evolution, having experienced no recent major mergers, star formation being concentrated in its centre.

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Section: As 10mentioning

confidence: 99%

On the dust and gas components of the $z$ = 2.8 gravitationally lensed quasar host RX J0911.4+0551

Tuan-Anh¹,

Hoai²,

Nhung³

et al. 2017

Mon. Not. R. Astron. Soc.

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“…To reveal the nature of heavily obscured Active Galactic Nuclei (AGNs) whose line-of-sight hydrogen column density is log N H /cm −2 ≥ 24, so-called Compton-thick AGNs (CTAGNs), is an important, yet unresolved issue in modern astronomy (Ueda 2015). CTAGNs are thought to be key objects to understand the origin of the co-evolution of Supermassive Black Holes (SMBHs) and their host galaxies (Kormendy & Ho 2013).…”

Section: Introductionmentioning

confidence: 99%

Suzaku Observations of Heavily Obscured (Compton-thick) Active Galactic Nuclei Selected by the Swift/BAT Hard X-Ray Survey

Tanimoto

Ueda

Kawamuro

et al. 2018

ApJ

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We present a uniform broadband X-ray (0.5-100.0 keV) spectral analysis of 12 Swift/Burst Alert Telescope (BAT) selected Compton-thick (log N H /cm −2 ≥ 24) Active Galactic Nuclei (CTAGNs) observed with Suzaku. The Suzaku data of 3 objects are published here for the first time. We fit the Suzaku and Swift spectra with models utilizing an analytic reflection code and those utilizing (Kawamuro et al. 2016a) suggests that the properties of these CTAGNs can be understood as a smooth extension from Compton-thin AGNs with heavier obscuration; we find no evidence that the bulk of the population of hard X-ray selected CTAGN is different from less obscured objects.

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“…17). Figure 18 plots the time variation of the normalized BH mass density computed from the quasar luminosity function by different authors (Shankar et al [23], Shen et al [57], Ueda et al [22] and Kim et al [21]). Analytical results of the BH mass density are also presented for comparison.…”

Section: Deriving Evolution Of Smbh Mass Functionmentioning

confidence: 99%

“…The second reason for the "co-evolution" between SMBHs and host galaxies follows from the striking similarity between the star formation rate (SFR) and the BH accretion rate (BHAR) over cosmic The cosmic evolution of the stellar mass and the mass of supermassive black holes from Kim et al [21], Ueda [22], and Shankar et al [23].…”

Section: Introductionmentioning

confidence: 99%

Cosmic quenching and scaling laws for evolution of galaxies and SMBHs

2024

Preprint

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Observations suggest a tight coupling between spuermassive black hole (SMBH) growth and star formation in the host galaxy. Based on Illustris simulations and astronomical observations, a cosmic quenching over the cosmic time scale is proposed to regulate the synchronized evolution of both SMBH and host. A central quantity of cosmic quenching is the parameter 𝜀𝑏 (unit: 𝑚2/𝑠3) that describes the rate of mass and energy flow of gases along the bulge radial direction. The parameter 𝜀𝑏 also controls the efficiency of gas cooling and the supply of cold gas. The value 𝜀𝑏 ≈ 10−4 (1 + 𝑧)5/2𝑚2/𝑠3 can be determined which decreases with time. For a larger 𝜀𝑏 in the early universe, gas cooling is more efficient in providing a richer supply of cold gas for a rapid initial evolution of both SMBH and host. At lower redshifts, a smaller 𝜀𝑏 means less efficient gas cooling, less cold gas supply, and slower star formation and black hole growth (quenched). The rate of mass accretion naturally exhibits a peak at 𝑧 ≈ 2 due to the decrease in 𝜀𝑏. Scaling laws involving 𝜀𝑏 are identified that govern the evolution of both SMBHs and their hosts. For host galaxies, we identify the mass-size relation 𝑀𝑏 ∝ 𝜀2/3 𝑏 𝑟5/3 𝑏 𝐺−1 and the dispersion-size relation 𝜎2 𝑏 ∝ (𝜀𝑏𝑟𝑏)2/3 ∝ (1 + 𝑧), where 𝑟𝑏 ∝ (1 + 𝑧)−1 is the bulge size. For SMBH, an initial rapid growth is identified with a sharp increase in luminosity 𝐿𝐵 ∝ (𝜀𝑏𝑀𝐵𝐻)4/5𝐺−1/5𝑐, followed by a transition stage with a decreasing luminosity 𝐿𝐵 ∝ 𝜀2𝑏𝑀𝐵𝐻 ∝ (1 + 𝑧)5, and a dormant stage with 𝐿𝐵 ∝ (𝜀𝑏𝑀𝐵𝐻)4/3𝐺1/3𝑐−5/3. Here 𝐺 is the gravitational constant, 𝑐 is the speed of light, 𝑀𝐵𝐻 is the mass of BH. For SMBH-galaxy co-evolution, the observed M-σ correlation can be analytically derived as 𝑀𝐵𝐻 ∝ 𝜎5 𝑏 /(𝜀𝑏𝐺). Using these scaling laws, analytical solutions are formulated for the evolution of the SMBH mass function Φ𝐵𝐻 (𝑀, 𝑧), the AGN mass function Φ𝐴𝐺𝑁 (𝑀, 𝑧), duty cycle 𝑈(𝑀, 𝑧), and the Eddington ratio distribution. The model predicts Φ𝐿 ∝ 𝐿−1/5 for the faint-end quasar luminosity function, Φ𝐴𝐺𝑁 ∝ 𝑀−1/5 for a small-mass-end AGN mass function, and 𝑈 ∝ 𝑀−1/5 for the duty cycle at high redshift. Finally, the complete redshift evolution of some observed high-redshift SMBHs can be modeled. The results suggest an initial super-Eddington growth in a short period when the SMBHs are still small, followed by a slow growth due to cosmic quenching when the SMBHs become large.

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Cosmological evolution of supermassive black holes in galactic centers unveiled by hard X-ray observations

Cited by 7 publications

References 101 publications

On the dust and gas components of the $z$ = 2.8 gravitationally lensed quasar host RX J0911.4+0551

On the dust and gas components of the $z$ = 2.8 gravitationally lensed quasar host RX J0911.4+0551

Suzaku Observations of Heavily Obscured (Compton-thick) Active Galactic Nuclei Selected by the Swift/BAT Hard X-Ray Survey

Cosmic quenching and scaling laws for evolution of galaxies and SMBHs

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