# Growth of Accreting Supermassive Black Hole Seeds and Neutrino Radiation

Authors: Gagik Ter-Kazarian
Journal: Journal of Astrophysics
 (2015)

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## Abstract

In the framework ofmicroscopic theory of black hole (MTBH), which explores the most important processes of rearrangement of vacuum state and spontaneous breaking of gravitation gauge symmetry at huge energies, we have undertaken a large series of numerical simulations with the goal to trace an evolution of the mass assembly history of 377 plausible accreting supermassive black hole seeds in active galactic nuclei (AGNs) to the present time and examine the observable signatures today. Given the redshifts, masses, and luminosities of these black holes at present time collected from the literature, we compute the initial redshifts and masses of the corresponding seed black holes. For the present masses MBH/M⊙≃1.1×106 to 1.3×1010 of 377 black holes, the computed intermediate seed masses are ranging from MBHSeed/M⊙≃26.4 to 2.9×105. We also compute the fluxes of ultrahigh energy (UHE) neutrinos produced via simple or modified URCA processes in superdense protomatter nuclei. The AGNs are favored as promising pure UHE neutrino sources, because the computed neutrino fluxes are highly beamed along the plane of accretion disk, peaked at high energies, and collimated in smaller opening angle (θ≪1).


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## Body

## 1. Introduction

With typical bolometric luminosities ~1045−48 erg s−1, the AGNs are amongst the most luminous emitters in the universe, particularly at high energies (gamma-rays) and radio wavelengths. From its historical development, up to current interests, the efforts in the AGN physics have evoked the study of a major unsolved problem of how efficiently such huge energies observed can be generated. This energy scale severely challenges conventional source models. The huge energy release from compact regions of AGN requires extremely high efficiency (typically ≥10 per cent) of conversion of rest mass to other forms of energy. This serves as the main argument in favour of supermassive black holes, with masses of millions to billions of times the mass of the Sun, as central engines of massive AGNs. The astrophysical black holes come in a wide range of masses, from ≥3M⊙ for stellar mass black holes [1] to ~1010M⊙ for supermassive black holes [2, 3]. Demography of local galaxies suggests that most galaxies harbour quiescent supermassive black holes in their nuclei at the present time and that the mass of the hosted black hole is correlated with properties of the host bulge. The visible universe should therefore contain at least 100 billion supermassive black holes. A complex study of evolution of AGNs requires an answer to the key questions such as how did the first black holes form, how did massive black holes get to the galaxy centers, and how did they grow in accreting mass, namely, an understanding of the important phenomenon of mass assembly history of accreting supermassive black hole seeds. The observations support the idea that black holes grow in tandem with their hosts throughout cosmic history, starting from the earliest times. While the exact mechanism for the formation of the first black holes is not currently known, there are several prevailing theories [4]. However, each proposal towards formation and growth of initial seed black holes has its own advantage and limitations in proving the whole view of the issue. In this report we review the mass assembly history of 377 plausible accreting supermassive black hole seeds in AGNs and their neutrino radiation in the framework of gravitation theory, which explores the most important processes of rearrangement of vacuum state and a spontaneous breaking of gravitation gauge symmetry at huge energies. We will proceed according to the following structure. Most observational, theoretical, and computational aspects of the growth of black hole seeds are summarized in Section 2. The other important phenomenon of ultrahigh energy cosmic rays, in relevance to AGNs, is discussed in Section 3. The objectives of suggested approach are outlined in Section 4. In Section 5 we review the spherical accretion on superdense protomatter nuclei, in use. In Section 6 we discuss the growth of the seed black hole at accretion and derive its intermediate mass, initial redshift, and neutrinopreradiation time (PRT). Section 7 is devoted to the neutrino radiation produced in superdense protomatter nuclei. The simulation results of the seed black hole intermediate masses, PRTs, seed redshifts, and neutrino fluxes for 377 AGN black holes are brought in Section 8. The concluding remarks are given in Section 9. We will refrain from providing lengthy details of the proposed gravitation theory at huge energies and neutrino flux computations. For these the reader is invited to visit the original papers and appendices of the present paper. In the latter we also complete the spacetime deformation theory, in the model context of gravitation, by new investigation of building up the complex ofdistortion (DC) of spacetime continuum and showing how it restores theworld-deformation tensor, which still has been put in by hand. Finally, note that we regard the considered black holes only as the potential neutrino sources. The obtained results, however, may suffer if not all live black holes at present reside in final stage of their growth driven by the formation of protomatter disk at accretion and they radiate neutrino. We often suppress the indices without notice. Unless otherwise stated, we take geometrized units throughout this paper.


## 2. A Breakthrough in Observational and Computational Aspects on Growth of Black Hole Seeds

Significant progress has been made in the last few years in understanding how supermassive black holes form and grow. Given the current masses of106-9M⊙, most black hole growth happens in the AGN phase. A significant fraction of the total black hole growth, 60% [6], happens in the most luminous AGN, quasars. In an AGN phase, which lasts ~108 years, the central supermassive black hole can gain up to ~107−8M⊙, so even the most massive galaxies will have only a few of these events over their lifetime. Aforesaid gathers support especially from a breakthrough made in recent observational, theoretical, and computational efforts in understanding of evolution of black holes and their host galaxies, particularly through self-regulated growth and feedback from accretion-powered outflows; see, for example, [4, 7–18]. Whereas the multiwavelength methods are used to trace the growth of seed BHs, the prospects for future observations are reviewed. The observations provide strong support for the existence of a correlation between supermassive black holes and their hosts out to the highest redshifts. The observations of the quasar luminosity function show that the most supermassive black holes get most of their mass at high redshift, while at low redshift only low mass black holes are still growing [19]. This is observed in both optical [20] and hard X-ray luminosity functions [19, 21], which indicates that this result is independent of obscuration. Natarajan [13] has reported that the initial black hole seeds form at extremely high redshifts from the direct collapse of pregalactic gas discs. Populating dark matter halos with seeds formed in this fashion and using a Monte-Carlo merger tree approach, he has predicted the black hole mass function at high redshifts and at the present time. The most aspects of the models that describe the growth and accretion history of supermassive black holes and evolution of this scenario have been presented in detail by [9, 10]. In these models, at early times the properties of the assembling black hole seeds are more tightly coupled to properties of the dark matter halo as their growth is driven by the merger history of halos. While a clear picture of the history of black hole growth is emerging, significant uncertainties still remain [14], and in spite of recent advances [6, 13], the origin of the seed black holes remains an unsolved problem at present. The NuSTAR deep high-energy observations will enable obtaining a nearly complete AGN survey, including heavily obscured Compton-thick sources, up to z~1.5 [22]. A similar mission, ASTRO-H [23], will be launched by Japan in 2014. These observations in combination with observations at longer wavelengths will allow for the detection and identification of most growing supermassive black holes at z~1. The ultradeep X-ray and near-infrared surveys covering at least ~1 deg⁡2⁡ are required to constrain the formation of the first black hole seeds. This will likely require the use of the next generation of space-based observatories such as the James Webb Space Telescope and the International X-ray Observatory. The superb spatial resolution and sensitivity of the Atacama Large Millimeter Array (ALMA) [24] will revolutionize our understanding of galaxy evolution. Combining these new data with existing multiwavelength information will finally allow astrophysicists to pave the way for later efforts by pioneering some of the census of supermassive black hole growth, in use today.


## 3. UHE Cosmic-Ray Particles

The galactic sources like supernova remnants (SNRs) or microquasars are thought to accelerate particles at least up to energies of3×1015 eV. The ultrahigh energy cosmic-ray (UHECR) particles with even higher energies have since been detected (comprehensive reviews can be found in [25–29]). The accelerated protons or heavier nuclei up to energies exceeding 1020 eV are firstly observed by [30]. The cosmic-ray events with the highest energies so far detected have energies of 2×1011 GeV [31] and 3×1011 GeV [32]. These energies are 107 times higher than the most energetic man-made accelerator, the LHC at CERN. These highest energies are believed to be reached in extragalactic sources like AGNs or gamma-ray bursts (GRBs). During propagation of such energetic particles through the universe, the threshold for pion photoproduction on the microwave background is ~2 × 1010 GeV, and at ~3 × 1011 GeV the energy-loss distance is about 20 Mpc. Propagation of cosmic rays over substantially larger distances gives rise to a cutoff in the spectrum at ~1011 GeV as was first shown by [33, 34], the GZK cutoff. The recent confirmation [35, 36] of GZK suppression in the cosmic-ray energy spectrum indicates that the cosmic rays with energies above the GZK cutoff, EGZK~40 EeV, mostly come from relatively close (within the GZK radius, rGZK~100 Mpc) extragalactic sources. However, despite the detailed measurements of the cosmic-ray spectrum, the identification of the sources of the cosmic-ray particles is still an open question as they are deflected in the galactic and extragalactic magnetic fields and hence have lost all information about their origin when reaching Earth. Only at the highest energies beyond ~1019.6 GeV cosmic-ray particles may retain enough directional information to locate their sources. The latter must be powerful enough to sustain the energy density in extragalactic cosmic rays of about 3×10-19 erg cm−3 which is equivalent to ~8 × 1044 erg Mpc−3 yr−1. Though it has not been possible up to now to identify the sources of galactic or extragalactic cosmic rays, general considerations allow limiting potential source classes. For example, the existing data on the cosmic-ray spectrum and on the isotropic 100 MeV gamma-ray background limit significantly the parameter space in which topological defects can generate the flux of the highest energy cosmic rays and rule out models with the standard X-particle mass of 1016 GeV and higher [37]. Eventually, the neutrinos will serve as unique astronomical messengers, and they will significantly enhance and extend our knowledge on galactic and extragalactic sources of the UHE universe. Indeed, except for oscillations induced by transit in a vacuum Higgs field, neutrinos can penetrate cosmological distances and their trajectories are not deflected by magnetic fields as they are neutral, providing powerful probes of high energy astrophysics in ways which no other particle can. Moreover, the flavor composition of neutrinos originating at astrophysical sources can serve as a probe of new physics in the electroweak sector. Therefore, an appealing possibility among the various hypotheses of the origin of UHECR is so-called Z-burst scenario [38–51]. This suggests that if ZeV astrophysical neutrino beam is sufficiently strong, it can produce a large fraction of observed UHECR particles within 100 Mpc by hitting local light relic neutrinos clustered in dark halos and form UHECR through the hadronic Z (s-channel production) and W-bosons (t-channel production) decays by weak interactions. The discovery of UHE neutrino sources would also clarify the production mechanism of the GeV-TeV gamma rays observed on Earth [43, 52, 53] as TeV photons are also produced in the up-scattering of photons in reactions to accelerated electrons (inverse-Compton scattering). The direct link between TeV gamma-ray photons and neutrinos through the charged and neutral pion production, which is well known from particle physics, allows for a quite robust prediction of the expected neutrino fluxes provided that the sources are transparent and the observed gamma rays originate from pion decay. The weakest link in the Z-burst hypothesis is probably both unknown boosting mechanism of the primary neutrinos up to huge energies of hundreds ZeV and their large flux required at the resonant energy Eν≃MZ2/2mν≃4.2×1021eVeV/mν well above the GZK cutoff. Such a flux severely challenges conventional source models. Any concomitant photon flux should not violate existing upper limits [37, 48, 49, 54]. The obvious question is then raised: where in the Cosmos are these neutrinos coming from? It turns out that currently, at energies in excess of 1019 eV, there are only two good candidate source classes for UHE neutrinos: AGNs and GRBs. The AGNs as significant point sources of neutrinos were analyzed in [50, 55, 56]. While hard to detect, neutrinos have the advantage of representing aforesaid unique fingerprints of hadron interactions and, therefore, of the sources of cosmic rays. Two basic event topologies can be distinguished: track-like patterns of detected Cherenkov light (hits) which originate from muons produced in charged-current interactions of muon neutrinos (muon channel); spherical hit patterns which originate from the hadronic cascade at the vertex of neutrino interactions or the electromagnetic cascade of electrons from charged-current interactions of electron neutrinos (cascade channel). If the charged-current interaction happens inside the detector or in case of charged-current tau-neutrino interactions, these two topologies overlap which complicates the reconstruction. At the relevant energies, the neutrino is approximately collinear with the muon and, hence, the muon channel is the prime channel for the search for point-like sources of cosmic neutrinos. On the other hand, cascades deposit all of their energy inside the detector and therefore allow for a much better energy reconstruction with a resolution of a few 10%. Finally, numerous reports are available at present in literature on expected discovery potential and sensitivity of experiments to neutrino point-like sources. Currently operating high energy neutrino telescopes attempt to detect UHE neutrinos, such as ANTARES [57, 58] which is the most sensitive neutrino telescope in the Northern Hemisphere, IceCube [35, 59–64] which is worldwide largest and hence most sensitive neutrino telescope in the Southern Hemisphere, BAIKAL [65], as well as the CR extended experiments of The Telescope Array [66], Pierre Auger Observatory [67, 68], and JEM-EUSO mission [69]. The JEM-EUSO mission, which is planned to be launched by a H2B rocket around 2015-2016, is designed to explore the extremes in the universe and fundamental physics through the detection of the extreme energy (E>1020 eV) cosmic rays. The possible origins of the soon-to-be famous 28 IceCube neutrino-PeV events [59–61] are the first hint for astrophysical neutrino signal. Aartsen et al. have published an observation of two ~1 PeV neutrinos, with a P value 2.8σ beyond the hypothesis that these events were atmospherically generated [59]. The analysis revealed an additional 26 neutrino candidates depositing “electromagnetic equivalent energies” ranging from about 30 TeV up to 250 TeV [61]. New results were presented at the IceCube Particle Astrophysics Symposium (IPA 2013) [62–64]. If cosmic neutrinos are primarily of extragalactic origin, then the 100 GeV gamma ray flux observed by Fermi-LAT constrains the normalization at PeV energies at injection, which in turn demands a neutrino spectral index Γ<2.1 [70].


## 4. MTBH, Revisited: Preliminaries

For the benefit of the reader, a brief outline of the key ideas behind themicroscopic theory of black hole, as a guiding principle, is given in this section to make the rest of the paper understandable. There is a general belief reinforced by statements in textbooks that, according to general relativity (GR), a long-standing standard phenomenological black hole model (PBHM)—namely, the most general Kerr-Newman black hole model, with parameters of mass (M), angular momentum (J), and charge (Q),still has to be put in by hand—can describe the growth of accreting supermassive black hole seed. However, such beliefs are suspect and should be critically reexamined. The PBHM cannot be currently accepted as convincing model for addressing the aforementioned problems, because in this framework the very source of gravitational field of the black hole is a kind of curvature singularity at the center of the stationary black hole. A meaningless central singularity develops which is hidden behind the event horizon. The theory breaks down inside the event horizon which is causally disconnected from the exterior world. Either the Kruskal continuation of the Schwarzschild (J=0, Q=0) metric, or the Kerr (Q=0) metric, or the Reissner-Nordstrom (J=0) metric, shows that the static observers fail to exist inside the horizon. Any object that collapses to form a black hole will go on to collapse to a singularity inside the black hole. Thereby any timelike worldline must strike the central singularity which wholly absorbs the infalling matter. Therefore, the ultimate fate of collapsing matter once it has crossed the black hole surface is unknown. This, in turn, disables any accumulation of matter in the central part and, thus, neither the growth of black holes nor the increase of their mass-energy density could occur at accretion of outside matter, or by means of merger processes. As a consequence, the mass and angular momentum of black holes will not change over the lifetime of the universe. But how can one be sure that some hitherto unknown source of pressure does not become important at huge energies and halt the collapse? To fill the void which the standard PBHM presents, one plausible idea to innovate the solution to alluded key problems would appear to be the framework ofmicroscopic theory of black hole. This theory has been originally proposed by [71] and references therein and thoroughly discussed in [72–75]. Here we recount some of the highlights of the MTBH, which is the extension of PBHM and rather completes it by exploring the most important processes of rearrangement of vacuum state and a spontaneous breaking of gravitation gauge symmetry at huge energies [71, 74, 76]. We will not be concerned with the actual details of this framework but only use it as a backdrop to validate the theory with some observational tests. For details, the interested reader is invited to consult the original papers. Discussed gravitational theory is consistent with GR up to the limit of neutron stars. But this theory manifests its virtues applied to the physics of internal structure of galactic nuclei. In the latter a significant change of properties of spacetime continuum, so-calledinner distortion (ID), arises simultaneously with the strong gravity at huge energies (see Appendix A). Consequently the matter undergoes phase transition of second kind, which supplies a powerful pathway to form a stable superdense protomatter core (SPC) inside the event horizon. Due to this, the stable equilibrium holds in outward layers too and, thus, an accumulation of matter is allowed now around the SPC. The black hole models presented in phenomenological and microscopic frameworks have been schematically plotted in Figure 1, to guide the eye. A crucial point of the MTBH is that a central singularity cannot occur, which is now replaced by finite though unbelievably extreme conditions held in the SPC, where the static observers existed. The SPC surrounded by the accretion disk presents the microscopic model of AGN. The SPC accommodates the highest energy scale up to hundreds of ZeV in central protomatter core which accounts for the spectral distribution of the resulting radiation of galactic nuclei. External physics of accretion onto the black hole in earlier part of its lifetime is identical to the processes in Schwarzschild’s model. However, a strong difference in the model context between the phenomenological black hole and the SPC is arising in the second part of its lifetime (see Section 6). The seed black hole might grow up driven by the accretion of outside matter when it was getting most of its mass. An infalling matter with time forms the protomatter disk around the protomatter core tapering off faster at reaching out the thin edge of the event horizon. At this, metric singularity inevitably disappears (see appendices) and the neutrinos may escape through vista to outside world, even after the neutrino trapping. We study the growth of protomatter disk and derive the intermediate mass and initial redshift of seed black hole and examine luminosities, neutrino surfaces for the disk. In this framework, we have computed the fluxes of UHE neutrinos [75], produced in the medium of the SPC via simple (quark and pionic reactions) or modified URCA processes, even after the neutrino trapping(G. Gamow was inspired to name the process URCA after the name of a casino in Rio de Janeiro, when M. Schenberg remarked to him that “the energy disappears in the nucleus of the supernova as quickly as the money disappeared at that roulette table”). The “trapping” is due to the fact that as the neutrinos are formed in protomatter core at superhigh densities they experience greater difficulty escaping from the protomatter core before being dragged along with the matter; namely, the neutrinos are “trapped” comove with matter. The part of neutrinos annihilates to produce, further, the secondary particles of expected ultrahigh energies. In this model, of course, a key open question is to enlighten the mechanisms that trigger the activity, and how a large amount of matter can be steadily funneled to the central regions to fuel this activity. In high luminosity AGNs the large-scale internal gravitational instabilities drive gas towards the nucleus which trigger big starbursts, and the coeval compact cluster just formed. It seemed they have some connection to the nuclear fueling through mass loss of young stars as well as their tidal disruption and supernovae. Note that we regard the UHECR particles as a signature of existence ofsuperdence protomatter sources in the universe. Since neutrino events are expected to be of sufficient intensity, our estimates can be used to guide investigations of neutrino detectors for the distant future.Figure 1
(a) The phenomenological model of AGN with the central stationary black hole. The meaningless singularity occurs at the center inside the black hole. (b) The microscopic model of AGN with the central stable SPC. In due course, the neutrinos of huge energies may escape through the vista to outside world. Accepted notations: EH = event horizon, AD = accretion disk, SPC = superdense protomatter core, PC = protomatter core.
(a)
(b)


## 5. Spherical Accretion onto SPC

As alluded to above, the MTBH framework supports the idea of accreting supermassive black holes which link to AGNs. In order to compute the mass accretion rateM˙, in use, it is necessary to study the accretion onto central supermassive SPC. The main features of spherical accretion can be briefly summed up in the following three idealized models that illustrate some of the associated physics [72].


### 5.1. Free Radial Infall

We examine the motion of freely moving test particle by exploring the external geometry of the SPC, with the line element (A.7), at x=0. Let us denote the 4-vector of velocity of test particle vμ=dx~μ/ds~,  x~μ=(t~,r~,θ~,φ~), and consider it initially for simplest radial infall v2=v3=0. We determine the value of local velocity vr^<0 of the particle for the moment of crossing the EH sphere, as well as at reaching the surface of central stable SPC. The equation of geodesics is derived from the variational principle δ∫‍dS=0, which is the extremum of the distance along the wordline for the Lagrangian at hand (1)2L=1-x02t~˙2-1+x02r~˙2-r~2sin2θ~φ~˙2-r~2θ~˙2,where t~˙≡dt~/dλ is the t-component of 4-momentum and λ is the affine parameter along the worldline. We are using an affine parametrization (by a rescaling λ→λ(λ′)) such that L=const is constant along the curve. A static observer makes measurements with local orthonormal tetrad: (2)e→t^=1-x0-1e→t,e→r^=1+x0-1e→r,e→θ^=r~-1e→θ,e→φ^=r~sinθ~-1e→θ.The Euler-Lagrange equations for θ~, ϕ~, and t~ can be derived from the variational principle. A local measurement of the particle’s energy made by a static observer in the equatorial plane gives the time component of the 4-momentum as measured in the observer’s local orthonormal frame. This is the projection of the 4-momentum along the time basis vector. The Euler-Lagrange equations show that if we orient the coordinate system as initially the particle is moving in the equatorial plane (i.e., θ~=π/2, θ~˙=0), then the particle always remains in this plane. There are two constants of the motion corresponding to the ignorable coordinates t~ and ϕ~, namely, the E-“energy-at-infinity” and the l-angular momentum. We conclude that the free radial infall of a particle from the infinity up to the moment of crossing the EH sphere, as well as at reaching the surface of central body, is absolutely the same as in the Schwarzschild geometry of black hole (Figure 2(a)). We clear up a general picture of orbits just outside the event horizon by considering the Euler-Lagrange equation for radial component with “effective potential.” The circular orbits are stable if V is concave up, namely, at r~>4M~, where M~ is the mass of SPC. The binding energy per unit mass of a particle in the last stable circular orbit at r~=4M~ is E~bind=m-E/M~≃1-27/321/2. Namely, this is the fraction of rest-mass energy released when test particle originally at rest at infinity spirals slowly toward the SPC to the innermost stable circular orbit and then plunges into it. Thereby one of the important parameters is the capture cross section for particles falling in from infinity: σcapt=πbmax⁡2, where bmax⁡ is the maximum impact parameter of a particle that is captured.Figure 2
(a) The free radial infall of a particle from the infinity to EH sphere (x0=1), which is similar to the Schwarzschild geometry of BH. Crossing the EH sphere, a particle continues infall reaching finally the surface (x0=2) of the stable SPC. (b) Approaching the EH sphere (x0=1), the particle concentration increases asymptotically until the threshold value of protomatter. Then, due to the action of cutoff effect, the metric singularity vanishes and the particles well pass EH sphere.
(a)
(b)


### 5.2. Collisionless Accretion

The distribution function for a collisionless gas is determined by the collisionless Boltzmann equation or Vlasov equation. For the stationary and spherical flow we obtain then(3)M˙E>0=16πGM~2ρ∞v∞-1c-2,where the particle density ρ∞ is assumed to be uniform at far from the SPC and the particle speed is v∞≪1. During the accretion process the particles approaching the EH become relativistic. Approaching event horizon, the particle concentration increases asymptotically as n~r~/n∞x0→1≈-ln⁡g~00/2v∞, up to the ID threshold value n~dr~-1/3=0.4fm (Figure 2(b)). Due to the action of cutoff effect, the metric singularity then vanishes and the particles well pass EH sphere x0=1 and in the sequel form the protomatter disk around the protomatter core.


### 5.3. Hydrodynamic Accretion

For real dynamical conditions found in considered superdense medium, it is expected that the mean free path for collisions will be much shorter than the characteristic length scale; that is, the accretion of ambient gas onto a stationary, nonrotating compact SPC will be hydrodynamical in nature. For any equation of state obeying the causality constraint the sound speed impliesa2<1 and the flow must pass through a critical sonic point rs outside the event horizon. The locally measured particle velocity reads vr^=1-g~00/E2, where E=E∞/m=g~00/1-u21/2 and E∞ is the energy at infinity of individual particle of the mass m. Thus, the proper flow velocity vr^=u→0 and is subsonic. At r~=Rg/2, the proper velocity equals the speed of light vr^=u=1>a and the flow is supersonic. This condition is independent of the magnitude of u and is not sufficient by itself to guarantee that the flow passes through a critical point outside EH. For large r~≥rs, it is expected that the particles be nonrelativistic with a≤as≪1 (i.e., T≪mc2/K=1013K), as they were nonrelativistic at infinity (a∞≪1). Considering the equation of accretion onto superdense protomatter core, which is an analogue of Bondi equations for spherical, steady-state adiabatic accretion onto the SPC, we determine a mass accretion rate (4)M˙=2πmnsrs5/2ln⁡g~00s′,where prime ′s denotes differentiation with respect to r~ at the point rs. The gas compression can be estimated as (5)n~n∞≈rs5/22r2ln⁡g~00s′1+g~rr(r~)1/2.The approximate equality between the sound speed and the mean particle speed implies that the hydrodynamic accretion rate is larger than the collisionless accretion rate by the large factor ≈109.


## 5.1. Free Radial Infall

We examine the motion of freely moving test particle by exploring the external geometry of the SPC, with the line element (A.7), at x=0. Let us denote the 4-vector of velocity of test particle vμ=dx~μ/ds~,  x~μ=(t~,r~,θ~,φ~), and consider it initially for simplest radial infall v2=v3=0. We determine the value of local velocity vr^<0 of the particle for the moment of crossing the EH sphere, as well as at reaching the surface of central stable SPC. The equation of geodesics is derived from the variational principle δ∫‍dS=0, which is the extremum of the distance along the wordline for the Lagrangian at hand (1)2L=1-x02t~˙2-1+x02r~˙2-r~2sin2θ~φ~˙2-r~2θ~˙2,where t~˙≡dt~/dλ is the t-component of 4-momentum and λ is the affine parameter along the worldline. We are using an affine parametrization (by a rescaling λ→λ(λ′)) such that L=const is constant along the curve. A static observer makes measurements with local orthonormal tetrad: (2)e→t^=1-x0-1e→t,e→r^=1+x0-1e→r,e→θ^=r~-1e→θ,e→φ^=r~sinθ~-1e→θ.The Euler-Lagrange equations for θ~, ϕ~, and t~ can be derived from the variational principle. A local measurement of the particle’s energy made by a static observer in the equatorial plane gives the time component of the 4-momentum as measured in the observer’s local orthonormal frame. This is the projection of the 4-momentum along the time basis vector. The Euler-Lagrange equations show that if we orient the coordinate system as initially the particle is moving in the equatorial plane (i.e., θ~=π/2, θ~˙=0), then the particle always remains in this plane. There are two constants of the motion corresponding to the ignorable coordinates t~ and ϕ~, namely, the E-“energy-at-infinity” and the l-angular momentum. We conclude that the free radial infall of a particle from the infinity up to the moment of crossing the EH sphere, as well as at reaching the surface of central body, is absolutely the same as in the Schwarzschild geometry of black hole (Figure 2(a)). We clear up a general picture of orbits just outside the event horizon by considering the Euler-Lagrange equation for radial component with “effective potential.” The circular orbits are stable if V is concave up, namely, at r~>4M~, where M~ is the mass of SPC. The binding energy per unit mass of a particle in the last stable circular orbit at r~=4M~ is E~bind=m-E/M~≃1-27/321/2. Namely, this is the fraction of rest-mass energy released when test particle originally at rest at infinity spirals slowly toward the SPC to the innermost stable circular orbit and then plunges into it. Thereby one of the important parameters is the capture cross section for particles falling in from infinity: σcapt=πbmax⁡2, where bmax⁡ is the maximum impact parameter of a particle that is captured.Figure 2
(a) The free radial infall of a particle from the infinity to EH sphere (x0=1), which is similar to the Schwarzschild geometry of BH. Crossing the EH sphere, a particle continues infall reaching finally the surface (x0=2) of the stable SPC. (b) Approaching the EH sphere (x0=1), the particle concentration increases asymptotically until the threshold value of protomatter. Then, due to the action of cutoff effect, the metric singularity vanishes and the particles well pass EH sphere.
(a)
(b)


## 5.2. Collisionless Accretion

The distribution function for a collisionless gas is determined by the collisionless Boltzmann equation or Vlasov equation. For the stationary and spherical flow we obtain then(3)M˙E>0=16πGM~2ρ∞v∞-1c-2,where the particle density ρ∞ is assumed to be uniform at far from the SPC and the particle speed is v∞≪1. During the accretion process the particles approaching the EH become relativistic. Approaching event horizon, the particle concentration increases asymptotically as n~r~/n∞x0→1≈-ln⁡g~00/2v∞, up to the ID threshold value n~dr~-1/3=0.4fm (Figure 2(b)). Due to the action of cutoff effect, the metric singularity then vanishes and the particles well pass EH sphere x0=1 and in the sequel form the protomatter disk around the protomatter core.


## 5.3. Hydrodynamic Accretion

For real dynamical conditions found in considered superdense medium, it is expected that the mean free path for collisions will be much shorter than the characteristic length scale; that is, the accretion of ambient gas onto a stationary, nonrotating compact SPC will be hydrodynamical in nature. For any equation of state obeying the causality constraint the sound speed impliesa2<1 and the flow must pass through a critical sonic point rs outside the event horizon. The locally measured particle velocity reads vr^=1-g~00/E2, where E=E∞/m=g~00/1-u21/2 and E∞ is the energy at infinity of individual particle of the mass m. Thus, the proper flow velocity vr^=u→0 and is subsonic. At r~=Rg/2, the proper velocity equals the speed of light vr^=u=1>a and the flow is supersonic. This condition is independent of the magnitude of u and is not sufficient by itself to guarantee that the flow passes through a critical point outside EH. For large r~≥rs, it is expected that the particles be nonrelativistic with a≤as≪1 (i.e., T≪mc2/K=1013K), as they were nonrelativistic at infinity (a∞≪1). Considering the equation of accretion onto superdense protomatter core, which is an analogue of Bondi equations for spherical, steady-state adiabatic accretion onto the SPC, we determine a mass accretion rate (4)M˙=2πmnsrs5/2ln⁡g~00s′,where prime ′s denotes differentiation with respect to r~ at the point rs. The gas compression can be estimated as (5)n~n∞≈rs5/22r2ln⁡g~00s′1+g~rr(r~)1/2.The approximate equality between the sound speed and the mean particle speed implies that the hydrodynamic accretion rate is larger than the collisionless accretion rate by the large factor ≈109.


## 6. The Intermediate Mass, PRT, and Initial Redshift of Seed Black Hole

The key objectives of the MTBH framework are then an increase of the mass,MBHSeed, gravitational radius, RgSeed, and of the seed black hole, BHSeed, at accretion of outside matter. Thereby an infalling matter forms protomatter disk around protomatter core tapering off faster at reaching the thin edge of event horizon. So, a practical measure of growth BHSeed→BH may most usefully be the increase of gravitational radius or mass of black hole: (6)ΔRg=RgBH-RgSeed=2Gc2Md=2Gc2ρdVd,ΔMBH=MBH-MBHSeed=MBHSeedΔRgRgSeed,where Md, ρd, and Vd, respectively, are the total mass, density, and volume of protomatter disk. At the value R^gBH of gravitational radius, when protomatter disk has finally reached the event horizon of grown-up supermassive black hole, the volume V^d can be calculated in polar coordinates (ρ,z,φ) from Figure 3: (7)iV^d=∫ρ0R^gBH‍dρ∫02π‍ρdϕ∫-z1ρz1ρ‍dzmkm-∫ρ0Rd‍dρ∫02π‍ρdϕ∫-z0ρz0ρ‍dz≃Rd≪R^gBH2π3RdR^gBH2,where z1ρ≃z0-z0ρ-ρ0/R^gBH-ρ0, z0ρ=Rd2-ρ2, and in approximation Rd≪R^gBH we set z0ρ0≃ρ0≃Rd/2.Figure 3
A schematic cross section of the growth of supermassive black hole driven by the formation of protomatter disk at accretion, when protomatter disk has finally reached the event horizon of grown-up supermassive black hole.


### 6.1. The Intermediate Mass of Seed Black Hole

From the first line of (6), by virtue of (7), we obtain(8)R^gBH=k1±1-2kRgSeed,where 2/k=8.73[km]Rdρd/M⊙. The (8) is valid at 2/kRgSeed≤1; namely, (9)R⊙Rd≥2.09kmR⊙ρdρ-⊙RgSeedR⊙.For the values ρd=2.6×1016gcm-3 (see below) and RgSeed≃2.95km103to106, inequality (9) is reduced to R⊙/Rd≥2.34×1081to103 or cm/Rd≥0.3410-2to10. This condition is always satisfied, because for considered 377 black holes, with the masses MBH/M⊙≃1.1×106to1.3×1010, we approximately have Rd/rOV≃10-10to10-7 [71]. Note that Woo and Urry [5] collect and compare all the AGN/BH mass and luminosity estimates from the literature. According to (6), the intermediate mass of seed black hole reads (10)MBHSeedM⊙≃MBHM⊙1-1.68×10-6RdcmMBHM⊙.


### 6.2. PRT

The PRT is referred to as a lapse of timeTBH from the birth of black hole till neutrino radiation, the earlier part of the lifetime. That is, TBH=Md/M˙, where M˙ is the accretion rate. In approximation at hand Rd≪Rg, the PRT reads (11)TBH=ρdVdM˙≃9.33·1015gcm-3RdRg2M˙.In case of collisionless accretion, (3) and (11) give (12)TBH≃2.6·1016Rdcm10-24gcm-3ρ∞v∞10kms-1yr.In case of hydrodynamic accretion, (4) and (11) yield(13)TBH≃8.8·1038RdRg2cm-3nsrs5/2ln⁡g00s′.Note that the spherical accretion onto black hole, in general, is not necessarily an efficient mechanism for converting rest-mass energy into radiation. Accretion onto black hole may be far from spherical accretion, because the accreted gas possesses angular momentum. In this case, the gas will be thrown into circular orbits about the black hole when centrifugal forces will become significant before the gas plunges through the event horizon. Assuming a typical mass-energy conversion efficiency of about ϵ~10%, in approximation Rd≪Rg, according to (12) and (13), the resulting relationship of typical PRT versus bolometric luminosity becomes (14)TBH≃0.32RdrOVMBHM⊙21039WLbolyr.We supplement this by computing neutrino fluxes in the next section.


### 6.3. Redshift of Seed Black Hole

Interpreting the redshift as a cosmological Doppler effect and that the Hubble law could most easily be understood in terms of expansion of the universe, we are interested in the purely academic question of principle to ask what could be the initial redshift,zSeed, of seed black hole if the mass, the luminosity, and the redshift, z, of black hole at present time are known. To follow the history of seed black hole to the present time, let us place ourselves at the origin of coordinates r=0 (according to the Cosmological Principle, this is mere convention) and consider a light traveling to us along the -r direction, with angular variables fixed. If the light has left a seed black hole, located at rs, θs, and φs, at time ts, and it has to reach us at a time t0, then a power series for the redshift as a function of the time of flight is zSeed=H0t0-ts+⋯, where t0 is the present moment and H0 is Hubble’s constant. Similar expression, z=H0(t0-t1)+⋯, can be written for the current black hole, located at r1, θ1, and φ1, at time t1, where t1=ts+TBH, as seed black hole is an object at early times. Hence, in the first-order approximation by Hubble’s constant, we may obtain the following relation between the redshifts of seed and present black holes: zSeed≃z+H0TBH. This relation is in agreement with the scenario of a general recession of distant galaxies away from us in all directions, the furthest naturally being those moving the fastest. This relation, incorporating with (14), for the value H0=70[km]/[sMpc] favored today yields (15)zSeed≃z+2.292×1028RdrOVMBHM⊙2WLbol.


## 6.1. The Intermediate Mass of Seed Black Hole

From the first line of (6), by virtue of (7), we obtain(8)R^gBH=k1±1-2kRgSeed,where 2/k=8.73[km]Rdρd/M⊙. The (8) is valid at 2/kRgSeed≤1; namely, (9)R⊙Rd≥2.09kmR⊙ρdρ-⊙RgSeedR⊙.For the values ρd=2.6×1016gcm-3 (see below) and RgSeed≃2.95km103to106, inequality (9) is reduced to R⊙/Rd≥2.34×1081to103 or cm/Rd≥0.3410-2to10. This condition is always satisfied, because for considered 377 black holes, with the masses MBH/M⊙≃1.1×106to1.3×1010, we approximately have Rd/rOV≃10-10to10-7 [71]. Note that Woo and Urry [5] collect and compare all the AGN/BH mass and luminosity estimates from the literature. According to (6), the intermediate mass of seed black hole reads (10)MBHSeedM⊙≃MBHM⊙1-1.68×10-6RdcmMBHM⊙.


## 6.2. PRT

The PRT is referred to as a lapse of timeTBH from the birth of black hole till neutrino radiation, the earlier part of the lifetime. That is, TBH=Md/M˙, where M˙ is the accretion rate. In approximation at hand Rd≪Rg, the PRT reads (11)TBH=ρdVdM˙≃9.33·1015gcm-3RdRg2M˙.In case of collisionless accretion, (3) and (11) give (12)TBH≃2.6·1016Rdcm10-24gcm-3ρ∞v∞10kms-1yr.In case of hydrodynamic accretion, (4) and (11) yield(13)TBH≃8.8·1038RdRg2cm-3nsrs5/2ln⁡g00s′.Note that the spherical accretion onto black hole, in general, is not necessarily an efficient mechanism for converting rest-mass energy into radiation. Accretion onto black hole may be far from spherical accretion, because the accreted gas possesses angular momentum. In this case, the gas will be thrown into circular orbits about the black hole when centrifugal forces will become significant before the gas plunges through the event horizon. Assuming a typical mass-energy conversion efficiency of about ϵ~10%, in approximation Rd≪Rg, according to (12) and (13), the resulting relationship of typical PRT versus bolometric luminosity becomes (14)TBH≃0.32RdrOVMBHM⊙21039WLbolyr.We supplement this by computing neutrino fluxes in the next section.


## 6.3. Redshift of Seed Black Hole

Interpreting the redshift as a cosmological Doppler effect and that the Hubble law could most easily be understood in terms of expansion of the universe, we are interested in the purely academic question of principle to ask what could be the initial redshift,zSeed, of seed black hole if the mass, the luminosity, and the redshift, z, of black hole at present time are known. To follow the history of seed black hole to the present time, let us place ourselves at the origin of coordinates r=0 (according to the Cosmological Principle, this is mere convention) and consider a light traveling to us along the -r direction, with angular variables fixed. If the light has left a seed black hole, located at rs, θs, and φs, at time ts, and it has to reach us at a time t0, then a power series for the redshift as a function of the time of flight is zSeed=H0t0-ts+⋯, where t0 is the present moment and H0 is Hubble’s constant. Similar expression, z=H0(t0-t1)+⋯, can be written for the current black hole, located at r1, θ1, and φ1, at time t1, where t1=ts+TBH, as seed black hole is an object at early times. Hence, in the first-order approximation by Hubble’s constant, we may obtain the following relation between the redshifts of seed and present black holes: zSeed≃z+H0TBH. This relation is in agreement with the scenario of a general recession of distant galaxies away from us in all directions, the furthest naturally being those moving the fastest. This relation, incorporating with (14), for the value H0=70[km]/[sMpc] favored today yields (15)zSeed≃z+2.292×1028RdrOVMBHM⊙2WLbol.


## 7. UHE Neutrino Fluxes

The flux can be written in terms of luminosity asJνε=L~νε/4πDL2z1+z, where z is the redshift and DL(z) is the luminosity distance depending on the cosmological model. The 1+z-1 is due to the fact that each neutrino with energy E~ν′ if observed near the place and time of emission t′ will be red-shifted to energy E~ν=E~ν′Rt1/Rt0=E~ν′1+z-1 of the neutrino observed at time t after its long journey to us, where Rt is the cosmic scale factor. Computing the UHE neutrino fluxes in the framework of MTBH, we choose the cosmological model favored today, with a flat universe, filled with matter ΩM=ρM/ρc and vacuum energy densities ΩV=ρV/ρc, thereby ΩV+ΩM=1, where the critical energy density ρc=3H02/(8πGN) is defined through the Hubble parameter H0 [77]: (16)DLz=1+zcH0ΩM∫11+z‍dxΩV/ΩM+x3=2.4×1028Izcm.Here I(z)=1+z∫11+z‍dx/2.3+x3, we set the values H0=70km/sMpc, ΩV=0.7 and ΩM=0.3.


### 7.1. URCA Reactions

The neutrino luminosity of SPC of given mass,M~, by modified URCA reactions with no muons reads [75] (17)L~νεURCA=3.8×1050εdM⊙M~1.75ergs-1,where εd=d/2Rg and d is the thickness of the protomatter disk at the edge of even horizon. The resulting total UHE neutrino flux of cooling of the SPC can be obtained as(18)JνεURCA≃5.22×10-8×εdI2z1+zM⊙M~1.75ergcm-2s-1sr⁡-1,where the neutrino is radiated in a cone with the beaming angle θ~εd≪1, I(z)=1+z∫11+z‍dx/2.3+x3. As it is seen, the nucleon modified URCA reactions can contribute efficiently only to extragalactic objects with enough small redshift z≪1.


### 7.2. Pionic Reactions

The pionic reactions, occurring in the superdense protomatter medium of SPC, allow both the distorted energy and momentum to be conserved. This is the analogue of the simple URCA processes:(19)π-+n⟶n+e-+ν-e,π-+n⟶n+μ-+ν-μand the two inverse processes. As in the modified URCA reactions, the total rate for all four processes is essentially four times the rate of each reaction alone. The muons are already present when pions appear. The neutrino luminosity of the SPC of given mass, M~, by pionic reactions reads [75] (20)L~νεπ=5.78×1058εdM⊙M~1.75ergs-1.Then, the UHE neutrino total flux is (21)Jνεπ≃7.91εdI2z1+zM⊙M~1.75ergcm-2s-1sr-1.The resulting total energy-loss rate will then be dramatically larger due to the pionic reactions (19) rather than the modified URCA processes.


### 7.3. Quark Reactions

In the superdense protomatter medium the distorted quark Fermi energies are far below the charmed c-, t-, and b-quark production thresholds. Therefore, only up-, down-, and strange quarks are present. Theβ equilibrium is maintained by reactions like (22)d⟶u+e-+ν-e,u+e-⟶d+νe,(23)s⟶u+e-+ν-e,u+e-⟶s+νe,which are β decay and its inverse. These reactions constitute simple URCA processes, in which there is a net loss of a νlν-l pair at nonzero temperatures. In this application a sufficient accuracy is obtained by assuming β-equilibrium and that the neutrinos are not retained in the medium of Λ-like protomatter. The quark reactions (22) and (23) proceed at equal rates in β equilibrium, where the participating quarks must reside close to their Fermi surface. Hence, the total energy of flux due to simple URCA processes is rather twice than that of (22) or (23) alone. For example, the spectral fluxes of the UHE antineutrinos and neutrinos for different redshifts from quark reactions are plotted, respectively, in Figures 4 and 5 [75]. The total flux of UHE neutrino can be written as (24)Jνεq≃70.68εdI2z1+zM⊙M~1.75ergcm-2s-1sr-1.Figure 4
The spectral fluxes of UHE antineutrinos for different redshifts from quark reactions.Figure 5
The spectral fluxes of UHE neutrinos for different redshifts from quark reactions.


## 7.1. URCA Reactions

The neutrino luminosity of SPC of given mass,M~, by modified URCA reactions with no muons reads [75] (17)L~νεURCA=3.8×1050εdM⊙M~1.75ergs-1,where εd=d/2Rg and d is the thickness of the protomatter disk at the edge of even horizon. The resulting total UHE neutrino flux of cooling of the SPC can be obtained as(18)JνεURCA≃5.22×10-8×εdI2z1+zM⊙M~1.75ergcm-2s-1sr⁡-1,where the neutrino is radiated in a cone with the beaming angle θ~εd≪1, I(z)=1+z∫11+z‍dx/2.3+x3. As it is seen, the nucleon modified URCA reactions can contribute efficiently only to extragalactic objects with enough small redshift z≪1.


## 7.2. Pionic Reactions

The pionic reactions, occurring in the superdense protomatter medium of SPC, allow both the distorted energy and momentum to be conserved. This is the analogue of the simple URCA processes:(19)π-+n⟶n+e-+ν-e,π-+n⟶n+μ-+ν-μand the two inverse processes. As in the modified URCA reactions, the total rate for all four processes is essentially four times the rate of each reaction alone. The muons are already present when pions appear. The neutrino luminosity of the SPC of given mass, M~, by pionic reactions reads [75] (20)L~νεπ=5.78×1058εdM⊙M~1.75ergs-1.Then, the UHE neutrino total flux is (21)Jνεπ≃7.91εdI2z1+zM⊙M~1.75ergcm-2s-1sr-1.The resulting total energy-loss rate will then be dramatically larger due to the pionic reactions (19) rather than the modified URCA processes.


## 7.3. Quark Reactions

In the superdense protomatter medium the distorted quark Fermi energies are far below the charmed c-, t-, and b-quark production thresholds. Therefore, only up-, down-, and strange quarks are present. Theβ equilibrium is maintained by reactions like (22)d⟶u+e-+ν-e,u+e-⟶d+νe,(23)s⟶u+e-+ν-e,u+e-⟶s+νe,which are β decay and its inverse. These reactions constitute simple URCA processes, in which there is a net loss of a νlν-l pair at nonzero temperatures. In this application a sufficient accuracy is obtained by assuming β-equilibrium and that the neutrinos are not retained in the medium of Λ-like protomatter. The quark reactions (22) and (23) proceed at equal rates in β equilibrium, where the participating quarks must reside close to their Fermi surface. Hence, the total energy of flux due to simple URCA processes is rather twice than that of (22) or (23) alone. For example, the spectral fluxes of the UHE antineutrinos and neutrinos for different redshifts from quark reactions are plotted, respectively, in Figures 4 and 5 [75]. The total flux of UHE neutrino can be written as (24)Jνεq≃70.68εdI2z1+zM⊙M~1.75ergcm-2s-1sr-1.Figure 4
The spectral fluxes of UHE antineutrinos for different redshifts from quark reactions.Figure 5
The spectral fluxes of UHE neutrinos for different redshifts from quark reactions.


## 8. Simulation

For simulation we use the data of AGN/BH mass and luminosity estimates for 377 black holes presented by [5]. These masses are mostly based on the virial assumption for the broad emission lines, with the broad-line region size determined from either reverberation mapping or optical luminosity. Additional black hole mass estimates based on properties of the host galaxy bulges, either using the observed stellar velocity dispersion or using the fundamental plane relation. Since the aim is to have more than a thousand of realizations, each individual run is simplified, with a use of previous algorithm of the SPC-configurations [71] as a working model, given in Appendix G. Computing the corresponding PRTs, seed black hole intermediate masses, and total neutrino fluxes, a main idea comes to solving an inverse problem. Namely, by the numerous reiterating integrations of the state equations of SPC-configurations we determine those required central values of particle concentration n~(0) and ID-field x(0), for which the integrated total mass of configuration has to be equal to the black hole mass MBH given from observations. Along with all integral characteristics, the radius Rd is also computed, which is further used in (10), (14), (15), (18), (21), and (24) for calculating MBHSeed, TBH, zSeed, and Jνεi, respectively. The results are summed up in Tables 1, 2, 3, 4 and 5. Figure 6 gives the intermediate seed masses MBHSeed/M⊙ versus the present masses MBH/M⊙ of 337 black holes, on logarithmic scales. For the present masses MBH/M⊙≃1.1×106to1.3×1010, the computed intermediate seed masses are ranging from MBHSeed/M⊙≃26.4to2.9×105. The computed neutrino fluxes are ranging from (1) (quark reactions)—Jνεq/εdergcm-2s-1sr-1≃8.29×10-16to3.18×10-4, with the average J¯νεq≃5.53×10-10εdergcm-2s-1sr-1; (2) (pionic reactions)—Jνεπ≃0.112Jνεq, with the average Jνεπ≃3.66×10-11εd[ergcm-2s-1sr-1]; and (3) (modified URCA processes)—JνεURCA≃7.39×10-11Jνεq, with the average J¯νεURCA≃2.41×10-20εd[ergcm-2s-1sr-1]. In accordance, the AGNs are favored as promising pure neutrino sources because the computed neutrino fluxes are highly beamed along the plane of accretion disk and peaked at high energies and collimated in smaller opening angle θ~εd=d/2rg≪1. To render our discussion here a bit more transparent and to obtain some feeling for the parameter εd we may estimate εd≃1.69×10-10, just for example, only, for the suppermassive black hole of typical mass ~109M⊙(2Rg=5.9×1014cm), and so d~1km. But the key problem of fixing the parameter εd more accurately from experiment would be an important topic for another investigation elsewhere.Table 1
Seed black hole intermediate masses, preradiation times, redshifts, and neutrino fluxes from spatially resolved kinematics. Columns: (1) name, (2) redshift, (3) AGN type: SY2: Seyfert 2, (4) log of the bolometric luminosity (ergs−1), (5) log of the radius of protomatter core in special unit rOV = 13.68 km, (6) log of the black hole mass in solar masses, (7) log of the seed black hole intermediate mass in solar masses, (8) log of the neutrino preradiation time (yrs), (9) redshift of seed black hole, (10) Ji=q, (11) Ji=URCA, and (12) Ji=π, where Ji≡log⁡(Jvεi/εdergcm-2s-1sr⁡-1).
Name
z
Type
log
⁡
L
bol
log
⁡
(
R
d
r
ov
)
log
⁡
(
M
BH
M
⊙
)
log
⁡
(
M
BH
Seed
M
⊙
)
log
⁡
T
BH
z
Seed
J
q
J
URCA
J
π
NGC 1068
0.004
SY2
44.98
−7.59201
7.23
2.5922
8.02
0.006
−5.49
−15.62
−6.44
NGC 4258
0.001
SY2
43.45
−7.98201
7.62
2.9822
10.33
0.148
−4.97
−15.10
−5.92Table 2
Seed black hole intermediate masses, preradiation times, redshifts, and neutrino fluxes from reverberation mapping. Columns: (1) name, (2) redshift, (3) AGN type: SY2: Seyfert 2, (4) log of the bolometric luminosity (ergs−1), (5) log of the radius of protomatter core in special unit rOV = 13.68 km, (6) log of the black hole mass in solar masses, (7) log of the seed black hole intermediate mass in solar masses, (8) log of the neutrino preradiation time (yrs), (9) redshift of seed black hole, (10) Ji=q, (11) Ji=URCA, and (12) Ji=π, where Ji≡log⁡(Jvεi/εdergcm-2s-1sr⁡-1).
Name
z
Type
log
⁡
L
bol
log
⁡
(
R
d
r
ov
)
log
⁡
(
M
BH
M
⊙
)
log
⁡
(
M
BH
Seed
M
⊙
)
log
⁡
T
BH
z
Seed
J
q
J
URCA
J
π
3C 120
0.033
SY1
45.34
−7.78201
7.42
2.7822
8.04
0.034
−7.69
−17.82
−8.64
3C 390.3
0.056
SY1
44.88
−8.91201
8.55
3.9122
10.76
0.103
−10.15
−20.28
−11.10
Akn 120
0.032
SY1
44.91
−8.63201
8.27
3.6322
10.17
0.055
−9.15
−19.28
−10.10
F9
0.047
SY1
45.23
−8.27201
7.91
3.2722
9.13
0.052
−8.87
−19.00
−9.82
IC 4329A
0.016
SY1
44.78
−7.13201
6.77
2.1322
7.30
0.017
−5.91
−16.04
−6.86
Mrk 79
0.022
SY1
44.57
−8.22201
7.86
3.2222
9.69
0.041
−8.10
−18.23
−9.05
Mrk 110
0.035
SY1
44.71
−7.18201
6.82
2.1822
7.47
0.036
−6.69
−16.82
−7.64
Mrk 335
0.026
SY1
44.69
−7.05201
6.69
2.0522
7.23
0.027
−6.20
−16.33
−7.15
Mrk 509
0.034
SY1
45.03
−8.22201
7.86
3.2222
9.23
0.041
−8.49
−18.62
−9.44
Mrk 590
0.026
SY1
44.63
−7.56201
7.20
2.5622
8.31
0.030
−7.09
−17.22
−8.04
Mrk 817
0.032
SY1
44.99
−7.96201
7.60
2.9622
8.75
0.036
−7.98
−18.11
−8.93
NGC 3227
0.004
SY1
43.86
−8.00201
7.64
3.0022
9.96
0.064
−6.21
−16.34
−7.16
NGC 3516
0.009
SY1
44.29
−7.72201
7.36
2.7222
8.97
0.021
−6.43
−16.56
−7.38
NGC 3783
0.010
SY1
44.41
−7.30201
6.94
2.3022
8.01
0.013
−5.79
−15.92
−6.74
NGC 4051
0.002
SY1
43.56
−6.49201
6.13
1.4922
7.24
0.006
−2.96
−13.10
−3.91
NGC 4151
0.003
SY1
43.73
−7.49201
7.13
2.4922
9.07
0.028
−5.07
−15.20
−6.02
NGC 4593
0.009
SY1
44.09
−7.27201
6.91
2.2722
8.27
0.016
−5.64
−15.77
−6.59
NGC 5548
0.017
SY1
44.83
−8.39201
8.03
3.3922
9.77
0.033
−8.16
−18.30
−9.11
NGC 7469
0.016
SY1
45.28
−7.20201
6.84
2.2022
6.94
0.016
−6.03
−16.16
−6.98
PG 0026 + 129
0.142
RQQ
45.39
−7.94201
7.58
2.9422
8.31
0.144
−9.35
−19.48
−10.30
PG 0052 + 251
0.155
RQQ
45.93
−8.77201
8.41
3.7722
9.43
0.158
−10.89
−21.02
−11.84
PG 0804 + 761
0.100
RQQ
45.93
−8.60201
8.24
3.6022
9.09
0.102
−10.16
−20.29
−11.11
PG 0844 + 349
0.064
RQQ
45.36
−7.74201
7.38
2.7422
7.94
0.065
−8.23
−18.36
−9.18
PG 0953 + 414
0.239
RQQ
46.16
−8.60201
8.24
3.6022
8.86
0.240
−11.04
−21.17
−11.99
PG 1211 + 143
0.085
RQQ
45.81
−7.85201
7.49
2.8522
7.71
0.085
−8.69
−18.82
−9.64
PG 1229 + 204
0.064
RQQ
45.01
−8.92201
8.56
3.9222
10.65
0.099
−10.29
−20.42
−11.24
PG 1307 + 085
0.155
RQQ
45.83
−8.26201
7.90
3.2622
8.51
0.156
−9.99
−20.12
−10.94
PG 1351 + 640
0.087
RQQ
45.50
−8.84201
8.48
3.8422
10.00
0.097
−10.44
−20.57
−11.39
PG 1411 + 442
0.089
RQQ
45.58
−7.93201
7.57
2.9322
8.10
0.090
−8.87
−19.00
−9.82
PG 1426 + 015
0.086
RQQ
45.19
−8.28201
7.92
3.2822
9.19
0.091
−9.45
−19.58
−10.40
PG 1613 + 658
0.129
RQQ
45.66
−8.98201
8.62
3.9822
10.12
0.138
−11.07
−21.20
−12.02
PG 1617 + 175
0.114
RQQ
45.52
−8.24201
7.88
3.2422
8.78
0.116
−9.65
−19.78
−10.60
PG 1700 + 518
0.292
RQQ
46.56
−8.67201
8.31
3.6722
8.60
0.293
−11.38
−21.51
−12.33
PG 2130 + 099
0.061
RQQ
45.47
−8.10201
7.74
3.1022
8.55
0.063
−8.81
−18.94
−9.76
PG 1226 + 023
0.158
RLQ
47.35
−7.58201
7.22
2.5822
5.63
0.158
−8.82
−18.95
−9.77
PG 1704 + 608
0.371
RLQ
46.33
−8.59201
8.23
3.5922
8.67
0.372
−11.50
−21.64
−12.45Table 3
Seed black hole intermediate masses, preradiation times, redshifts, and neutrino fluxes from optimal luminosity. Columns: (1) name, (2) redshift, (3) AGN type: SY2: Seyfert 2, (4) log of the bolometric luminosity (ergs−1), (5) log of the radius of protomatter core in special unit rOV = 13.68 km, (6) log of the black hole mass in solar masses, (7) log of the seed black hole intermediate mass in solar masses, (8) log of the neutrino preradiation time (yrs), (9) redshift of seed black hole, (10) Ji=q, (11) Ji=URCA, and (12) Ji=π, where Ji≡log⁡(Jvεi/εdergcm-2s-1sr⁡-1).
Name
z
Type
log
⁡
L
bol
log
⁡
(
R
d
r
ov
)
log
⁡
(
M
BH
M
⊙
)
log
⁡
(
M
BH
Seed
M
⊙
)
log
⁡
T
BH
z
Seed
J
q
J
URCA
J
π
Mrk 841
0.036
SY1
45.84
−8.46201
8.10
3.4622
8.90
0.038
−8.96
−19.09
−9.91
NGC 4253
0.013
SY1
44.40
−6.90201
6.54
1.9022
7.22
0.014
−5.32
−15.45
−6.27
NGC 6814
0.005
SY1
43.92
−7.64201
7.28
2.6422
9.18
0.028
−5.78
−15.91
−6.73
0054 + 144
0.171
RQQ
45.47
−9.26201
8.90
4.2622
10.87
0.198
−11.84
−21.97
−12.79
0157 + 001
0.164
RQQ
45.62
−8.06201
7.70
3.0622
8.32
0.165
−9.70
−19.83
−10.65
0204 + 292
0.109
RQQ
45.05
−7.03201
6.67
2.0322
6.83
0.109
−7.49
−17.62
−8.44
0205 + 024
0.155
RQQ
45.45
−8.22201
7.86
3.2222
8.81
0.158
−9.92
−20.05
−10.87
0244 + 194
0.176
RQQ
45.51
−8.39201
8.03
3.3922
9.09
0.179
−10.35
−20.48
−11.30
0923 + 201
0.190
RQQ
46.22
−9.30201
8.94
4.3022
10.20
0.195
−12.02
−22.15
−12.97
1012 + 008
0.185
RQQ
45.51
−8.15201
7.79
3.1522
8.61
0.187
−9.98
−20.11
−10.93
1029 − 140
0.086
RQQ
46.03
−9.44201
9.08
4.4422
10.67
0.097
−11.48
−21.61
−12.43
1116 + 215
0.177
RQQ
46.02
−8.57201
8.21
3.5722
8.94
0.179
−10.67
−20.80
−11.62
1202 + 281
0.165
RQQ
45.39
−8.65201
8.29
3.6522
9.73
0.173
−10.74
−20.87
−11.69
1309 + 355
0.184
RQQ
45.39
−8.36201
8.00
3.3622
8.91
0.186
−10.34
−20.47
−11.29
1402 + 261
0.164
RQQ
45.13
−7.65201
7.29
2.6522
7.99
0.165
−8.98
−19.11
−9.93
1444 + 407
0.267
RQQ
45.93
−8.42201
8.06
3.4222
8.73
0.268
−10.84
−20.97
−11.79
1635 + 119
0.146
RQQ
45.13
−8.46201
8.10
3.4622
9.61
0.155
−10.28
−20.41
−11.23
0022 − 297
0.406
RLQ
44.98
−8.27201
7.91
3.2722
9.38
0.414
−11.05
−21.18
−12.00
0024 + 348
0.333
RLQ
45.31
−6.73201
6.37
1.7322
5.97
0.333
−8.13
−18.26
−9.08
0056 − 001
0.717
RLQ
46.54
−9.07201
8.71
4.0722
9.42
0.718
−13.13
−23.26
−14.08
0110 + 495
0.395
RLQ
45.78
−8.70201
8.34
3.7022
9.44
0.399
−11.77
−21.90
−12.72
0114 + 074
0.343
RLQ
44.02
−7.16201
6.80
2.1622
8.12
0.349
−8.91
−19.04
−9.86
0119 + 041
0.637
RLQ
45.57
−8.74201
8.38
3.7422
9.73
0.643
−12.41
−22.54
−13.36
0133 + 207
0.425
RLQ
45.83
−9.88201
9.52
4.8822
11.75
0.474
−13.92
−24.05
−14.87
0133 + 476
0.859
RLQ
46.69
−9.09201
8.73
4.0922
9.31
0.860
−13.40
−23.53
−14.35
0134 + 329
0.367
RLQ
46.44
−9.10201
8.74
4.1022
9.58
0.369
−12.38
−22.52
−13.33
0135 − 247
0.831
RLQ
46.64
−9.49201
9.13
4.4922
10.16
0.834
−14.06
−24.19
−15.01
0137 + 012
0.258
RLQ
45.22
−8.93201
8.57
3.9322
10.46
0.280
−11.70
−21.83
−12.65
0153 − 410
0.226
RLQ
44.74
−7.92201
7.56
2.9222
8.92
0.233
−9.79
−19.92
−10.74
0159 − 117
0.669
RLQ
46.84
−9.63201
9.27
4.6322
10.24
0.672
−14.03
−24.16
−14.98
0210 + 860
0.186
RLQ
44.92
−6.90201
6.54
1.9022
6.70
0.186
−7.80
−17.93
−8.75
0221 + 067
0.510
RLQ
44.94
−7.65201
7.29
2.6522
8.18
0.512
−10.23
−20.36
−11.18
0237 − 233
2.224
RLQ
47.72
−8.88201
8.52
3.8822
7.86
2.224
−14.39
−24.52
−15.34
0327 − 241
0.888
RLQ
46.01
−8.96201
8.60
3.9622
9.73
0.892
−13.22
−23.35
−14.17
0336 − 019
0.852
RLQ
46.32
−9.34201
8.98
4.3422
10.18
0.857
−13.83
−23.96
−14.78
0403 − 132
0.571
RLQ
46.47
−9.43201
9.07
4.4322
10.21
0.575
−13.48
−23.61
−14.43
0405 − 123
0.574
RLQ
47.40
−9.83201
9.47
4.8322
10.08
0.575
−14.19
−24.32
−15.14
0420 − 014
0.915
RLQ
47.00
−9.39201
9.03
4.3922
9.60
0.916
−14.01
−24.14
−14.96
0437 + 785
0.454
RLQ
46.15
−9.15201
8.79
4.1522
9.97
0.458
−12.72
−22.85
−13.67
0444 + 634
0.781
RLQ
46.12
−8.89201
8.53
3.8922
9.48
0.784
−12.93
−23.06
−13.88
0454 − 810
0.444
RLQ
45.32
−8.49201
8.13
3.4922
9.48
0.450
−11.54
−21.67
−12.49
0454 + 066
0.405
RLQ
45.12
−7.78201
7.42
2.7822
8.26
0.407
−10.19
−20.32
−11.14
0502 + 049
0.954
RLQ
46.36
−9.24201
8.88
4.2422
9.94
0.957
−13.80
−23.93
−14.75
0514 − 459
0.194
RLQ
45.36
−7.91201
7.55
2.9122
8.28
0.196
−9.61
−19.74
−10.56
0518 + 165
0.759
RLQ
46.34
−8.89201
8.53
3.8922
9.26
0.761
−12.89
−23.02
−13.84
0538 + 498
0.545
RLQ
46.43
−9.94201
9.58
4.9422
11.27
0.559
−14.32
−24.45
−15.27
0602 − 319
0.452
RLQ
45.69
−9.38201
9.02
4.3822
10.89
0.473
−13.11
−23.25
−14.07
0607 − 157
0.324
RLQ
46.30
−9.04201
8.68
4.0422
9.60
0.326
−12.14
−22.27
−13.09
0637 − 752
0.654
RLQ
47.16
−9.77201
9.41
4.7722
10.20
0.656
−14.24
−24.37
−15.19
0646 + 600
0.455
RLQ
45.58
−9.10201
8.74
4.1022
10.44
0.469
−12.63
−22.76
−13.58
0723 + 679
0.846
RLQ
46.41
−9.03201
8.67
4.0322
9.47
0.848
−13.27
−23.41
−14.23
0736 + 017
0.191
RLQ
46.41
−8.36201
8.00
3.3622
8.57
0.192
−10.38
−20.51
−11.33
0738 + 313
0.631
RLQ
46.94
−9.76201
9.40
4.7622
10.40
0.634
−14.18
−24.31
−15.13
0809 + 483
0.871
RLQ
46.54
−8.32201
7.96
3.3222
7.92
0.871
−12.07
−22.20
−13.02
0838 + 133
0.684
RLQ
46.23
−8.88201
8.52
3.8822
9.35
0.686
−12.74
−22.87
−13.69
0906 + 430
0.668
RLQ
45.99
−8.26201
7.90
3.2622
8.35
0.669
−11.63
−21.76
−12.58
0912 + 029
0.427
RLQ
45.26
−8.08201
7.72
3.0822
8.72
0.430
−10.77
−20.90
−11.72
0921 − 213
0.052
RLQ
44.63
−8.50201
8.14
3.5022
10.19
0.084
−9.36
−19.50
−10.32
0923 + 392
0.698
RLQ
46.26
−9.64201
9.28
4.6422
10.84
0.708
−14.10
−24.23
−15.05
0925 − 203
0.348
RLQ
46.35
−8.82201
8.46
3.8222
9.11
0.349
−11.83
−21.97
−12.78
0953 + 254
0.712
RLQ
46.59
−9.36201
9.00
4.3622
9.95
0.715
−13.63
−23.76
−14.58
0954 + 556
0.901
RLQ
46.54
−8.43201
8.07
3.4322
8.14
0.901
−12.31
−22.44
−13.26
1004 + 130
0.240
RLQ
46.21
−9.46201
9.10
4.4622
10.53
0.248
−12.55
−22.68
−13.50
1007 + 417
0.612
RLQ
46.71
−9.15201
8.79
4.1522
9.41
0.613
−13.08
−23.21
−14.03
1016 − 311
0.794
RLQ
46.63
−9.25201
8.89
4.2522
9.69
0.796
−13.58
−23.71
−14.53
1020 − 103
0.197
RLQ
44.87
−8.72201
8.36
3.7222
10.39
0.228
−11.04
−21.18
−11.99
1034 − 293
0.312
RLQ
46.20
−9.11201
8.75
4.1122
9.84
0.316
−12.22
−22.35
−13.17
1036 − 154
0.525
RLQ
44.55
−8.16201
7.80
3.1622
9.59
0.543
−11.16
−21.29
−12.11
1045 − 188
0.595
RLQ
45.80
−7.19201
6.83
2.1922
6.40
0.595
−9.61
−19.74
−10.56
1100 + 772
0.311
RLQ
46.49
−9.67201
9.31
4.6722
10.67
0.318
−13.20
−23.33
−14.15
1101 − 325
0.355
RLQ
46.33
−8.97201
8.61
3.9722
9.43
0.357
−12.12
−22.25
−13.07
1106 + 023
0.157
RLQ
44.97
−7.86201
7.50
2.8622
8.57
0.160
−9.31
−19.44
−10.26
1107 − 187
0.497
RLQ
44.25
−7.26201
6.90
2.2622
8.09
0.501
−9.52
−19.65
−10.47
1111 + 408
0.734
RLQ
46.26
−10.18201
9.82
5.1822
11.92
0.770
−15.11
−25.24
−16.06
1128 − 047
0.266
RLQ
44.08
−7.08201
6.72
2.0822
7.90
0.270
−8.49
−18.62
−9.44
1136 − 135
0.554
RLQ
46.78
−9.14201
8.78
4.1422
9.32
0.555
−12.94
−23.07
−13.89
1137 + 660
0.656
RLQ
46.85
−9.72201
9.36
4.7222
10.41
0.659
−14.16
−24.29
−15.11
1150 + 497
0.334
RLQ
45.98
−9.09201
8.73
4.0922
10.02
0.340
−12.26
−22.39
−13.21
1151 − 348
0.258
RLQ
45.56
−9.38201
9.02
4.3822
11.02
0.287
−12.26
−22.39
−13.21
1200 − 051
0.381
RLQ
46.41
−8.77201
8.41
3.7722
8.95
0.382
−12.26
−22.39
−13.21
1202 − 262
0.789
RLQ
45.81
−9.36201
9.00
4.3622
10.73
0.804
−13.76
−23.89
−14.71
1217 + 023
0.240
RLQ
45.83
−8.77201
8.41
3.7722
9.53
0.244
−11.34
−21.47
−12.29
1237 − 101
0.751
RLQ
46.63
−9.64201
9.28
4.6422
10.47
0.755
−14.19
−24.32
−15.14
1244 − 255
0.633
RLQ
46.48
−9.40201
9.04
4.4022
10.14
0.637
−13.55
−23.69
−14.51
1250 + 568
0.321
RLQ
45.61
−8.78201
8.42
3.7822
9.77
0.327
−11.67
−21.81
−12.62
1253 − 055
0.536
RLQ
46.10
−8.79201
8.43
3.7922
9.30
0.538
−12.28
−22.42
−13.24
1254 − 333
0.190
RLQ
45.52
−9.19201
8.83
4.1922
10.68
0.210
−11.83
−21.96
−12.78
1302 − 102
0.286
RLQ
45.86
−8.66201
8.30
3.6622
9.28
0.289
−11.34
−21.47
−12.29
1352 − 104
0.332
RLQ
45.81
−8.51201
8.15
3.5122
9.03
0.334
−11.24
−21.37
−12.19
1354 + 195
0.720
RLQ
47.11
−9.80201
9.44
4.8022
10.31
0.722
−14.42
−24.55
−15.37
1355 − 416
0.313
RLQ
46.48
−10.09201
9.73
5.0922
11.52
0.331
−13.94
−24.07
−14.89
1359 − 281
0.803
RLQ
46.19
−8.43201
8.07
3.4322
8.49
0.804
−12.16
−22.29
−13.11
1450 − 338
0.368
RLQ
43.94
−6.82201
6.46
1.8222
7.52
0.371
−8.40
−18.53
−9.35
1451 − 375
0.314
RLQ
46.16
−9.18201
8.82
4.1822
10.02
0.319
−12.35
−22.48
−13.30
1458 + 718
0.905
RLQ
46.93
−9.34201
8.98
4.3422
9.57
0.906
−13.91
−24.04
−14.86
1509 + 022
0.219
RLQ
44.54
−8.35201
7.99
3.3522
9.98
0.247
−10.51
−20.64
−11.46
1510 − 089
0.361
RLQ
46.38
−9.01201
8.65
4.0122
9.46
0.363
−12.21
−22.34
−13.16
1545 + 210
0.266
RLQ
45.86
−9.29201
8.93
4.2922
10.54
0.278
−12.36
−22.49
−13.31
1546 + 027
0.412
RLQ
46.00
−9.08201
8.72
4.0822
9.98
0.417
−12.48
−22.61
−13.43
1555 − 140
0.097
RLQ
44.94
−7.61201
7.25
2.6122
8.10
0.099
−8.39
−18.53
−9.34
1611 + 343
1.401
RLQ
46.99
−9.93201
9.57
4.9322
10.69
1.405
−15.54
−25.67
−16.49
1634 + 628
0.988
RLQ
45.47
−7.64201
7.28
2.6422
7.63
0.989
−11.05
−21.18
−12.00
1637 + 574
0.750
RLQ
46.68
−9.54201
9.18
4.5422
10.22
0.753
−14.01
−24.14
−14.96
1641 + 399
0.594
RLQ
46.89
−9.78201
9.42
4.7822
10.49
0.597
−14.14
−24.27
−15.09
1642 + 690
0.751
RLQ
45.78
−8.12201
7.76
3.1222
8.28
0.752
−11.53
−21.66
−12.48
1656 + 053
0.879
RLQ
47.21
−9.98201
9.62
4.9822
10.57
0.882
−14.99
−25.12
−15.94
1706 + 006
0.449
RLQ
44.01
−6.99210
6.63
2.9922
7.79
0.453
−8.92
−19.06
−9.87
1721 + 343
0.206
RLQ
45.63
−8.40201
8.04
3.4022
8.99
0.209
−10.53
−20.66
−11.48
1725 + 044
0.293
RLQ
46.07
−8.43201
8.07
3.4322
8.61
0.294
−10.96
−21.09
−11.91Table 4
Seed black hole intermediate masses, preradiation times, redshifts, and neutrino fluxes from observed stellar velocity dispersions. Columns: (1) name, (2) redshift, (3) AGN type: SY2: Seyfert 2, (4) log of the bolometric luminosity (ergs−1), (5) log of the radius of protomatter core in special unit rOV = 13.68 km, (6) log of the black hole mass in solar masses, (7) log of the seed black hole intermediate mass in solar masses, (8) log of the neutrino preradiation time (yrs), (9) redshift of seed black hole, (10) Ji=q, (11) Ji=URCA, and (12) Ji=π, where Ji≡log⁡(Jvεi/εdergcm-2s-1sr⁡-1).
Name
z
Type
log
⁡
L
bol
log
⁡
(
R
d
r
ov
)
log
⁡
(
M
BH
M
⊙
)
log
⁡
(
M
BH
Seed
M
⊙
)
log
⁡
T
BH
z
Seed
J
q
J
URCA
J
π
NGC 1566
0.005
SY1
44.45
−7.28201
6.92
2.2822
7.93
0.008
−5.15
−15.28
−6.10
NGC 2841
0.002
SY1
43.67
−8.57201
8.21
3.5722
11.29
0.347
−6.60
−16.74
−7.55
NGC 3982
0.004
SY1
43.54
−6.45201
6.09
1.45220
7.18
0.008
−3.50
−13.63
−4.45
NGC 3998
0.003
SY1
43.54
−9.31201
8.95
4.3122
12.90
2.561
−8.25
−18.38
−9.20
Mrk 10
0.029
SY1
44.61
−7.83291
7.47
4.7908
8.87
0.036
−7.66
−17.79
−8.61
UGC 3223
0.016
SY1
44.27
−7.38201
7.02
2.3822
8.31
0.022
−6.34
−16.47
−7.29
NGC 513
0.002
SY2
42.52
−8.01201
7.65
3.0122
11.32
1.345
−5.62
−15.76
−6.57
NGC 788
0.014
SY2
44.33
−7.87201
7.51
2.8722
9.23
0.029
−7.08
−17.21
−8.03
NGC 1052
0.005
SY2
43.84
−8.55201
8.19
3.5522
11.08
0.228
−7.37
−17.50
−8.32
NGC 1275
0.018
SY2
45.04
−8.87201
8.51
3.8722
10.52
0.047
−9.05
−19.19
−10.01
NGC 1320
0.009
SY2
44.02
−7.54201
7.18
2.5422
8.88
0.023
−6.12
−16.25
−7.07
NGC 1358
0.013
SY2
44.37
−8.24201
7.88
3.2422
9.93
0.045
−7.66
−17.80
−8.62
NGC 1386
0.003
SY2
43.38
−7.60201
7.24
2.6022
9.64
0.075
−0.020
−15.39
−6.21
NGC 1667
0.015
SY2
44.69
−8.24201
7.88
3.2422
9.61
0.030
−7.79
−17.92
−8.74
NGC 2110
0.008
SY2
44.10
−8.66201
8.30
3.6622
11.04
0.166
−7.97
−18.10
−8.92
NGC 2273
0.006
SY2
44.05
−7.66201
7.30
2.6622
9.09
0.024
−5.97
−16.10
−6.92
NGC 2992
0.008
SY2
43.92
−8.08201
7.72
3.0822
10.06
0.071
−6.96
−17.09
−7.91
NGC 3185
0.004
SY2
43.08
−6.42201
6.06
1.4222
7.58
0.014
−3.45
−13.58
−4.40
NGC 3362
0.028
SY2
44.27
−7.13201
6.77
2.1322
7.81
0.031
−6.40
−16.54
−7.36
NGC 3786
0.009
SY2
43.47
−7.89201
7.53
2.8922
10.13
0.123
−6.73
−16.86
−7.68
NGC 4117
0.003
SY2
43.64
−7.19201
6.83
2.1922
8.56
0.018
−4.54
−14.67
−5.49
NGC 4339
0.004
SY2
43.38
−7.76201
7.40
2.7622
9.96
0.108
−5.79
−15.92
−6.74
NGC 5194
0.002
SY2
43.79
−7.31201
6.95
2.3122
8.65
0.016
−4.40
−14.53
−5.35
NGC 5252
0.023
SY2
45.39
−8.40201
8.04
3.4022
9.23
0.027
−8.45
−18.58
−9.40
NGC 5273
0.004
SY2
43.03
−6.87201
6.51
1.8722
8.53
0.034
−4.23
−14.36
−5.18
NGC 5347
0.008
SY2
43.81
−7.15201
6.79
2.1522
8.31
0.018
−5.33
−15.46
−6.28
NGC 5427
0.009
SY2
44.12
−6.75201
6.39
1.7522
7.20
0.011
−4.73
−14.86
−5.68
NGC 5929
0.008
SY2
43.04
−7.61201
7.25
2.6122
10.00
0.169
−6.13
−16.27
−7.09
NGC 5953
0.007
SY2
44.05
−7.30201
6.94
2.3022
8.37
0.015
−5.48
−15.61
−6.43
NGC 6104
0.028
SY2
43.60
−7.96201
7.60
2.9622
10.14
0.128
−7.86
−17.99
−8.81
NGC 7213
0.006
SY2
44.30
−8.35201
7.99
3.3522
10.22
0.055
−7.18
−17.31
−8.13
NGC 7319
0.023
SY2
44.19
−7.74201
7.38
2.7422
9.11
0.038
−7.30
−17.43
−8.25
NGC 7603
0.030
SY2
44.66
−8.44201
8.08
3.4422
10.04
0.056
−8.76
−18.89
−9.71
NGC 7672
0.013
SY2
43.86
−7.24201
6.88
2.2422
8.44
0.023
−5.91
−16.05
−6.87
NGC 7682
0.017
SY2
43.93
−7.64201
7.28
2.6422
9.17
0.039
−6.85
−16.98
−7.80
NGC 7743
0.006
SY2
43.60
−6.95201
6.59
1.9522
8.12
0.016
−4.73
−14.86
−5.68
Mrk 1
0.016
SY2
44.20
−7.52201
7.16
2.5222
8.66
0.025
−6.59
−16.72
−7.54
Mrk 3
0.014
SY2
44.54
−9.01201
8.65
4.0122
11.30
0.142
−9.08
−19.21
−10.03
Mrk 78
0.037
SY2
44.59
−8.23201
7.87
3.2322
9.69
0.056
−8.58
−18.71
−9.53
Mrk 270
0.010
SY2
43.37
−7.96201
7.60
2.9622
10.37
0.179
−6.94
−17.07
−7.89
Mrk 348
0.015
SY2
44.27
−7.57201
7.21
2.5722
8.69
0.024
−6.62
−16.75
−7.57
Mrk 533
0.029
SY2
45.15
−7.92201
7.56
2.9222
8.51
0.032
−7.82
−17.95
−8.77
Mrk 573
0.017
SY2
44.44
−7.64201
7.28
2.6422
8.66
0.024
−6.85
−16.98
−7.80
Mrk 622
0.023
SY2
44.52
−7.28201
6.92
2.2822
7.86
0.026
−6.49
−16.62
−7.44
Mrk 686
0.014
SY2
44.11
−7.92201
7.56
2.9222
9.55
0.042
−7.17
−17.30
−8.12
Mrk 917
0.024
SY2
44.75
−7.98201
7.62
2.9822
9.03
0.031
−7.75
−17.89
−8.70
Mrk 1018
0.042
SY2
44.39
−8.45201
8.09
3.4522
10.33
0.092
−9.08
−19.21
−10.03
Mrk 1040
0.017
SY2
44.53
−8.00201
7.64
3.0022
9.29
0.030
−7.48
−17.61
−8.43
Mrk 1066
0.012
SY2
44.55
−7.37201
7.01
2.3722
8.01
0.015
−6.07
−16.20
−7.02
Mrk 1157
0.015
SY2
44.27
−7.19201
6.83
2.1922
7.93
0.019
−5.95
−16.08
−6.90
Akn 79
0.018
SY2
45.24
−7.90201
7.54
2.9022
8.38
0.020
−7.36
−17.49
−8.31
Akn 347
0.023
SY2
44.84
−8.36201
8.00
3.3622
9.70
0.037
−8.38
−18.51
−9.33
IC 5063
0.011
SY2
44.53
−8.10201
7.74
3.1022
9.49
0.027
−7.27
−17.40
−8.22
II ZW55
0.025
SY2
44.54
−8.59201
8.23
3.5922
10.46
0.074
−8.86
−18.99
−9.81
F 341
0.016
SY2
44.13
−7.51201
7.15
2.5122
8.71
0.026
−6.57
−16.70
−7.52
UGC 3995
0.016
SY2
44.39
−8.05201
7.69
3.0522
9.53
0.036
−7.52
−17.65
−8.47
UGC 6100
0.029
SY2
44.48
−8.06201
7.70
3.0622
9.46
0.046
−8.06
−18.20
−9.01
1ES 1959 + 65
0.048
BLL
—
−10.39501
8.09
3.4522
7.79
0.052
−9.20
−19.34
−10.15
Mrk 180
0.045
BLL
—
−10.51501
8.21
3.5722
7.91
0.051
−9.35
−19.49
−10.31
Mrk 421
0.031
BLL
—
−10.59501
8.29
3.6522
7.99
0.038
−9.16
−19.29
−10.11
Mrk 501
0.034
BLL
—
−11.51501
9.21
4.5722
8.91
0.092
−10.85
−20.98
−11.80
I Zw 187
0.055
BLL
—
−10.16501
7.86
3.2222
7.56
0.058
−8.93
−19.06
−9.88
3C 371
0.051
BLL
—
−10.81501
8.51
3.8722
8.21
0.063
−9.99
−20.13
−10.95
1514 − 241
0.049
BLL
—
−10.40501
8.10
3.4622
7.80
0.054
−9.24
−19.37
−10.19
0521 − 365
0.055
BLL
—
−10.95501
8.65
4.0122
8.35
0.071
−10.31
−20.44
−11.26
0548 − 322
0.069
BLL
—
−10.45501
8.15
3.5122
7.85
0.074
−9.65
−19.78
−10.60
0706 + 591
0.125
BLL
—
−10.56501
8.26
3.6222
7.96
0.132
−10.41
−20.54
−11.36
2201 + 044
0.027
BLL
—
−10.40501
8.10
3.4622
7.80
0.032
−8.70
−18.83
−9.65
2344 + 514
0.044
BLL
—
−11.10501
8.80
4.1622
8.50
0.067
−10.37
−20.50
−11.32
3C 29
0.045
RG
—
−10.50501
8.20
3.5622
7.90
0.051
−9.34
−19.47
−10.29
3C 31
0.017
RG
—
−10.80501
8.50
3.8622
8.20
0.028
−8.99
−19.12
−9.94
3C 33
0.059
RG
—
−10.68501
8.38
3.7422
8.08
0.068
−9.90
−20.03
−10.85
3C 40
0.018
RG
—
−10.16501
7.86
3.2222
7.56
0.021
−7.92
−18.05
−8.87
3C 62
0.148
RG
—
−10.97501
8.67
4.0322
8.37
0.165
−11.29
−21.43
−12.25
3C 76.1
0.032
RG
—
−10.43501
8.13
3.4922
7.83
0.037
−8.90
−19.04
−9.86
3C 78
0.029
RG
—
−10.90501
8.60
3.9622
8.30
0.043
−9.64
−19.77
−10.59
3C 84
0.017
RG
—
−10.79501
8.49
3.8522
8.19
0.028
−8.97
−19.10
−9.92
3C 88
0.030
RG
—
−10.33501
8.03
3.3922
7.73
0.034
−8.67
−18.80
−9.62
3C 89
0.139
RG
—
−10.82501
8.52
3.8822
8.22
0.151
−10.97
−21.10
−11.92
3C 98
0.031
RG
—
−10.18501
7.88
3.2422
7.58
0.034
−8.44
−18.57
−9.39
3C 120
0.033
RG
—
−10.43501
8.13
3.4922
7.83
0.038
−8.93
−19.06
−9.88
3C 192
0.060
RG
—
−10.36501
8.06
3.4222
7.76
0.064
−9.36
−19.49
−10.31
3C 196.1
0.198
RG
—
−10.51501
8.21
3.5722
7.91
0.204
−10.79
−20.92
−11.74
3C 223
0.137
RG
—
−10.45501
8.15
3.5122
7.85
0.142
−10.31
−20.44
−11.26
3C 293
0.045
RG
—
−10.29501
7.99
3.3522
7.69
0.048
−8.97
−19.10
−9.92
3C 305
0.041
RG
—
−10.22501
7.92
3.2822
7.62
0.044
−8.76
−18.89
−9.71
3C 338
0.030
RG
—
−11.08501
8.78
4.1422
8.48
0.052
−9.98
−20.12
−10.93
3C 388
0.091
RG
—
−11.48501
9.18
4.5422
8.88
0.145
−11.71
−21.84
−12.66
3C 444
0.153
RG
—
−9.98501
7.68
3.0422
7.38
0.155
−9.60
−19.73
−10.55
3C 449
0.017
RG
—
−10.63501
8.33
3.6922
8.03
0.025
−8.69
−18.82
−9.64
gin 116
0.033
RG
—
−11.05501
8.75
4.1122
8.45
0.053
−10.02
−20.15
−10.97
NGC 315
0.017
RG
—
−11.20501
8.90
4.2622
8.60
0.045
−9.69
−19.82
−10.64
NGC 507
0.017
RG
—
−11.30501
9.00
4.3622
8.70
0.053
−9.86
−19.99
−10.81
NGC 708
0.016
RG
—
−10.76501
8.46
3.8222
8.16
0.026
−8.86
−18.99
−9.81
NGC 741
0.018
RG
—
−11.02501
8.72
4.0822
8.42
0.037
−9.42
−19.55
−10.37
NGC 4839
0.023
RG
—
−10.78501
8.48
3.8422
8.18
0.034
−9.22
−19.35
−10.17
NGC 4869
0.023
RG
—
−10.42501
8.12
3.4822
7.82
0.028
−8.59
−18.72
−9.54
NGC 4874
0.024
RG
—
−10.93501
8.63
3.9922
8.33
0.039
−9.52
−19.65
−10.47
NGC 6086
0.032
RG
—
−11.26501
8.96
4.3222
8.66
0.065
−10.36
−20.49
−11.31
NGC 6137
0.031
RG
—
−11.11501
8.81
4.1722
8.51
0.054
−10.07
−20.20
−11.02
NGC 7626
0.025
RG
—
−11.27501
8.97
4.3322
8.67
0.058
−10.15
−20.28
−11.10
0039 − 095
0.000
RG
—
−11.02501
8.72
4.0822
8.42
0.019
−2.89
−13.02
−3.84
0053 − 015
0.038
RG
—
−11.12501
8.82
4.1822
8.52
0.062
−10.27
−20.40
−11.22
0053 − 016
0.043
RG
—
−10.81501
8.51
3.8722
8.21
0.055
−9.84
−19.97
−10.79
0055 − 016
0.045
RG
—
−11.15501
8.85
4.2122
8.55
0.070
−10.47
−20.61
−11.43
0110 + 152
0.044
RG
—
−10.39501
8.09
3.4522
7.79
0.048
−9.12
−19.26
−10.07
0112 − 000
0.045
RG
—
−10.83501
8.53
3.8922
8.23
0.057
−9.91
−20.05
−10.87
0112 + 084
0.000
RG
—
−11.48501
9.18
4.5422
8.88
0.054
−3.70
−13.83
−4.65
0147 + 360
0.018
RG
—
−10.76501
8.46
3.8222
8.16
0.028
−3.70
−13.83
−4.65
0131 − 360
0.030
RG
—
−10.83501
8.53
3.8922
8.23
0.042
−9.55
−19.68
−10.50
0257 − 398
0.066
RG
—
−10.59501
8.29
3.6522
7.99
0.073
−9.85
−19.98
−10.80
0306 + 237
0.000
RG
—
−10.81501
8.51
3.8722
8.21
0.012
−2.52
−12.66
−3.48
0312 − 343
0.067
RG
—
−10.87501
8.57
3.9322
8.27
0.080
−10.35
−20.48
−11.30
0325 + 024
0.030
RG
—
−10.59501
8.29
3.6522
7.99
0.037
−9.13
−19.26
−10.08
0431 − 133
0.033
RG
—
−10.95501
8.65
4.0122
8.35
0.049
−9.84
−19.97
−10.79
0431 − 134
0.035
RG
—
−10.61501
8.31
3.6722
8.01
0.042
−9.30
−19.43
−10.25
0449 − 175
0.031
RG
—
−10.02501
7.72
3.0822
7.42
0.033
−8.16
−18.29
−9.11
0546 − 329
0.037
RG
—
−11.59501
9.29
4.6522
8.99
0.107
−11.07
−21.20
−12.02
0548 − 317
0.034
RG
—
−9.58501
7.28
2.6422
6.98
0.035
−7.47
−17.60
−8.42
0634 − 206
0.056
RG
—
−10.39501
8.09
3.4522
7.79
0.060
−9.35
−19.48
−10.30
0718 − 340
0.029
RG
—
−11.31501
9.01
4.3722
8.71
0.066
−10.36
−20.49
−11.31
0915 − 118
0.054
RG
—
−10.99501
8.69
4.0522
8.39
0.072
−10.36
−20.49
−11.31
0940 − 304
0.038
RG
—
−11.59501
9.29
4.6522
8.99
0.108
−11.09
−21.22
−12.04
1043 − 290
0.060
RG
—
−10.67501
8.37
3.7322
8.07
0.068
−9.90
−20.03
−10.85
1107 − 372
0.010
RG
—
−11.11501
8.81
4.1722
8.51
0.033
−9.06
−19.19
−10.01
1123 − 351
0.032
RG
—
−11.83501
9.53
4.8922
9.23
0.153
−11.35
−21.49
−12.31
1258 − 321
0.015
RG
—
−10.91501
8.61
3.9722
8.31
0.030
−9.07
−19.20
−10.02
1333 − 337
0.013
RG
—
−11.07501
8.77
4.1322
8.47
0.034
−9.22
−19.35
−10.17
1400 − 337
0.014
RG
—
−11.19501
8.89
4.2522
8.59
0.042
−9.50
−19.63
−10.45
1404 − 267
0.022
RG
—
−11.11505
8.81
4.8798
8.51
0.045
−9.76
−19.89
−10.71
1510 + 076
0.053
RG
—
−11.33501
9.03
4.3922
8.73
0.091
−10.94
−21.07
−11.89
1514 + 072
0.035
RG
—
−10.95501
8.65
4.0122
8.35
0.051
−9.90
−20.03
−10.85
1520 + 087
0.034
RG
—
−10.59501
8.29
3.6522
7.99
0.041
−9.24
−19.37
−10.19
1521 − 300
0.020
RG
—
−10.10501
7.80
3.1622
7.50
0.022
−7.91
−18.04
−8.86
1602 + 178
0.041
RG
—
−10.54501
8.24
3.6022
7.94
0.047
−9.32
−19.45
−10.27
1610 + 296
0.032
RG
—
−11.26501
8.96
4.3222
8.66
0.065
−10.36
−20.49
−11.31
2236 − 176
0.070
RG
—
−10.79501
8.49
3.8522
8.19
0.081
−10.25
−20.39
−11.20
2322 + 143
0.045
RG
—
−10.47501
8.17
3.5322
7.87
0.050
−9.28
−19.42
−10.24
2322 − 122
0.082
RG
—
−10.63501
8.33
3.6922
8.03
0.090
−10.12
−20.25
−11.07
2333 − 327
0.052
RG
—
−10.95501
8.65
4.0122
8.35
0.068
−10.26
−20.39
−11.21
2335 + 267
0.030
RG
—
−11.38501
9.08
4.4422
8.78
0.073
−10.51
−20.64
−11.46Table 5
Seed black hole intermediate masses, preradiation times, redshifts, and neutrino fluxes from fundamental plane-derived velocity dispersions. Columns: (1) name, (2) redshift, (3) AGN type: SY2: Seyfert 2, (4) log of the bolometric luminosity (ergs−1), (5) log of the radius of protomatter core in special unit rOV = 13.68 km, (6) log of the black hole mass in solar masses, (7) log of the seed black hole intermediate mass in solar masses, (8) log of the neutrino preradiation time (yrs), (9) redshift of seed black hole, (10) Ji=q, (11) Ji=URCA, and (12) Ji=π, where Ji≡log⁡(Jvεi/εdergcm-2s-1sr⁡-1).
Name
z
Type
log
⁡
(
R
d
r
ov
)
log
⁡
(
M
BH
M
⊙
)
log
⁡
(
M
BH
Seed
M
⊙
)
log
⁡
T
BH
z
Seed
J
q
J
URCA
J
π
0122 + 090
0.339
BLL
−11.12501
8.82
4.1822
8.52
0.363
−12.43
−22.57
−13.39
0145 + 138
0.124
BLL
−10.72501
8.42
3.7822
8.12
0.133
−10.68
−20.81
−11.63
0158 + 001
0.229
BLL
−10.38501
8.08
3.4422
7.78
0.233
−10.71
−20.84
−11.66
0229 + 200
0.139
BLL
−11.54501
9.24
4.6022
8.94
0.201
−12.23
−22.36
−13.18
0257 + 342
0.247
BLL
−10.96501
8.66
4.0222
8.36
0.263
−11.81
−21.94
−12.76
0317 + 183
0.190
BLL
−10.25501
7.95
3.3122
7.65
0.193
−10.29
−20.42
−11.24
0331 − 362
0.308
BLL
−11.05501
8.75
4.1122
8.45
0.328
−12.21
−22.34
−13.16
0347 − 121
0.188
BLL
−10.95501
8.65
4.0122
8.35
0.204
−11.50
−21.63
−12.45
0350 − 371
0.165
BLL
−11.12501
8.82
4.1822
8.52
0.189
−11.67
−21.80
−12.62
0414 + 009
0.287
BLL
−10.86501
8.56
3.9222
8.26
0.300
−11.80
−21.93
−12.75
0419 + 194
0.512
BLL
−10.91501
8.61
3.9722
8.31
0.527
−12.54
−22.68
−13.50
0506 − 039
0.304
BLL
−11.05501
8.75
4.1122
8.45
0.324
−12.19
−22.32
−13.14
0525 + 713
0.249
BLL
−11.33501
9.03
4.3922
8.73
0.287
−12.46
−22.60
−13.41
0607 + 710
0.267
BLL
−10.95501
8.65
4.0122
8.35
0.283
−12.46
−22.60
−13.41
0737 + 744
0.315
BLL
−11.24501
8.94
4.3022
8.64
0.346
−12.56
−22.69
−13.51
0922 + 749
0.638
BLL
−11.91501
9.61
4.9722
9.31
0.784
−14.56
−24.69
−15.51
0927 + 500
0.188
BLL
−10.64501
8.34
3.7022
8.04
0.196
−10.96
−21.09
−11.91
0958 + 210
0.344
BLL
−11.33501
9.03
4.3922
8.73
0.382
−12.82
−22.95
−13.77
1104 + 384
0.031
BLL
−11.69501
9.39
4.7522
9.09
0.119
−11.08
−21.21
−12.03
1133 + 161
0.460
BLL
−10.62501
8.32
3.6822
8.02
0.467
−11.91
−22.04
−12.86
1136 + 704
0.045
BLL
−11.25501
8.95
4.3122
8.65
0.077
−10.65
−20.78
−11.60
1207 + 394
0.615
BLL
−11.40501
9.10
4.4622
8.80
0.660
−13.62
−23.76
−14.58
1212 + 078
0.136
BLL
−11.29501
8.99
4.3522
8.69
0.171
−11.77
−21.90
−12.72
1215 + 303
0.130
BLL
−10.42501
8.12
3.4822
7.82
0.135
−10.20
−20.33
−11.15
1218 + 304
0.182
BLL
−10.88501
8.58
3.9422
8.28
0.196
−11.35
−21.48
−12.30
1221 + 245
0.218
BLL
−10.27501
7.97
3.3322
7.67
0.221
−10.47
−20.60
−11.42
1229 + 643
0.164
BLL
−11.71501
9.41
4.7722
9.11
0.256
−12.69
−22.82
−13.64
1248 − 296
0.370
BLL
−11.31501
9.01
4.3722
8.71
0.407
−12.87
−23.00
−13.82
1255 + 244
0.141
BLL
−10.88501
8.58
3.9422
8.28
0.155
−11.09
−21.22
−12.04
1407 + 595
0.495
BLL
−11.60501
9.30
4.6622
9.00
0.566
−13.71
−23.84
−14.66
1418 + 546
0.152
BLL
−11.33501
9.03
4.3922
8.73
0.190
−11.95
−22.08
−12.90
1426 + 428
0.129
BLL
−11.43501
9.13
4.4922
8.83
0.177
−11.96
−22.09
−12.91
1440 + 122
0.162
BLL
−10.74501
8.44
3.8022
8.14
0.172
−10.98
−21.11
−11.93
1534 + 014
0.312
BLL
−11.10501
8.80
4.1622
8.50
0.335
−12.31
−22.44
−13.26
1704 + 604
0.280
BLL
−11.07501
8.77
4.1322
8.47
0.301
−12.14
−22.27
−13.09
1728 + 502
0.055
BLL
−10.43501
8.13
3.4922
7.83
0.060
−9.40
−19.53
−10.35
1757 + 703
0.407
BLL
−11.05501
8.75
4.1122
8.45
0.427
−12.52
−22.65
−13.47
1807 + 698
0.051
BLL
−12.40501
10.10
5.4622
9.80
0.502
−12.78
−22.91
−13.73
1853 + 671
0.212
BLL
−10.53501
8.23
3.5922
7.93
0.218
−10.89
−21.02
−11.84
2005 − 489
0.071
BLL
−11.33501
9.03
4.3922
8.73
0.109
−11.21
−21.34
−12.16
2143 + 070
0.237
BLL
−10.76501
8.46
3.8222
8.16
0.247
−11.41
−21.54
−12.36
2200 + 420
0.069
BLL
−10.53501
8.23
3.5922
7.93
0.075
−9.79
−19.92
−10.74
2254 + 074
0.190
BLL
−10.92501
8.62
3.9822
8.32
0.205
−11.46
−21.59
−12.41
2326 + 174
0.213
BLL
−11.04501
8.74
4.1022
8.44
0.233
−11.79
−21.92
−12.74
2356 − 309
0.165
BLL
−10.90501
8.60
3.9622
8.30
0.179
−11.28
−21.41
−12.23
0230 − 027
0.239
RG
−10.27501
7.97
3.3322
7.67
0.242
−10.56
−20.70
−11.52
0307 + 169
0.256
RG
−10.96501
8.66
4.0222
8.36
0.272
−11.85
−21.98
−12.80
0345 + 337
0.244
RG
−9.42501
7.12
2.4822
6.82
0.244
−9.10
−19.23
−10.05
0917 + 459
0.174
RG
−10.51501
8.21
3.5722
7.91
0.180
−10.65
−20.78
−11.60
0958 + 291
0.185
RG
−10.23501
7.93
3.2922
7.63
0.188
−10.23
−20.36
−11.18
1215 − 033
0.184
RG
−10.23501
7.93
3.2922
7.63
0.187
−10.22
−20.35
−11.17
1215 + 013
0.118
RG
−10.50501
8.20
3.5622
7.90
0.124
−10.25
−20.38
−11.20
1330 + 022
0.215
RG
−10.12501
7.82
3.1822
7.52
0.217
−10.19
−20.32
−11.14
1342 − 016
0.167
RG
−10.71501
8.41
3.7722
8.11
0.176
−10.96
−21.09
−11.91
2141 + 279
0.215
RG
−10.12501
7.82
3.1822
7.52
0.217
−10.19
−20.32
−11.14
0257 + 024
0.115
RQQ
−11.05501
8.75
4.1122
8.45
0.135
−11.18
−21.32
−12.13
1549 + 203
0.250
RQQ
−9.22501
6.92
2.2822
6.62
0.250
−8.78
−18.91
−9.73
2215 − 037
0.241
RQQ
−10.50501
8.20
3.5622
7.90
0.247
−10.98
−21.11
−11.93
2344 + 184
0.138
RQQ
−9.37501
7.07
2.4322
6.77
0.138
−8.42
−18.56
−9.38
0958 + 291
0.185
RG
−10.23501
7.93
3.2922
7.63
0.188
−10.23
−20.36
−11.18
1215 − 033
0.184
RG
−10.23501
7.93
3.2922
7.63
0.187
−10.22
−20.35
−11.17
1215 + 013
0.118
RG
−10.50501
8.20
3.5622
7.90
0.124
−10.25
−20.38
−11.20
1330 + 022
0.215
RG
−10.12501
7.82
3.1822
7.52
0.217
−10.19
−20.32
−11.14
1342 − 016
0.167
RG
−10.71501
8.41
3.7722
8.11
0.176
−10.96
−21.09
−11.91
2141 + 279
0.215
RG
−10.12501
7.82
3.1822
7.52
0.217
−10.19
−20.32
−11.14
0257 + 024
0.115
RQQ
−11.05501
8.75
4.1122
8.45
0.135
−11.18
−21.32
−12.13
1549 + 203
0.250
RQQ
−9.22501
6.92
2.2822
6.62
0.250
−8.78
−18.91
−9.73
2215 − 037
0.241
RQQ
−10.50501
8.20
3.5622
7.90
0.247
−10.98
−21.11
−11.93
2344 + 184
0.138
RQQ
−9.37501
7.07
2.4322
6.77
0.138
−8.42
−18.56
−9.38Figure 6
TheMBHSeed/M⊙-MBH/M⊙ relation on logarithmic scales of 337 black holes from [5]. The solid line is the best fit to data of samples.


## 9. Conclusions

The growth of accreting supermassive black hole seeds and their neutrino radiation are found to be common phenomena in the AGNs. In this report, we further expose the assertions made in the framework of microscopic theory of black hole via reviewing the mass assembly history of 377 plausible accreting supermassive black hole seeds. After the numerous reiterating integrations of the state equations of SPC-configurations, we compute their intermediate seed masses,MBHSeed, PRTs, initial redshifts, zSeed, and neutrino fluxes. All the results are presented in Tables 1–5. Figure 6 gives the intermediate seed masses MBHSeed/M⊙ versus the present masses MBH/M⊙ of 337 black holes, on logarithmic scales. In accordance, the AGNs are favored as promising pure UHE neutrino sources. Such neutrinos may reveal clues on the puzzle of origin of UHE cosmic rays. We regard the considered black holes only as the potential neutrino sources. The obtained results, however, may suffer and that would be underestimated if not all 377 live black holes in the MBH/M⊙≃1.1×106to1.3×1010 mass range at present reside in final stage of their growth, when the protomatter disk driven by accretion has reached the event horizon.



---

*Source: 205367-2015-03-24.xml*