PoS(MULTIF2019)013 https://pos.sissa.it/ 10) universe is presented. Also the data on the recently ∼ z ∗† [email protected] Speaker. The support of the RNF Grant 19-42-02004 is acknowledged. A review of the astronomical dataholes of in several the last contemporary years and on earlyobserved an peculiar ( astonishingly stars high in amount the ofthe are black universe discussed. are primordial It (PBH) is and arguedis that suggested realized: practically that all an supermassive black inverted black picture holesseeded of holes in the the were latter. galaxy formed formation Possibilities priorand of to of cosmological galaxy abundant dark cosmological formation matter antimatter and consisting are subsequently considered. A of mechanism primordial of black holes 1993 anticipatingmass all spectrum these of phenomena PBH and is described. predicting an extended log-normal † ∗ Copyright owned by the author(s) under the terms of the Creative Commons c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). Multifrequency Behaviour of High Energy Cosmic3-8 Sources June - 2019 XIII - MULTIF2019 Palermo, Italy A.D. Dolgov Massive Primordial Black Holes Novosibirsk State University and ITEP, Russia E-mail: PoS(MULTIF2019)013 10 ∼ z A.D. Dolgov years, and the 9 10 · years. So the stellar 6 . 10 14 10 ; =

≈ U M t U t 10 10 10 is multifold more pronounced. ∼ ∼ z years. M 33 ], but of course during the last one-two years 3 , 1 ,

M , ) M 5

M 10 100 ) 9 − & 3 10 10 − ( 6 up to ∼ 10

( M M ∼ M g the life-time is close to the universe age 14 10 · 5 = 0, universe is much more abundantly populated by all kind of black holes, than it was BH ], which neatly solves the above mentioned problems, is described. Not only abundant ∼ 2 M z , 1 Existence of black holes (BHs) was first envisaged by John Mitchell in 1784, who predicted This is not precisely true, because BHs can emit all kind of radiation in the process of their BHs strongly interact with the surrounding matter and it makes them very visible. For exam- Recent astronomical data, which keep on appearing almost every day, show that the contem- In addition, there is a population of peculiar stars in theMoreover, Galaxy the data (too collected old, during too last fast, several years and indicate with that an the young universe at The canonical mechanism of formation of SMBH even in the present day universe demands In this talk a review of these surprising astronomical observations is presented and the mech- intermediate mass (IMBH) bright QSOs, alias supermassive BHs, with masses up to superluminous young ; supernovae, gamma-bursters; dust and heavy elements. massive, from a fraction of supermassive (SMBH), that there might be bodies withbe so larger strong than gravitational the field speed of thatabsolutely light. the dark, second He and cosmic concluded it that velocity is they would impossible neither to shine observe not to reflect them. light, i.e.evaporation they predicted are by Stephen Hawking and, thoughthat nobody such yet process has exists. seen The it, life-timeand there of are for a no doubts BH with respect to evaporation scales as its mass cube, ple, the most powerful sources of radiation in the universe are (QSO) which are pointl-like PBHs but also a significant amount ofa rather considerable strange or primordial even stars 100% are contribution predicted, totent They the of may cosmological make this dark talk matter. coincides To some withmuch extent more the the new con- author’s observational review data [ have been obtained. 2. Black Holes: what’s that 2.1 Observations of black holes mass BHs (and of coursedecay, heavier since ones) their will life-time is survive presumably even finite, after about all 10 the protons in the universe will expected even a few years ago.• There are lots of black holes• in all mass intervals: porary, Massive PBH 1. Introduction • unusual chemical content) which are at odds with the conventional astrophysics. The origin of most of these black hole is not clear, to say the least. is grossly overpopulated with unexpectedly high• amount of: at least an order of magnitude longer time than the universe age, • • • anism suggested a quarter of centurytion ago [ of primordial black hole (PBH) and peculiar star forma- problem of their formation in ten times younger universe at PoS(MULTIF2019)013 , its M ] in full , It is the 4

A.D. Dolgov M 9 10 · ) 7 . 0 0. ± 5 = . 6 z = ( 0; M 0; = = a a = Q 0, but 0, whatever tiny, electric hairs do not exist. 6= 6= Q γ 2 0. m 6= a 0; 1. = < Q a 0 and < 6= 0 but Q 0. 6= = a γ m 0 to 6= γ , and the angular momentum, spin, characterized by the dimensionless parameter m Q Note that if the photon mass is nonzero, There are four types of the (analytic!) solutions of the General Relativity equations describing Less massive BHs are also observed through emission of X-raysAnother from way the to heated observe BHs gas is around based on studying the star motion aroundAll an these invisible gravitat- methods are indirect. They indicate only that in aBHs small may also volume be spotted a by large the gravitational mass lensing is of some invisible objects. In this way the Because of all that some skepticism concerning an existence of BH was not eliminated,The but form of the signal created by gravitational waves is best fit to the hypothesis that it is The Event Horizon Telescope Collaboration have made a snapshot of BH shadow [ According to General Relativity four and only four different types of BHs can exist. These Kerr-Newman solution (1965) Reissner-Nordström solution (1916,1918), with Kerr solutiion (1963) with Schwarzschild solution (1916), the simplest BH with , which is confined in the limits: 0 • agreement with the GRM87, predictions. at the The distance 16.4 photographed Mpc. BH The is measured BH situated mass in is giant huge, • • Coulomb field around electricallytransition charged from BH completely disappears. There is no continuous a all four possible types of BHs: • most massive BH registered in the present day universe, at the redshift electric charge them. ing object of small size. That’s how the central BH in ourconcentrated. Galaxy Based manifests itself. on the theory,inside General this Relativity volume. (GR), one may conclude that there is aMassive BH Astrophysical Compact Halo Objects (MACHOs)cannot have exclude been that these discovered. invisible One, objects of are course, e.g. some low luminosity stars. recently it was strongly hit byphoto the of registration a of black gravitational hole waves shadow (LIGO (see and below). ) and by the emitted by a coalescinginitial BH BH binary and the with final the onefirst Schwarzschild are observations accurately metric proving determined of the and validity each theirtests of spins BH. were GR are performed Masses measured. only for of for strong These very both gravitational are weak the fields. fields. All numerous earlier solutions are characterized by three parameters, thethe so gravitational called and electric hairs, fields which by can an be observer measured outside through BH. These "hairs" are the BH mass Massive PBH objects, within the accuracy ofsible the telescopes, mechanism and of shine explanation asradiation thousands for in of the the galaxies. process operation of The of collisions onlyhole of the plau- (SMBH) ultra-relativistic in particles central accreting the QSO to center. a Such engine supermassive process is black can the heat the emission surrounding of matter up to million degrees. 2.2 GR solutions predicting black holes PoS(MULTIF2019)013 ] ) = 1 5 g r (2.1) with the

A.D. Dolgov M 8 ≈ M , 2 φ d has the form: θ , and normally quite close to it. 2

M M sin 2 r 1, at the cosmological horizon scale. in elliptic and lenticular galaxies and − ∼ ].

15 Gyr. A longer, more than by an order 2 6 ρ M θ ≈ 9 / d 2 U t r 10 δρ − ∼ 3 2 M dr ) η / 1 ( − 2 dt η GeV is the Planck mass. In the natural system of units (see Sec. = 2 19 ds 10 , but large fluctuations at small scales are not excluded. Such a piece of · 4 2 − . in elliptic galaxies, like Milky Way. , with the gravitational radius (or Schwartzschildt horizon) equal to (see below). There is no convincing explanation of these data. 1 r 10

/ g ≈ ∼ M M r ) ) Pl 7 ρ 2 − / m 1 10 − ] and elaborated later by Carr and Hawking [ ]) could make PBH with masses exceeding millions solar masses and with the extended 1 δρ 5 − 2 = ( and 6 η ∼ BH crated by accretion of matter to the regions with excessive matter density. Presum- is equal to the Newtonian gravitational coupling constant. Primordial black holes (PBH) created at pre-stellar epoch in the very early universe. The 2 Pl Astrophysical black holes, which are created by stellar collapse, when star exhausted its fuel 10 ( m Usually this mechanism leads to creation of PBHs with rather low masses and with sharp This metric has a striking property that an object falling into a BH never cross the horizon (by There are three possible types of BH creation and accordingly the black holes have the names: • The metric around the Schwarzschild black hole with mass However, the known mechanisms of accretion is not efficient enough to create such monsters It is tempting to conclude that the SMBH are primordial and• type of the galaxy is determined • 2 Pl / ∼ m M / (see also [ log-normal mass spectrum which became quite popular recently. almost delta-function mass spectrum. A different mechanism suggested in our paper with J. Silk [ 2 1 the clock of a distantstars. observer). That’s why Zeldovich and Novikov called black2.3 holes as Black frozen holes by creation mechanisms astrophysical BHs, supermassive BHsPBH), in though such galactic a devision centers is (SMBH), rather arbitrary. and primordial blackand holes the internal pressure becameexpected so expected weak to that it be could just not above resist the . neutron Masses star of masses, such 3 BHs are volume would be inside itsand gravitational became radius, a so black it hole. decoupled SuchNovikov from a [ the scenario cosmological of expansion PBH formation has been suggested by Zeldovich and during the available time equal to the universe age by the mass of BH and not vice versa. canonical picture of theirthe creation density is contrast the was following. accidentally very It large, might happen in the early universe that Massive PBH where Instead the observed masswidth: spectrum of BHs in the Galaxy has maximumably at in any large galaxyare there in is the a rangeM supermassive from BH billions (SMBH). solar The masses, masses of these black holes of magnitude, time duration isone necessary. SMBH Moreover lives even SMBH in are almostuniverse found with empty in the space. very age small SMBH about galaxies areare 0.5 also and necessary, -1 but discovered Gyr. their recently origin in Their is quite formation mysterious. young is multifold less probable. Massive seed Normally PoS(MULTIF2019)013 .

M ) 5 at ]. 10

10 , M − 2 6 3 , 1 10 10 × A.D. Dolgov 4 = ( /yr. Thus the in spiral galax-

∼ M

per year and po- M 8 M

− 6 M 10 6 10 − ∼ ∼ 10 ]. × 15 3 ] with the host galaxy having , horizon ˙ per year is required. At present, ∼ 11 14 M , ˙

M M 13 ]. This creates serious problems for 4 , − 10 12 10 × ]. The probability of finding a quadruple 16 2 [ 4 ≈ z . The origin of these BHs is not understood. The accepted . 7 − 2.1 10 ] but some galaxies may have huge BH: e.g. NGC 1277 has the ∼ 9 , , or 60% of its bulge mass. [ 8

M 10 ] to create the SgrA* with the mass 10 7 in giant elliptical and compact lenticular galaxies and , see subsection × ]. Such a structure can only satisfy one of the three scenarios: a triple supermas-

7 . M 17 M 9 9 10 · ) 7 . 0 Hence an inverted picture looks more plausible, when first a supermassive BH was formed and There are some more systems of multiple SMBH in close vicinity, which is highly improbable An orthodox point of view for the explanation of appearance of such structures is merging of Intermediate mass black holes (MBH) are those with the masses in the interval A really striking piece of evidence in favor of creation of SMBH prior to the galaxy formation Every large galaxy and even several smaller ones contain a central supermassive BH with mass Even more puzzling: SMHBs are observed inThere small are galaxies a and few even more in pieces of almost evidence EMPTY indicating that the conventional picture of SMBH ± 5 . a physical association of four quasars at four binaries of SMBH discovered during recent years [ triple [ 6 attracted matter being a seed for subsequent galaxy formation, as it is suggested in refs. [ in the conventional model. There are: • the standard scenario of thecentral formation part of of a central galaxy. supermassive BHs by accretion of matter in the much smaller mass than the SMBH. quasar in such close vicinity is • Nobody expected them and now they came out as if from cornucopia (cornu copiae). According sive black hole (SMBH) interacting system, a triple AGN, or a recoilingtwo SMBH. spiral galaxies creating anmerged elliptical elliptical. galaxy, No leaving other two way or ishard more found to SMBHs create. in the in Heretic traditional but the simpler approach. centerearly suggestion However, universe of is even and that the one seeded primordial SMBH galaxy SMBH is formation formed binaries in the very 3.2 Intermediate mass black holes is a discovery of "A Nearly Naked Supermassive Black Hole"[ X-ray observations constrain the rate of hot gas accretion to central BH of 1 • faith is that these BHsefficiency are is created insufficient by to matter create accretioncalculations them to of during a ref. the central [ Universe seed. life-time, 14.6 Gyr. But, According the to usual accretion the larger than 10 space, where the material to make a SMBH cannot be found. formation is not compatible withthe observations. stellar The bulge mass of of galaxy BH [ is typically 0.1% of the mass of Massive PBH 3. Puzzles of the present day universe 3.1 Supermassive black holes today ies like Milky Way. The most massive( out of them is the recently observed BH with the mass mass the centre of our Galaxy the mean accretion rate oflarization 4 measurements constrain ituniverse near age is the short event by horizon two orders to of magnitude. PoS(MULTIF2019)013 ] was . This ]. The

25 23 M 4 A.D. Dolgov 10 > ]. Definite evidence is 24 , 23 , seeded globular clusters and

M ]. According to the authors state- 3 22 10 ∼ M per one SMPBH with mass 5 ] identified a sample of 305 IMBH candidates . The results provide new circumstantial evi- 10 strongly accreted matter and grew up to billion

21 5 M −

4 4 M ] and more and more are appearing in different mass 4 10 ] the discovery of 204 black holes with masses in the 19 10 [ × 20 ) 9 > . Forty of them, but somewhat more mssive, are found re- 6 .

10 0 · M higher than those of the other comparison clusters under the found in the core of the globular cluster 47 Tucanae [ M residing in galaxy centers and are accreting gas that creates 3 is about 10 ± 5

σ , 2

. <

10 M CDM Universe. 3 M ( M Λ × M 3 5 2 < 10 seeded dwarf galaxies. Three years ago only 10 IMBH, were known 2000 10 − 7 5 × ≈ 4 × ) ." is reported. The group [ 10 2 3 10 M

− ] that such IMBHs are primordial. If the parameters of the log-normal mass < ] the intermediate mass BHs: with − M × 4 5 2 3 18 18 ( BH 10 10 = M ∼ × M ) < M 4 20 10 − 1 × ( It is assumed that all PBH with Very recent a surprising discovery of "A young in the old Universe" [ A very interesting example of IMBH is reported in ref. [ We assumed [ Such a blue cluster seems to be in accord with our prediction of predominantly helium rich It is tempting to conclude that such particular object isOnly a one or primordial two black massive hole, BH as are well observed a in all Globular clusters [ predicted density of IMBHs isaccording sufficient to to the seed published the estimates. formationglobular This of clusters density all of in globular IMBHs clusters galaxies. is indifficult sufficient Our galaxies. to to prediction observe seed them. is the formation that of IMBHs exist in all globular clusters but it is solar masses. 3.3 A strange galaxy intervals with an impressive rate.range In ref. [ characteristic signatures of a type-I . ment an invisible massive object inmolecular line the observations central with the region Atacama of Large ourmorphology Millimeter/submillimeter Array Galaxy, and (ALMA). based kinematics The on of these the streams high-resolution around can a be single reproduced well point through mass two of Keplerian orbits standard model does not have an explanation for the origin of suchdistribution relatively of light PBHs IMBHs. are chosen toPBH fit with the masses LIGO data and the density of SMBH, then the number of announced. There was discovereddentedly a high fraction blue of cluster, blue that star-formingblue galaxies is fraction yet a is hosted local by 0.57, a which galaxy massive is cluster dark 4.0 matter with halo. an The unprece- "bubbles" in the universe.nucleosynthesis Indeed could produce in considerably higher the abundance bubbles ofusual the with 25%. primordial high helium-4, than baryon-to-photon the ratio the big bang other IMBH, mentioned above, whose abundance is difficult to explain other way. with 3 dences for a wandering intermediate-mass blacksuggesting hole also in that the high-velocity Galactic compactin center clouds our (tramp can Galaxy. in be the probes galaxy), of quiescent black holes abound same selection and identification criteria.individual cluster The is only probability 0.003%, to whichformation find challenges and such the evolution current a in standard the high frameworks blue of the fraction galaxy in an Massive PBH to our conjecture [ IMBH with presented for BH with with masses. cently by Chandra with 10 PoS(MULTIF2019)013 , ] ] ], 1 27 28 26 5. So . 12 = 4 Gyr [ A.D. Dolgov U ± t 8 . 74, and 3, as determined from ] and a special search . = 32 67 H = 7 Gyr, according to ref. [ . ]. The central value of the age 0 H ± 29 4 . 8. On the other hand, according to . 13 31 Gyr [ = . 3248 was estimated as 13 0 U o . t ± σ ] 2 46 . , 6 1 ] The origin of this star is mysterious. It may be a compact 31 by the traditional astronomical methods, H ]. For comparison the age of the Earth is 4.54 Gyr. The planet formation is 30 Gyr [ ]. The authors conclude that the origin of the discovered stars is unclear. They might 5 3 . . 1 1 33 + − 6 . High velocity and unusual chemical content stars in the Galaxy Too old stars in the Milky Way: • The Galaxy, as discovered recently, has quite significant number of very fast stats, with veloci- A discovery of high speed low-mass white dwarf (LP 40-365) that "travels at a velocity greater The age of a star in the , HE 1523-0901, was estimated to be about 13.2The Gyr most [ striking example of stellar Methuselah is the metal deficient high velocity subgiant in Let us mention in conclusion a very old planet in the Kepler-10 Planetary System with the Some more references to recently discovered high velocity stars in the galaxy includes the This cannot be so, of course, in the conventional cosmology and astrophysics but bur model [ • Employing thorium and uranium abundances in comparison with each other and with several ] predicts unusual initial chemical content for a small number of stars, so they may look older than primordial star, predicted by the model of refs. [ for very such quicklyGalaxy" [ moving stars: "Gaia DR2 in 6D: Searching for the fastest stars in the ties higher than the escape velocity andstellar of stars velocity with in rather surprising the chemical galaxy content.velocities is The about in normal 1000 the km/sec. range 100-200stellar The km/sec. collapse origin and Some of even pulsars a the tiny are letter non-sphericitymomentum, observed is of sufficient with the to evident. the emitted accelerate neutrino the Pulsars flux up are wouldfaster to created create than 1000 huge km/sec. galactic through recoil escape However, the the velocity origin is of puzzling. the stars moving than the Galactic escape velocitymass elements", and is whose reported peculiar in atmosphere ref. is [ dominated by intermediate- a slow process, it should beHowever, as preceded we by see a in supernova what explosion, formation follows, the of early molecules, universe and is dust. unexpectedly dusty. the solar neighborhood HD 140283 has the age 14 they are. "Our’" stars areis primordial hinted and by they HD may 140283.following have Moreover, subsection. ubusually there high are velocity more in very the fast Galaxy stars as in the Galaxy,age as 10 we see in the "Old, Metal-Poor Extreme Velocity Stars in the Solar Neighborhood" [ which noticeably exceeds the age of inner halo of the Galaxy 11 In this work first time many differentto chronometers, measure such the as star the U/Th, age U/Ir, have Th/Eu been and employed. Th/Os ratios of this star exceeds the universe age by two standard deviations,the if, recent determination of the star age exceed the universe age by more than 10 2 During the last several yearsimproved the since precision not in only determination uranium and ofnuclear thorium the chronometers. abundances stellar but age several other has elements been were drastically used as stable elements the age of metal-poor, halo star BD+17 Massive PBH 3.4 Peculiar stars in the Milky Way the angular fluctuations of CMB and correspondingly PoS(MULTIF2019)013 , f (3.1) 1 for . 0 < f A.D. Dolgov 2 (95% CL) . ]. Briefly, the 0 40 < , f ] gives 39 43 , 38 , . The origin is unknown. It

37 , M 8 . 36 0 < ]. The authors found red host star and . The life-time of main sequence star M ⊕ 34 , M 50 34 12 . . + − 0

, respectively, as is stated in the paper, these 18 M <

9 7 f R . already for = ]. Discovery of three chemically peculiar runaway ]: "A hyper-runaway white dwarf in Gaia DR2 as 0 p U < t 35 35 < m 08 . M 0 and <

M M 27 10 ] is in the interval: and 0.16-0.60 . . 15 0 0 , and is gravitationally unbound to the Milky Way, We rule out . 1 41 + −

− ] has placed the upper limit on the halo fraction, M 15 . 42 0 ] reported registration of 13 - 17 microlensing events towards the Large = 41 host 605 km s M ' gal MACHO group [ MACHOs is the abbreviation for Massive Astrophysical Compact Halo Objects discovered The data on the MACHO abundance presented by different groups are rather controversial. EROS collaboration [ A discovery of a very unusual star is reported in ref. [ And at last, the discovery of this year [ Another puzzling discovery of "A class of partly burnt runaway stellar remnants from peculiar situation is the following. according to the observations [ at 95% CL for the mass range 0 for the objects in the specified above MACHO mass range, while EROS-2 [ Magellanic Cloud (LMC), whichfrom is the significantly known low higher luminosity stars. thandark On the matter the in number other the hand halo. which this The couldmicrolensing amount fraction effects, is originate of not with the sufficient mass respect to density to explain of the all the energy observed objects, density which of created the the dark matter in the galactic halo, through gravitational microlensing by Macholuminous and or Eros even groups. non-luminous)halo, objects They in are masses the invisible about center (very of asignificantly weakly the greater half than Galaxy, of the and density the recently expectedsimilar in solar from mass. the the mass known Andromeda in low (M31) luminosity the galaxy. stars Galactic and Their the density BH is of The present date situation is reviewed and summarized in refs. [ an extragalactic origin. Theunbound Type trajectory, Iax given supernova ejection anomalousspectroscopic scenario elemental follow-up. is abundances This consistent discovery are with reflects detectedoccur recent its often." models in peculiar This that its could suggest be photosphere stellar a ejections via peculiar likely WD or a3.5 remnant MACHOs of a primordial star. a Type Iax supernova primary remnantknown candidate" example Quoting of the an authors: unboundremnant white "We report dwarf to the that a likely is first Type consistentvelocity Iax with being of supernova. the v fully-cooled The primary candidate, LP 93-21, is travelling with a galactocentric Massive PBH be accelerated to high velocity bynumber a of IMBHs. population of IMBH in Globular clusters, if there isplanet sufficient masses of stars, survivors of thermonuclear explosionsranging - between according to 0.20-0.28 theinflated authors. white dwarfs are the "With partly masses burntsupernovae". remnants and of radii either peculiar Type SNIa or electron-capture thermonuclear supernovae" is announced in [ with the solar chemical content ismay larger be than a primordial helium star? PoS(MULTIF2019)013 ] is ] the (3.2) 47 . 49 ], finds

] towards 45 ] with the M 5 . A.D. Dolgov 44 . 47 7 ], where it is

− does not differ M 55 5 10 .

> M M ]. 53 ]. However, according to the 51 ) 1 at the standard local halo density. , ] was published where, on the ba- 1 obtained at 95% confidence level . . 0

0 50 54 − M < f 43 01 . ], some more arguments against abundant 0 ] with masses in still allowed intervals, but > ( 9. while MEGA group presented the upper 2 49 . , M 0 ∼ 1 < 2 for MACHOs with the mass 0 . 8 f 0 DM < ρ < MACHO f ρ 2 . = and

M ] were presented. 2 MACHO f − 49 for the survey of Large Magellanic Clouds. It is considerably less

M ] with an uncertain conclusion. E.g. AGAPE collaboration [ 15 37 , < 36 M ]. On the other hand, the recent discovery of 10 new microlensing events [ < 46

3 [ . M 0 ]. 7 ], the approach of the mentioned works have serious flaws and so their results are ques- − < 48 ] 52 10 f 43 A nice review of the state of the art and some new data is presented in ref. [ The latest investigation on the "end of MACHO era" was presented in ref. [ Later, however, another paper of the Cambridge group [ Some more recent observational data and the other aspects of the microlensing are discussed The data in support of smaller density of MACHOs in the direction to SMC is presented in According to the results of different groups the fraction of MACHO mass density with respect It would be exciting if all DM were constituted by old stars and black holes made from the There is a series of papers claiming the end of MACHO era. For example in ref. [ The new analysis of 2013 by EROS-2, OGLE-II, and OGLE-III collaborations [ Search for microlensing in the direction of Andromeda galaxy (M31) demonstrated some con- In addition to the criticism raised in the paper [ × 6 . much from the previous one.MACHO Together mass, with our microlensing results essentially studies exclude that the provide existence lower of limits such on objects the in the galactic halo". galactic population of MACHOspaper are [ also presented in ref. [ sis of studies ofpessimistic binary conclusions stars, of ref. arguments [ in favor of real existenceconcluded of that MACHOs "the and against upper the bound of the MACHO mass tends to less than 5 Notice a large variance of the results by different groups. tionable. A reply to this criticism is presented in the subsequent paper [ in ref. [ ref. [ to the total mass density of dark matter varies in rather wide range: the Small Magellanic Cloud (SMC).EROS revealed and four five by microlensing OGLE), events which lead towardsfor to the MACHO’s the with SMC upper the limits (one mass by 10 very much in favor of MACHO existence.microlensing The events authors point conclude: to “statistical a studies non-negligiblemass and MACHO remains individual population, uncertain”. though the fraction in the halo high density baryon bubbles as suggested in refs. [ conclusion that some statistical studies and individualMACHO microlensing population, events point though to the a fraction non-negligible in the halo mass remains uncertain. more detailed analysis of this possibility has to be done. tradicting results [ Massive PBH 0 than that measured by the MACHO collaboration in the central region of the LMC. the halo MACHO fraction in the range 0 authors stated "we exclude MACHOs with masses limit This removes the last permitted window for a full MACHO halo for masses PoS(MULTIF2019)013

= M m M 100 are ob-

> M A.D. Dolgov M is analyzed and found to

M ) 29 + 36 ( ]: 39 , and a sharp drop-off above 10

. (surprise, but can be reconciled with stellar evo- M

9

M M 30 ∼ Stellar binaries were formed from common interstellar gas ]. This result agrees with another paper where a peak around 57 ]. Clumping of primordial back holes, due to dynamical friction, [ 56

was found - a puzzle for stellar evolution. (borrowed from K.Postnov M )

2 . M Such BHs are believed to be created by massive star collapse, though a 1 ± 8 . 7 ( ], These features are not easily explained in the standard model of BH formation by .

Formation of BH binaries. 58 M ) 9 , a paucity of sources with masses below 5 It was discovered during the last decade that the BH masses in the Galaxy are concentrated in On the other hand, primordial BH with the observed2. by LIGO masses may be created with Mass of BH in LIGO binaries is up to 50 The problem of the binary formation is simply solved if the observed sources of GWs are the Registration of gravitational waves (GW) from coalescing BH binaries solved long existed An interesting option is that the spatial distribution of MACHOs may be very inhomogeneous Massive BH origin.

− 2. Formation of BH binaries from3. the Low original spins stellar of binaries. the coalescing BHs . 1. Origin of heavy BHs with the masses M 7 the narrow range sufficiently high density. ( 3.6 Mass spectrum of astrophysical BH in the Galaxy • • 1. lution), rumors that a 100 talk at Isaak Markovich Khalatnikov Centennial Conference). clouds and are quite frequentsphericity in leads galaxies. to a If very BH largeof recoil is such velocity created effect of through is the stellar demonstrated BHPopIII collapse, and by stars a the and huge binary small subsequent velocities is formation non- of destroyed. of pulsars BH An in binaries example with the Galaxy.) BH formation from convincing theory is still lacking. To form so heavy BHs, the progenitors should have • binaries of primordial black holes (PBH).non-negligible They probability were to at become rest gravitationally in bound. the comoving volume and may have i.e. the masses twoto orders avoid of too magnitude much higher massstar-forming than galaxies loss but the during they solar are the not mass evolution. observed and in a the Such necessary low heavy amount. metal stars abundance might be present in young be negligible. problems of test of GR forit strong field opens and immediately presented several a more first problems.three direct proof very "In of interesting much BH problems existence. wisdom addressed However, in is our much paper grief". [ In short there are may be much stronger thanhypothesis the would allow clumping to of avoid contradiction dark betweenthe matter the predicted consisting observed high of much density elementary smaller of MACHOs particles. density and of This them based on the log-normal mass spectrum with 8 stellar collapse. 3.7 Gravitational waves from BH binaries and non-isotropic. Duewhere to their density selection is effect, much higher MACHOsdark than matter are the clumping average observed see one. e.g. only For [ a in review over-dense and the clumps list of references on Massive PBH served [ PoS(MULTIF2019)013

] L ]. 14 63 and 68 10

3 Gyr. · . M 1 3 ∼ = A.D. Dolgov 10 is grossly L U t and 30 ∼ z

M ] This result is in agree- 60 , 59 0006. According to their conclusion "This ] much weaker gain of the angular momen- . 0 62 ± , 61 10 1096 . 9 = z 3. Residing in the most massive dark matter halos at their red- > 6 which was created when the universe was about 0.5 Gyr old [ . z 9 ]. ].This galaxy already existed, when the universe age was ≈ 66 8. The discovery of another unexpectedly early created galaxy at red-shift 11 has been detected which was formed earlier than the universe age was z 65 − ≈ 6 z = z ], of the submillimeter (wavelength 870um) detections of 39 massive star-forming galaxies The low value of the BH spins in GW150914 and in almost all (except for three) other events. 3, which are unseen in the spectral region from the deepest ultraviolet to the near-infrared. 67 To finish with the list of these surprises let us mention almost yesterday discovery, reported in An onset of the star formation 250 million years after the Big Bang is claimed in ref. [ The data collected during last several years indicate that the young universe at Several galaxies have been observed at high redshifts, with natural gravitational lens “tele- The discovery of not so young but extremely luminous galaxy with the luminosity 3. However, individual PBH forming a binary initially rotating on elliptic orbit could gain collinear > 11 is reported in ref. [ , when our universe was only a tenth of its present age of 13.8 billion years. "Another way to z

= The authors observed the oxygen line at 0.41 Gyr (or even shorterother galaxies with at larger H). Thisz galaxy is three times more luminous in UV than ref. [ They contribute a tota star-formation-rate density tenultraviolet-bright times galaxies larger at than that of equivalently massive probably with GW151216 . Earlier in the works [ Moreover, galaxy at The galactic seeds, ormight embryonic be black bigger holes, than necessary thoughtdo for possible. you the get Ona creatkon an of of elephant? theM such authors One a of way huge the is galaxy work startgrow P. with Eisenhardt: this a big said baby is "How elephant." to Thepossible." have A BH gone low was spin on already of a billions the sustained seed of binge, is necessary. consuming food faster than typically thought at shifts, they are probably the progenitorsclusters. of Such the a high largest abundance present-day of galaxiesunderstanding massive of in and massive-galaxy massive dusty formation. groups galaxies and in the early universe challenges our precisely determined redshift indicates that the red rest-frame optical colour arises from a dominant scopes, e.g. a galaxy at ment with the GW170729 LIGO event produced by the binarytum with gain masses was 50 obtained. 4. Surprises of the Early Universe overpopulated with unexpectedly high amount of: 4.1 Superluminous young galaxies was announced in ref. [ It strongly constrains astrophysical BHare formation expected to from have close considerable binary angularmassive low-spin systems. momentum BHs but in Astrophysical still dense the BH stellar dynamical clustersPBH is practically formation not do of excluded, not double though rotate difficult. becausevanishingly On vorticity small. the perturbations other in hand, the early universe are known to be spins about 0.1 - 0.3, rising with the PBH masses and eccentricity [ Massive PBH PoS(MULTIF2019)013 ,

] L 74 13 6 1, 10 − . · 9 6 . =

≈ z M L 9 11 is 10 ) appeared A.D. Dolgov 10

≈ M z ∼ 75 Gyr. . 10 M ] with the outrageously 085, luminocity 72 . 7 7. = z during 320 Myr in a halo with a > z

M ], the density of galaxies at 69 ] at the redshift 71 11 black holes appeared so quickly after the big bang ] is about 2200 black holes (to say nothing about 10

73 M

9 M 9 5. It is by far less than is necessary. . , The quasar was formed before the universe reached 0 7

= ] "Rapid emergence of high-z galaxies so soon after big bang may actually M . There is already a serious problem with formation of lighter and less 9 z 70

at 10 M ·

2 10 M 6 were known three years ago, each quasar containing BH with = 10 ] indicated that accretion in this particular case is absent, otherwise the plasma · > 10 2 M 75 z . 10 × , an order of magnitude higher than estimated from the data at lower z. The origin of these 3 In addition to this forty quasars, one more monster was discovered [ To conclude on QSO/SMBH: Another and even more striking example of early formed objects are high z quasars. About 40 It is difficult to understand how 10 According to ref. [ The observation of a 800 million solar mass black hole in a significantly neutral universe at Recent observations by SUBARU practically doubled the number of discovered high z quasars [ The accretion rate, as estimated in ref. [ As is stated in the paper "Monsters in the Dark" [ − 6. It is difficult to understand how 10 ∼ and the mass The quasars are supposed to beconventional supermassive mechanisms black looks holes problematic, and to their say formationSuch the in black least. such holes, short formed time when by the Universechallenges was to less theories than of one the billion formation years andand old, growth galaxies. of present black substantial holes and the coevolutionEven of black the holes origin of SMBHstandard in accretion contemporary physics and universe during thethem is 14 formation observed of Gyr in massive is the seeds present difficult day seem to universe. to explain. be Non- necessary. Neither of so quickly after the big bangmassive without seeds, invoking non-standard both accretion of physics which and are the not formation seen of in the local Universe. quasars with without invoking non-standard accretion physics and theare formation not of massive seen seeds, in both the of local which Universe." 4.2 Supermassive BH and/or QSO should be ionized. redshift 7.5 [ Mpc galaxies is unclear. The maximum redshift QSO is discovered in ref. [ huge mass 1 In particular this group reported the first low luminosity QSO at mass of 3 be in conflict with current understandingof of how the they better came to known be. (andz This probably problem related) is very premature reminiscent appearance of supermassive black holes at luminous quasars which is multifoldthan deepened 10 with billion this solas masses new is "creature". absolutely The forbidden in new the one standard with approach. more Massive PBH stellar component that formedredshift about of about 200 15. million Although years we are after observing the a Big secondary episode Bang, of corresponding star formation to at a the galaxy formed the bulk of its stars at a much earlier epoch." PoS(MULTIF2019)013 34 and of dust . 6

= M A.D. Dolgov 8 z He and traces 10 4 ∼ ratio leading to abundant γ ] confirms earlier observations and 81 12 ]. The authors conclude that the mechanism of dust 82 ]. . ]. Copious Amounts of Dust and Gas is seen in a z=7.5 Quasar Host 80 78 6 is not only enriched by metals but also is quite dusty, as observed in the 3 is presented in [ . 55 [ . 8 > 7 z − = 6 z ∼ z ]. Abundant dust is observed in several early galaxies, e.g. in HFLS3 at 77 ]. Dusty galaxies show up at redshifts corresponding to a Universe which is only about , ]. 79 76 2 , 1 An analysis of the observations and a review of possible scenarios of dust dust production To make dust a long succession of processes is necessary: first, supernovae explode to deliver Existence of heavy elements, molecules, and dust inObservations the of early high redshift universe gamma indicates ray but bursters there (GBR) also indicate a high abundance of In order to explain these dust masses, SNe would have to have maximum efficiency and not Or non-standard big bang nucleosynthesis with large baryon-to- Later made catalogue of the observed dusty sources [ The universe at The medium around the observed early quasars contains considerable amount of “metals” (el- Another possibility is a non-standard BBN in bubbles with very high baryonic density, which in galaxies at heavy elements into spacemake (metals), dust then which metals could cool formplanets. macroscopic and Note pieces form in of molecules, brackets matter, that and turning we subsequently lastly all into are molecules dust early from rocky SN explosions,already at could much be later life time. .Several hundred million years may be enough forsupernova birth at of large living redshifts. creatures. Themore highest GBRs redshift with smaller of but the still observed high GBR redshifts. is 9.4 and there are a few indicates that the number ofcanonical theory. dusty sources is an order of magnitude larger than predicted by the formation of heavy elements, see below. destroy the dust which theythe formed. early universe Therefore, were the formedinstance either observed the by amounts grain efficient growth of in supernovae dust the or in interstellar by medium. the a galaxies non-stellar in mechanism, for formation in galaxies at highexplosions redshift of is supernovae still (SNe) unknown. arestantially Asymptotic possible giant contribute dust branch to producers, (AGB) dust stars production. andthe and non-stellar amounts However, processes of AGB dust stars may observed are sub- in not the efficient galaxies. enough to produce papers [ Galaxy [ 500 Myr old. Very highimplied past by star the formation observations is [ needed to explain the presence of ements heavier than He). According to the standard picture, only elements up to allows for formation of heavy elementsrefs beyond [ lithium in the very early universe, as suggested in Massive PBH 4.3 Evolved chemistry, dust, supernovae, and gamma-bursters of Li, Be, B were formedwas by about big a bang 100 hucleosynthesis second (BBN), old. whichcreated The took much heavier place elements, later when according by the to universe stellar theexplosions. nucleosynthesis conventional cosmology, and Hence, were dispersed an in evident the butously interstellar not with space the necessarily QSO by true formation supernova conclusion ato was rapid a that large star prior number formation of to should supernovae take or enriching place. simultane- interstellar These space by stars metals should through evolve their explosions. in A1689-zD1 at PoS(MULTIF2019)013 ]. 85 (5.1) (5.2) (5.3) ]. The au- A.D. Dolgov 82 GeV. 19 ]. Now in many works 10 · 84 22 0. Such scalar bosons may . 1 6= = 1. In this system the Newtonian , B ] but in tension with the Standard )] Pl = 1 , α k m )] ) 2 0 3 was reviewed in ref. [ θ . + M 8 ) = / θ π − 2 2 M cos4 ( . It can be easily generalized to a superpo- ( 6 ( 0 / 2 − h = M cos ln 1 z , ( = γ − γ 4 c | , − 1 13 [ [ χ µ | 2 | λ χ exp | 2 2 µ ) = : m 2 χ ∗ = ( χ , where th Planck mass is λ ) = 2 2 Pl U ∗ χ dN dM ( m m m / ]. The highest redshift of the observed GBR is 9.4 and there are a 1 + U 2 83 = χ 2 N m G Such a simple form pf the PBH mass spectrum is a resultLog-normal result mass of spectrum quantum of diffusion PBHs of was bary- rediscovered later in ref. [ Here we use the natural system of units where the speed of light, the reduced Planck constant, The necessary star formation rate for explanation of these early GBRs isThese facts at are in odds good agreement with with the the our 1993 model [ Dust production scenarios in galaxies at high Observations of high redshift gamma ray bursters (GBR) also indicate a high abundance of In 1993 we suggested a model AD-JS of PBH creation which allowed an abundant formation onic scalar field during inflation. Probably such spectrum is a general consequence of diffusion. gravitational constant is and the Boltzmann constant are all equal to unity: sition of several log-normal spectra with several separated maxima. depending only on three constant parameters: such spectrum is postulated withouton any the supersymmetry justification. (SUSY) In motivated baryogenesis,SUSY our proposed predicts model by existence the Affleck of and PBH scalars Dine creation with (AD) non-zero was [ baryon based number, and/or of the mass term, condense along flat directions of the quartic potential: canonical star formation theory.photon ratio leading Non-standard to big formation of bang heavy nucleosynthesis elements in with the very large early baryon-to- universe may be needed. few more GBRs with smaller but still high redshifts. supernova at large redshifts [ of very massive black holes with the log-normal mass spectrum: Massive PBH thors concluded that the mechanism ofAsymptotic dust giant formation branch in galaxies (AGB) at starsducers, high and redshift and explosions is non-stellar still of processes unknown. supernovae may (SNe)are substantially not are contribute efficient possible to enough dust dust to production. produce pro- In the However, order amounts AGS to of explain dust these dust observed masses, inthe SNe the dust would galaxies. have which to they have formed. maximumuniverse efficiency and Therefore, were not the formed destroy observed either amounts bythe of efficient grain dust growth supernovae in in or the the by interstellar galaxies a medium. in non-stellar the mechanism, early for instance Cosmological Model. 5. Possible mechanism explaining the surprises in the data PoS(MULTIF2019)013 (5.4) (5.5) (5.6) -plane. χ A.D. Dolgov , created by can quantum- 10 . ) − χ . c . 10 · h 6 + 2 ≈ χ still during inflation but β 2 1 m Φ can acquire a large baryonic χ could be created, occupying a ) + ( . β c . h + . 4 0. 0 χ ( . 6= 1 χ ) = . λ B 2 χ | ( is open only during a short period, cosmolog- 0 χ ) + | is small but non-vanishing, both baryonic and 1 ˙ U 2 θ 2 | Φ 14 α + χ σ 0, charge symmetry (between particles and antipar- = | 0, Its evolution is described by the equation similar ˙ ≈ χ ( passes through the value χ 6= = H ln B Φ Φ 3 α χ 4 | + χ | ¨ . If χ would have have the almost the same density as the average λ α (the first term in the equation below): w.r.t. phase rotation. e β | + ) Φ 2 m χ | ) ( is normally away from the origin and, when inflation is over, starts 1 = U Φ χ m . If CP-odd phase − χ Φ ( and the window in the potential to the flat directions is open and 2 is equal to : | ) 1 χ θ χ | Φ i g ( = exp . to the inlfaton field | 9 U χ χ − 0, the angular momentum, B, can generated by a different direction of the quartic and | 6= is close to = . m decays transferred the accumulated baryonic charge to that of quarks in B-conserving pro- Φ χ χ χ We slightly generalized the original Affleck-Dine model introducing a general renormalizable If If the window to flat direction, when If Initially (after inflation) Initially the bubble with large In Grand Unified version of SUSY baryonic number is naturally non-conserved, which is coupling of Baryonic charge of Due to instability of effectively massless fieldnamber. in De It Sitter is like analogous stage toThe mechanical angular momentum incess. two dimensional AD complex baryogenesis couldobserved lead 10 to baryon asymmetry of order of unity,quadratic much valleys larger at than low the antibaryonic domains might be formed withMatter possible and dominance antimatter of domains one may of exist them. but globally fluctuate to acquire ratherderived high by Starobinsky, amplitude. generalized to a It complex field evolves according to quantum diffusion equation not too close to the end of it. ically small but possibly astronomicallysmall large fraction bubbles of with the high universe, while the rest of the universe has normal to that governing the motin of a point-like particle in Newtonian mechanics: Massive PBH where to evolve down to the equilibrium point, The other terms in this potentialcorrections. presents We the assume usual that Affleck-Dine potential the with inflaton one loop radiation small cosmological density because before the QCDthe phase initial transition quarks perturbations are are essentially the masslessOnly and isocurvature after ones, the though QCD they phaseisocurvature might transition perturbations have transformed when quite into massless density large quarks perturbations. amplitude. number turn The can into bubbles heavy with either high nucleons form baryonic the PBHsize. original or compact stellar like objects, depending on their magnitude and reflected in non-invariance of ticles) C and CP are broken. PoS(MULTIF2019)013 (5.7) A.D. Dolgov density. B n 10 universe: abundant pop- ∼ z sec. 5 2 − ) 2 10 Φ & − t Φ (( 2 ) in the core of globular cluster and the observed 1

Φ 15 M − , could be: Φ γ ( 2 n | / χ B n ∼ | = U β " stars may exist; the older age is mimicked by the unusual initial chemistry. U t Such mechanism of massive PBH formation is very much different from other ones studied The emerging universe looks like a piece ofThe outcome, Swiss depending cheese, on where holes are high baryonic A modification of inflaton interaction with scalar baryons as e.g. may be negative leading to compact antistars which could survive annihilation with the homo- 5. There is persuasive data in favor of the inverted picture of galaxy formation, when first a 1. Natural baryogenesis model leads to abundant formation of PBHs and compact stellar-like 2. These objects had originally log-normal mass spectrum, though it may be subsequently dis- 7. An existence of supermassive black holes observed in all large and some small galaxies and 14. A possible by-product: plenty of (compact) anti-stars, even in the Galaxy, not yet excluded 10. Explanation of origin of BHs with 2000 4. The considered mechanism solves the numerous mysteries of PBHs with log-normal mass spectrum. Compact stellar-like objects, as e.g. cores of red giants. 11. A large number of the recently observed IMBH was predicted. 6. Inverted picture of galaxy formation is advocated. 8. "Older than 9. Existence of high density invisible "stars" (machos) is understood. β 3. PBHs formed at this scenario can explain the peculiar features of the sources of GWs observed Disperse hydrogen and helium clouds with (much) higher than average 12. A large fraction of dark matter or 100% can be made of PBHs. in the literature. Theture fundament fluctuations of at relatively PBH small creation scales,isocurvature is with perturbations build practically are at vanishing in density inflation chemical perturbations.generated by content rather Initial making late of large after massless the isocurva- quarks. QCD phase Density transition. perturbations are density objects occupying a minor fraction of the universe volume. objects in the early universe after QCD phase transition, by observations. Massive PBH • • • • geneous baryonic background. gives rise to a superposition of two log-normal spectra or multi-log. 6. Conclusion • density of GCs is presented. • • 13. Clouds of matter with high• baryon-to-photon ratio may exist. torted due to matter accretion, especially• for very heavy ones. by LIGO. • • ulation of supermassive black holes,galaxies, and early evolved chemistry created including gamma-bursters dust. • and supernovae, early bright supermassive BH seeds are formed and• later they accrete matter forming galaxies. • even in almost empty environment is• naturally explained. • • PoS(MULTIF2019)013 , 659 . (2004), (2017) 604 A.D. Dolgov 834 , published in (2018) 115 61 (2006) 49 646 (2019) L4 Mon. Not. R. Astron. Soc. , (1974), 399. Phys.Usp. 875 BH. 5 168 , 10 − 4 A Cool Accretion Disk around the (2018) 121; First M87 Event Horizon Telescope 188 10. = z 16 Inhomogeneous baryogenesis, cosmic antimatter, and BHs, dwarfs by 10 (2012) 729 [asro-ph/1211.6429]. (2019) 83. 4 (1967), 602. 491 10 570 , − 10 , 3 The Hypothesis of Cores Retarded during Expansion and the Hot (2009) 229 [hep-ph/0806.2986]. Nature Black holes in the early Universe, MNRAS (2015) 74 [astro-ph/1501.01375 ]. B807 On the Black Hole Mass - Bulge Mass Relation, Astrophys. J. Lett. 518 A compact supermassive binary black hole system. Ap. J. A possible close supermassive black-hole binary in a quasar with optical Baryon isocurvature fluctuations at small scales and baryonic dark matter, , [asrto-ph/1709.06258]. A Nearly Naked Supermassive Black Hole. The Astrophysical Journal, New orbit solutions for the precessing binary black hole model of OJ 287, Ap.J (1993) 4244. A candidate sub-parsec binary black hole in the NGC 7674 Massive and supermassive black holes in the contemporary and early Universe and The Spitzer/IRAC view of black hole - bulge scaling relations D47 (2011) 1479. [asro-ph/1012.3073]. Results. IV. Imaging the Central Supermassive[astro-ph.GA/1906.11240]. Black Hole, Astrophys.J. Cosmological Model, Sov. Astron. Galactic Centre Black Hole, Nature, (2007) 1074 periodicity, Nature, [astro-ph/1705.06859]. L89 [astro-ph/0402376] 184 [astro-ph/1606.04067]. Nature Astronomy [astro-ph/0604042]. dark matter, Nucl.Phys. 413 problems in cosmology and astrophysics, Usp.Fiz.Nauk, Phys.Rev. Extreme claims: Inverted picture of galaxy formation: seedingSeeding of of galaxies globular by clusters SMPBH by or 10 IMPBH; Black holes in the universe arePrimordial mostly BHs primordial. make all or dominantAll part QSO of were dark created matter. in theMetals very and early dust universe. are made much earlier than at [5] Ya,B. Zeldovich, I.D. Novikov, [6] B.J. Carr, S.W. Hawking, [7] E.M. Murchikova, E.S. Phinney, A. Pancoast, R.D. Blandford, [8] Häring N., Rix H.-W., [4] Event Horizon Telescope Collaboration (K. Akiyama et al) [9] E. Sani, et al, [3] A.D. Dolgov, [2] A.D. Dolgov, M. Kawasaki, N. Kevlishvili, [1] A. Dolgov, J. Silk, [15] M.J. Graham et al. [12] P. Kharb, et al [13] C. Rodriguez et al. [14] M.J. Valtonen, [11] J.J. Condon, et al [10] R.C.E, van den Bosch, et al., References • • • • • • Massive PBH PoS(MULTIF2019)013 , 1704 Ap.J. , A.D. Dolgov 3248 o ´ LÅŠ 2.4 in the [astro-ph/1908.01666]. (2012) 90 [astro-ph/1205.6802]. 486 , Nature , 17 A Planetary Microlensing Event with an Unusually RED Gaia DR2 in 6D: Searching for the fastest stars in the (2014) 154 [astro-ph/1405.7881]. SDSS J1056+5516: A Triple AGN or an SMBH Recoil An intermediate-mass black hole in the centre of the globular (2007) L117 [astro-ph/0703414]. 789 [astro-ph/1802.01567]. [astro-ph/1805.01467]. , (2017) 203 [[astro-ph/1702.02149]. 660 (2015), 779. (2013) L12 [astro-ph/1302.3180]. 542 , , 2047 (2010) [astro-ph/1001.2707]. 348 A hyper-runaway white dwarf in Gaia DR2 as a Type Iax supernova primary (2017) 680 [astro-ph/1708.05568]. , 765 Quasar quartet embedded in giant nebula reveals rare massive structure in 42 Globular Cluster Seeding by Primordial Black Hole Population, JCAP A Population of Bona Fide Intermediate Mass Black Holes Identified as Low Evidence for an intermediate-mass black hole in the globular cluster NGC 6624 357 A young galaxy cluster in the old Universe, Nature Indication of Another Intermediate-mass Black Hole in the Galactic Center, Astrophys.J. [astro-ph/1908.00670]. , , , HD 140283: A Star in the Solar Neighborhood that Formed Shortly After the Big Intermediate-mass black holes in dwarf galaxies out to redshift ôc Old, Metal-Poor Extreme Velocity Stars in the Solar Neighborhood, The chemical composition and age of the metal-poor halo star BD+17 et al The Kepler-10 Planetary System Revisited by HARPS-N: A Hot Rocky World and Discovery of HE 1523-0901: A Strongly r-Process Enhanced Metal-Poor Star with (2017) 2114 [astro-ph/1705.01612]. [astro-ph/1712.03909]. An unusual white dwarf star may be a surviving remnant of a subluminous Type Ia Microlensing as a probe of the Galactic structure: 20 years of microlensing optical depth , [astro-ph/1806.06106]. The Age of the Milky Way Inner Halo 468 [astro-ph/1804.10607]. , (2002) 861 [astro-ph/0202429]. Detected Uranium Bang Astrophys. J. Lett. (2017) 036, [astro-ph/1702.07621]. 572 Candidate?" Chandra COSMOS Legacy Survey, cluster 47 Tucanae MNRAS [astro-ph/1803.04330]. [astro-ph/1812.10733]. Luminosity Active Galactic Nuclei distant universe, Science a Solid Neptune-Mass Planet Ap J. supernova, Science Galaxy, Source Star [astro-ph/1805.03194] remnant candidate studies, Gen. Rel. Grav. [28] A. Frebe, et al [29] H. E. Bond, et al, Massive PBH [16] J.F. Hennawi J.F., et al, [17] E. Kalfountzou, M.S. Lleo, M. Trichas, [19] M. Mezcua, et al [30] X. Dumusque, [31] Vennes et al, [27] J. Kalirai, [32] K. Hattori et al. [33] T. Marchetti, E. M. Rossi A.G.A. Brown [34] D.P. Bennett, A. Udalski, I.A. Bond, et al, [35] N.J. Ruffini, A.R. Casey, [18] A. Dolgov, K. Postnov, [36] M. Moniez, [21] I.V. Chilingarian, et al. [23] B. Kiziltan, H. Baumgardt, A. Loeb, [20] He-Yang Liu, et al, it A Uniformly Selected Sample of Low-Mass Black Holes in Seyfert 1 Galaxies [22] S. Takekawa, et al., [24] Perera B.B.P., et al., [25] T. Hashimoto, et al, [26] .J. Cowan, et al PoS(MULTIF2019)013 A , 947 12 Usp. Fiz. A.D. Dolgov On the Reported , no. 2, 161 (2015) , 233 (2004) , 1093 (2008) , 806 352 , 895 (2007) (2014) 183; [ 684 57 462 , 1582 (2013) , 387 (2007) [astro-ph/0607207]. 435 469 Microlensing events from the 11-year , [astro-ph/0505167]. , 11 (2009) [astro-ph/0903.1644]. Microlensing towards the SMC: a new Solving puzzles of GW150914 by primordial 396 18 , 464 (2005) [astro-ph/0412443]. Antimatter and antistars in the universe and in the Limits on the Macho Content of the Galactic Halo from The MACHO project: Microlensing results from 5.7 years 359 Lightcurve classification in massive variability surveys, Lightcurve classification in massive variability surveys 2: , 281 (2000) [astro-ph/0001272]. , 311 (2004) [astro-ph/0307437]. The M31 microlensing event WeCAPP-GL1/Point-AGAPE-S3: 542 The end of the MACHO era: limits on halo dark matter from stellar 601 , 1373 (2003) [astro-ph/0211121]. Is there a microlensing puzzle? Contamination in the MACHO dataset and the puzzle of LMC 341 , (2016) 036 [astro-ph/1611.00541]. , (2015) 023516 [astro-ph/1409.5736] 92 Massive primordial black holes in contemporary universe Spectroscopic Studies of the Two Eros Candidate Microlensed Stars, Astron. 1611 , , [EROS-2 Collaboration], [MACHO Collaboration], Mirror matter and other dark matter models, Phys. Usp. , 168 (1995) [astro-ph/9411051]. et al. et al. 299 et al. , (2014) 194]. Astrophysical Applications of Gravitational Microlensing, Res. Astron. Astrophys. 184 , Death of the MACHO Era, Mon. Not. Roy. Astron. Soc. [astro-ph/0404232]. microlensing, Mon. Not. Roy. Astron. Soc. halo wide binaries, Astrophys. J. (2012) [astro-ph/1207.3720]. Mon. Not. Roy. Astron. Soc. Transients towards the Large Magellanic Cloud, Mon. Not. Roy. Astron. Soc. [astro-ph/1504.07246]. [astro-ph/0805.0137]. new analysis of the MEGA M31[astro-ph/0610239]. microlensing events, Astron. Astrophys. observations of the Wendelstein Calar Alto Pixellensing Project, Astrophys. J. evidence for a MACHO component in the dark halo of M31?, Astrophys. J. [astro-ph/1308.4281]. analysis of OGLE and EROS results, Mon. Not. Roy. Astron. Soc. Nauk the EROS-2 Survey of the Magellanic Clouds, Astron. Astrophys. Astrophys. Galaxy, Phys. Rev. D of LMC observations, Astrophys. J. black holes, JCAP [astro-ph/1905.10972]. [53] N. W. Evans and V. Belokurov, [54] D. P. Quinn, M. I. Wilkinson, M. J. Irwin, J. Marshall, A. Koch and V. Belokurov, [52] K. Griest and C. L. Thomas, [50] V. Belokurov, N. W. Evans and Y. Le Du, [51] V. Belokurov, N. W. Evans and Y. Le Du, [49] J. Yoo, J. Chaname and A. Gould, [48] S. Mao, [46] G. Ingrosso, S. Calchi Novati, F. De Paolis, P. Jetzer, A. A. Nucita, G. Scarpetta and F. Strafella, [47] C.-H. Lee, A. Riffeser, S. Seitz, R. Bender and J. Koppenhoefer, [45] A. Riffeser, S. Seitz and R. Bender, [44] S. Calchi Novati, S. Mirzoyan, P. Jetzer and G. Scarpetta, [38] S. I. Blinnikov, A. D. Dolgov, K. A. Postnov, [43] P. Tisserand Massive PBH [37] S. I. Blinnikov, [39] S. Blinnikov, A. Dolgov, N. K. Porayko and K. Postnov, [40] D. Dolgov, S. Porey, [42] J. P. Beaulieu [41] C. Alcock PoS(MULTIF2019)013 762 1906 (2019) 557 (2018) 150 1905 A.D. Dolgov 869 , no.5 (2014) 120 (2011) 616 147 Galaxy, Astrophys. J. , [astro-ph/1901.05963]. 474 11 Monsters in the Dark: , Astrophys. J. ∼ 6 = Mass Measurements of Black Holes in X-Ray Small-scale clumps of dark matter, Phys. Usp. The Black Hole Mass Distribution in the (2012) 36 [astro-ph/1205.1805]. , no. 2, 159 (2014) [astro-ph/1406.5169]. , no.4 (2018) 5016 [astro-ph/1801.07685]. 757 19 790 , [astro-ph/1903.08177]. 476 Galaxy in the Rest-Optical with Spitzer/IRAC and the Spin of Primordial Black Holes Spins of black holes in coalescing compact binaries, Early growth of typical high redshift black holes seeded by The most luminous galaxies discovered by WISE, Astrophys. 11 The end of the MACHO era- revisited: new limits on MACHO , ≈ et al , 3 (2014)] [astro-ph/1405.2204]. Spins of primordial binary black holes before coalescence, JCAP, 184 (2010) 1918 [astro-ph/1006.2834]. (2012) 406 [astro-ph/1204.2305]. 725 , no. 1 (2016) L51 [astro-ph/1604.00413]. (2019) No. 11, [astro-ph/1907.04218]. A luminous quasar at a redshift of z = 7.085, Nature, An ultra-luminous quasar with a twelve-billion-solar-mass black hole at redshift The onset of star formation 250 million years after the Big Bang, Nature, , , Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). V. Quasar 489 62 461 , (2015) 512 [astro-ph/1502.07418]. The initial spin probability distribution of primordial black holes, JCAP , A highly magnified candidate for a young galaxy seen when the Universe was 500 , A dominant population of optically invisible massive galaxies in the early Universe, et al et al , Detection of a Lensed z CLASH: Three Strongly Lensed Images of a Candidate z et al 518 , (2019) no.7768, 211 [astro-ph/1908.02372]. , et al. The Premature Formation of High-Redshift Galaxies, Astronom. J. et al. et al 572 et al (2015) 90 [astro-ph/1410.1751] , 1 (2014) [Usp. Fiz. Nauk 805 masses from halo wide binaries, Astrophys. J. 57 Physics-Uspekhi (2019) 044 [astro-ph/1904.00570]. 018 [astro-ph/903.01179]. Myrs old, Nature, (2013) 32 [astro-ph/1211.3663]. J. [astro-ph/1811.01963]. Galaxy, Astrophys. J. Transients: Is There a Mass Gap, Astrophys. J. Inferred SFR, Stellar Mass, and Physical Size Nature, Luminosity Function and Contribution to Cosmic Reionization at z (2018) 392 [astro-ph/1805.05966]. [astro-ph/1403.0908]]. [astro-ph/1106.6088]. 6.30, Nature direct collapse, Mon. Not. Roy. Astron. Soc. Predictions for Luminous Galaxies in theRoy. Early Astron. Universe Soc. from the BlueTides Simulation, Mon. Not. [56] V. S. Berezinsky, V. I. Dokuchaev and Y. N. Eroshenko, [57] F. Ozel, D. Psaltis, R. Narayan and J. E. McClintock, [61] M. Mirbabayi, A. Gruzinov and J. Noreña, [66] D. Lam [60] K. Postnov, A. Kuranov and N. Mitichkin, [63] W. Zheng [64] D. Coe [65] Chao-Wei Tsai, P.R.M. Eisenhardt Massive PBH [55] M. A. Monroy-Rodriguez and C. Allen, [59] K. Postnov and N. Mitichkin, [62] V. De Luca, et al [58] L. Kreidberg, C. D. Bailyn, W. M. Farr and V. Kalogera, [67] T. Wang [68] T. Hashimoto, et al [74] Y. Matsuoka [69] D. Waters, S. M. Wilkins, T. Di Matteo, Y. Feng, R. Croft and D. Nagai, [71] D.J. Mortlock, [72] Xue-Bing Wu [73] M. A. Latif, M. Volonteri and J. H. Wise, [70] F. Melia, PoS(MULTIF2019)013 451 (2016)

823 M A.D. Dolgov , Astron. 5 3 . , no. 2 (2016) 10 8 − ∼ 462 6 (1985) 361. 249 ?, Mon. Not. Roy. Astron. Soc. 1 zD Quasar Host Galaxy, Astrophys. J. , [astro-ph/1505.04758]. − 5 . 7 = 1689 Jet-powered supernovae of galaxy A (2016) 84. , no.2 (2015) 023524 [astro-ph/1501.07565]. 5 . 7 92 20 319 = Dust production scenarios in galaxies at z Massive Primordial Black Holes from Hybrid Inflation as Dark A New Mechanism for Baryogenesis, Nucl. Phys. B A merger in the dusty, z Dusty Galaxies at the Highest Redshifts Galaxies at High Redshift and Their , Copious Amounts of Dust and Gas in a z , The dust mass in z > 6 normal star forming galaxies Mon. Not. R. Astron. Soc., (2018) 473 [astro-ph/1712.01860] HerMES: A search for high-redshift dusty galaxies in the HerMES Large Mode et al (2019) L13 [astro-ph/1904.11185]. , et al The sudden appearance of dust in the early Universe 553 Do you foresee primordial black holes as a source of spectral distiortion of CMBR? et al An 800-million-solar-mass black hole in a significantly neutral Universe at redshift 624 et al (2017) L8 [astro-ph/1712.01886]. Yes, they can create spectral distortion at the level which leads to noticeable constraints ´ sniewska and M.J. Michałowski, 851 , no.1 (2017) 138 [astro-ph/1603.03222]. population III stars are observable by83 Euclid, [astro-ph/1512.03058]. WFIRST, WISH, and JWST, Astrophys. J. Matter and the seeds of Galaxies, Phys. Rev. D 466 Lett. (2015), 70 [astro-ph1505.01841]. Survey - Catalogue, number counts and1989 early [astro-ph/1601.02665] results, Mon. Not. Roy. Astron. Soc. Astrophys. 7.5, Nature, Evolution Over Cosmic Time, IAU Symposium [85] I. Affleck and M. Dine, DISCUSSION BATISTELLI: DOLGOV: in some interesting mass intervals. [84] S. Clesse and J. Garcia-Bellido, [80] M. Mancini et al, [83] T. Matsumoto, D. Nakauchi, K. Ioka and T. Nakamura, [79] B. Venemans [81] V. Asboth [82] A. Le [78] K. K. Knudsen [77] L. Mattsson, Massive PBH [75] E. Bañados [76] D.L. Clements et al