scholarly journals Calibrating the binary black hole population in nuclear star clusters through tidal disruption events

2020 ◽  
Vol 500 (4) ◽  
pp. 4307-4318
Author(s):  
Giacomo Fragione ◽  
Rosalba Perna ◽  
Abraham Loeb
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Star Clusters ◽  
Mass Function ◽  
Intermediate Mass ◽  
Tidal Disruption ◽  
Scientific Question ◽  
Binary Black Hole ◽  
The Masses ◽  
Optical Transient

ABSTRACT As the sensitivity of gravitational wave (GW) instruments improves and new networks start operating, hundreds of merging stellar-mass black holes (SBHs) and intermediate-mass black holes (IMBHs) are expected to be observed in the next few years. The origin and distribution of SBH and IMBH binaries in various dynamical environments is a fundamental scientific question in GW astronomy. In this paper, we discuss ways tidal disruption events (TDEs) may provide a unique electromagnetic window into the assembly and merger of binary SBHs and IMBHs in nuclear star clusters (NSCs). We discuss how the host NSC mass and density and the slope of the BH mass function set the orbital properties and the masses of the binaries that undergo a TDE. For typical NSC properties, we predict a TDE rate of ∼10−6–10−7 yr−1 per galaxy. The light curve of TDEs in NSCs could be interrupted and modulated by the companion BH on the orbital period of the binary. These should be readily detectable by optical transient surveys such as the Zwicky Transient Facility and LSST.

scholarly journals Monte Carlo modeling of globular star clusters: many primordial binaries and IMBH formation

2014 ◽  
Vol 10 (S312) ◽  
pp. 213-222
Author(s):  
Mirek Giersz ◽  
Nathan Leigh ◽  
Michael Marks ◽  
Arkadiusz Hypki ◽  
Abbas Askar
Keyword(s):  
Black Holes ◽  
Monte Carlo ◽  
Black Hole ◽  
Star Clusters ◽  
Orbital Parameter ◽  
Intermediate Mass ◽  
Cluster Evolution ◽  
Global Cluster ◽  
Cluster Properties ◽  
Intermediate Mass Black Holes

AbstractWe will discuss the evolution of star clusters with a large initial binary fraction, up to 95%. The initial binary population is chosen to follow the invariant orbital-parameter distributions suggested by Kroupa (1995). The Monte Carlo MOCCA simulations of star cluster evolution are compared to the observations of Milone et al. (2012) for photometric binaries. It is demonstrated that the observed dependence on cluster mass of both the binary fraction and the ratio of the binary fractions inside and outside of the half mass radius are well recovered by the MOCCA simulations. This is due to a rapid decrease in the initial binary fraction due to the strong density-dependent destruction of wide binaries described by Marks, Kroupa & Oh (2011). We also discuss a new scenario for the formation of intermediate mass black holes in dense star clusters. In this scenario, intermediate mass black holes are formed as a result of dynamical interactions of hard binaries containing a stellar mass black hole, with other stars and binaries. We will discuss the necessary conditions to initiate the process of intermediate mass black hole formation and the dependence of its mass accretion rate on the global cluster properties.

THE PERIODICITY ANALYSIS OF THE LIGHT CURVE OF PKS 0735+178 AND IMPLICATIONS FOR ITS CENTRAL STRUCTURE

2004 ◽  
Vol 13 (04) ◽  
pp. 771-782 ◽  
Author(s):  
S. X. DING ◽  
G. Z. XIE ◽  
E. W. LIANG ◽  
S. B. ZHOU ◽  
L. MA
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Light Curve ◽  
Observation Data ◽  
Binary Black Hole ◽  
Periodicity Analysis ◽  
Power Spectrum Method ◽  
Hole Model ◽  
The Masses ◽  
Good Agreement

The observation data in the B band for BL Lacerate object PKS 0735+178 during 1970–1998 from twenty two publications have been compiled into a light curve. The light curve shows that PKS 0735+178 is very active and exhibits very complicated non-sinusoidal variations. Using both Jurkevich's method and Power spectrum method to analyze these data we have found two periods of 5.26±0.98 years and 1.24±0.05 years for the outbursts in PKS 0735+178. It is of interest to note that the results of the two methods are the same (almost). In addition, these values are in good agreement with the results found by Smith et al.47 and Webb et al.61 We also apply the binary black hole model to explain the central structure of this object and obtain the masses of the primary and secondary black holes are 1.7×109M⊙ and 2.88×107M⊙ respectively. It should be monitored in future to obtain more data for further analysis to test the hypothesis.

scholarly journals mocca-survey Database I: Binary black hole mergers from globular clusters with intermediate mass black holes

2020 ◽  
Vol 498 (3) ◽  
pp. 4287-4294
Author(s):  
Jongsuk Hong ◽  
Abbas Askar ◽  
Mirek Giersz ◽  
Arkadiusz Hypki ◽  
Suk-Jin Yoon
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Waves ◽  
Globular Clusters ◽  
Stellar Mass ◽  
Intermediate Mass ◽  
Binary Black Holes ◽  
Black Hole Binaries ◽  
Binary Black Hole ◽  
Intermediate Mass Black Holes

ABSTRACT The dynamical formation of black hole binaries in globular clusters that merge due to gravitational waves occurs more frequently in higher stellar density. Meanwhile, the probability to form intermediate mass black holes (IMBHs) also increases with the density. To explore the impact of the formation and growth of IMBHs on the population of stellar mass black hole binaries from globular clusters, we analyse the existing large survey of Monte Carlo globular cluster simulation data (mocca-survey Database I). We show that the number of binary black hole mergers agrees with the prediction based on clusters’ initial properties when the IMBH mass is not massive enough or the IMBH seed forms at a later time. However, binary black hole formation and subsequent merger events are significantly reduced compared to the prediction when the present-day IMBH mass is more massive than ${\sim}10^4\, \rm M_{\odot }$ or the present-day IMBH mass exceeds about 1 per cent of cluster’s initial total mass. By examining the maximum black hole mass in the system at the moment of black hole binary escaping, we find that ∼90 per cent of the merging binary black holes escape before the formation and growth of the IMBH. Furthermore, large fraction of stellar mass black holes are merged into the IMBH or escape as single black holes from globular clusters in cases of massive IMBHs, which can lead to the significant underpopulation of binary black holes merging with gravitational waves by a factor of 2 depending on the clusters’ initial distributions.

scholarly journals Eccentric binary black hole mergers in globular clusters hosting intermediate-mass black holes

2019 ◽  
Vol 488 (3) ◽  
pp. 4370-4377 ◽  
Author(s):  
Giacomo Fragione ◽  
Omer Bromberg
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Globular Clusters ◽  
Dynamical Friction ◽  
Intermediate Mass ◽  
Triple Systems ◽  
Binary Black Hole ◽  
Binary Orbit ◽  
Short Time ◽  
Intermediate Mass Black Holes

Abstract Globular clusters (GCs) may harbour intermediate-mass black holes (IMBHs) at their centres. In these dynamically active environments, stellar-mass black holes (SBHs) sink to the centre soon after formation, due to dynamical friction and start interacting among themselves and with the central IMBH. Likely, some of the SBHs will form bound systems with the IMBH. A fraction of those will be triple systems composed of binary SBHs and the IMBH acting as a third distant perturber. If the SBH binary orbit is sufficiently inclined, it can develop Lidov–Kozai (LK) oscillations, which can drive the system to high eccentricities and eventually to a merger due to gravitational wave (GW) emission on short time-scales. In this work, we focus on the dynamics of the IMBH–SBH–SBH triples and illustrate that these systems can be possible sources of GWs. A distinctive signature of this scenario is that a considerable fraction of these mergers are highly eccentric when entering the LIGO band (10 Hz). Assuming that $\sim 20{{\ \rm per\ cent}}$ of GCs host IMBHs and a GC density in the range $n_{{\rm GC}}=0.32\!-\!2.31\, \mathrm{Mpc}^{-3}$, we have estimated a rate $\Gamma =0.06\!-\!0.46\, \mathrm{Gpc}^{-3}\, \mathrm{yr}^{-1}$ of these events. This suggests that dynamically driven binary SBH mergers in this scenario could contribute to the merger events observed by LIGO/VIRGO. Full N-body simulations of GCs harbouring IMBHs are highly desirable to give a more precise constrain on this scenario.

scholarly journals Probingintermediate-mass black holes in M87 through multiwavelength gravitational wave observations

2020 ◽  
Vol 495 (1) ◽  
pp. 536-543 ◽  
Author(s):  
Razieh Emami ◽  
Abraham Loeb
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Gravitational Wave ◽  
Parameter Space ◽  
Intermediate Mass ◽  
Triple Systems ◽  
Supermassive Black Hole ◽  
Binary Black Hole ◽  
Wide Range

ABSTRACT We analyse triple systems composed of the supermassive black hole (SMBH) near the centre of M87 and a pair of black holes (BHs) with masses in the range of $10{-}10^3\, {\rm M}_{\odot }$. We consider the post Newtonian precession as well as the Kozai–Lidov interactions at the quadruple and octupole levels in modelling the evolution of binary black hole (BBH) under the influence of the SMBH. Kozai–Lidov oscillations enhance the gravitational wave (GW) signal in some portions of the parameter space. We identify frequency peaks and examine the detectability of GWs with LISA as well as future observatories such as μAres and DECIGO. We show examples in which GW signal can be observed with a few or all of these detectors. Multiwavelength GW spectroscopy holds the potential to discover stellar to intermediate mass BHs near the centre of M87. We estimate the rate, Γ, of collisions between the BBHs and fly-by stars at the centre of M87. Our calculation suggest $\Gamma \lt 10\, \rm {Gyr}^{-1}$ for a wide range of the mass and semimajor axes of the inner binary.

Growth of intermediate mass black holes in first star clusters

2019 ◽  
Vol 14 (S351) ◽  
pp. 220-223
Author(s):  
Yuya Sakurai ◽  
Naoki Yoshida ◽  
Michiko S. Fujii
Keyword(s):  
Black Holes ◽  
Large Scale ◽  
Star Clusters ◽  
Star Cluster ◽  
Galaxy Mergers ◽  
Intermediate Mass ◽  
Tidal Disruption ◽  
Stellar Collisions ◽  
Gas Supply ◽  
Intermediate Mass Black Holes

AbstractWe study runaway stellar collisions in primordial star clusters and formation of intermediate mass black holes (IMBHs). Using cosmological simulations, we identify eight atomic-cooling halos in which the star clusters form. We follow stellar and dark matter (DM) dynamics for 3Myr using hybrid N-body simulations. We find that the runaway stellar collisions occur in all star clusters and IMBHs with masses ∼400–1900M⊙ form. Performing additional N-body simulations, we explore evolutions of the IMBHs in the star clusters for 15 Myr. The IMBH masses grow via stellar tidal disruption events (TDEs) to ∼700–2500 M⊙. The TDE rates are ∼0.3–1.3 Myr−1. DM motions affect the star cluster evolutions and reduce the TDE rates. The IMBHs may subsequently grow to SMBHs by gas supply through galaxy mergers or large-scale gas inflows, or they may remain within or around the clusters.

scholarly journals An accreting black hole in the nucleus of the bulgeless galaxy NGC 1042

2007 ◽  
Vol 3 (S245) ◽  
pp. 259-260
Author(s):  
Joseph C. Shields ◽  
Carl Jakob Walcher ◽  
Torsten Böker ◽  
Luis C. Ho ◽  
Hans-Walter Rix ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Compact Star ◽  
Star Clusters ◽  
Central Star ◽  
Supermassive Black Holes ◽  
Star Cluster ◽  
Intermediate Mass

AbstractCompact star clusters are commonly found in the centers of galaxies and may foster formation of intermediate-mass “seed” black holes that facilitate the growth of supermassive black holes in galaxy nuclei. Such star clusters can be studied with minimal background starlight contamination in bulgeless galaxies. We present new results that point to the presence of an accreting black hole associated with the central star cluster in the Sd galaxy NGC 1042, and discuss implications for the bulge-black hole connection.

Binary Black Hole Merger: Mass-Separation Relation and Intermediate Mass Black Holes

2020 ◽  
Author(s):  
Kushaal Kumar Pothula
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Globular Clusters ◽  
Mass Range ◽  
Mass Separation ◽  
Intermediate Mass ◽  
Binary Black Hole ◽  
Separation Relation ◽  
Hubble Time ◽  
Intermediate Mass Black Holes

Abstract Intermediate Mass Black Holes (IMBHs) are an elusive category of black holes in the mass range of 100 to 100000 Solar Masses. Binary IMBHs might form due to mergers of Globular Clusters, Pair Instability Supernovae, and in Young Massive Star Clusters. In this Research Note, merger timescale, constraints on the separation based on the timescale, and other parameters of Binary IMBHs are calculated analytically and are discussed. The calculations were conducted using Newtonian and Einstienian dynamics. The timescale of a Binary IMBH system to reach maximum gravitational wave amplitude is also calculated ad discussed. We also present the relation between the combined Mass of a Binary Black Hole (BBH) System and the Separation between two BHs required for a BBH system to merge within a given timescale tc, solely due to Gravitational Radiation is a function of the total mass of the system. In this article, tc is set equal to Hubble time tH. Now, the relation obtained is essentially the relation between separation of a BBH system (collide within tH) and its Mass. The calculations were conducted for all three categories of Black Holes: Stellar, Intermediate, and Supermassive. Time ahead, the relation might be used for determining whether a BBH merger would be observational. The relation is also solved for Intermediate Mass Black Holes (IMBHs), and and tc separation for collision within tH was calculated.

scholarly journals Intermediate-Mass Black Holes

2020 ◽  
Vol 58 (1) ◽  
pp. 257-312 ◽  
Author(s):  
Jenny E. Greene ◽  
Jay Strader ◽  
Luis C. Ho
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Globular Clusters ◽  
High Redshift ◽  
Mass Function ◽  
Intermediate Mass ◽  
The Galaxy ◽  
Robust Measurements ◽  
Black Hole Masses ◽  
Intermediate Mass Black Holes

We describe ongoing searches for intermediate-mass black holes with MBH ≈ 10–105 M⊙. We review a range of search mechanisms, both dynamical and those that rely on accretion signatures. We find the following conclusions: ▪  Dynamical and accretion signatures alike point to a high fraction of 109–1010 M⊙ galaxies hosting black holes with MBH∼ 105 M⊙. In contrast, there are no solid detections of black holes in globular clusters. ▪  There are few observational constraints on black holes in any environment with MBH ≈ 100–104 M⊙. ▪  Considering low-mass galaxies with dynamical black hole masses and constraining limits, we find that the MBH–σ* relation continues unbroken to MBH ∼105 M⊙, albeit with large scatter. We believe the scatter is at least partially driven by a broad range in black hole masses, because the occupation fraction appears to be relatively high in these galaxies. ▪  We fold the observed scaling relations with our empirical limits on occupation fraction and the galaxy mass function to put observational bounds on the black hole mass function in galaxy nuclei. ▪  We are pessimistic that local demographic observations of galaxy nuclei alone could constrain seeding mechanisms, although either high-redshift luminosity functions or robust measurements of off-nuclear black holes could begin to discriminate models.

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