A 17-billion-solar-mass black hole in a group galaxy with a diffuse core

Thomas, Jens; Pei, Chung; McConnell, Nicholas J.; Greene, Jenny E.; Blakeslee, John P.; Janish, Ryan

doi:10.1038/nature17197

Cited by 143 publications

(194 citation statements)

References 64 publications

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“…By combining the above data with the near-infrared J, H, K-band spectra acquired by the Gemini and Magellan telescopes in Chile on 6 August and 7 October 2014, respectively, this quasar BH mass is estimated to be (1.24 ± 0.19) × 10 10 M ⊙ . This is the first evidence for the theoretically predicted HMBHs in the early Universe (z > ∼ 6), even though there are other evidence for HMBHs at lower z [29, 30,31]. Given selection effects, HMBHs and SMBHs should be actually more abundant than what we have detected so far.…”

Section: Observational Evidence For Hmbhs In the Early Universecontrasting

confidence: 47%

“…We have detected numerous SMBHs and a couple of HMBHs in quasars near and far [26,30,31] − the farthest one with high redshift z = 7.085. The most massive quasar is close to…”

Section: Neutral Hydrogen Environments Of Quasars Near and Farmentioning

confidence: 97%

“…Other observed cases are described and discussed more recently by Lou and Hu [8]. For example, NGC1600, an isolated massive elliptical galaxy 64 Mpc away, hosts a (1.7 ± 0.15) × 10 10 M ⊙ HMBH [30].…”

Section: Pos(ssc2015)025mentioning

confidence: 99%

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Hypermassive Black Hole Shines in the Childhood Universe

Lou¹

2016

Proceedings of SALT Science Conference 2015 — PoS(SSC2015)

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Based on the general polytropic hydrodynamic formalism of self-similar gravitational collapse with spherical symmetry, we study the self-similar dynamic formation of black holes (BHs) in several astrophysical and cosmological contexts such as stellar mass BHs (sMBHs), intermediate mass BHs (IMBHs), supermassive BHs (SMBHs) and hypermassive BHs (HMBHs) -the latter two in the early Universe are of special interest here. We invoke the Paczynski-Wiita gravity to capture the key effects of general relativity and show the growth of BHs including SMBHs and HMBHs can be very rapid and effective in sufficiently massive host halos within timescales shorter than the Universe age of ∼ 13.8 billion years. The effective pressure in our hydrodynamic formalism can represent that of gas in stars, that of random stellar motions in globular clusters, in bulges of spiral galaxies, and in elliptical galaxies, that of random galaxy motions in clusters of galaxies and that of random motions of dark matter (DM) particles as well as that of combinations of various pertinent components (including turbulence). In particular, we have predicted in 2013 that HMBHs in the mass range of ∼ 10 10 − 10 12 M ⊙ or larger can exist in the Universe and even in the early Universe in the forms of hard X-ray/gamma-ray sources or quasars [1]. We discuss several observational evidence for pertinent aspects and classifications and further speculate the possibility of DM BHs (DMBHs) and mixed matter BHs (MMBHs) in reference to the Bonnor-Ebert critical equilibrium condition with two tentative observed candidates. Based on the three-dimensional perturbation analysis of a spherical dynamic collapse [2,3], certain internal gravity modes (g-modes) and all vorticity modes (v-modes) are unstable, implying inevitable turbulent massive motions during a dynamic collapse of forming a BH. Physical consequences including gravitational wave emissions, magnetohydrodynamic (MHD) dynamo processes, and acceleration of ultra-high energy cosmic rays (UHECRs) associated with such massive turbulence during dynamic collapses are also discussed. For the Southern African Large Telescope (SALT) further strengthened with infrared spectrometers, it is certainly capable of identifying quasars and ultra and extremely luminous infrared galaxies harboring SMBHs and/or HMBHs in the Universe including the early Universe. It would be of considerable interest to study the neutral hydrogen environments of SMBHs and HMBHs with increasing redshift z in a systematic manner.

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Section: Observational Evidence For Hmbhs In the Early Universecontrasting

confidence: 47%

“…We have detected numerous SMBHs and a couple of HMBHs in quasars near and far [26,30,31] − the farthest one with high redshift z = 7.085. The most massive quasar is close to…”

Section: Neutral Hydrogen Environments Of Quasars Near and Farmentioning

confidence: 97%

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Hypermassive Black Hole Shines in the Childhood Universe

Lou¹

2016

Proceedings of SALT Science Conference 2015 — PoS(SSC2015)

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“…More likely their descendants will not be in privileged sites but in rather isolated galaxies (e.g. Thomas et al 2016) Our work and the finding that black hole growth is linked to tidal field theory offers some explanation as to the origin of the most massive BHs in most compact galaxies. It is interesting that Barber et al (2016) using the EAGLE simulation at z = 0 also found a strong link between compactness of the host and the most (positive) outliers in the MBH − M * relation.…”

Section: Discussionmentioning

confidence: 96%

The origin of the most massive black holes at high-z: BlueTides and the next quasar frontier

Matteo

Croft

Feng

et al. 2017

Monthly Notices of the Royal Astronomical Society

114

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The growth of the most massive black holes in the early universe, consistent with the detection of highly luminous quasars at z > 6 implies sustained, critical accretion of material to grow and power them. Given a black hole seed scenario, it is still uncertain which conditions in the early Universe allow the fastest black hole growth. Large scale hydrodynamical cosmological simulations of structure formation allow us to explore the conditions conducive to the growth of the earliest supermassive black holes. We use the cosmological hydrodynamic simulation BlueTides, which incorporates a variety of baryon physics in a (400h −1 Mpc) 3 volume with 0.7 trillion particles to follow the earliest phases of black hole critical growth. At z = 8 the most massive black holes (a handful) approach masses of 10 8 M with the most massive (with M BH = 4 × 10 8 M ) being found in an extremely compact spheroid-dominated host galaxy. Examining the large-scale environment of hosts, we find that the initial tidal field is more important than overdensity in setting the conditions for early BH growth. In regions of low tidal fields gas accretes 'cold' onto the black hole and falls along thin, radial filaments straight into the center forming the most compact galaxies and most massive black holes at earliest times. Regions of high tidal fields instead induce larger coherent angular momenta and influence the formation of the first population of massive compact disks. The extreme early growth depends on the early interplay of high gas densities and the tidal field that shapes the mode of accretion. Mergers play a minor role in the formation of the first generation, rare massive BHs.

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“…Recent progress detecting high-mass black holes in Brightest Cluster Galaxies (BCGs) and other large early-type galaxies hint that these objects may be positive outliers from M BH − σ ⋆ and M BH − L bul (e.g., McConnell et al 2012;Rusli et al 2013;Thomas et al 2016), but there are still too few measurements to firmly characterize the scaling relations at M BH 10 9 M ⊙ . The uncertainties are equally severe at the opposite end, where spiral galaxies with low-mass black holes (M BH 10 7 M ⊙ ) measured from water megamaser disks exhibit substantial scatter below the global black hole -host galaxy relations (e.g., Greene et al 2010;Läsker et al 2016;Greene et al 2016).…”

Section: Introductionmentioning

confidence: 99%

A Black Hole Mass Determination for the Compact Galaxy Mrk 1216

Walsh

Bosch

Gebhardt

et al. 2017

ApJ

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Mrk 1216 is a nearby, early-type galaxy with a small effective radius of 2.8 kpc and a large stellar velocity dispersion of 308 km s −1 for its K-band luminosity of 1.4 × 10 11 L ⊙ . Using integral-field spectroscopy assisted by adaptive optics from Gemini North, we measure spatially resolved stellar kinematics within ∼450 pc of the galaxy nucleus. The galaxy exhibits regular rotation with velocities of ±180 km s −1 and a sharply peaked velocity dispersion profile that reaches 425 km s −1 at the center. We fit axisymmetric, orbit-based dynamical models to the combination of these high angular resolution kinematics, large-scale kinematics extending to roughly three effective radii, and Hubble Space Telescope imaging, resulting in a constraint of the mass of the central black hole in Mrk 1216. After exploring several possible sources of systematics that commonly affect stellar-dynamical black hole mass measurements, we find a black hole mass of M BH = (4.9±1.7)×10 9 M ⊙ and a H-band stellar mass-to-light ratio of Υ H = 1.3±0.4 Υ ⊙ (1σ uncertainties). Mrk 1216 is consistent with the local black hole mass -stellar velocity dispersion relation, but is a factor of ∼5 − 10 larger than expectations from the black hole mass -bulge luminosity and black hole mass -bulge mass correlations when conservatively using the galaxy's total luminosity or stellar mass. This behavior is quite similar to the extensively studied compact galaxy NGC 1277. Resembling the z ∼ 2 quiescent galaxies, Mrk 1216 may be a passively evolved descendant, and perhaps reflects a previous era when galaxies contained over-massive black holes relative to their bulge luminosities/masses, and the growth of host galaxies had yet to catch up.

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A 17-billion-solar-mass black hole in a group galaxy with a diffuse core

Cited by 143 publications

References 64 publications

Hypermassive Black Hole Shines in the Childhood Universe

Hypermassive Black Hole Shines in the Childhood Universe

The origin of the most massive black holes at high-z: BlueTides and the next quasar frontier

A Black Hole Mass Determination for the Compact Galaxy Mrk 1216

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