The impact of reionization on the formation of supermassive black hole seeds

ABSTRACT We use a semi-analytic model to explore the potential impact of a brief and violent period of radio-loud accretion on to black holes (The Radio Scream) during the Cosmic Dawn on the H i hyperfine 21 cm signal. We find that radio emission from supermassive black hole seeds can impact the global 21 cm signal at the level of tens to hundreds of per cent provided that they were as radio loud as $z$ ≈ 1 black holes and obscured by gas with column depths of NH ≳ 1023 cm−2. We determine plausible sets of parameters that reproduce some of the striking features of the EDGES absorption feature including its depth, timing, and side steepness while producing radio/X-ray backgrounds and source counts that are consistent with published limits. Scenarios yielding a dramatic 21 cm signature also predict large populations of ∼$\mu$Jy point sources that will be detectable in future deep surveys from the Square Kilometer Array (SKA). Thus, 21 cm measurements, complemented by deep point-source surveys, have the potential to constrain optimistic scenarios where supermassive black hole progenitors were radio loud.

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Outbursts from the supermassive black hole in M87 and the impact on the hot gas

Advances in Space Research ◽

10.1016/j.asr.2004.12.063 ◽

2005 ◽

Vol 36 (4) ◽

pp. 597-600 ◽

Cited By ~ 1

Author(s):

C. Jones ◽

W. Forman ◽

R. Kraft ◽

M. Markevitch ◽

P. Nulsen ◽

...

Keyword(s):

Black Hole ◽

Hot Gas ◽

Supermassive Black Hole ◽

The Impact

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Supermassive black hole seed formation and the impact on black hole populations across cosmic time

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320003142 ◽

2019 ◽

Vol 15 (S356) ◽

pp. 292-292

Author(s):

Colin DeGraf

Keyword(s):

Black Hole ◽

Cosmic Time ◽

Analysis Method ◽

Seed Formation ◽

Formation Pathway ◽

Supermassive Black Hole ◽

Luminosity Functions ◽

Initial Seed ◽

The Impact

AbstractAlthough it is well understood that supermassive black holes are found in essentially all galaxies, the mechanisms by which they initially form remain highly uncertain, despite the importance that the formation pathway can have on AGN and quasar behaviour at all redshifts. Using a post-processing analysis method combining cosmological simulations and analytic modeling, I will discuss how varying the conditions for formation of supermassive black hole seeds leads to changes in AGN populations. Looking at formation via direct collapse or from PopIII remnants, I will discuss the impact on black hole mass and luminosity functions, scaling relations, and black hole mergers, which each have effects at both high- and low-redshifts. In addition to demonstrating the importance of initial seed formation on our understanding of long-term black hole evolution, I will also show that the signatures of seed formation suggest multiple means by which upcoming electromagnetic and GW surveys (at both high- and low-z) can provide the data required to constrain initial supermassive black hole formation.

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The Bardeen–Petterson effect in accreting supermassive black hole binaries: a systematic approach

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa1693 ◽

2020 ◽

Vol 496 (3) ◽

pp. 3060-3075 ◽

Cited By ~ 1

Author(s):

Davide Gerosa ◽

Giovanni Rosotti ◽

Riccardo Barbieri

Keyword(s):

Black Hole ◽

Systematic Investigation ◽

Stationary Solutions ◽

Evolutionary Stage ◽

Black Hole Binaries ◽

Frame Dragging ◽

Supermassive Black Hole ◽

Complete Alignment ◽

Hydrodynamical Simulations ◽

The Impact

ABSTRACT Disc-driven migration is a key evolutionary stage of supermassive black hole binaries hosted in gas-rich galaxies. Besides promoting the inspiral, viscous interactions tend to align the spins of the black holes with the orbital angular momentum of the disc. We present a critical and systematic investigation of this problem, also known as the Bardeen–Petterson effect. We design a new iterative scheme to solve the non-linear dynamics of warped accretion discs under the influence of both relativistic frame dragging and binary companion. We characterize the impact of the disc ‘critical obliquity’, which marks regions of the parameter space where stationary solutions do not exist. We find that black hole spins reach either complete alignment or a critical configuration. Reaching the critical obliquity might imply that the disc breaks as observed in hydrodynamical simulations. Our findings are important to predict the spin configurations with which supermassive black hole binaries enter their gravitational-wave driven regime and become detectable by LISA.

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The impact of magnetic fields on the IMF in star-forming clouds near a supermassive black hole

Astronomy and Astrophysics ◽

10.1051/0004-6361/201219628 ◽

2012 ◽

Vol 545 ◽

pp. A46 ◽

Cited By ~ 4

Author(s):

S. Hocuk ◽

D. R. G. Schleicher ◽

M. Spaans ◽

S. Cazaux

Keyword(s):

Black Hole ◽

Magnetic Fields ◽

Star Forming ◽

Supermassive Black Hole ◽

The Impact ◽

The Imf

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The Impact of Stripped Nuclei on the Supermassive Black Hole Number Density in the Local Universe

The Astrophysical Journal ◽

10.3847/1538-4357/aaf735 ◽

2019 ◽

Vol 871 (2) ◽

pp. 159 ◽

Cited By ~ 12

Author(s):

Karina T. Voggel ◽

Anil C. Seth ◽

Holger Baumgardt ◽

Steffen Mieske ◽

Joel Pfeffer ◽

...

Keyword(s):

Black Hole ◽

Number Density ◽

Local Universe ◽

Supermassive Black Hole ◽

The Impact ◽

Hole Number

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The effect of impact parameter on tidal disruption events

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa3627 ◽

2020 ◽

Vol 501 (2) ◽

pp. 1748-1754

Author(s):

Alexandra Spaulding ◽

Philip Chang

Keyword(s):

Black Hole ◽

Energy Distribution ◽

Impact Parameter ◽

Moving Mesh ◽

Tidal Disruption ◽

Tidal Gravity ◽

Supermassive Black Hole ◽

Complete Destruction ◽

The Impact ◽

Peak Luminosity

ABSTRACT Stars that pass too close to a supermassive black hole are disrupted by the black hole’s tidal gravity. Some debris is ejected while the remainder accretes into the black hole. To better study the physics of these debris, we use the moving mesh code manga to follow the evolution of the star from its initial encounter to its complete destruction. By varying the impact parameter (β) of the star, we study the energy distribution of the remaining material and the fallback rate of the material into the black hole as a function of time. We show that the spread of energy in the debris and peak luminosity time (tpeak) are both directly related to the impact parameter. In particular, we find a β1/2 scaling for the energy spread for β = 2 − 10 that levels off at β ≳ 10. We discuss implication of this scaling for the rise time of the light curve and broadness of the luminosity peak for these lower β’s. These relationships provide a possible means of inferring the impact parameters for observed tidal disruption events.

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Star's rosette-shaped orbit around a supermassive black hole supports general relativity

AccessScience ◽

10.1036/1097-8542.br0429201 ◽

2020 ◽

Keyword(s):

General Relativity ◽

Black Hole ◽

Supermassive Black Hole

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Central kiloparsec of NGC 1326 observed with SINFONI

Astronomy and Astrophysics ◽

10.1051/0004-6361/201936451 ◽

2020 ◽

Vol 638 ◽

pp. A53

Author(s):

Nastaran Fazeli ◽

Gerold Busch ◽

Andreas Eckart ◽

Françoise Combes ◽

Persis Misquitta ◽

...

Keyword(s):

Black Hole ◽

Galaxy Evolution ◽

Near Infrared ◽

Velocity Fields ◽

Molecular Gas ◽

Nearby Galaxy ◽

Stellar Content ◽

Stellar Rotation ◽

Supermassive Black Hole ◽

Integral Field Spectrograph

Gas inflow processes in the vicinity of galactic nuclei play a crucial role in galaxy evolution and supermassive black hole growth. Exploring the central kiloparsec of galaxies is essential to shed more light on this subject. We present near-infrared H- and K-band results of the nuclear region of the nearby galaxy NGC 1326, observed with the integral-field spectrograph SINFONI mounted on the Very Large Telescope. The field of view covers 9″ × 9″ (650 × 650 pc2). Our work is concentrated on excitation conditions, morphology, and stellar content. The nucleus of NGC 1326 was classified as a LINER, however in our data we observed an absence of ionised gas emission in the central r ∼ 3″. We studied the morphology by analysing the distribution of ionised and molecular gas, and thereby detected an elliptically shaped, circum-nuclear star-forming ring at a mean radius of 300 pc. We estimate the starburst regions in the ring to be young with dominating ages of < 10 Myr. The molecular gas distribution also reveals an elongated east to west central structure about 3″ in radius, where gas is excited by slow or mild shock mechanisms. We calculate the ionised gas mass of 8 × 105 M⊙ completely concentrated in the nuclear ring and the warm molecular gas mass of 187 M⊙, from which half is concentrated in the ring and the other half in the elongated central structure. The stellar velocity fields show pure rotation in the plane of the galaxy. The gas velocity fields show similar rotation in the ring, but in the central elongated H2 structure they show much higher amplitudes and indications of further deviation from the stellar rotation in the central 1″ aperture. We suggest that the central 6″ elongated H2 structure might be a fast-rotating central disc. The CO(3–2) emission observations with the Atacama Large Millimeter/submillimeter Array reveal a central 1″ torus. In the central 1″ of the H2 velocity field and residual maps, we find indications for a further decoupled structure closer to a nuclear disc, which could be identified with the torus surrounding the supermassive black hole.

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