Black hole mergers from dwarf to massive galaxies with the NewHorizon and Horizon-AGN simulations

Volonteri, Marta; Pfister, Hugo; Beckmann, Ricarda S.; Dubois, Yohan; Colpi, M.; Conselice, Christopher J.; Dotti, Massimo; Martin, Garreth; Jackson, R.; Kraljic, Katarina; Pichon, Christophe; Trebitsch, Maxime; Yi, Sukyoung K.; Devriendt, Julien; Peirani, Sébastien

doi:10.1093/mnras/staa2384

Cited by 106 publications

(94 citation statements)

References 129 publications

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“…The relatively high occupation fraction in low-mass galaxies allows for MBH mergers to also occur in low-mass galaxies, following galaxy mergers. This is studied in further detail in Volonteri et al (2020).…”

Section: Mbh-to-galaxy Mass Relationmentioning

confidence: 98%

“…The MBHs are allowed to merge when they get closer than 4∆x (∼150 pc) and when the relative velocity of the pair is smaller than the escape velocity of the binary. A detailed analysis of MBH mergers in NewHorizon is presented in Volonteri et al (2020).…”

Section: Formation Growth and Dynamics Of Mbhmentioning

confidence: 99%

“… See Park et al (2019,Volonteri et al (2020),Martin et al (2021),Jackson et al (2021a), andJackson et al (2021b) for early results on the origin of discs and spheroids, the thickness of discs, the mergers of black holes, the role of interactions in the evolution of dwarf galaxies, the DM deficient galaxies, and low-surface brightness dwarf galaxies, respectively.…”

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confidence: 99%

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Introducing the NEWHORIZON simulation: Galaxy properties with resolved internal dynamics across cosmic time

Dubois

Beckmann

Bournaud

et al. 2021

A&A

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Hydrodynamical cosmological simulations are increasing their level of realism by considering more physical processes and having greater resolution or larger statistics. However, usually either the statistical power of such simulations or the resolution reached within galaxies are sacrificed. Here, we introduce the NEWHORIZON project in which we simulate at high resolution a zoom-in region of ∼(16 Mpc)3 that is larger than a standard zoom-in region around a single halo and is embedded in a larger box. A resolution of up to 34 pc, which is typical of individual zoom-in, up-to-date resimulated halos, is reached within galaxies; this allows the simulation to capture the multi-phase nature of the interstellar medium and the clumpy nature of the star formation process in galaxies. In this introductory paper, we present several key fundamental properties of galaxies and their black holes, including the galaxy mass function, cosmic star formation rate, galactic metallicities, the Kennicutt–Schmidt relation, the stellar-to-halo mass relation, galaxy sizes, stellar kinematics and morphology, gas content within galaxies and its kinematics, and the black hole mass and spin properties over time. The various scaling relations are broadly reproduced by NEWHORIZON with some differences with the standard observables. Owing to its exquisite spatial resolution, NEWHORIZON captures the inefficient process of star formation in galaxies, which evolve over time from being more turbulent, gas rich, and star bursting at high redshift. These high-redshift galaxies are also more compact, and they are more elliptical and clumpier until the level of internal gas turbulence decays enough to allow for the formation of discs. The NEWHORIZON simulation gives access to a broad range of galaxy formation and evolution physics at low-to-intermediate stellar masses, which is a regime that will become accessible in the near future through surveys such as the LSST.

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Section: Mbh-to-galaxy Mass Relationmentioning

confidence: 98%

Section: Formation Growth and Dynamics Of Mbhmentioning

confidence: 99%

mentioning

confidence: 99%

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Introducing the NEWHORIZON simulation: Galaxy properties with resolved internal dynamics across cosmic time

Dubois

Beckmann

Bournaud

et al. 2021

A&A

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151

100

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“…It is worth noting that BHs that do exist in dwarf galaxies exhibit very little growth (e.g. Volonteri et al 2020;Dubois et al 2020). Finally, galaxies with BHs do not occupy a preferential position in the locus.…”

Section: Differential Supernova Feedback At Early Epochsinitiating Thmentioning

confidence: 99%

The origin of low-surface-brightness galaxies in the dwarf regime

Jackson

Martin

Kaviraj

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Low-surface-brightness galaxies (LSBGs) – defined as systems that are fainter than the surface-brightness limits of past wide-area surveys – form the overwhelming majority of galaxies in the dwarf regime (M⋆ < 109 M⊙). Using NewHorizon, a high-resolution cosmological simulation, we study the origin of LSBGs and explain why LSBGs at similar stellar mass show the large observed spread in surface brightness. NewHorizon galaxies populate a well-defined locus in the surface brightness – stellar mass plane, with a spread of ∼3 mag arcsec−2, in agreement with deep SDSS Stripe data. Galaxies with fainter surface brightnesses today are born in regions of higher dark-matter density. This results in faster gas accretion and more intense star formation at early epochs. The stronger resultant supernova feedback flattens gas profiles at a faster rate which, in turn, creates shallower stellar profiles (i.e. more diffuse systems) more rapidly. As star formation declines towards late epochs (z < 1), the larger tidal perturbations and ram pressure experienced by these systems (due to their denser local environments) accelerate the divergence in surface brightness, by increasing their effective radii and reducing star formation respectively. A small minority of dwarfs depart from the main locus towards high surface brightnesses, making them detectable in past wide surveys (e.g. standard-depth SDSS images). These systems have anomalously high star-formation rates, triggered by recent, fly-by or merger-driven starbursts. We note that objects considered extreme/anomalous at the depth of current datasets, e.g. ‘ultra-diffuse galaxies’, actually dominate the predicted dwarf population and will be routinely visible in future surveys like LSST.

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“…Feedback processes such as jets or intense quasar outflows from AGN can affect the evolution of the host galaxy (Salomé et al 2016;Harrison et al 2018). Enhanced multiple-AGN feedback effects may lead to faster SMBH growth (Volonteri et al 2020). There may be additional star formation if the AGN outflows interact with one another.…”

Section: Implications For Our Triple-agn Detectionmentioning

confidence: 99%

A triple active galactic nucleus in the NGC 7733–7734 merging group

Yadav

Das

Barway

et al. 2021

A&A

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Context. Galaxy interactions and mergers can lead to supermassive black hole (SMBH) binaries, which become active galactic nucleus (AGN) pairs when the SMBHs start accreting mass. If there is a third galaxy involved in the interaction, then a triple-AGN system can form. Aims. Our goal is to investigate the nature of the nuclear emission from the galaxies in the interacting pair NGC 7733-NGC 7734 using archival VLT/MUSE integral field spectrograph data and study its relation to the stellar mass distribution traced by near-infrared (NIR) observations from the South African Astronomical Observatory (SAAO). Methods. We conducted NIR observations using the SAAO and identified the morphological properties of bulges in each galaxy. We used MUSE data to obtain a set of ionized emission lines from each galaxy and studied the ionization mechanism. We also examined the relation of the galaxy pair with any nearby companions with far-ultraviolet observations using the UVIT. Results. The emission line analysis from the central regions of NGC 7733 and NGC 7734 shows Seyfert and low ionization nuclear emission-line regions (LINER) type AGN activity. The galaxy pair NGC 7733-34 also shows evidence of a third component, which has Seyfert-like emission. Hence, the galaxy pair NGC 7733-34 forms a triple-AGN system. We also detected an extended narrow-line region (ENLR) associated with the nucleus of NGC 7733.

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Black hole mergers from dwarf to massive galaxies with the NewHorizon and Horizon-AGN simulations

Cited by 106 publications

References 129 publications

Introducing the NEWHORIZON simulation: Galaxy properties with resolved internal dynamics across cosmic time

Introducing the NEWHORIZON simulation: Galaxy properties with resolved internal dynamics across cosmic time

The origin of low-surface-brightness galaxies in the dwarf regime

A triple active galactic nucleus in the NGC 7733–7734 merging group

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