Connecting traces of galaxy evolution: the missing core mass–morphological fine structure relation

Bonfini, P.; Bitsakis, T.; Zezas, A.; Duc, Pierre–Alain; Iodice, E.; González‐Martín, O.; Bruzual, G.; Sanoja, A.J. González

doi:10.1093/mnrasl/slx169

Cited by 6 publications

(3 citation statements)

References 74 publications

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“…When the merger relic hosts a BHB, the density profile is noticeably carved out beyond the radius including two times the BHB mass; this is a well established result (e.g. Milosavljević & Merritt 2001;Gualandris & Merritt 2012) and is supported by observations (Ferrarese et al 1994;Lauer et al 1995;Bonfini et al 2018). As a matter of fact, even the infall of a single MBH can produce a core in the system (Gualandris & Merritt 2008;Goerdt et al 2010); however our simulations suggest that in the single MBH scenario the effect of core scouring is significantly smaller compared to the BHB case (Figure 13, central panel).…”

Section: One or Two Mbhssupporting

confidence: 57%

The influence of massive black hole binaries on the morphology of merger remnants

Bortolas

Gualandris

Dotti

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Massive black hole (MBH) binaries, formed as a result of galaxy mergers, are expected to harden by dynamical friction and three-body stellar scatterings, until emission of gravitational waves (GWs) leads to their final coalescence. According to recent simulations, MBH binaries can efficiently harden via stellar encounters only when the host geometry is triaxial, even if only modestly, as angular momentum diffusion allows an efficient repopulation of the binary loss cone. In this paper, we carry out a suite of N-body simulations of equal-mass galaxy collisions, varying the initial orbits and density profiles for the merging galaxies and running simulations both with and without central MBHs. We find that the presence of an MBH binary in the remnant makes the system nearly oblate, aligned with the galaxy merger plane, within a radius enclosing 100 MBH masses. We never find binary hosts to be prolate on any scale. The decaying MBHs slightly enhance the tangential anisotropy in the centre of the remnant due to angular momentum injection and the slingshot ejection of stars on nearly radial orbits. This latter effect results in about 1% of the remnant stars being expelled from the galactic nucleus. Finally, we do not find any strong connection between the remnant morphology and the binary hardening rate, which depends only on the inner density slope of the remnant galaxy. Our results suggest that MBH binaries are able to coalesce within a few Gyr, even if the binary is found to partially erase the merger-induced triaxiality from the remnant.

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Section: One or Two Mbhssupporting

confidence: 57%

The influence of massive black hole binaries on the morphology of merger remnants

Bortolas

Gualandris

Dotti

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Prugniel et al (1988) also point out that this galaxy might be in an advanced merger state which would significantly affect our dynamical models. Large scale signatures of this merger (such as shells) are also visible in the MATLAS images from Duc et al (2015), also shown in Bonfini et al (2018). However, Krajnović et al (2011) analyzed the ATLAS 3D kinematics of NGC 3640 with Kinemetry (Krajnović et al 2006) and found only very small residuals and a very regular shape within one R e , indicating that the center of NGC 3640 is relaxed now.…”

Section: Kinematic Resultsmentioning

confidence: 72%

Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations

Thater

Krajnović

Cappellari

et al. 2019

A&A

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Different massive black hole mass -host galaxy scaling relations suggest that the growth of massive black holes is entangled with the evolution of their host galaxies. The number of measured black hole masses is still limited, and additional measurements are necessary to understand the underlying physics of this apparent co-evolution. We add six new black hole mass (M BH ) measurements of nearby fast rotating early-type galaxies to the known black hole mass sample, namely NGC 584, NGC 2784, NGC 3640, NGC 4570, NGC 4281 and NGC 7049. Our target galaxies have effective velocity dispersions (σ e ) between 170 and 245 km s −1 , and thus this work provides additional insight into the black hole properties of intermediate-mass early-type galaxies. We combine high-resolution adaptive-optics SINFONI data with large-scale MUSE, VIMOS and SAURON data from ATLAS 3D to derive two-dimensional stellar kinematics maps. We then build both Jeans Anisotropic Models and axisymmetric Schwarzschild models to measure the central black hole masses. Our Schwarzschild models provide black hole masses of (1.3 ± 0.5) × 10 8 M for NGC 584, (1.0 ± 0.6) × 10 8 M for NGC 2784, (7.7 ± 5) × 10 7 M for NGC 3640, (5.4 ± 0.8) × 10 8 M for NGC 4281, (6.8 ± 2.0) × 10 7 M for NGC 4570 and (3.2 ± 0.8) × 10 8 M for NGC 7049 at 3σ confidence level, which are consistent with recent M BH -σ e scaling relations. NGC 3640 has a velocity dispersion dip and NGC 7049 a constant velocity dispersion in the center, but we can clearly constrain their lower black hole mass limit. We conclude our analysis with a test on NGC 4570 taking into account a variable mass-to-light ratio (M/L) when constructing dynamical models. When considering M/L variations linked mostly to radial changes in the stellar metallicity, we find that the dynamically determined black hole mass from NGC 4570 decreases by 30%. Further investigations are needed in the future to account for the impact of radial M/L gradients on dynamical modeling.

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“…This mechanism possibly justifies the almost ubiquitous presence of stellar cores at the centre of the most massive galaxies (i.e. the ones that likely experienced the largest number of mergers; Bonfini et al 2018).…”

Section: Hardening In Stellar Environmentsmentioning

confidence: 92%

Astrophysics with the Laser Interferometer Space Antenna

et al. 2023

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The Laser Interferometer Space Antenna (LISA) will be a transformative experiment for gravitational wave astronomy, and, as such, it will offer unique opportunities to address many key astrophysical questions in a completely novel way. The synergy with ground-based and space-born instruments in the electromagnetic domain, by enabling multi-messenger observations, will add further to the discovery potential of LISA. The next decade is crucial to prepare the astrophysical community for LISA’s first observations. This review outlines the extensive landscape of astrophysical theory, numerical simulations, and astronomical observations that are instrumental for modeling and interpreting the upcoming LISA datastream. To this aim, the current knowledge in three main source classes for LISA is reviewed; ultra-compact stellar-mass binaries, massive black hole binaries, and extreme or interme-diate mass ratio inspirals. The relevant astrophysical processes and the established modeling techniques are summarized. Likewise, open issues and gaps in our understanding of these sources are highlighted, along with an indication of how LISA could help making progress in the different areas. New research avenues that LISA itself, or its joint exploitation with upcoming studies in the electromagnetic domain, will enable, are also illustrated. Improvements in modeling and analysis approaches, such as the combination of numerical simulations and modern data science techniques, are discussed. This review is intended to be a starting point for using LISA as a new discovery tool for understanding our Universe.

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Connecting traces of galaxy evolution: the missing core mass–morphological fine structure relation

Cited by 6 publications

References 74 publications

The influence of massive black hole binaries on the morphology of merger remnants

The influence of massive black hole binaries on the morphology of merger remnants

Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations

Astrophysics with the Laser Interferometer Space Antenna

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