We present the first self-consistent prediction for the distribution of
formation timescales for close Supermassive Black Hole (SMBH) pairs following
galaxy mergers. Using Romulus25, the first large-scale cosmological simulation
to accurately track the orbital evolution of SMBHs within their host galaxies
down to sub-kpc scales, we predict an average formation rate density of close
SMBH pairs of 0.013 cMpc^-3 Gyr^-1. We find that it is relatively rare for
galaxy mergers to result in the formation of close SMBH pairs with sub-kpc
separation and those that do form are often the result of Gyrs of orbital
evolution following the galaxy merger. The likelihood and timescale to form a
close SMBH pair depends strongly on the mass and morphology of the accreted
satellite galaxy. Low stellar mass ratio mergers with galaxies that lack a
dense stellar core are more likely to become tidally disrupted and deposit
their SMBH at large radii without any stellar core to aid in their orbital
decay, resulting in a population of long-lived 'wandering' SMBHs. Conversely,
SMBHs in galaxies that remain embedded within a stellar core form close pairs
in much shorter timescales on average. This timescale is a crucial, though
often ignored or very simplified, ingredient to models predicting SMBH mergers
rates and the connection between SMBH and star formation activity.
Описание
[1708.07126] Dancing to ChaNGa: A Self-Consistent Prediction For Close SMBH Pair Formation Timescales Following Galaxy Mergers
%0 Generic
%1 tremmel2017dancing
%A Tremmel, Michael
%A Governato, Fabio
%A Volonteri, Marta
%A Quinn, Thomas R.
%A Pontzen, Andrew
%D 2017
%K SMBH formation pairs
%T Dancing to ChaNGa: A Self-Consistent Prediction For Close SMBH Pair
Formation Timescales Following Galaxy Mergers
%U http://arxiv.org/abs/1708.07126
%X We present the first self-consistent prediction for the distribution of
formation timescales for close Supermassive Black Hole (SMBH) pairs following
galaxy mergers. Using Romulus25, the first large-scale cosmological simulation
to accurately track the orbital evolution of SMBHs within their host galaxies
down to sub-kpc scales, we predict an average formation rate density of close
SMBH pairs of 0.013 cMpc^-3 Gyr^-1. We find that it is relatively rare for
galaxy mergers to result in the formation of close SMBH pairs with sub-kpc
separation and those that do form are often the result of Gyrs of orbital
evolution following the galaxy merger. The likelihood and timescale to form a
close SMBH pair depends strongly on the mass and morphology of the accreted
satellite galaxy. Low stellar mass ratio mergers with galaxies that lack a
dense stellar core are more likely to become tidally disrupted and deposit
their SMBH at large radii without any stellar core to aid in their orbital
decay, resulting in a population of long-lived 'wandering' SMBHs. Conversely,
SMBHs in galaxies that remain embedded within a stellar core form close pairs
in much shorter timescales on average. This timescale is a crucial, though
often ignored or very simplified, ingredient to models predicting SMBH mergers
rates and the connection between SMBH and star formation activity.
@misc{tremmel2017dancing,
abstract = {We present the first self-consistent prediction for the distribution of
formation timescales for close Supermassive Black Hole (SMBH) pairs following
galaxy mergers. Using Romulus25, the first large-scale cosmological simulation
to accurately track the orbital evolution of SMBHs within their host galaxies
down to sub-kpc scales, we predict an average formation rate density of close
SMBH pairs of 0.013 cMpc^-3 Gyr^-1. We find that it is relatively rare for
galaxy mergers to result in the formation of close SMBH pairs with sub-kpc
separation and those that do form are often the result of Gyrs of orbital
evolution following the galaxy merger. The likelihood and timescale to form a
close SMBH pair depends strongly on the mass and morphology of the accreted
satellite galaxy. Low stellar mass ratio mergers with galaxies that lack a
dense stellar core are more likely to become tidally disrupted and deposit
their SMBH at large radii without any stellar core to aid in their orbital
decay, resulting in a population of long-lived 'wandering' SMBHs. Conversely,
SMBHs in galaxies that remain embedded within a stellar core form close pairs
in much shorter timescales on average. This timescale is a crucial, though
often ignored or very simplified, ingredient to models predicting SMBH mergers
rates and the connection between SMBH and star formation activity.},
added-at = {2017-08-25T09:48:34.000+0200},
author = {Tremmel, Michael and Governato, Fabio and Volonteri, Marta and Quinn, Thomas R. and Pontzen, Andrew},
biburl = {https://www.bibsonomy.org/bibtex/259165eefd3d1198d6a0af3783d55a4c2/miki},
description = {[1708.07126] Dancing to ChaNGa: A Self-Consistent Prediction For Close SMBH Pair Formation Timescales Following Galaxy Mergers},
interhash = {290a3c2b9273fbf478f4945f8f22b0db},
intrahash = {59165eefd3d1198d6a0af3783d55a4c2},
keywords = {SMBH formation pairs},
note = {cite arxiv:1708.07126Comment: 10 pages, 6 figures, submitted to MNRAS. Comments welcome},
timestamp = {2017-08-25T09:48:34.000+0200},
title = {Dancing to ChaNGa: A Self-Consistent Prediction For Close SMBH Pair
Formation Timescales Following Galaxy Mergers},
url = {http://arxiv.org/abs/1708.07126},
year = 2017
}