Intermediate Mass Black Hole (IMBH) mergers with masses $10^4 - 10^6$ $M_{\odot}$ are expected to produce gravitational waves (GWs) detectable by the Laser Interferometer Space Antenna (LISA) with high signal to noise ratios out to redshift 20. IMBH mergers are expected to take place within dwarf galaxies, however, the dynamics, timescales, and effect on their hosts are largely unexplored. In a previous study, we examined how IMBHs would pair and merge within nucleated dwarf galaxies. IMBHs in nucleated hosts evolve very efficiently, forming a binary system and coalescing within a few hundred million years. Although the fraction of dwarf galaxies ($10^7$ M$_{\odot} \leq$ $M_{\star} \leq 10^{10}$ M$_{\odot}$) hosting nuclear star clusters is between 60-100\%, this fraction drops to 20-70\% for lower-mass dwarfs ($M_{\star}\approx 10^7$ M$_{\odot}$), with the largest drop in low-density environments. Here, we extend our previous study by performing direct $N-$body simulations to explore the dynamics and evolution of IMBHs within non-nucleated dwarf galaxies, under the assumption that IMBHs exist within these dwarfs. To our surprise, none of IMBHs in our simulation suite merge within a Hubble time, despite many attaining high eccentricities $e \sim 0.7-0.95$. We conclude that extremely low stellar density environments in the centers of non-nucleated dwarfs do not provide an ample supply of stars to interact with IMBHs binary resulting in its stalling, in spite of triaxiality and high eccentricity, common means to drive a binary to coalescence. Our findings underline the importance of considering all detailed host properties to predict IMBH merger rates for LISA.
Dynamics and detectability of long-lived non-accretion phases for massive black hole binaries in cold, thermally regulating disks
Niels Bohr International Academy, Niels Bohr Institute（尼尔斯·玻尔国际学院，尼尔斯·玻尔研究所）；Institute of Science and Technology Austria (ISTA)（奥地利科学与技术研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）
A sample of short-lived Galactic radio transients from ASKAP VAST
University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）；University of Wisconsin-Milwaukee（威斯康星大学密尔沃基分校）；Curtin University（科廷大学）；California Institute of Technology（加州理工学院）；Carnegie Institution for Science（卡内基科学研究所）；University of Sydney（悉尼大学）
School of Natural Sciences, Institute for Advanced Study（自然科学院，高等研究院）；Rudolf Peierls Centre for Theoretical Physics, University of Oxford（鲁道夫·皮尔斯理论物理中心，牛津大学）
The Binary Populations of Stellar Streams are Set by Cluster Dynamics
Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理科学系）；School of Physics and Astronomy, Sun Yat-sen University（中山大学物理与天文学院）；The Observatories of the Carnegie Institution for Science（卡内基科学研究所天文台）；Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University（密歇根州立大学物理与天文学院数据密集与时域天文中心）
Optimizing Optical Searches for Supermassive Black Hole Binaries in AGN Light Curves: Fourier versus Bayesian Periodicity Detection
Vanderbilt University（范德堡大学）；Wake Forest University（维克森林大学）；Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA)（天体物理跨学科探索与研究中心）；Northwestern University（西北大学）
McFACTS II: Mass Ratio--Effective Spin Relationship of Black Hole Mergers in the AGN Channel
New Mexico State University（新墨西哥州立大学）；Center for Computational Astrophysics, Flatiron Institute（计算天体物理中心，平顿研究所）；Department of Astrophysics, American Museum of Natural History（美国自然历史博物馆天体物理学系）；Department of Science, BMCC, City University of New York（纽约市立学院科学系，纽约市立大学）；Graduate Center, City University of New York（纽约市立大学研究生中心）；Gravitational Astrophysics Laboratory, NASA Goddard Space Flight Center（引力天体物理学实验室，NASA戈达德太空飞行中心）；Center for Computational Relativity and Gravitation, Rochester Institute of Technology（计算相对论与引力中心，罗切斯特理工学院）
