Weighing the IMBH candidate CO-0.40-0.22* in the Galactic Centre

Ballone, Alessandro; Mapelli, Michela; Pasquato, Mario

doi:10.1093/mnras/sty2139

Cited by 14 publications

(12 citation statements)

References 105 publications

(155 reference statements)

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“…An emission counterpart of the IMBH could be identified through future multiwavelength observations. Similar to the simulations conducted for HVCC CO-0.40-0.22 (Ballone et al 2018), the hydrodynamical simulations of the molecular clouds would more accurately restrict the orbital geometries and IMBH mass. Although only ∼ 60 black holes have been identified in our Galaxy to date (Corral-Santana et al 2016), the total number of black holes in our Galaxy is theoretically estimated as ∼ 10 8 -10 9 (Agol & Kamionkowski 2002;Caputo et al 2017).…”

Section: Indication Of An Imbhmentioning

confidence: 92%

Indication of Another Intermediate-mass Black Hole in the Galactic Center

Takekawa

Oka

Iwata

et al. 2019

ApJL

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We report the discovery of molecular gas streams orbiting around an invisible massive object in the central region of our Galaxy, based on the high-resolution molecular line observations with the Atacama Large Millimeter/submillimeter Array (ALMA). The morphology and kinematics of these streams can be reproduced well through two Keplerian orbits around a single point mass of (3.2±0.6)×10 4 M . We also found ionized gas toward the inner part of the orbiting gas, indicating dissociative shock and/or photoionization. Our results provide new circumstantial evidences for a wandering intermediate-mass black hole in the Galactic center, suggesting also that high-velocity compact clouds can be probes of quiescent black holes abound in our Galaxy.

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Section: Indication Of An Imbhmentioning

confidence: 92%

Indication of Another Intermediate-mass Black Hole in the Galactic Center

Takekawa

Oka

Iwata

et al. 2019

ApJL

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“…Medium-weight seeds would extend the correlation between the stellar and nuclear black hole masses to dwarf galaxies (Greene et al 2010;Safonova & Shastri 2010;Reines & Volonteri 2015;Mezcua et al 2018), they could explain the existence of Ultra Luminous X-ray sources (Miller et al 2004;Fritze et al 2018;Shen 2019;Barrows et al 2019;Baldassare et al 2020), and are necessary to prevent tidal distruption events in young star clusters observed in the galactic nucleus (Kim et al 2004). These ∼ 10 3 M BHs will be targeted by future third-generation gravitational telescopes, such as the Laser Interferometer Space Antenna (LISA) (Coleman Miller & Hamilton 2002;Sesana et al 2005; Amaro-Seoane & Santamaria 2010; Kremer et al 2019), but recent observations (Ballone et al 2018;Argo et al 2018;Takekawa et al 2019;Nguyen et al 2019;Woo et al 2019;Barack et al 2019) have found evidence of their existence in the Local Universe.…”

Section: Introductionmentioning

confidence: 99%

Light, medium-weight, or heavy? The nature of the first supermassive black hole seeds

Sassano

Schneider

Valiante

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Observations of hyper-luminous quasars at z > 6 reveal the rapid growth of supermassive black holes (SMBHs $>10^9 \rm M_{\odot }$) whose origin is still difficult to explain. Their progenitors may have formed as remnants of massive, metal free stars (light seeds), via stellar collisions (medium-weight seeds) and/or massive gas clouds direct collapse (heavy seeds). In this work we investigate for the first time the relative role of these three seed populations in the formation of z > 6 SMBHs within an Eddington-limited gas accretion scenario. To this aim, we implement in our semi-analytical data-constrained model a statistical description of the spatial fluctuations of Lyman-Werner (LW) photo-dissociating radiation and of metal/dust enrichment. This allows us to set the physical conditions for BH seeds formation, exploring their relative birth rate in a highly biased region of the Universe at z > 6. We find that the inclusion of medium-weight seeds does not qualitatively change the growth history of the first SMBHs: although less massive seeds ($<10^3 \rm M_\odot$) form at a higher rate, the mass growth of a $\sim 10^9 \rm M_\odot$ SMBH at z < 15 is driven by efficient gas accretion (at a sub-Eddington rate) on to its heavy progenitors ($10^5 \rm M_\odot$). This conclusion holds independently of the critical level of LW radiation and even when medium-weight seeds are allowed to form in higher metallicity galaxies, via the so-called super-competitive accretion scenario. Our study suggests that the genealogy of z ∼ 6 SMBHs is characterized by a rich variety of BH progenitors, which represent only a small fraction ($< 10 - 20{{\ \rm per\ cent}}$) of all the BHs that seed galaxies at z > 15.

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“…Astrophysical System -IMBHs are a class of BHs with masses M BH = 10 2 − 10 5 M . Thought to reside in the centres of smaller spiral galaxies, as well as in dense stellar environments such as globular clusters [51], a growing number of observations point toward the existence of IMBHs in nature [52][53][54][55]. In addition, there are multiple plausible formation mechanisms, such as runaway growth through the mergers of stellar mass objects [56][57][58]; by the direct collapse of gas clouds at high redshift [59,60]; or primordial formation through the collapse of large density perturbations before Big Bang Nucleosynthesis [61][62][63].…”

Section: Introduction -mentioning

confidence: 99%

Unique Multimessenger Signal of QCD Axion Dark Matter

et al. 2020

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We propose a multi-messenger probe of the natural parameter space of QCD axion dark matter based on observations of black hole-neutron star binary inspirals. It is suggested that a dense dark matter spike may grow around intermediate mass black holes (10 3 − 10 5 M ). The presence of such a spike produces two unique effects: a distinct phase shift in the gravitational wave strain during the inspiral and a enhancement of the radio emission due to the resonant axion-photon conversion occurring in the neutron star magnetosphere throughout the inspiral and merger. Remarkably, the observation of the gravitational wave signal can be used to infer the dark matter density and, consequently, to predict the radio emission. We study the projected sensitivity to the axion-photon coupling in the light of the LISA interferometer and next-generation radio telescopes such as the Square Kilometre Array. Given a sufficiently nearby detection, such observations will explore the QCD axion in the mass range 10 −7 eV to 10 −5 eV.

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Weighing the IMBH candidate CO-0.40-0.22* in the Galactic Centre

Cited by 14 publications

References 105 publications

Indication of Another Intermediate-mass Black Hole in the Galactic Center

Indication of Another Intermediate-mass Black Hole in the Galactic Center

Light, medium-weight, or heavy? The nature of the first supermassive black hole seeds

Unique Multimessenger Signal of QCD Axion Dark Matter

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