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

Takekawa, Shunya; Oka, Tomoharu; Iwata, Yuhei; Tsujimoto, Shiho; Nomura, Munehiro

doi:10.3847/2041-8213/aafb07

Cited by 41 publications

(38 citation statements)

References 49 publications

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“…We conclude with the remark that Kepler's game changing three laws remain as relevant to our exploration of the universe and the laws that govern it today as when they were first formulated. No better illustration of this fact may be found than in [26,27]. Studying the motion of matter around a black hole could provide a test for the validity/corrections of Kepler's laws at the large scale.…”

Section: Discussionmentioning

confidence: 99%

“Kepler Harmonies” and conformal symmetries

et al. 2019

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Kepler's rescaling becomes, when "Eisenhart-Duval lifted" to 5-dimensional "Bargmann" gravitational wave spacetime, an ordinary spacetime symmetry for motion along null geodesics, which are the lifts of Keplerian trajectories. The lifted rescaling generates a well-behaved conserved Noether charge upstairs, which takes an unconventional form when expressed in conventional terms. This conserved quantity seems to have escaped attention so far. Applications include the Virial Theorem and also Kepler's Third Law. The lifted Kepler rescaling is a Chrono-Projective transformation. The results extend to celestial mechanics and Newtonian Cosmology.

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Section: Discussionmentioning

confidence: 99%

“Kepler Harmonies” and conformal symmetries

et al. 2019

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“…We also discuss the effect from a possible massive dark perturber, such as an intermediate-mass black hole. A number of IMBH candidates have been suggested near the Galactic Center [54][55][56]. An IMBH orbiting around the black hole can cause Kozai oscillations of the orbital parameters of a star if the IMBH is located outside of the stellar orbit.…”

Section: Effects From Ambient Perturbersmentioning

confidence: 99%

Testing the black hole no-hair theorem with Galactic Center stellar orbits

O’Shaughnessy

Brady

2021

Phys. Rev. D

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Theoretical investigations have provided proof-of-principle calculations suggesting measurements of stellar or pulsar orbits near the Galactic Center could strongly constrain the properties of the Galactic Center black hole, local matter, and even the theory of gravity itself. As in previous studies, we use a Markov chain Monte Carlo to quantify what properties of the Galactic Center environment measurements can constrain. In this work, however, we also develop an analytic model (Fisher matrix) to understand what parameters are well-constrained and why. Using both tools, we conclude that existing astrometric measurements cannot constrain the spin of the Galactic Center black hole. Extrapolating to the precision and cadence of future experiments, we anticipate that the black hole spin can be measured with the known star S2. Our calculations show that we can measure the dimensionless black hole spin to a precision of ∼0.1 with weekly measurements of the orbit of S2 for 40 years using the GRAVITY telescope's best resolution at the Galactic Center, i.e., an angular resolution of 10 μarcsec and a radial velocity resolution of 500 m=s. An analytic expression is derived for the measurement uncertainty of the black hole spin using the Fisher matrix in terms of observation strategy, star's orbital parameters, and instrument resolution. From it we conclude that highly eccentric orbits can provide better constraints on the spin, and that an orbit with a higher eccentricity is more favorable even when the orbital period is longer. We also apply it to S62, S4711, and S4714 to show whether they can constrain the black hole spin sooner than S2. If in addition future measurements include the discovery of a new, tighter stellar orbit, then future data could conceivably enable tests of strong field gravity, by directly measuring the black hole quadrupole moment. Our simulations show that with a stellar orbit similar to that of S2 but at one-fifth the distance to the Galactic Center and GRAVITY's resolution limits on the Galactic Center, we can start to test the no-hair theorem with 20 years of weekly orbital measurements.

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

Cited by 41 publications

References 49 publications

“Kepler Harmonies” and conformal symmetries

“Kepler Harmonies” and conformal symmetries

Testing the black hole no-hair theorem with Galactic Center stellar orbits

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

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