Modeling the Black hole Merger of QSO 3C 186

Carlos O.Lousto, Yosef Zlochower, Manuela Campanelli
Astrophysical Journal Letter
Volume 841, Number 2
Publication date: 
June 1, 2017
E-print ID: 

Recent detailed observations of the radio-loud quasar
  3C 186 indicate the possibility that a supermassive recoiling black
  hole is moving away from the host galaxy at a speed of nearly
  2100km/s. If this is the case, we can model the mass ratio and spins
  of the progenitor binary black hole using the results of numerical
  relativity simulations. We find that the black holes in the
  progenitor must have comparable masses with a mass ratio
  $q=m_1/m_2>1/4$ and the spin of the primary black hole must be
  $\alpha_2=S_2/m_2^2>0.4$. The final remnant of the merger is bounded
  by $\alpha_f>0.45$ and at least $4\%$ of the total mass of the
  binary system is radiated into gravitational waves.  We consider
  four different pre-merger scenarios that further narrow those
  values.  Assuming, for instance, a cold accretion driven merger
  model, we find that the binary had comparable masses with
  $q=0.70^{+0.29}_{-0.21}$ and the normalized spins of the larger and
  smaller black holes were $\alpha_2=0.94^{+0.06}_{-0.22}$ and
  $\alpha_1=0.95^{+0.05}_{-0.09}$.  We can also estimate the final
  recoiling black hole spin $\alpha_f=0.93^{+0.02}_{-0.03}$ and that
  the system radiated $9.6^{+0.8}_{-1.4}\%$ of its total mass, making
  the merger of those black holes the most energetic event ever

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