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SUMMARY:Numerical-relativity-informed effective-one-body model for black-h
 ole–neutron-star mergers with higher modes and spin precession - Alejand
 ra González (FSU Jena)
DTSTART:20240216T130000Z
DTEND:20240216T140000Z
UID:TALK212317@talks.cam.ac.uk
CONTACT:Daniela Cors
DESCRIPTION:We present the first effective-one-body model for generic-spin
 s quasicircular black-hole–neutron-star (BHNS) inspiral-merger-ringdown 
 gravitational waveforms (GWs). Our model is based on a new numerical-relat
 ivity (NR) informed expression of the BH remnant and its ringdown. It repr
 oduces the NR (ℓ\, m ) = ( 2\, 2 ) waveform with typical phase agreement
  of ≲0.5 rad ( ≲1 rad) to merger (ringdown). The maximum (minimum) mis
 match between the (2\, 2) and the NR data is 4% (0.6%). Higher modes (HMs)
  (2\, 1)\, (3\, 2)\, (3\, 3)\, (4\, 4)\, and (5\, 5) are included\, and th
 eir mismatch with the available NR waveforms are up to (down to) a 60% (1%
 ) depending on the inclination. Phase comparison with a 16 orbit precessin
 g simulation shows differences within the NR uncertainties. We demonstrate
  the applicability of the model in GW parameter estimation by performing t
 he first BHNS Bayesian analysis with HMs (and nonprecessing spins) of the 
 event GW190814\, together with new (2\, 2)-mode analysis of GW200105 and G
 W200115. For the GW190814 study\, the inclusion of HMs gives tighter param
 eter posteriors. The Bayes factors of our analyses on this event show deci
 sive evidence for the presence of HMs\, but no clear preference for a BHNS
  or a binary black hole source. Similarly\, we confirm GW200105 and GW2001
 15 show no evidence for tidal effects.
LOCATION:Potter room/Zoom
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