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• W4200328400 endingPage "035009" @default.
• W4200328400 startingPage "035009" @default.
• W4200328400 abstract "Abstract We have previously constructed a waveform model, <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{E}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> </mml:math> , for spinning binary black hole (BBH) moving along eccentric orbit based on effective-one-body (EOB) formalism. In the current paper, we update <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{E}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> </mml:math> waveform model in the following three respects. Firstly, we update the EOB dynamics from <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{v}mathtt{1}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>v</mml:mi> <mml:mi mathvariant=monospace>1</mml:mi> </mml:math> to <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{v}mathtt{4}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>v</mml:mi> <mml:mi mathvariant=monospace>4</mml:mi> </mml:math> . Secondly we properly treat the Schott term which has been ignored in previous <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{E}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> </mml:math> . Thirdly, we construct a new factorized waveform including ( l , | m |) = (2, 2), (2, 1), (3, 3), (4, 4) modes based on EOB formalism, which is valid for spinning BBHs in general equatorial orbit. Following our previous <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{E}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> </mml:math> waveform model, we call our new waveform model <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{E}mathtt{H}mathtt{M}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>H</mml:mi> <mml:mi mathvariant=monospace>M</mml:mi> </mml:math> . The ( l , | m |) = (2, 2) mode waveform of <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{E}mathtt{H}mathtt{M}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>H</mml:mi> <mml:mi mathvariant=monospace>M</mml:mi> </mml:math> can fit the original <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{v}mathtt{4}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>v</mml:mi> <mml:mi mathvariant=monospace>4</mml:mi> </mml:math> waveform very well in the case of a quasi-circular orbit. We have validated <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{E}mathtt{H}mathtt{M}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>H</mml:mi> <mml:mi mathvariant=monospace>M</mml:mi> </mml:math> waveform model through comparing the waveform against the Simulating eXtreme Spacetimes (SXS) catalog. The comparison is done for BBH with total mass in (20, 200) M ⊙ using Advanced LIGO designed sensitivity. For the quasi-circular cases we have compared our (2, 2) mode waveforms to the 281 numerical relativity (NR) simulations of BBH along quasi-circular orbits. All of the matching factors are bigger than 98%. For the elliptical cases, 24 NR simulations of BBH along an elliptic orbit are used. For each elliptical BBH system, we compare our modeled gravitational polarizations against the NR results for different combinations of the inclination angle, the initial orbit phase and the source localization in the sky. We use the minimal matching factor respect to the inclination angle, the initial orbit phase and the source localization to quantify the performance of the higher modes waveform. We found that after introducing the higher modes, the minimum of the minimal matching factor among the 24 tested elliptical BBHs increases from 90% to 98%. Our <?CDATA $mathtt{S}mathtt{E}mathtt{O}mathtt{B}mathtt{N}mathtt{R}mathtt{E}mathtt{H}mathtt{M}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML display=inline overflow=scroll> <mml:mi mathvariant=monospace>S</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>O</mml:mi> <mml:mi mathvariant=monospace>B</mml:mi> <mml:mi mathvariant=monospace>N</mml:mi> <mml:mi mathvariant=monospace>R</mml:mi> <mml:mi mathvariant=monospace>E</mml:mi> <mml:mi mathvariant=monospace>H</mml:mi> <mml:mi mathvariant=monospace>M</mml:mi> </mml:math> waveform model can match all tested 305 SXS waveforms better than 98% including highly spinning ( χ = 0.99) BBH, highly eccentric ( e ≈ 0.6 at reference frequency Mf 0 = 0.002) BBH and large mass ratio ( q = 10) BBH." @default.
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• W4200328400 date "2022-01-06" @default.
• W4200328400 modified "2023-10-13" @default.
• W4200328400 title "A higher-multipole gravitational waveform model for an eccentric binary black holes based on the effective-one-body-numerical-relativity formalism" @default.
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• W4200328400 cites W2029040036 @default.
• W4200328400 cites W2052486954 @default.
• W4200328400 cites W2064816908 @default.
• W4200328400 cites W2077590995 @default.
• W4200328400 cites W2081895114 @default.
• W4200328400 cites W2083106201 @default.
• W4200328400 cites W2095105526 @default.
• W4200328400 cites W2106723786 @default.
• W4200328400 cites W2110701413 @default.
• W4200328400 cites W2116108818 @default.
• W4200328400 cites W2118780319 @default.
• W4200328400 cites W2129637746 @default.
• W4200328400 cites W2137130944 @default.
• W4200328400 cites W2147286576 @default.
• W4200328400 cites W2148994792 @default.
• W4200328400 cites W2154444782 @default.
• W4200328400 cites W2154591922 @default.
• W4200328400 cites W2156317737 @default.
• W4200328400 cites W2162520084 @default.
• W4200328400 cites W2176588768 @default.
• W4200328400 cites W2252795400 @default.
• W4200328400 cites W2479210508 @default.
• W4200328400 cites W2550934118 @default.
• W4200328400 cites W2738941556 @default.
• W4200328400 cites W2741736477 @default.
• W4200328400 cites W2751467253 @default.
• W4200328400 cites W2778863159 @default.
• W4200328400 cites W2784624502 @default.
• W4200328400 cites W2784926093 @default.
• W4200328400 cites W2795203094 @default.
• W4200328400 cites W2921103789 @default.
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• W4200328400 cites W2937039551 @default.
• W4200328400 cites W2937580915 @default.
• W4200328400 cites W2940483016 @default.
• W4200328400 cites W2945766209 @default.
• W4200328400 cites W2971836485 @default.
• W4200328400 cites W2977635368 @default.
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• W4200328400 cites W2982457586 @default.
• W4200328400 cites W3001567423 @default.
• W4200328400 cites W3001597254 @default.
• W4200328400 cites W3003338883 @default.
• W4200328400 cites W3003843868 @default.
• W4200328400 cites W3005657359 @default.
• W4200328400 cites W3013826632 @default.
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