gravitational wave template and its overlap
DESCRIPTION
Gravitational Wave Template and its overlap. Hyung Won Lee, Inje University w ith Chunglee Kim(SNU) and Jeongcho Kim( Inje University). Contents. Motivation CBC Inspiral GW Waveform Time domain template Frequency domain template Overlap Calculation - PowerPoint PPT PresentationTRANSCRIPT
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Gravitational Wave Tem-plate and its overlap
Hyung Won Lee, Inje Universitywith Chunglee Kim(SNU) and Jeongcho Kim(Inje University)
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Motivation CBC Inspiral GW Waveform Time domain template Frequency domain template Overlap Calculation Parameter Dependence of overlap Remarks
Contents
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Theoretical derivation of GW tem-plate
Understanding LAL library
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Motivation
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Neutron star / Black hole binary Mass range : Frequency range : Inspiral, Merger, Ringdown
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CBC GW sources
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CBC Inspiral GW Waveform
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Gravitational Waveform
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Dominant mode
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, ,
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Energy and flux in PN ap-prox.
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XLALSimInspiralChooseTDWaveform() TaylorEt : TaylorT1 : TaylorT2 : TaylorT3 : TaylorT4 : IMRPhenomA : IMRPhenomB : EOBNRv2HM : effective one body EOBNRv2 : SpinTaylorT2 : SpinTaylorT4 : PhenSpinTaylor : PhenSpinTaylorRD : SEOBNRv1 :
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Time Domain Template
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Phys. Rev. D 80, 084043 (2009) , arxiv : 0907.0700
XLALSimInspiralTaylorEtPNGenera-tor()
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TaylorEt
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Numerical integration of equations
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TaylorT1
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Parametric solution of TaylorT1
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TaylorT2
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Solving TaylorT2 w.r.t. surrogate time
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TaylorT3
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Expand in TaylorT1, then integrate numerically
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TaylorT4
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PRD84, 124052(2011) XLALSimIMREOBNRv2AllModes()
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EOBNRv2HM
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PRD84, 124052(2011) XLALSimIMREOBNRv2Dominant-
Mode()
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EOBNRv2
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arxiv : gr-qc/0405090, gr-qc/0310034
XLALSimInspiralSpinTaylorT2()
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SpinTaylorT2
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arxiv : gr-qc/0405090, gr-qc/0310034
XLALSimInspiralSpinTaylorT4()
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SpinTaylorT4
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IMRPhenom references XLALSimSpinInspiralGenerator() Phenomenological waveform without
ring-down
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PhenSpinTaylor
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IMRPhenom references XLALSimIMRPhenSpinInspiralRDGenera-
tor() Phenomenological waveform with
ring-down
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PhenSpinTaylorRD
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PRD 86, 024011 (2012), arxiv : 1202.0790
XLALSimIMRSpinAlignedEOBWave-form()
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SEOBNRv1
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SEOBNRv1
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XLALSimInspiralChooseFDWaveform() TaylorF2 TaylorF2Amp IMRPhenomA : non-spinning IMR model IMRPhenomB : spinning IMR model IMRPhenomC : non-precessing IMR model IMRPhenomP : generic spins IMR model SpinTaylorF2 : spinning inspiral TaylorF2RedSpin : TaylorF2 reduced spin TaylorF2RedSpinTidal : TaylorF2 reduced spin with
tidal effect TaylorF1, PadeF1, BCV, BCVSpin (not active)
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Frequency Domain Tem-plate
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Solve equations
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TyalorF1
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arxiv : 0810.5336, 1303.7412, astro-ph/0504538
TaylorT2 using stationary phase ap-proximation(SPA)
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TaylorF2
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TaylorF2
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arxiv: 0710.2335, 0712.0343 XLALSimIMRPhenomAGenerateFD()
XLALSimIMRPhenomAGenerateTD()
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IMRPhenomA
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IMRPhenomA
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IMRPhenomA
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arxiv:0909.2867 XLALSimIMRPhenomBGenerateFD()
XLALSimIMRPhenomBGenerateTD()
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IMRPhenomB
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IMRPhenomB
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Phys.Rev.D82:064016,2010, arxiv:1005.3306
XLALSimIMRPhenomCGenerateFD()XLALSimIMRPhenomCGenerateTD()
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IMRPhenomC
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IMRPhonemC
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IMRPhonemC
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arxiv:1308.3271 XLALSimIMRPhenomP()
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IMRPhenomP
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arxiv: 0810.5336 (spin correction) XLALSimInspiralSpinTaylorF2() Spin correction to TaylorF2
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SpinTaylorF2
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arxiv: 1107.1267 XLALSimInspiralTaylorF2Reduced-
Spin()
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TaylorF2RedSpin
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TaylorF2RedSpin
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arxiv: 1107.1267, 1101.1673 XLALSimInspiralTaylorF2ReducedSpinTi-
dal()
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TaylorF2RedSpinTidal
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arxiv : 0810.5336, 1303.7412, astro-ph/0504538
TaylorT2 using stationary phase ap-proximation(SPA) and 2.5PN ampli-tude correction
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TaylorF2Amp
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Arun et.al., PRD79, 104023(2009) Amplitude corrections up to n=5
(2.5pN) are newly included
TaylorF2Amp
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Phase corrections up to 3.5PN (s-tandard in LAL)
TaylorF2Amp
+
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int XLALSimInspiralTaylorF2AmpPlus()Calculate
int XLALSimInspiralTaylorF2AmpCross()Calculate
REAL8 sf2_psi_SPA()Calculate
COMPLEX16 sf2_amp_SPA_plus(), cross()Calculate for ,
TaylorF2Amp Codes
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Overlap CalculationDataTemplate
One-sided power spectral density of noise
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LALInferencetest.c
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Likelihood Calculation
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Physical parameters
1d graph : change just one parameter 2d graph : change two parameters
No Results Yet!
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Parameter dependence of Overlap
Binary Chirp mass Mc
(Msun)
Symmetric mass ratio
η
distance(Mpc)
Inclination(rad)
Polarization(rad)
Orbital phase (rad)
Coales-cence time
(s)
RA(rad)
Dec(rad)
NS-NS
1.219 0.245 12.0
0.785 2.606 3.31 8943836790.64
50.575
BH-NS
2.9943 0.1077 23.1
BH-BH
8.705 0.245 45.0
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Changing one parameter does not give the correct physics
We need marginalized distribution using MCMC or similar methods
Theoretical integration over some physical parameters will help very much for computation time
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Remarks