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Modelling the gravitational radiation emitted by merging black holes - - PowerPoint PPT Presentation

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Modelling the gravitational radiation emitted by merging black holes Harald Pfeiffer CITA, University of Toronto AEI, Potsdam Stephen Hawking 75th Birthday Conference July 4, 2017 LIGO-G1701238 Waveform-knowledge essential to GW astronomy

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SLIDE 1

Modelling the gravitational radiation emitted by merging black holes

Harald Pfeiffer

CITA, University of Toronto AEI, Potsdam Stephen Hawking 75th Birthday Conference July 4, 2017

LIGO-G1701238

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SLIDE 2

Waveform-knowledge essential to GW astronomy

2 Harald Pfeiffer Hawking 75 Jul 4, 2017

“GW150914” Abbott+ PRL 116, 061102 (2016) “GW151226” Abbott+ PRL 116, 241203 (2016)

Detection by matched filtering Parameter estimation Testing GR

“GW170104” Abbott+ PRL 118, 221101 (2017)

Modelling ⇒ physics & astronomy

➔ Pablo Laguna ➔ Gaby Gonzalez ➔ Bruce Allen ➔ Frans Pretorius

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SLIDE 3

3 Harald Pfeiffer Hawking 75 Jul 4, 2017

Waveforms! Accurately & comprehensively

https://youtu.be/Zt8Z_uzG71o

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SLIDE 4

3 Harald Pfeiffer Hawking 75 Jul 4, 2017

Waveforms! Accurately & comprehensively

https://youtu.be/Zt8Z_uzG71o

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SLIDE 5

Tools to model BBH

4 Harald Pfeiffer Hawking 75 Jul 4, 2017

Inspiral Ringdown Merger

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SLIDE 6

Tools to model BBH

5 Harald Pfeiffer Hawking 75 Jul 4, 2017

Inspiral Ringdown Merger Perturbative expansion in v/c

Blanchet, Living Reviews

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SLIDE 7

6 Harald Pfeiffer Hawking 75 Jul 4, 2017

Blanchet, Living Reviews

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SLIDE 8

Tools to model BBH

7 Harald Pfeiffer Hawking 75 Jul 4, 2017

Merger Ringdown Inspiral

0 mass-ratio 1

Berti+ 06

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SLIDE 9

Tools to model BBH

8 Harald Pfeiffer Hawking 75 Jul 4, 2017

Inspiral Ringdown Merger

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SLIDE 10

Tools to model BBH

9 Harald Pfeiffer Hawking 75 Jul 4, 2017

Merger Ringdown Inspiral

0 mass-ratio 1

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SLIDE 11

Tools to model BBH

10 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

S , e

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SLIDE 12

Tools to model BBH

11 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

S , e

LIGO/Caltech/MIT/Sonoma State (Aurore Simonnet)

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SLIDE 13

Tools to model BBH

12 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

LIGO/Caltech/MIT/Sonoma State (Aurore Simonnet)

NS-BH (stellar mass) S , e

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SLIDE 14

Tools to model BBH

13 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

NS-NS NS-BH (stellar mass) SMBH mergers Extreme-mass-ratio inspirals S , e Congrats to the approved mission!

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SLIDE 15

Numerical Relativity

Harald Pfeiffer Hawking 75 Jul 4, 2017 14

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SLIDE 16

50 Years of numerical relativity for BBH


1994 Cook 


Bowen-York 
 initial data

1989-95 
 Bona-Masso 


modified ADM, (hyperbolicity)

1999-2005 JW York, Cornell, Caltech, LSU 


hyperbolic formulations

1975-77
 Smarr-Eppley


head-on collision 


1962 ADM 


3+1 formulation

1994-95
 NCSA-WashU


improved
 head-on collision

1999 
 BSSN 


evolution 
 system

1964 
 Hahn-Lindquist


2 wormholes

2000-02
 Alcubierre


gauge conditions

Courtesy Carlos Lousto, updated by HP

1999 York


conformal thin sandwich ID

2003-08
 Cook, Pfeiffer ea


improved ID

2006,07
 Baker ea;
 Gonzalez ea


non-spinning BBH kicks

2007-11
 RIT; Jena; AEI;…


BBH superkicks

2000 Ashtekar 


isolated horizons

2008
 all of NR


NINJA

2007 SXS


PN-NR
 comparison

2006-08 


Scheel+ (SXS)
 IMR w/ spectral

2005-06 


Campanelli+; Baker+
 IMR w/ BSSN &
 moving punctures

2000-04


AEI/UTB-NASA
 revive crashing codes (Lazarus)

1984
 Unruh 


excision

1997 
 Brandt- Brügmann 


puncture data

2004
 Brügmann ea 


  • ne orbit

2005 Pretorius


inspiral-merger-
 ringdown (IMR) 
 w/ harmonic

1999-00
 AEI/PSU 


grazing collisions

2007-
 Ajith, AEI, Jena


phenom GW models

2009-
 UMD, SXS


EOB GW models

2011 
 Schmidt ea; Boyle ea


Radiation aligned frame

2011
 Lousto ea


q=100

1992,3 
 Choptuik;

Abrahams+Evans


critical phenomena

~2000 Choptuik;
 Schnetter;Brügmann


mesh refinement

15 Harald Pfeiffer Hawking 75 Jul 4, 2017 1994-98


BBH Grand Challenge

2015 ~1999 1964

1979 York 


kinematics and dynamics of GR

~2005

2005
 Gundlach ea


constraint damping

2015
 Szilagyi ea


175 orbits

2014-


precessing 
 GW models

2011
 Lovelace ea


S/M2=0.97

2011-
 Le Tiec ea

self-force studies

2009-11 
 Bishop, ...


Cauchy 
 characteristic extraction

2010 
 Bernuzzi ea


C4z

2013
 GaTech; SXS

Precessing parameter studies

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SLIDE 17

First simulations

16 Harald Pfeiffer Hawking 75 Jul 4, 2017

Pretorius 05

Important early result: Simplicity of merger Continuous transition 
 inspiral → ringdown

Campanelli+06 Baker+07 Baker+06

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SLIDE 18

The two main approaches to BBH

17 Harald Pfeiffer Hawking 75 Jul 4, 2017

Quasi-equilibrium excision initial-data

(Cook&HP 04, 
 Lovelace..HP+ 08)

Generalized Harmonic
 w/ constraint damping

(Gundlach+ 05, Pretorius 05)

Damped harmonic gauge
 Constraint preserving and minimally reflective outer BC Multi-domain spectral methods SpEC/SXS collaboration 


Cornell/Caltech/CITA/WSU/Fullerton/AEI

Puncture initial-data

(Brandt&Brügmann 97)

BSSN or C4z 
 w/ moving punctures

(Campanelli ea 06, Baker ea 06, 
 Bernuzzi, Hildtich 10, Alic ea 12)




1+log, Gamma-driver gauge Sommerfeld outer BC Finite differences w/ AMR

RIT, GATech, Goddard, Jena, 
 Palma, Cardiff, Perimeter

Pretorius FD, AMR, GH

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SLIDE 19

Einstein constraints …

18 Harald Pfeiffer Hawking 75 Jul 4, 2017

R + (trK)2 K2 = 0 r · (K g trK) = 0

g = ψ4˜ g K = 1

3trK g + A

Lichnerowicz 44 York(+) 72;74;99 HP,York 03

˜ r2ψ = . . . ˜ r·( 1

˜ σ ˜

LV ) = . . .

conformal scaling conformal scaling

TT decomp. conformal
 TT decomp.

˜ A

A = ATT + 1 σ (LV ) ˜ A = ˜ ATT + 1 ˜ σ (˜ LV )

A = ψ−10 ˜ A

ATT = ψ−10 ˜ ATT σ = ψ6˜ σ

A

Hamiltonian picture ≡ Lagrangian picture

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SLIDE 20

… for binary black holes

  • Asymptotics/boundary conditions
  • Elliptic solver
  • High spin

19 Harald Pfeiffer Hawking 75 Jul 4, 2017

  • Control eccentricity

HP+ 02, Ansorg 04 Brandt,Brügmann 97; Cook,HP 04 Lovelace..HP+ 08 HP+ 05; Buonanno..HP+ 08

˜ r2ψ = . . . ˜ r·( 1

˜ N ˜

Lβ)= . . . ˜ r2 ˜ N = . . .

Erot / Erot, max

0.25 0.5 0.75 1 0.2 0.4 0.6 0.8 1

S/M

2

w/ conformal flatness

0.9995

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SLIDE 21

20 Harald Pfeiffer Hawking 75 Jul 4, 2017

Einstein Evolution Equations

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SLIDE 22

Spectral Einstein Code (SpEC)

  • Expand in basis-functions



 
 
 


  • Compute derivatives


analytically
 
 
 


21 Harald Pfeiffer Hawking 75 Jul 4, 2017

u(x, t) =

N

  • k=1

˜ u(t)kΦk(x)

http://www.black-holes.org/SpEC.html

u0(x, t) =

N

X

k=1

˜ u(t)kΦ0

k(x)

Simulations of Extreme Spacetimes (SXS) collaboration

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SLIDE 23

Spectral Einstein Code (SpEC)

  • Expand in basis-functions



 
 
 


  • Compute derivatives


analytically
 
 
 


21 Harald Pfeiffer Hawking 75 Jul 4, 2017

u(x, t) =

N

  • k=1

˜ u(t)kΦk(x)

http://www.black-holes.org/SpEC.html

u0(x, t) =

N

X

k=1

˜ u(t)kΦ0

k(x)

Simulations of Extreme Spacetimes (SXS) collaboration

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SLIDE 24

Spectral Einstein Code (SpEC)

  • Expand in basis-functions



 
 
 


  • Compute derivatives


analytically
 
 
 


21 Harald Pfeiffer Hawking 75 Jul 4, 2017

u(x, t) =

N

  • k=1

˜ u(t)kΦk(x)

http://www.black-holes.org/SpEC.html

u0(x, t) =

N

X

k=1

˜ u(t)kΦ0

k(x)

Simulations of Extreme Spacetimes (SXS) collaboration

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SLIDE 25

Spectral Einstein Code (SpEC)

  • Expand in basis-functions



 
 
 


  • Compute derivatives


analytically
 
 
 


21 Harald Pfeiffer Hawking 75 Jul 4, 2017

u(x, t) =

N

  • k=1

˜ u(t)kΦk(x)

http://www.black-holes.org/SpEC.html

u0(x, t) =

N

X

k=1

˜ u(t)kΦ0

k(x)

Simulations of Extreme Spacetimes (SXS) collaboration

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SLIDE 26

BH boundaries

  • Excise inside BH horizons
  • Grid rotates with BHs, 


and conforms to shape of AH

  • Outer boundary
  • constraint preserving
  • minimally reflective

22 Harald Pfeiffer Hawking 75 Jul 4, 2017

Scheel, HP+ 06, 08; Szilagyi+08; Hemberger+ 13 Lindblom, Rinne+ 06

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SLIDE 27

23 Harald Pfeiffer Hawking 75 Jul 4, 2017

https://youtu.be/p647WrQd684

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SLIDE 28

23 Harald Pfeiffer Hawking 75 Jul 4, 2017

https://youtu.be/p647WrQd684

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SLIDE 29

24 Harald Pfeiffer Hawking 75 Jul 4, 2017

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SLIDE 30

Equal mass, zero spin

25 Harald Pfeiffer Hawking 75 Jul 4, 2017

Scheel,HP+ 09

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SLIDE 31

Equal mass, zero spin

25 Harald Pfeiffer Hawking 75 Jul 4, 2017

Scheel,HP+ 09

  • Rapid convergence due to spectral methods
  • Small errors due to moving grid
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SLIDE 32

post-Newtonian vs. NR

26 Harald Pfeiffer Hawking 75 Jul 4, 2017 1200 2400 3600

  • 0.6
  • 0.3

0.3 26 18 10 2

TaylorT1 TaylorT2 TaylorT3 TaylorT4

PN order 2.0

GW-cycles to merger

φPN - φNR (radians)

t/m

PN order 2.5 PN order 3.0 PN order 3.5

Boyle..HP+ 07 PN approximants Equally justified approaches to derive inspiral rate from energy balance

dE dt = −FGW

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SLIDE 33

post-Newtonian vs. NR

26 Harald Pfeiffer Hawking 75 Jul 4, 2017 1200 2400 3600

  • 0.6
  • 0.3

0.3 26 18 10 2

TaylorT1 TaylorT2 TaylorT3 TaylorT4

PN order 2.0

GW-cycles to merger

φPN - φNR (radians)

t/m

PN order 2.5 PN order 3.0 PN order 3.5

Boyle..HP+ 07 PN approximants Equally justified approaches to derive inspiral rate from energy balance

dE dt = −FGW

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SLIDE 34

post-Newtonian vs. NR

26 Harald Pfeiffer Hawking 75 Jul 4, 2017 1200 2400 3600

  • 0.6
  • 0.3

0.3 26 18 10 2

TaylorT1 TaylorT2 TaylorT3 TaylorT4

PN order 2.0

GW-cycles to merger

φPN - φNR (radians)

t/m

PN order 2.5 PN order 3.0 PN order 3.5

Boyle..HP+ 07 PN approximants Equally justified approaches to derive inspiral rate from energy balance

dE dt = −FGW

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SLIDE 35

post-Newtonian vs. NR

26 Harald Pfeiffer Hawking 75 Jul 4, 2017 1200 2400 3600

  • 0.6
  • 0.3

0.3 26 18 10 2

TaylorT1 TaylorT2 TaylorT3 TaylorT4

PN order 2.0

GW-cycles to merger

φPN - φNR (radians)

t/m

PN order 2.5 PN order 3.0 PN order 3.5

Boyle..HP+ 07 PN approximants Equally justified approaches to derive inspiral rate from energy balance

dE dt = −FGW

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SLIDE 36

post-Newtonian vs. NR

27 Harald Pfeiffer Hawking 75 Jul 4, 2017

1000 2000 3000 4000

  • 0.0004

0.0004

NR TaylorT4 3.5

3500 3600 3700 3800 3900

  • 0.005

0.005

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SLIDE 37

post-Newtonian vs. NR

  • NR & PN agree!

27 Harald Pfeiffer Hawking 75 Jul 4, 2017

1000 2000 3000 4000

  • 0.0004

0.0004

NR TaylorT4 3.5

3500 3600 3700 3800 3900

  • 0.005

0.005

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SLIDE 38

post-Newtonian vs. NR

  • NR & PN agree!
  • Or do they?
  • Some versions of PN

match well

  • No a priori

knowledge which

  • nes work (if any)

27 Harald Pfeiffer Hawking 75 Jul 4, 2017

1000 2000 3000 4000

  • 0.0004

0.0004

NR TaylorT1 3.5

3200 3400 3600 3800

  • 0.004

0.004

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SLIDE 39

post-Newtonian vs. NR

  • NR & PN agree!
  • Or do they?
  • Some versions of PN

match well

  • No a priori knowledge

which ones work (if any)

  • q=1, S=0 best case
  • unequal masses and/
  • r spinning BH give

larger deviations

28 Harald Pfeiffer Hawking 75 Jul 4, 2017

Ohme+ 11, MacDonald..HP+ 12

goal

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SLIDE 40

Waveform modeling for GW astronomy

Harald Pfeiffer Hawking 75 Jul 4, 2017 29

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SLIDE 41

Waveform models

  • Analytical results


for early inspiral

  • Numerical Relativity (NR) for 


late inspiral, merger, ringdown

  • Combine. Interpolate to

continuous parameters.

30 Harald Pfeiffer Hawking 75 Jul 4, 2017

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SLIDE 42

Progress: Length of simulations

31 Harald Pfeiffer Hawking 75 Jul 4, 2017

Baker ea 07 Pretorius 05

  • 100
  • 80
  • 60
  • 40
  • 20
  • 0.20
  • 0.10

0.00 0.10 0.20

q=6 Buchman et al. ’12

(t − tpeak) / 1000M

Re(DL h22 / M)

Szilagyi ea 15 Campanelli ea 06

Scheel..HP+ 09, MacDonald..HP+ 12

Baker ea 06

q=1/7, S=0

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SLIDE 43

Progress: Number of simulations

32 Harald Pfeiffer Hawking 75 Jul 4, 2017

NINJA

Aylott ea 09

1st SXS Catalog

Mroue .. HP, ea 13

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SLIDE 44

Progress: Number of simulations

32 Harald Pfeiffer Hawking 75 Jul 4, 2017

NINJA

Aylott ea 09

1st SXS Catalog

Mroue .. HP, ea 13

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SLIDE 45

Now 1000’s of simulations

  • BAM/Cardiff/Palma

waveform modelling “Phenom” e.g. Husa+ 15, Hannam+ 14, Kahn+16

  • Georgia Tech

merger/ringdown properties e.g. Pekowsky+ 13, Jani+ 15

  • RIT

remnant mass/spin/kick formulae e.g. Healy+ 14, Zlochower+ 15, Healy+ 17

  • SXS

waveform modelling “SEOBNR” e.g. Mroue..HP+ 13, Chu..HP+ 15, Hemberger+ 15,
 Blackman..HP+ 17

33 Harald Pfeiffer Hawking 75 Jul 4, 2017

Blackman+ 16 Jani+ 
 1605.03204

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SLIDE 46

Some records

34 Harald Pfeiffer Hawking 75 Jul 4, 2017

  • 100
  • 80
  • 60
  • 40
  • 20
  • 0.20
  • 0.10

0.00 0.10 0.20

q=6 Buchman et al. ’12

(t − tpeak) / 1000M

Re(DL h22 / M)

Szilagyi..HP+15 Scheel+ 14 Lovelace..HP+15

q=1: S/M2=0.994 q<1: S/M2=0.95

q=1/7, χ=0

Husa+ 15

q=1/18, S1z=-0.8 or +0.4

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SLIDE 47

Fully generic (eccentric & precessing) BBH

  • Ωθ- Ωr resonances
  • At extreme mass-

ratios: 
 strong impact 


  • n GW-phase
  • At our q=1/7:


no discernible impact

35 Harald Pfeiffer Hawking 75 Jul 4, 2017

Lewis, Zimmerman, HP 17 Flanagan,Hinderer 12
 Flanagan+ 14

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SLIDE 48

Effective one body (EOB)

  • Mapping of post-Newtonian onto geodesic


motion in non-physical spacetime

  • Effective Hamiltonian

  • Add radiation reaction terms



 


  • Many other features
  • Big benefits for waveform modeling:
  • Schwarzschild geodesics built in by construction (𝝃➔0)
  • Easy to utilize non-PN information

36 Harald Pfeiffer Hawking 75 Jul 4, 2017

H = µ ⌅ p2

r + A(r)

  • 1 + p2

r

r2 + 2(4 − 3ν)ν p4

r

r2 ⇥ , A(r) =

4

⇤

k=0

ak(ν) rk + a5(ν) r5 dpr dt = −∂H ∂pr + ar

RR

˙ r r2Ω

  • Fφ

Buonanno, Damour 99; many papers since

dpϕ dt = 0 − v3

Ω

νV 6

φ

F 4

4 (Vφ; ν, vpole)

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SLIDE 49

Tools to model BBH

37 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

S , e

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SLIDE 50

Tools to model BBH

38 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

S , e

∆φ=2π(K-1) K=1.28

O(𝜉) corrections to 
 Schwarzschild periastron-advance

Barack,Damour,Sago 10

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SLIDE 51

Tools to model BBH

39 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

S , e

∆φ=2π(K-1) K=1.28

EOB Hamiltonian

O(𝜉) corrections to 
 Schwarzschild periastron-advance

Barack,Damour,Sago 10

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SLIDE 52

Tools to model BBH

40 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

S , e

NR inspiral phasing 
 NR GW-amplitudes

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SLIDE 53

Tools to model BBH

41 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

S , e

EOB Hamiltonian & radiation reaction

NR inspiral phasing 
 NR GW-amplitudes

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SLIDE 54

EOB inspiral-merger-ringdown

42 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

S , e EOB Hamiltonian & radiation reaction

(some coefficients fitted from NR)

N R 


p h e n

  • m

e n

  • l
  • g

y

ringdown modes 
 (initial conditions from NR)

Incorporates q➔0 perturbation theory

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SLIDE 55

SEOBNR models

  • Time-domain model
  • slow
  • State of the art
  • SEOBNRv4 (aligned spin)
  • SEOBNRv3 (precession)

43 Harald Pfeiffer Hawking 75 Jul 4, 2017

Bohe..HP+, 17 Pan..HP+ 14 Taracchini..HP+ 14

slide-56
SLIDE 56

1/q

K0+K1/q+O(q-2)

Periastron Advance: 3-way comparison

44 Harald Pfeiffer Hawking 75 Jul 4, 2017

Mroue..HP+ 09; Le Tiec..HP+ 11

∆φ=2π(K-1) K=1.28

PN SF

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SLIDE 57

1/q

K0+K1/q+O(q-2)

Periastron Advance: 3-way comparison

44 Harald Pfeiffer Hawking 75 Jul 4, 2017

Mroue..HP+ 09; Le Tiec..HP+ 11

∆φ=2π(K-1) K=1.28

K0+K1ν+O(q-2)

Expressed in symmetric mass- ratio ν=q/(1+q)2, perturbation theory works at equal masses!

PN SF

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SLIDE 58

Phenomenological models

  • frequency-domain model
  • very fast
  • State of the art:
  • PhenomD (aligned spin)
  • PhenomPv2 (precessing)

45 Harald Pfeiffer Hawking 75 Jul 4, 2017

Khan+15 Hannam+13

analytical

Mf

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SLIDE 59

Phenomenological models

  • frequency-domain model
  • very fast
  • State of the art:
  • PhenomD (aligned spin)
  • PhenomPv2 (precessing)

46 Harald Pfeiffer Hawking 75 Jul 4, 2017

Khan+15 Hannam+13

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SLIDE 60

PhenomD vs. SEOBNRv4

  • Aligned spin, (2,2)-mode only
  • Agreement, except for large


spins and/or large mass-ratio

47 Harald Pfeiffer Hawking 75 Jul 4, 2017

Bohe+ 16

faithfulness

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SLIDE 61

PhenomD vs. SEOBNRv4

  • Aligned spin, (2,2)-mode only
  • Agreement, except for large


spins and/or large mass-ratio

47 Harald Pfeiffer Hawking 75 Jul 4, 2017

Bohe+ 16

faithfulness

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SLIDE 62

Orbital and spin precession

  • post-Newtonian reproduces NR-precession very

well

48 Harald Pfeiffer Hawking 75 Jul 4, 2017

Ossokine..HP+, 1502.01747

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SLIDE 63

Factoring out precession

49 Harald Pfeiffer Hawking 75 Jul 4, 2017

Figure courtesy J. Blackman Buonanno+ 03 O’Shaughnessy+ 11 Boyle..HP 11
 Schmidt+ 13

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SLIDE 64

Analysis of GW-events with two models

50 Harald Pfeiffer Hawking 75 Jul 4, 2017

SEOBNRv3 & PhenomPv2:

  • analytical precession
  • underlying NR-fitted aligned-spin

model

  • l=2 modes only

In progress: improved near-merger precession & subdominant modes

PhenomPv2 SEONRv3_opt accelerated for fast evaluation Etienne+; Pürrer

“GW170104” Abbott+ PRL 118, 221101 (2017)

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SLIDE 65

NR validation of GW150914

51 Harald Pfeiffer Hawking 75 Jul 4, 2017

All physics/all-mode NR injection

  • vs. (2,2) waveform model

recovery as GW150914

LIGO & Virgo Collaborations: Effects of waveform model systematics on the interpretation of GW150914 (2017)

NR vs NR consistency RIT vs. SpEC h22 overlap 0.998

Lovelace, Lousto..HP+ 16

slide-66
SLIDE 66

GW151226

  • SEOBNRv2 templates vs. independent NR simulation

52 Harald Pfeiffer Hawking 75 Jul 4, 2017

“GW151226” Abbott+ PRL 116, 241203 (2016)

slide-67
SLIDE 67

NR-based surrogate models

  • Ingredients
  • Basis ei(t)
  • temporal compression
  • interpolation in λ
  • Most ambitious so far:


precession & subdominant modes


7-D parameter space

  • mass-ratio, S1, S2
  • 1/2≦q≦1, S/M2≦0.8
  • last ~20 orbits
  • 744 SpEC simulations
  • all (l,m) modes with l≦4

53 Harald Pfeiffer Hawking 75 Jul 4, 2017

Field+ 13
 Blackman+ 15
 Pürrer 16 Blackman..HP+ 16 Blackman..HP+ 16

slide-68
SLIDE 68

NR-based surrogate models

54 Harald Pfeiffer Hawking 75 Jul 4, 2017

0 mass-ratio 1

Merger Ringdown Inspiral

S , e NR
 surrogate EOB waveform

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SLIDE 69

Eccentric BBH

  • Inspiral-merger-ringdown
  • unequal mass
  • non-spinning
  • e10Hz ≲ 0.4
  • Intense efforts
  • better accuracy
  • aligned-spins

55 Harald Pfeiffer Hawking 75 Jul 4, 2017

Huerta..HP+ 17

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SLIDE 70

Challenges

  • BH-NS-like mass-ratios: q~1/10
  • previous grandiose plots were for q~1
  • not to speak of IMRI or EMRI
  • Higher SNR
  • Advanced LIGO design ~100
  • 3rd generation & LISA ~1000
  • More events
  • some will be special

edge-on (precession) eccentricity

  • multi-event testing GR

56 Harald Pfeiffer Hawking 75 Jul 4, 2017

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SLIDE 71

Summary

  • BBH sims stunningly successful in past years
  • Several analytical waveform models which underpin

today’s GW astronomy

  • Big challenge: 


Push capabilities 
 by 10x. Any of

  • spins
  • mass-ratio
  • length
  • accuracy

57 Harald Pfeiffer Hawking 75 Jul 4, 2017

https://youtu.be/c-2XIuNFgD0

slide-72
SLIDE 72

Summary

  • BBH sims stunningly successful in past years
  • Several analytical waveform models which underpin

today’s GW astronomy

  • Big challenge: 


Push capabilities 
 by 10x. Any of

  • spins
  • mass-ratio
  • length
  • accuracy

57 Harald Pfeiffer Hawking 75 Jul 4, 2017

https://youtu.be/c-2XIuNFgD0