Manuela Campanelli, LSC Worshop 3/20/2002

The Lazarus Project:The Lazarus Project:Modeling gravitational radiation Modeling gravitational radiation

from coalescing binary black from coalescing binary black holesholes

MANUELA CAMPANELLIDepartment Physics & Astronomy

The University of Texas at Brownsville

www.phys.utb.edu

Collaboration: John Baker (NASA) Carlos Lousto (UTB)

Warren Anderson (UTB)Bernd Bruegman (AEI/PSU) Wolfgang Tichy

(AEI/PSU) Peter Diener (AEI) Ryoji Takahashi (TAC)

LIGO-G020080-00-Z

Manuela Campanelli, LSC Worshop 3/20/2002

plunge/merger FN

inspiral FL/PN

ring-downCL

time

+10-21-

–10-21-

LazarusLazarus = PNPN + interface + FNFN + interface + CLCL

interface:cross-checking

interface:cross-checking

~ 40 M ~ 100 MIBBH

Manuela Campanelli, LSC Worshop 3/20/2002

Binary black Binary black holes in quasi-holes in quasi-circular orbitscircular orbits

•We need a model and some early robust results: (Flanagan & Hughes, 98)

•A first `early stage’ model: equal mass and non spinning BBH Conformally flat puncture data (Cook 94; Brandt, Brügmann 97)

• Meet PN regime at larger separation L

Assess the validity of initial conditions dynamicallyAssess the validity of initial conditions dynamically

(Baker, Campanelli, Lousto,Takahashi, 02)

Manuela Campanelli, LSC Worshop 3/20/2002

A first glimpse on Plunge A first glimpse on Plunge RadiationRadiation

What are the robust features of the

plunge waveforms?

• 3% total mass

• 12% angular momentum (polar axis)• Merge in less haft orbital time.

• Spectrum peak close to QNR of the final Kerr hole f ~ 300 Hz for 35 M.

• Internal consistency: vary transition time (accuracy 20%)

(Baker, Campanelli, Lousto,Takahashi, 02)

Manuela Campanelli, LSC Worshop 3/20/2002

Circular Circular polarizationpolarizationRe 4 and Im 4 90 deg out of phase

4 = A(t) e i (t)

(Observer along the polar axis)

• Dynamics dominated by rotational motion.

• ID artifact (not circularized) shrinks with increasing L. Not so bad …

(Baker, Campanelli, Lousto, Takahashi, 02)

Manuela Campanelli, LSC Worshop 3/20/2002

• 3PN-E1B-ISCO and QC3/QC4 parameters are very close, but PN not converging …

Comparisons with PNComparisons with PN

(Baker, Campanelli, Lousto, Takahashi 02)

Going byond QC4 …• Longer numerical simulations!

• Comparisons with FN needed!

(work in progress … AEI)

Manuela Campanelli, LSC Worshop 3/20/2002

PN initial dataPN initial data

• Solving the Einstein’s contraints including free PN information.

• Evolve and compare waveforms to explore dependencies on ID !

Quadratic convergence

(Bruegman, Campanelli, Diener, Tichy)

(work in progress … UTB/AEI/PSU)

Manuela Campanelli, LSC Worshop 3/20/2002

(Baker, Campanelli, Lousto) (work in progress … UTB/NASA)

Matching Lazarus to 2.5 PN inspiral waveforms (simple analytic representation with 8 parameters).

Analytic Analytic FittingFitting

• To give estimate on how waveforms depend on these parameters.

Explore the transition to more complicated dynamics of spinning andunequal-mass, black holes.

•To reduce the number of simulations needed by interpolating between analytic fits.

Manuela Campanelli, LSC Worshop 3/20/2002

Black hole mergers: from simulation to detection

numrel

Source modelling(templates, etc)

RR

Data analysis(parameter density, detection strategies

etc)

Astrophysics(parameter ranges, etc)

• What is the number of templates needed vs those that can be realistically generated?• What data analysis tecnique we use, given a certain a priori knowledge about the signal?

The Kudu Project: A proposal to use Lazarus waveforms for a first small step in the interface between source modeling and data analysis. (a) Determine robust features of the waveforms. (b) Explore parameter space dependencies of the waveforms. (c) Design optimal detection strategies.

How waveformdepend on

astrophysicalparameters ?

There is no one way street!

Manuela Campanelli, LSC Worshop 3/20/2002