Binary Compact Objects and their Powerful ... - Northwestern

Gravitational Wavesspacetime deformationsare communicatedthrough gravitationalwaves:Mass curves spacetimeand affects distances betweenreference pointstransverse wavespropagatingat the speed of light

Gravitational RadiationSource:moment tensor I jk :Time-dependent mass quadrupoleAmplitude:

The Effect of Gravitational Waves

The Effect of Gravitational Wavestranserve-wave oscillatory disturbances ofreference (undisturbed) spacetimequadrupole nature: 2 polarizations at 45 degree angle

The Effect of Gravitational Wavestranserve-wave oscillatory disturbances ofreference (undisturbed) spacetimequadrupole nature: 2 polarizations at 45 degree angle

The Effect of Gravitational Wavesvery weak:ideally: highly compact, fast moving, nearby objects

The Effect of Gravitational Wavesvery weak:ideally: highly compact, fast moving, nearby objectsdirect detection goal:measure relative distance changes

The Effect of Gravitational Wavesvery weak:ideally: highly compact, fast moving, nearby objectsdirect detection goal:measure relative distance changesBlack Hole of 10 solar masses moving at the speed of lightlocated at the Galactic center: h ~ 10 -17at the nearest major cluster of galaxies: h ~ 10 -20

The Effect of Gravitational Wavesvery weak:ideally: highly compact, fast moving, nearby objectsdirect detection goal:measure relative distance changesBlack Hole of 10 solar masses moving at the speed of lightlocated at the Galactic center: h ~ 10 -17at the nearest major cluster of galaxies: h ~ 10 -20challenging, but we know gravitational wavesare real ...

Do Gravitational Waves Really Exist?Hulse-Taylor Binary Pulsar: The first relativistic binary pulsar

Do Gravitational Waves Really Exist?Hulse-Taylor Binary Pulsar: The first relativistic binary pulsarA binary system with two neutron stars,one or two of which emit radio pulses:

Do Gravitational Waves Really Exist?Hulse-Taylor Binary Pulsar: The first relativistic binary pulsarA binary system with two neutron stars,one or two of which emit radio pulses:Rate of orbital decay consistent withgravitational wave losses within 0.3% !Orbital Decay RateWeisberg & Taylor 2003Year

Do Gravitational Waves Really Exist?Hulse-Taylor Binary Pulsar: The first relativistic binary pulsarA binary system with two neutron stars,one or two of which emit radio pulses:Rate of orbital decay consistent withgravitational wave losses within 0.3% !Orbital Decay RateWeisberg & Taylor 2003Year4 more relativistic NS-NS have been discovered,one of them is a double pulsar, the most relativistic NS-NS so far!GR tested and confirmed at < 0.05 % (Burgay et al, Lyne et al, Kramer et al)

How about direct detection?LIGOGEOVirgoTAMAAIGO

How about direct detection?Coincidence:detection confidencesource localizationLIGOGEOVirgoTAMAAIGO

How about direct detection?Laser Interferometry

LIGO sensitivity

LIGO sensitivity

LIGO sensitivity

LIGO sensitivity

Studies of Binary Compact ObjectsSome questions of interest ...How do they form ?What are the expected ratesfor LIGO detections ?How do you detect & decode such weak signals?

Compact Binary Inspiral: Event RatesTwo main paths for rate estimation

Compact Binary Inspiral: Event RatesTwo main paths for rate estimationEmpiricalfrom the knownGalactic binary pulsarsonly for NS-NSinspirals

Compact Binary Inspiral: Event RatesTwo main paths for rate estimationEmpiricalfrom the knownGalactic binary pulsarsonly for NS-NSinspiralsTheoreticalfrom our understandingof binary star evolutionfor NS-NSNS-BH & BH-BHinspirals

Compact Binary Inspiral: Event RatesEmpirical Rate EstimatesVK et al 2001, 2004Kim et al 2003, 2008Burgay et al 2003large statistical uncertainty:factor of ~50 at 99% C.I.PDF has a clear peak with tailfactor of ~5 at 68% C.Isystematic uncertainty:factor of ~20

Compact Binary Inspiral: Event RatesEmpirical Rate EstimatesVK et al 2001, 2004Kim et al 2003, 2008Burgay et al 2003large statistical uncertainty:factor of ~50 at 99% C.I.PDF has a clear peak with tailfactor of ~5 at 68% C.Isystematic uncertainty:factor of ~20

Compact Binary Inspiral Rates:What about Black Hole Binaries?

Compact Binary Inspiral Rates:What about Black Hole Binaries?No BH-NS or BH-BH known from E&M observationsSo far, inspiral rate predictionsonly from population calculationswith uncertainties of ~ 3 orders of mag

Compact Binary Inspiral Rates:What about Black Hole Binaries?No BH-NS or BH-BH known from E&M observationsSo far, inspiral rate predictionsonly from population calculationswith uncertainties of ~ 3 orders of magWe can use NS-NS empirical rates as constraintson population synthesis modelsO’Shaughnessy et al 2005, 2007, 2008

Compact Binary Inspiral Rates:Empirical Constraints onPopulation Model PredictionsO’Shaughnessy et al 2005, 2007, 2008Select models that satisfy empirical constraintsObtain rate predictions for BH binaries

Compact Binary Inspiral Rates:Current PredictionsLSC - CBC Rates Document 2008

Compact Binary Inspiral Rates:Current Predictions@ peak probabilityLSC - CBC Rates Document 2008

Compact Binary Inspiral Rates:Current Predictions@ peak probabilitywithrealisticoptimismLSC - CBC Rates Document 2008

Compact Binary Inspiral Rates:Current Predictions@ peak probabilitywithrealisticoptimismLSC - CBC Rates Document 2008

Compact Binary Inspiral Rates:Current Predictions@ peak probabilitywithrealisticoptimismLSC - CBC Rates Document 2008

Compact Binary Inspiral Rates:Current Predictions@ peak probabilitywithrealisticoptimismLSC - CBC Rates Document 2008

Compact Binary Inspiral Rates:Current PredictionsWhat is the probability that one or more inspiralswill be detected by enhanced LIGO?

ProbabilityCompact Binary Inspiral Rates:Current PredictionsWhat is the probability that one or more inspiralswill be detected by enhanced LIGO?O’Shaughnessy et al 2009

Going Beyond GW Detection ...Gravitational Wave Astronomy

Going Beyond GW Detection ...Gravitational Wave AstronomyThe challenge of GW detectionis clear and formidable ...

Going Beyond GW Detection ...Gravitational Wave AstronomyThe challenge of GW detectionis clear and formidable ...... but progress in astrophysics needs- (accurate) measurements of the physical propertiesof GW sources- systematic studies of source samples

Going Beyond GW Detection ...Gravitational Wave AstronomyThe challenge of GW detectionis clear and formidable ...... but progress in astrophysics needs- (accurate) measurements of the physical propertiesof GW sources- systematic studies of source samplesGiven how weak and rareGW sources arethe challenge of physicalparameter estimationis not to be ignored ...S/N ~ 17

Gravitational Wave Astronomy:Physical Parameter Estimation

Gravitational Wave Astronomy:Physical Parameter EstimationThe case ofNS-BH inspiralwith spinning BH:12 parameters!

Gravitational Wave Astronomy:Physical Parameter Estimationnon-spinning chirpThe case ofNS-BH inspiralwith spinning BH:12 parameters!

Gravitational Wave Astronomy:Physical Parameter EstimationExample MCMC run ( van der Sluys et al. 2008 )signal injected:MCMC:Sampling theposterior PDF of the“chirp mass”~3 days on a single 2.8GHz CPUaccuracy of 0.5%

Gravitational Wave Astronomy:Physical Parameter EstimationExample MCMC run ( van der Sluys et al. 2008 )signal injected:MCMC:Sampling theposterior PDF of the“chirp mass”~3 days on a single 2.8GHz CPUaccuracy of 0.5%

Gravitational Wave Astronomy:Physical Parameter EstimationMajor difficulties:large number of parameters (12 -15)relatively low S/N (~10)strong correlations among parametersvan der Sluys et al. 2008, Raymond et al 2009

Gravitational Wave Astronomy:Physical Parameter EstimationMajor difficulties:large number of parameters (12 -15)relatively low S/N (~10)strong correlations among parametersvan der Sluys et al. 2008, Raymond et al 2009

Gravitational Wave Astronomy:Physical Parameter EstimationMajor difficulties:large number of parameters (12 -15)relatively low S/N (~10)strong correlations among parametersvan der Sluys et al. 2008, Raymond et al 2009

Binary Compact ObjectsPowering Gamma Ray Bursts ?

Binary Compact ObjectsPowering Gamma Ray Bursts ?Some of the basics ...Most luminous E&Msince the Big Bang:Gamma-ray flashesof 0.1 - 100 secshort (2sec)

Binary Compact ObjectsPowering Gamma Ray Bursts ?Some of the basics ...Most luminous E&Msince the Big Bang:Gamma-ray flashesof 0.1 - 100 secCoordinated E&M observations(X-ray, optical, infrared, radio)reveal clues about progenitorsshort (2sec)

Binary Compact ObjectsPowering Gamma Ray Bursts ?Some of the basics ...Most luminous E&Msince the Big Bang:Gamma-ray flashesof 0.1 - 100 secshort (2sec)

Binary Compact ObjectsPowering Gamma Ray Bursts ?Some of the basics ...Most luminous E&Msince the Big Bang:Gamma-ray flashesof 0.1 - 100 secshort (2sec)central BHaccretingfrom gas toruswith jets

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitors

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsLong GRB

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsLong GRBalways found in galaxieswith very active star formationand young stellar populations

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsLong GRBalways found in galaxieswith very active star formationand young stellar populationsmost often associatedwith optical supernovasignals

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsLong GRBalways found in galaxieswith very active star formationand young stellar populationsmost often associatedwith optical supernovasignalscore collapse ofyoung, massive stars

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsinitiallyLong GRBShort GRBalways found in galaxieswith very active star formationand young stellar populationsmost often associatedwith optical supernovasignalscore collapse ofyoung, massive stars

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsLong GRBalways found in galaxieswith very active star formationand young stellar populationsShort GRBinitiallyTwo found in ellipticals,no star formation,old stellar populationsmost often associatedwith optical supernovasignalscore collapse ofyoung, massive stars

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsLong GRBalways found in galaxieswith very active star formationand young stellar populationsmost often associatedwith optical supernovasignalsShort GRBinitiallyTwo found in ellipticals,no star formation,old stellar populationsno supernovaassociationscore collapse ofyoung, massive stars

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsLong GRBalways found in galaxieswith very active star formationand young stellar populationsmost often associatedwith optical supernovasignalscore collapse ofyoung, massive starsShort GRBinitiallyTwo found in ellipticals,no star formation,old stellar populationsno supernovaassociationsNS-NS and/or BH-NS mergerswith long delay times betweenstar formation and merger

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsinitiallyLong GRBcore collapse ofyoung, massive starsShort GRBNS-NS and/or BH-NS mergerswith long delay times betweenstar formation and merger

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsinitiallyLong GRBcore collapse ofyoung, massive starshigh average redshift (~3):Short GRBNS-NS and/or BH-NS mergerswith long delay times betweenstar formation and merger@ large distances, early timeswhen star formation was highconsistent with short delaysand short lifetimesof very massive stars (~Myr)

Binary Compact ObjectsPowering Gamma Ray Bursts ?Identification of GRB host galaxies is crucialfor revealing their nature and progenitorsinitiallyLong GRBcore collapse ofyoung, massive starshigh average redshift (~3):@ large distances, early timeswhen star formation was highconsistent with short delaysand short lifetimesof very massive stars (~Myr)Short GRBNS-NS and/or BH-NS mergerswith long delay times betweenstar formation and mergerlow average redshift (~0.3):@ small distances, current timesconsistent with long delays(~5Gyr)

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?initiallyShort GRBNS-NS and/or BH-NS mergerswith long delay times betweenstar formation and mergerlow average redshift (~0.3):@ small distances, current timesconsistent with long delays(~5Gyr)

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?initiallyShort GRB But our theoretical models predicteddelay times: 10Myr - 10GyrNS-NS and/or BH-NS mergerswith long delay times betweenstar formation and mergerlow average redshift (~0.3):@ small distances, current timesconsistent with long delays(~5Gyr)Belczynski et al. 2001,2002a,bBelczynski et al. 2006

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?Present Status:(Berger 2009, Nakar 2007, Berger et al 2007, 2008,Ofek et al 2008)

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?Present Status:(Berger 2009, Nakar 2007, Berger et al 2007, 2008,Ofek et al 2008)`the majority of short GRBs appear to occur instar forming galaxies’ (at a 5:1 ratio)

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?Present Status:(Berger 2009, Nakar 2007, Berger et al 2007, 2008,Ofek et al 2008)`the majority of short GRBs appear to occur instar forming galaxies’ (at a 5:1 ratio)L ~ 0.1 - 1.5 L*SFR ~ 0.2 - 6 Msun per yrZ ~ 0.6 - 1.6 solar

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?Present Status:(Berger 2009, Nakar 2007, Berger et al 2007, 2008,Ofek et al 2008)`the majority of short GRBs appear to occur instar forming galaxies’ (at a 5:1 ratio)L ~ 0.1 - 1.5 L*SFR ~ 0.2 - 6 Msun per yrZ ~ 0.6 - 1.6 solarsample indicates that 1/3 of short GRBsare at redshifts > 1

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?Present Status:(Berger 2009, Nakar 2007, Berger et al 2007, 2008,Ofek et al 2008)`the majority of short GRBs appear to occur instar forming galaxies’ (at a 5:1 ratio)L ~ 0.1 - 1.5 L*SFR ~ 0.2 - 6 Msun per yrZ ~ 0.6 - 1.6 solarsample indicates that 1/3 of short GRBsare at redshifts > 1A wide range of ages is favored, from~10-100Myr to 10 Gyr

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?Population models for star formation in bothspirals and ellipticals with all available constraints:binary pulsar rates & GRB redshift distributionO’Shaughnessy et al 2008UNconstrainedconstrainedCumulative redshift distribution

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?Population models for star formation in bothspirals and ellipticals with all available constraints:binary pulsar rates & GRB redshift distributionO’Shaughnessy et al 2008UNconstrainedconstraineda small numberof models survivesif all short GRBare NS-NS mergersCumulative redshift distribution

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?Combining all available constraints on population models:binary pulsar rates & GRB redshift distributionO’Shaughnessy et al 2008UNconstrainedmore models surviveif all short GRBare NS-BH mergersconstrainedCumulative redshift distribution

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?Combining all available constraints on population models:binary pulsar rates & GRB redshift distributionO’Shaughnessy et al 2008UNconstrainedmore models surviveif all short GRBare NS-BH mergersconstrainedBUT requiressignificantly highbirth spin for BHCumulative redshift distributionBelczynski et al 2008

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?NS-NS or BH-NS?UNconstrainedFraction of spiral,star-forming hostsBH-NSNS-NSConstrainedO’Shaughnessy et al 2008, 2009

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?

Binary Compact ObjectsPowering Short Gamma Ray Bursts ?Based on lots of consistent clues, yes ...but conclusive proof can only come frommulti-messenger astronomycoincident E&M and GW observations:gamma-ray burst and inspiral signal in gravitational waves!mass (and spin) measurements from LIGO/Virgocould also answer the questionNS-NS vs. NS-BH or both ?

Multi-Messenger Astronomy:the beginnings ...

Multi-Messenger Astronomy:the beginnings ...LIGO observations restrict GRB 070201 origin:

Multi-Messenger Astronomy:the beginnings ...LIGO observations restrict GRB 070201 origin:Binary Merger in M31 excludedat > 99% probabilityThe LIGO Scientific Collaboration & Hurley 2008, ApJ

NS and BH compact binaries:GW chirpsinspiral chirpf GW = 2xf orbGW emission causes orbitalshrinkage leading to higherGW frequency & amplitude

NS and BH compact binaries:GW chirpsinspiral chirpf GW = 2xf orbGW emission causes orbitalshrinkage leading to higherGW frequency & amplitude

GW Sources: High Frequency

Binary Compact Objects: Formationfrom Tauris & van den Heuvel 2003

Binary Compact Objects: FormationMassive primordial binaryMass-transfer #1: hydrostatically andthermally Stable,but Non-Conservative: mass and A.M. lossSupernova and NS Formation #1:Mass Loss and Natal KickHigh-mass X-ray Binary: NS Accretionfrom Massive Companion’s Stellar WindMass-transfer #3: Dynamically UnstableMass-tranfer #4: Possible and StableSupernova and NS Formation #2:Mass Loss and Natal KickDouble Neutron-Star Formed!from Tauris & van den Heuvel 2003

Binary Compact Objects: FormationQ: What is the origin of NS and BH ?

Binary Compact Objects: FormationQ: What is the origin of NS and BH ?A: Use properties of observed systemsand derive physical constraints onNS, BH progenitors and stellar collapseDouble PulsarWillems et al. 2006, PRD