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FOR WHOM THE BLACK HOLE TOLLS: FROM RINGDOWN TO TESTS OF GENERAL RELATIVITY
�1FOR WHOM THE BLACK HOLE TOLLS: FROM RINGDOWN TO TESTS OF GENERAL RELATIVITY
Gregorio Carullo 104° Congresso Nazionale
Società Italiana di Fisica
Credits to: Buonanno, Ossokine
Gregorio Carullo
▸ Introduction
▸ Quasi-normal modes of a black hole
▸ GW150914: the day we saw a black hole ringing
▸ Recent developments
▸ Tests of General Relativity with second-generation detectors
▸ Conclusions
OUTLINE OF THE PRESENTATION
Gregorio Carullo
▸ Coalescences of binary black holes emit gravitational waves detectable on earth
BINARY BLACK HOLES COALESCENCES
GW170814: A Three-Detector Observation of Gravitational Waves from a Binary Black Hole Coalescence, LVC collaboration, PRL 119, 141101 (2017)
Gregorio Carullo
▸ Coalescences of binary black holes emit gravitational waves detectable on earth
▸ Three main phases of the coalescence:
BINARY BLACK HOLES COALESCENCES
Observation of Gravitational Waves from a Binary Black Hole Merger, LVC collaboration, PRL 116, 061102 (2016)
Gregorio Carullo
▸ Coalescences of binary black holes emit gravitational waves detectable on earth
▸ Three main phases of the coalescence:
▸ Inspiral: Post-Newtonian theory
BINARY BLACK HOLES COALESCENCES
Observation of Gravitational Waves from a Binary Black Hole Merger, LVC collaboration, PRL 116, 061102 (2016)
Gregorio Carullo
▸ Coalescences of binary black holes emit gravitational waves detectable on earth
▸ Three main phases of the coalescence:
▸ Inspiral: Post-Newtonian theory
▸ Plunge-merger: numerical simulations
BINARY BLACK HOLES COALESCENCES
Observation of Gravitational Waves from a Binary Black Hole Merger, LVC collaboration, PRL 116, 061102 (2016)
Gregorio Carullo
▸ Coalescences of binary black holes emit gravitational waves detectable on earth
▸ Three main phases of the coalescence:
▸ Inspiral: Post-Newtonian theory
▸ Plunge-merger: numerical simulations
▸ Ringdown: perturbation theory andnumerical simulations
BINARY BLACK HOLES COALESCENCES
Observation of Gravitational Waves from a Binary Black Hole Merger, LVC collaboration, PRL 116, 061102 (2016)
Gregorio Carullo
▸ Space-time is a geometrical dynamical entity
WHAT IS RINGDOWN?
Gregorio Carullo
▸ Space-time is a geometrical dynamical entity
▸ Space-time itself can undergo oscillations even when no matter is present
WHAT IS RINGDOWN?
Gregorio Carullo
▸ Space-time is a geometrical dynamical entity
▸ Space-time itself can undergo oscillations even when no matter is present
▸ The ringdown phase corresponds to the emission of the normal modes of the remnant black hole, damped by the presence of an horizon
WHAT IS RINGDOWN?
Vishveshwara, Nature 227, 936 (1970)
Gregorio Carullo
▸ Space-time is a geometrical dynamical entity
▸ Space-time itself can undergo oscillations even when no matter is present
▸ The ringdown phase corresponds to the emission of the normal modes of the remnant black hole, damped by the presence of an horizon
▸ Intrinsically dissipative system, unlike external damping of normal modes in classical systems
WHAT IS RINGDOWN?
Gregorio Carullo
▸ Space-time is a geometrical dynamical entity
▸ Space-time itself can undergo oscillations even when no matter is present
▸ The ringdown phase corresponds to the emission of the normal modes of the remnant black hole, damped by the presence of an horizon
▸ Intrinsically dissipative system, unlike external damping of normal modes in classical systems
▸ Analytical solution of the linearized Einstein equations on a Black Hole background
WHAT IS RINGDOWN?
Regge, Wheeler, Phys. Rev. 108, 1063 (1957)
Zerilli, Phys. Rev. Lett. 24, 737 (1970)
Gregorio Carullo
RINGDOWN: QUASI-NORMAL MODES SOLUTIONS
▸ In terms of gravitational wave multipoles:
Nollert, Characteristic Oscillations of Black Holes and Neutron Stars (CQG, 2000)
Gregorio Carullo
RINGDOWN: QUASI-NORMAL MODES SOLUTIONS
▸ In terms of gravitational wave multipoles:
▸ Frequencies and damping times spectrum predicted by perturbation theory, fixed only by mass and spin of the black hole
Nollert, Characteristic Oscillations of Black Holes and Neutron Stars (CQG, 2000)
Gregorio Carullo
RINGDOWN: QUASI-NORMAL MODES SOLUTIONS
▸ In terms of gravitational wave multipoles:
▸ Frequencies and damping times spectrum predicted by perturbation theory, fixed only by mass and spin of the black hole
▸ Amplitudes and relative phases predicted by numerical relativity
Nollert, Characteristic Oscillations of Black Holes and Neutron Stars (CQG, 2000)
Gregorio Carullo
RINGDOWN: QUASI-NORMAL MODES SOLUTIONS
▸ In terms of gravitational wave multipoles:
▸ Frequencies and damping times spectrum predicted by perturbation theory, fixed only by mass and spin of the black hole
▸ Amplitudes and relative phases predicted by numerical relativity
▸ Notion of linear regime (hence beginning of ringdown) ambiguous
Nollert, Characteristic Oscillations of Black Holes and Neutron Stars (CQG, 2000)
Gregorio Carullo
MOTIVATIONS OF THE ANALYSIS
▸ Ringdown will be much louder in the near future
Observation of Gravitational Waves from a Binary Black Hole Merger, LVC collaboration, PRL 116, 061102 (2016)
Gregorio Carullo
MOTIVATIONS OF THE ANALYSIS
▸ Ringdown will be much louder in the near future
▸ Standard LIGO-Virgo analyses infer the initial physical parameters of the binary
Observation of Gravitational Waves from a Binary Black Hole Merger, LVC collaboration, PRL 116, 061102 (2016)
Gregorio Carullo
MOTIVATIONS OF THE ANALYSIS
▸ Ringdown will be much louder in the near future
▸ Standard LIGO-Virgo analyses infer the initial physical parameters of the binary
▸ Final parameters are then fixed from the predictions of GR given the initial sampled parameters (masses and spins)
Observation of Gravitational Waves from a Binary Black Hole Merger, LVC collaboration, PRL 116, 061102 (2016)
Gregorio Carullo
MOTIVATIONS OF THE ANALYSIS
▸ Ringdown will be much louder in the near future
▸ Standard LIGO-Virgo analyses infer the initial physical parameters of the binary
▸ Final parameters are then fixed from the predictions of GR given the initial sampled parameters (masses and spins)
▸ We aim at an independent sampling of the parameters of the final black hole, enabling a consistency test of GR predictions
Observation of Gravitational Waves from a Binary Black Hole Merger, LVC collaboration, PRL 116, 061102 (2016)
Gregorio Carullo
GW150914: THE DAY WE SAW A BLACK HOLE RINGING
▸ First and only ringdown observation: GW150914
▸ Different start times yields different results
▸ Results completely consistent with General Relativity if start time is large enough
▸ Unmodelled analysis, not exploited all the available theoretical information
▸
Tests of General Relativity with GW150914, LVC collaboration, Phys. Rev. Lett. 116, 221101 (2016)
Gregorio Carullo
GW150914: THE DAY WE SAW A BLACK HOLE RINGING
▸ First and only ringdown observation: GW150914
▸ Different start times yields different results
▸ Results completely consistent with General Relativity if start time is large enough
▸ Unmodelled analysis, not exploited all the available theoretical information
▸
Tests of General Relativity with GW150914, LVC collaboration, Phys. Rev. Lett. 116, 221101 (2016)
Gregorio Carullo
GW150914: THE DAY WE SAW A BLACK HOLE RINGING
▸ First and only ringdown observation: GW150914
▸ Different start times yields different results
▸ Results completely consistent with General Relativity if start time is large enough
▸ Unmodelled analysis, not exploited all the available theoretical information
▸
Tests of General Relativity with GW150914, LVC collaboration, Phys. Rev. Lett. 116, 221101 (2016)
Gregorio Carullo
GW150914: THE DAY WE SAW A BLACK HOLE RINGING
▸ First and only ringdown observation: GW150914
▸ Different start times yields different results
▸ Results completely consistent with General Relativity if start time is large enough
▸ Unmodelled analysis, not exploited all the available theoretical information
▸
Tests of General Relativity with GW150914, LVC collaboration, Phys. Rev. Lett. 116, 221101 (2016)
Gregorio Carullo
GW150914 REVISITED
Carullo, Del Pozzo, Veitch (In preparation)
▸ Use Kerr model to provide a measurement of final mass and final spin from ringdown only
Gregorio Carullo
GW150914 REVISITED
Carullo, Del Pozzo, Veitch (In preparation)
▸ Use an unmodelled template to compute the evidence that ringdown contains a given GR frequency
Gregorio Carullo
GW150914 REVISITED
Carullo, Del Pozzo, Veitch (In preparation)
▸ Use an unmodelled template to compute the evidence that ringdown contains a given GR frequency
▸ BH spectroscopy is already here!
▸ Dreyer et al., CQG (2004) Berti, Cardoso, Will, PRD (2006)
Gregorio Carullo
RECENT DEVELOPMENTS
▸ Numerically calibrated theoretical model London et al., PRD 2014
▸ Dynamically adaptive method to isolate the linear regime
▸ New statistic keeping into account both statistical and systematic uncertainties
▸ Indipendent numerical techniques confirm our results (Bhagwat et al. PRD 2018)
Gregorio Carullo
RECENT DEVELOPMENTS
▸ Numerically calibrated theoretical model London et al., PRD 2014
▸ Dynamically adaptive method to isolate the linear regime
▸ New statistic keeping into account both statistical and systematic uncertainties
▸ Indipendent numerical techniques confirm our results (Bhagwat et al. PRD 2018)
60
70
80
Mf
(M�)
24.7 24.6 24.0 22.2 19.9 17.2 16.1 15.6 15.3 13.8 12.0SNR
0.6
0.8
a f
Simulated value
10 11 12 13 14 15 16 17 18 19 20
(tstart � tpeak)/M
0.5
1.0
B[]
Carullo et al., Phys. Rev. D 98, 104020 (2018)
Gregorio Carullo
RECENT DEVELOPMENTS
▸ Numerically calibrated theoretical model London et al., PRD 2014
▸ Dynamically adaptive method to isolate the linear regime
▸ New statistic keeping into account both statistical and systematic uncertainties
▸ Indipendent numerical techniques confirm our results (Bhagwat et al. PRD 2018)
60
70
80
Mf
(M�)
24.7 24.6 24.0 22.2 19.9 17.2 16.1 15.6 15.3 13.8 12.0SNR
0.6
0.8
a f
Simulated value
10 11 12 13 14 15 16 17 18 19 20
(tstart � tpeak)/M
0.5
1.0
B[]
Carullo et al., Phys. Rev. D 98, 104020 (2018)
Gregorio Carullo
RECENT DEVELOPMENTS
▸ Numerically calibrated theoretical model London et al., PRD 2014
▸ Dynamically adaptive method to isolate the linear regime
▸ New statistic keeping into account both statistical and systematic uncertainties
▸ Independent numerical techniques confirm our results Bhagwat et al. PRD 2018
60
70
80
Mf
(M�)
24.7 24.6 24.0 22.2 19.9 17.2 16.1 15.6 15.3 13.8 12.0SNR
0.6
0.8
a f
Simulated value
10 11 12 13 14 15 16 17 18 19 20
(tstart � tpeak)/M
0.5
1.0
B[]
Carullo et al., Phys. Rev. D 98, 104020 (2018)
Gregorio Carullo
PARAMETRIZED DEVIATIONS FROM GR: RESULTS
▸ Meidam et al. (2014):
▸ Detector: Einstein Telescope
▸ Accuracy: 6% (5 events) Gossan, Veitch, Sathyaprakash PRD 85, 124056 (2012)
Gregorio Carullo
PARAMETRIZED DEVIATIONS FROM GR: RESULTS
1 2 3 4 5 6Nevents
�0.15
�0.10
�0.05
0.00
0.05
0.10
0.15
�!̂22
0
probability density
▸ Meidam et al. (2014):
▸ Detector: Einstein Telescope
▸ Accuracy: 6% (5 events)
▸ Carullo et al. (2018):
▸ Detector: LIGO-Virgo network (design)
▸ Accuracy: 1.5% (5 events)
Agrees with Brito, Buonanno, Raymond Phys. Rev. D 98, 084038 (2018)
Gregorio Carullo
CONCLUSIONS
▸ Determined the effective start time of the ringdown
Gregorio Carullo
CONCLUSIONS
▸ Determined the effective start time of the ringdown
▸ Developed a pipeline able to perform an independent measure of the final regime of a binary black hole coalescence with current network of interferometers
Gregorio Carullo
CONCLUSIONS
▸ Determined the effective start time of the ringdown
▸ Developed a pipeline able to perform an independent measure of the final regime of a binary black hole coalescence with current network of interferometers
▸ Performed agnostic mode identification
Gregorio Carullo
CONCLUSIONS
▸ Determined the effective start time of the ringdown
▸ Developed a pipeline able to perform an independent measure of the final regime of a binary black hole coalescence with current network of interferometers
▸ Performed agnostic mode identification
▸ Measure deviations from GR predictions already with the LIGO-Virgo network
Gregorio Carullo
CONCLUSIONS
▸ Determined the effective start time of the ringdown
▸ Developed a pipeline able to perform an independent measure of the final regime of a binary black hole coalescence with current network of interferometers
▸ Performed agnostic mode identification
▸ Measure deviations from GR predictions already with the LIGO-Virgo network
▸ From multiple observations, constrain deviations from GR with a precision of 1.5%, already from a small (~5) number of sources
Gregorio Carullo
WHY DO WE NEED THIS
▸ Test Hawking’s Area Theorem (Cabero et al., PRD 97, 124069 (2018))
Gregorio Carullo
WHY DO WE NEED THIS
▸ Test Hawking’s Area Theorem (Cabero et al., PRD 97, 124069 (2018))
▸ Test of the Black Hole Uniqueness Theorems
Gregorio Carullo
WHY DO WE NEED THIS
▸ Test Hawking’s Area Theorem (Cabero et al., PRD 97, 124069 (2018))
▸ Test of the Black Hole Uniqueness Theorems
▸ Test energy and angular momentum conservation during strong-field gravitational processes (Ghosh et al., CQG (2017))
Gregorio Carullo
WHY DO WE NEED THIS
▸ Test Hawking’s Area Theorem (Cabero et al., PRD 97, 124069 (2018))
▸ Test of the Black Hole Uniqueness Theorems
▸ Test energy and angular momentum conservation during strong-field gravitational processes (Ghosh et al., CQG (2017))
▸ Extract implication on Black Hole astrophysics from final mass and spin measurements
Gregorio Carullo
WHY DO WE NEED THIS
▸ Test Hawking’s Area Theorem (Cabero et al., PRD 97, 124069 (2018))
▸ Test of the Black Hole Uniqueness Theorems
▸ Test energy and angular momentum conservation during strong-field gravitational processes (Ghosh et al., CQG (2017))
▸ Extract implication on Black Hole astrophysics from final mass and spin measurements
▸ Test the presence of alternative compact objects (spacetime signature)
Gregorio Carullo
WHY DO WE NEED THIS
▸ Test Hawking’s Area Theorem (Cabero et al., PRD 97, 124069 (2018))
▸ Test of the Black Hole Uniqueness Theorems
▸ Test energy and angular momentum conservation during strong-field gravitational processes (Ghosh et al., CQG (2017))
▸ Extract implication on Black Hole astrophysics from final mass and spin measurements
▸ Test the presence of alternative compact objects (spacetime signature)
▸ Constrain the graviton mass (Chung, Li (2018))
GRAZIE PER L’ATTENZIONE