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Desenvolvimento de Metodologias em Desenvolvimento de Metodologias em Análise de Dados no EstudoAnálise de Dados no Estudo
de Detectores e Fontes de Ondas de Detectores e Fontes de Ondas GravitacionaisGravitacionais
Cesar Costa
Supervisor: Odylio Denys Aguiar
CNPq/MCTI/INPEVIII Workshop PG-AST/DAS
Abril, 2015
z
Histórico
Mestrado e Doutorado em Astrofísica – DAS/INPE
Modelagem matemática do detector de ondas gravitacionais Mario Schenberg
Resposta do detector a fontes astrofísicas
Pós-Doutorado USP (FAPESP)
Implementação do sistema de aquisição de dados
Pós-Doutorado LSU-LIGO (NSF)
Caracterização instrumental e ambiental do LIGO (Data Quality)
Desenvolvimento pipeline para análise de canais auxiliares
Bolsa PQ-DA (INPE-CNPq)
Pós-Doutorado Sênior (INPE-CNPq)
LIGO Detchar
Schenberg
PTA
Onde me encontrar : SALA 41 – CEA I / Ramal 7220
Colaborações:
LSU, UTB, UNESP, UNIFESP, JPL/NASA
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 20153
measuring gravitational wavesmeasuring gravitational waves
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 20154
Gravitational Waves AstronomyGravitational Waves Astronomy
Gravitational wave detectors will study sources characterized by extreme physical conditions: strong non-linear gravity and relativistic motions, very high densities, temperatures and magnetic fields.
Some of the key scientific questions to which answers will be sought:
fundamental physics:• What are the properties of gravitationalwaves?• Is General Relativity still valid understrong-gravity conditions?• Are nature’s black holes the black holes ofGeneral Relativity?• How does matter behave under extremesof density and pressure?
cosmology:- What is the history of the acceleratingexpansion of the Universe?- Were there phase transitions in the earlyUniverse?
Astrophysics:• How abundant are stellar-mass black holes?• What is the mechanism that generatesgamma-ray bursts?• What are the conditions in the dense centralcores of galactic nuclei dominated bymassive black holes?• Where and when do massive black holesform, and what role do they play in theformation of galaxies?• What happens when a massive starcollapses?• How do compact binary stars form andevolve, and what has been their effect onstar formation rates?
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 20155
GW SpectrumGW Spectrum
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 20156
LIGO/VIRGOLIGO/VIRGO
Laser Interferometric Gravitational Wave Observatory (LIGO)
Two detectors (Hanford, WA, and Livingston, LA)
VIRGO (Cascina, Italy – near Pisa)
Michelson Interferometer with 4km long arms (Virgo - 3km) Fabry-Pérot cavity stores ~1kW of “light” Intended to be an inertial referential frame
on Earth.
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 20157
Noise and transientsNoise and transients
Sensitivity curve
Stationary PSD
Well known physics
seismic,residual gas, thermal noise, “shot noise”, etc
Transients (Glitches)
Non-gaussian artifacts
Due to ambient and instrument culprits
Undesired effects on data analysis and sensitivity
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 20158
Instrumental and EnvironmentalInstrumental and EnvironmentalCouplingsCouplings
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 20159
Data QualityData Quality
Compare h(t) (DARM_ERR) to auxiliary channels. Time coincidences point do probable culprits
“Data quality flags” isolate misbehaving times.
h(t)
ChannelX
time
ChannelY
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201510
MotivationMotivation
LIGO White Paper
Signal searchesIntegrate DQ information into search “clean 99% of single detector transients”
InstrumentalIdentify couplings, properties and pathwaysGive better information to instrumentalistsFast identification
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201511
Applying methods to data setsApplying methods to data sets
Collections of transient properties are compared(gpstime, amplitude, snr, frequency band, duration, etc)
Statistical methods must be applied and developed
Y = y1,y
2,...,y
nX = x
1,x
2,...,x
n
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201512
Desempenho
Deadtime: 13.9%
Upper limit
SNR>8 : ~ 85%
Critical Coupling LikelihoodCritical Coupling Likelihood
Livingston CCL > 1
SNR (>) %
5 14.44%
8 84.26%
10 88.83%
20 86.77%
50 92.42%
100 98.00%
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201513
Critical Coupling LikelihoodCritical Coupling Likelihoodperformance vs. Cat 4performance vs. Cat 4
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201514
Critical Coupling LikelihoodCritical Coupling LikelihoodROCROC
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201515
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201516
Bayesian Detection of Alternative Bayesian Detection of Alternative GW Polarizations by using Pulsar Timing ArrayGW Polarizations by using Pulsar Timing Array
ColaborationMárcio Alves (Unesp/SJC)Massimo Tinto (JPL/NASA)
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201517
LikelihoodsLikelihoods
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201518
SNR vs relative sky positionSNR vs relative sky position
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201519
Sky locationSky location
Cesar Costa, VIII Workshop PG-AST/DAS, Abril, 201520