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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

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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

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measuring gravitational wavesmeasuring gravitational waves

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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?

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GW SpectrumGW Spectrum

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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.

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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

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Instrumental and EnvironmentalInstrumental and EnvironmentalCouplingsCouplings

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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

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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

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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

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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%

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Critical Coupling LikelihoodCritical Coupling Likelihoodperformance vs. Cat 4performance vs. Cat 4

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Critical Coupling LikelihoodCritical Coupling LikelihoodROCROC

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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)

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LikelihoodsLikelihoods

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SNR vs relative sky positionSNR vs relative sky position

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Sky locationSky location

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