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Bayesian analysis for Pulsar Timing Arrays. Rutger van Haasteren (Leiden) Yuri Levin (Leiden) Pat McDonald (CITA) Ting-Ting Lu (Toronto). Pulsar Timing Array. GW timing residuals: Multidimentional Gaussian process; - PowerPoint PPT Presentation
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Bayesian analysis for Pulsar Timing Arrays
Rutger van Haasteren (Leiden)Yuri Levin (Leiden)Pat McDonald (CITA)Ting-Ting Lu (Toronto)
Pulsar Timing Array
• GW timing residuals:
Multidimentional Gaussian process;
coherence matrix
C (A, n)=G(t –t ) Qai bj
Jenet et al 04Hill & Benders 1981
amplitudeslope
Phinney 01Jaffe & Backer 03Wyithe & Loeb 03
j i ab
GWBspectrum
geometry
Pulsar Timing Array
C= C (A, n)+noise +noise +…+noiseai bj
Real coherence matrix:
1 2 20
Bayesian solution:
• parametrize each pulsar noise reasonably: N exp[-n f]+σ• construct multidimantional probability distribution
• marginalize over quadradic spindowns – analytical• marginalize over pulsar noises – numerical
P(A,n, N ,n | data)=exp[-X (2C) X - (1/2) log(det{C})] (Prior/Norm) x x-1
where X=(timing residuals) – (quadratic spidown)
a
a
a
a
ai
Markov Chain Monte-Carlo
• Direct integration unrealistic• Markoff chain cleverly explores parameter
space, dwelling in high-probability regions• Typically need few 10000 points for reliable
convergence• Can do white pulsar noises-last year’s talk
• However, problems with chain convergence when one allows for colored
pulsar noises. Need something different!
Maximum-likelihood method
• Find global maximum of log[P(A, n, N )]• Run a chain in the neighbourhood until enough points to fit a quadratic form:
log(P)=log(P ) – (p –p ) Q (p – p ) • Approximate P as a Gaussian and
marginalize over pulsar noises
a
0 i i i j j j
0 0
Results
10 pulsars 500 ns, 70 timings each over 9 yr
Results
10 pulsars 500 ns, 70 timings each over 9 yr
Results
10 pulsars 100 ns, 70 timings each over 9 yr
Results
10 pulsars 100 ns, 70 timings each over 9 yr
Results
10 pulsars, 50 ns timing error, 5 years, every 2.5 weeksA=10 E-15 n=-7/3
our algorithm:
• Does not rely on estimators – explores the
full multi-dimensional likelihood function• Measures simultaneously amplitude AND
slope of the gravitational-wave background• Deals easily with unevenly sampled data,
variable number of tracked pulsars, etc.• Deals easily with systematics-quadratic spindowns,
zero resets, pointing errors, and human errors of known functional form.
Example problem: finding the white noise amplitude b
Pulsar observer:
b =(b + … +b )/N2 2 2
1 N
Error = b/N0.5
Example problem: finding the white noise amplitude b
Bayesian Theorist:
P(data|b)=exp[(b + … +b )/2b -.5 log(b)]2 21 N
2
P(b|data)=(1/K) P(data|b) P (b)0
Example problem: finding the white noise amplitude b
Bayesian Theorist:
P(data|b)=exp[(b + … +b )/2b -.5 log(b)]2 21 N
2
P(b|data)=(1/K) P(data|b) P (b)0
normalizationprior
Example problem: finding the white noise amplitude b
Bayesian Theorist:
b
P
Complication: white noise + jump a
Complication: white noise + jump a
Complication: white noise + jump a
Pulsar observer: fit for a
Lazy Bayesian Theorist:
1. Find P(a,b|data)
2. Integrate over a
Complication: white noise + jump a
Pulsar observer: fit for a
Lazy Bayesian Theorist:
1. Find P(a,b|data)
2. Integrate over a
ANALYTICAL!
Complication: white noise + jump a
Pulsar observer: fit for a
Lazy Bayesian Theorist:
1. Find P(a,b|data)
2. Integrate over a
3. Get expression P(b|data), insensitive to jumps!
Jump removal:
Does not have to be jumps. ANYTHING of knownfunctional form, i.e.:
•Quadratic/cubic pulsar spindowns•Annual variations•Periodicity due to Jupiter•Zero resets•ISM variations, if measured independently
can be removed analytically when writing down P(b).
Don’t care if pre-fit by observers or not.
Pulsar Timing Array
C (A, n)ai bj
Bayesian analysis:
compute P(A,n| data), after
“removing” unwanted components of known functional form
easy
Pulsar Timing Array
C (A, n)ai bj
Bayesian analysis:
compute P(A.n| data), after
“removing” unwanted components of known functional form
Complication 1: low-frequency cut-off
Pulsar Timing Array
C (A, n)ai bj
Bayesian analysis:
compute P(A.n| data), after
“removing” unwanted components of known functional form
Complication 1: low-frequency cut-off
Pulsar Timing Array
C (A, n)ai bj
Bayesian analysis:
compute P(A.n| data), after
“removing” unwanted components of known functional form
Complication 2: pulsar noises, measured concurrentlywith GWs. This is the real difficulty with the BayesianMethod.
Results
Strengths of B. approach• Philosophy
• No loss of info, no need to choose optimal estimator
• No noise whitening, etc. Irregular time intervals, etc.
• Easy removal of unwanted functions
Weaknesses:
• Computational cost
Need better algorithms!
PhD position in Leiden
• Supported by 5-yr VIDI grant
• Collaboration with observers/other theorists essential
• ….