july 13, 2007 robert ward, caltech ligo-g070406-00-z 1 robert ward for the ligo scientific...
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July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 1
Robert Wardfor the
LIGO Scientific Collaboration
Amaldi 7Sydney, Australia
July 2007
A Radiometer for a Stochastic Background of Gravitational
Radiation
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 2
A Stochastic Backgroundof Gravitational Waves
Also see presentations by J. Whelan and B. Whiting
Characterized by gravitational wave spectrum
Approximate by power law in LIGO band
Signals from cosmological sourcesand astrophysical foregrounds
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 3
Isotropic Search:Average over the whole sky
S4 Science Run, H1L1+H2L1:H0 = 72 km/s/Mpc51-150 Hz (includes 99% of inverse variance)Ω0 σΩ = (-0.8 4.3) × 10-590% Bayesian UL: 6.5 × 10-5
Also see presentation by Nick Fotopoulos
Cross Correlation Estimator
Using an Optimal Filter
With a variance
Assuming a Source Strain Spectrum
γ(f) = Overlap Reduction Function
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 4
Stochastic GW Background due to Astrophysical Sources? Not isotropic if dominated by nearby sources Do a Targeted Stochastic Search with LIGO
Source position information from Signal time delay between different sites (sidereal time dependent) Sidereal variation of the single detector acceptance
Time-Shift and Cross-Correlate!
Effectively a Radiometer for Gravitational Waves
GW Radiometer Motivation
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 5
The Radiometer
''')(~
21 ttQtstsdtdtYsiderealt
),(4
)(2
siderealsidereal tt QQT
Detailed description in gr-qc/0510096S. Ballmer
fPfP
ffHfQ sidereal
sidereal
tt
21
)(
H(f) is the source spectrum
Δt
3000km
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 6
LIGO’s Fourth Science Run (S4)
3147%90 /10010)2.112.0( fHzHzH
astro-ph/0703234submitted to PRD
(β=-3 corresponds to scale-invariantprimordial perturbation spectrum)
Hz
ffH
100)(
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 7
Upper Limit map H(f)=const (=0)
148%90 Hz10)1.685.0( H
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 8
But the maps are convolved
Point spread function
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 9
Point Spread Function
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 10
Deconvolving the map to geta Maximum Likelihood
Estimation
Toy CMB map from Planck Simulator
Run through radiometer analysis to get “dirty” map; this convolves with point spread function
To deconvolve, invert the covariance matrix, which is large and varies with time & IFO sensitivity computationally expensive
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 11
Or use a Spherical Harmonic Basis:
Maximum Likelihood Estimation
Advantage of a smaller (tens instead of thousands), block diagonal, covariance matrix→lower computational cost.
Being actively pursued by the stochastic analysis group.
Rotational Symmetrycovariance =0 for m≠m’
different l’s at the same m are correlated
Symmetry broken due to diurnal sensitivity variations
Covariance matrix
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 12
Narrowband RadiometerSco-X1 (brightest LMXB), S4
Consistent with no signal
This is currently the best published limit on the gravitational wave flux coming from the direction of Sco-X1
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 13
Blinded Data from S5
SNR
S5 result should be at least 10x better than S4 result
time shift the detector streams by more than the light travel time between detectors→no true gw signal remains
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 14
Detector Noise Non-stationarity:The Sigma Ratio Data Quality Cut
Don’t include any 60 second segments whose PSD gives a 20% larger sigma than neighboring PSD’s to reduce effects of nonstationarity.
This rejects 1.80% of the data
1st 4 months of S5 (blind)
i = 1 2 3 …
t
60sec
0 0.5 .8 1 1.2 1.5 2 2.5 3 10
0
101
102
103
104
105
sigma ratio
num
ber
of s
egm
ents
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 15
Theoretical Sigma Maps from 2006 (S5, blind)
Nov 2005-Feb 2006 March 2006
Because the IFOs still work better at night, the region of best sensitivity moves across the sky as the earth goes around the sun
June 2006 -149 Hz1027.23.1
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 16
Another detection method:autocorrelation at each
declination
NOT a standard 2-point correlation function Can’t because of variability of
point spread function with sky position
X(ΔRA) at each declination (integral is over RA)
Yi’s are point estimates of GW strain
wi’s are statistical weights of each point on the sky (1st attempt: use reciprocal of theoretical sigma)
Overall normalization is X(0)
ji
jjii wYYwRAX,
)(
i
iiw
For all i,j separated by RA
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 17
Autocorrelation at each declination
Simulated data H(f) = const Working on a
“detection metric”—what quantifies absence/presence of signal?
90°
-90°
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 18
Average the autocorrelations at each declination, over all declinations
In the absence of signal, this can tell us about the resolving power of the instrument; consistent with other estimates.
11500
3000
Hz
kmD
diffraction limited gw astronomy
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 19
The Near Future
Projected sensitivity increase and longer run time means we should surpass BBN bound during S5, for the isotropic analysis (integrating over the whole sky).
Conduct narrowband searches from more directions (Virgo cluster, galactic plane)
Continue development of maximum likelihood analysis, in both point-source (pixel) basis and spherical harmonic basis.
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 20
The End
July 13, 2007 Robert Ward, Caltech LIGO-G070406-00-Z 21
Cross Correlate & InvFFT
Compute optimal filter Qi
and theoretical variance i2
Estimate PSD (data from i-1, i+1 intervals)
Detector 1 60 sec data segments
Data Analysis Flow
FFT
Detector 2 60 sec data segmentsi = 1 2 3 …
t
60sec
Estimate PSD (data from i-1, i+1 intervals)
Read out CC for each pixel
FFT
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