Stochastic background search using LIGO Livingston and ALLEGRO

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Presentation transcript:

Stochastic background search using LIGO Livingston and ALLEGRO Martin McHugh Loyola University New Orleans on behalf of the LIGO Scientific Collaboration LSU-ALLEGRO group LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

Outline Stochastic background searches Features of the LLO-ALLEGRO stochastic analysis Calibrated response of the ALLEGRO detector LIGO S2 science run data Expected sensitivity from S2 data LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

Stochastic background searches Set of unresolved gravitational wave sources Cosmological or astrophysical in origin Characterized by Search strategy -- look for correlations between two gravitational wave detectors Assume background is isotropic, gaussian, stationary and _ over the frequency band of the measurement Assume instrument noise is uncorrelated between detectors Optimally filtered cross-correlation statistic LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

Stochastic background searches Optimal filter Weighted by the noise in each detector  is the frequency dependent overlap reduction function Optimal for given GW spectrum LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

LLO - ALLEGRO correlation Key features: Ability to modulate the signal – rotate to align/misalign antenna patterns -- get direct measure of non-GW correlations. Aligned orientation at 40km separation gives overlap near unity up to kHz frequencies -- higher range than LLO-LHO (sensitive band of resonant detector is limiting factor) 40 km apart, explore PEM correlations at intermediate distances *Modulating the experimental signature of a stochastic gravitational wave background, Finn and Lazzarini Phys. Rev. D 64, 082002 (2001)

L1 A1 LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

Overview of technique Start with A1, L1 time domain data streams A1 signal is heterodyned in hardware reference frequency 899Hz for S2 different sampling rates 250 samples/sec for A1 - complex time series, 16384 samples/sec, downsampled to 2048 for L1 Frequency domain Equal time stretches give same frequency resolution match bins over appropriate frequency band 774Hz-1024Hz for A1 0-1024Hz for L1 LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

Calibration of A1 data This analysis is a fully coherent search, combining bar and interferometer data For event list based burst searches, a full phase consistent response function of the detector is not required New calibration code needed for this analysis LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

Signal path h z[i] x xI R(f) xQ H(f) Heterodyne Bar response DAQ and Low-pass F(f) DAQ 250 samps/s xQ Feedback Damping (weak) H(f) 899Hz reference oscillator GPS clock LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

ALLEGRO S2 data LIGO S2 run -- Feb 14-Apr 14, 2003 -- is only science run for which ALLEGRO was operational Bar was operational for roughly half of S2 ~180 hrs coincident with LIGO science segments made two rotations ~101hrs in misaligned null orientation ~45.5 hrs aligned with ifo Yarm ~33 hrs aligned with if Xarm Current status of S2 analysis Preliminary calibration for bar data calibration applied to 58x600 second playground segments Matlab analysis pipeline in place, have run playground jobs LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

Frequency domain optimal filter LIGO ALLEGRO GR17, Dublin LIGO-G040304-00-Z GR17, Dublin 23 July , 2004

Expected S2 sensitivity Over band 850Hz-950Hz, for ~75 hrs of aligned data (SNR=1), the projected sensitivity from the noise curves gives Corresponds to gravitational waves with amplitude noise spectral density of (for flat GW this is a f -3/2 spectrum -- nearly constant over narrow band) LIGO-G040304-00-Z GR17, Dublin 23 July , 2004