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LIGO-G050274-00-W Gregory Mendell, LIGO Hanford Observatory on behalf of the LIGO Scientific Collaboration Stackslide search for continuous gravitational.

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Presentation on theme: "LIGO-G050274-00-W Gregory Mendell, LIGO Hanford Observatory on behalf of the LIGO Scientific Collaboration Stackslide search for continuous gravitational."— Presentation transcript:

1 LIGO-G050274-00-W Gregory Mendell, LIGO Hanford Observatory on behalf of the LIGO Scientific Collaboration Stackslide search for continuous gravitational waves using LIGO S4 data. http://www.ligo.caltech.edu Supported by the National Science Foundation LIGO-G050374-00-WLIGO-G050635-00-WLIGO-G060177-00-W APS April 2006

2 LIGO-G050274-00-W LIGO-Gxxxxxx-00-W Frequency (Hz) Strain Sensitivity [1/Sqrt(Hz)] S5 is currently running at design sensitivity! APS April 2006 Fourth Science Run (S4) Sensitivity (February 22, 2005 – March 23, 2005)

3 LIGO-G050274-00-W LIGO-G060177-00-W Sources of Continuous Gravitational Waves (This talk shows results for isolated sources only.) Mountain on neutron star Precessing neutron star Accreting neutron star Oscillating neutron star AB C D Credits: A. image by Jolien Creighton; LIGO Lab Document G030163-03-Z. B. image by M. Kramer; Press Release PR0003, University of Manchester - Jodrell Bank Observatory, 2 August 2000. C. image by Dana Berry/NASA; NASA News Release posted July 2, 2003 on Spaceflight Now. D. image from a simulation by Chad Hanna and Benjamin Owen; B. J. Owen's research page, Penn State University. Search can detected any periodic source. Upper limits are set on gravitational-wave amplitude, h 0, of rotating triaxial ellipsoid. APS April 2006

4 LIGO-G050274-00-W The StackSlide Method Break up data into segments; FFT each, producing Short (30 min) Fourier Transforms (SFTs) = coherent step. StackSlide: stack SFTs, track frequency, slide to line up & add the power weighted by noise inverse = incoherent step. Other semi-coherent methods:  Hough Transform: Phys. Rev. D72 (2005) 102004; gr-qc/0508065.  PowerFlux: see next talk, W11.00005 Fully coherent methods:  Frequency domain match filtering/maximum likelihood estimation (C7.00001; W11.00006)  Time domain Bayesian parameter estimation (C7.00002) Improvements and hierarchical pipeline under development. Time Frequency Time APS April 2006 Track Doppler shift and df/dt

5 LIGO-G050274-00-W The StackSlide S4 Pipeline Read in command line argument, data, and initialize variables Clean narrow instrument lines For each point in the parameter space: Stack, slide, and sum the power Search for peaks above a threshold or the loudest power Clean narrow instrument lines For points surrounding the injection: Stack, slide, and sum the power Search for the loudest power Generate fake signal and add it to the data. Read in command line argument, data, and initialize variables Done? Matlab code: Finds upper limits Makes plots SearchMonte Carlo Simulation Yes No APS April 2006

6 LIGO-G050274-00-W LIGO-Gxxxxxx-00-W Line Cleaning Method (Only clean known lines; those wider than 0.021 Hz are not cleaned.) Frequency (Hz) Spectral Density [1/Sqrt(Hz)] APS April 2006

7 LIGO-G050274-00-W Analysis of Hardware Injections RA (hours) DEC (degrees) PRELIMINARY APS April 2006 LIGO-G060177-00-W Fake gravitational-wave signals corresponding to rotating neutron stars with varying degrees of asymmetry were injected for parts of the S4 run by actuating on one end mirror. Sky maps for the search for an injected signal with h 0 ~ 7.5e-24 are below. Black stars show the fake signal’s sky position.

8 LIGO-G050274-00-W S4 StackSlide “Loudest Events” 50-225 Hz LIGO-Gxxxxxx-00-W Searched 450 freq. per.25 Hz band, 51 values of df/dt, between 0 & -1e-8 Hz/s, up to 82,120 sky positions (up to 2e9 templates). The expected loudest StackSlide Power was ~ 1.22 (SNR ~ 7) Veto bands affected by harmonics of 60 Hz. Simple cut: if SNR > 7 in only one IFO veto; if in both IFOs, veto if abs(f H1 - f L1 ) > 1.1e-4*f0 StackSlide Power Frequency (Hz) APS April 2006 PRELIMINARY

9 LIGO-G050274-00-W S4 StackSlide “Loudest Events” 50-225 Hz LIGO-Gxxxxxx-00-W StackSlide Power Frequency (Hz) APS April 2006 PRELIMINARY FakePulsar3=> FakePulsar8=> <=Follow-up Indicates Instrument Line Searched 450 freq. per.25 Hz band, 51 values of df/dt, between 0 & -1e-8 Hz/s, up to 82,120 sky positions (up to 2e9 templates). The expected loudest StackSlide Power was ~ 1.22 (SNR ~ 7) Veto bands affected by harmonics of 60 Hz. Simple cut: if SNR > 7 in only one IFO veto; if in both IFOs, veto if abs(f H1 - f L1 ) > 1.1e-4*f0

10 LIGO-G050274-00-W LIGO-Gxxxxxx-00-W Best: 4.4e-24 For 139.5-139.75 Hz Band PRELIMINARY Frequency (Hz) S4 StackSlide h 0 95% Confidence All Sky Upper Limits 50-225 Hz APS April 2006 Note that h 0 is the gravitational-wave amplitude for a rotating triaxial ellipsoid. Monte Carlo injections of triaxial sources over the search parameter space & source orientations set the ULs. Best: 5.4e-24 For 140.75-141.0 Hz Band h 0 Upper Limit

11 LIGO-G050274-00-W Conclusions These results are interesting, but much better results are on the way! Improvements:  S5: ~ 2x better sensitivity, 12x or more data.  Increase time baseline of coherent step  Multi-ifo code  Refined coincidence steps Hierarchical pipeline under development that combines coherent and semi-coherent searches. APS April 2006 LIGO-G060177-00-W

12 LIGO-G050274-00-W END APS SLIDES

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