Difference: DataAnalysis (1 vs. 12)
Revision 122011-04-07 - GergelyDebreczeni
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| > > | Eccentricity studiesExternal force-free excentric binary systems are supposed to circularize in a relatively short time-scale.As a consequance, in the final stage of their inspiral evolution when the GW emitted by them is in the sensitivity band of current interferometers it's enough to use circular template banks for their detection. However under some circumstance - spinning systems or 3 body interactions in the galactic halo - binary system could have o non-negligible eccentricity. Tho goal of this study is to determine the conditions and the minimum value of eccentricity which result in a significant SNR dropp in the detection pipleine. Further details here. | |||||||
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Revision 112011-02-14 - GergelyDebreczeni
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(Matyas Vasuth, Peter Csizmadia)
Implementing new templates, efficiency test | |||||||||||||||||||||||||||
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| < < | The calculated new waveforms are transformed into ninja format and are injected into the detector signal. We use the already existing template banks to see with what efficiency the new injections are discovered with the old non-spinning, circular waveforms. The procedure is describe on the bank simulation howto page | ||||||||||||||||||||||||||
| > > | The calculated new waveforms are transformed into ninja format and are injected into the detector signal. We use the already existing template banks to see with what efficiency the new injections are discovered with the old non-spinning, circular waveforms. | ||||||||||||||||||||||||||
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Revision 102009-09-30 - GergelyDebreczeni
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(Matyas Vasuth, Peter Csizmadia)
Implementing new templates, efficiency test | |||||||||||||||||||||||||||
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| < < | The calculated new waveforms are transformed into ninja format and are injected into the detector signal. We use the already existing template banks to see with what efficiency the new injections are discovered with the old non-spinning, circular waveforms. | ||||||||||||||||||||||||||
| > > | The calculated new waveforms are transformed into ninja format and are injected into the detector signal. We use the already existing template banks to see with what efficiency the new injections are discovered with the old non-spinning, circular waveforms. The procedure is describe on the bank simulation howto page | ||||||||||||||||||||||||||
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Revision 92009-09-29 - MatyasVasuth
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Revision 82009-09-29 - GergelyDebreczeni
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| < < | Data analysis activities of the RMKI Virgo Group | ||||||||||||||||||||||||||
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| > > | Data analysis activities of the RMKI Virgo Group | ||||||||||||||||||||||||||
Noise and Wiener filter studies | |||||||||||||||||||||||||||
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| < < | In case when the detector noise is not perfectly white, the optimal matched filtering is not realized by simply taking the cross-correlation of the signal pattern and the measured time series, but by correctly implementing the Wiener filter, depending also on the actual time series. We investigate the gain in signal to noise ratio when implementing the Wiener filter correctly. Our preferred approach is based on performing the Wiener filtering in time domain, using unbiased statistical estimators of the necessary correlation functions, and on the Neumann series expansion for deconvolution (for this, see J.Phys. A39 (2006) 13621 ). (Andras Laszlo) | ||||||||||||||||||||||||||
| > > | In case when the detector noise is not perfectly white, the optimal matched filtering is not realized by simply taking the cross-correlation of the signal pattern and the measured time series, but by correctly implementing the Wiener filter, depending also on the actual time series. We investigate the gain in signal to noise ratio when implementing the Wiener filter correctly. Our preferred approach is based on performing the Wiener filtering in time domain, using unbiased statistical estimators of the necessary correlation functions, and on the Neumann series expansion for deconvolution (for this, see J.Phys. A39 (2006) 13621).
(Andras Laszlo) | ||||||||||||||||||||||||||
Calculating spinning eccentric GW templates | |||||||||||||||||||||||||||
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(Matyas Vasuth, Peter Csizmadia)
Implementing new templates, efficiency test | |||||||||||||||||||||||||||
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| < < | The calculated new waveforms are transformed into ninja format and are injected into the detector signal. We use the already existing template banks to see with what efficiency the new injections are discovered with the old non-spinning, circular waveforms. (Gergely Debreczeni) | ||||||||||||||||||||||||||
| > > | The calculated new waveforms are transformed into ninja format and are injected into the detector signal. We use the already existing template banks to see with what efficiency the new injections are discovered with the old non-spinning, circular waveforms. (Gergely Debreczeni) | ||||||||||||||||||||||||||
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Revision 72009-09-28 - MatyasVasuth
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Noise and Wiener filter studies | |||||||||||||||||||||||||||
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| < < | In case when the detector noise is not perfectly white, the optimal matched filtering is not realized by
simply taking the cross-correlation of the signal pattern and the measured time series, but by correctly
implementing the Wiener filter, depending also on the actual time series. We investigate the gain
in signal to noise ratio when implementing the Wiener filter correctly. Our preferred approach is based
on performing the Wiener filtering in time domain, using unbiased statistical estimators of the necessary
correlation functions, and on the Neumann series expansion for deconvolution (for this, see
J.Phys. A39 (2006) 13621).
(Andras Laszlo) | ||||||||||||||||||||||||||
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In case when the detector noise is not perfectly white, the optimal matched filtering is not realized by simply taking the cross-correlation of the signal pattern and the measured time series, but by correctly implementing the Wiener filter, depending also on the actual time series. We investigate the gain in signal to noise ratio when implementing the Wiener filter correctly. Our preferred approach is based on performing the Wiener filtering in time domain, using unbiased statistical estimators of the necessary correlation functions, and on the Neumann series expansion for deconvolution (for this, see J.Phys. A39 (2006) 13621). (Andras Laszlo) | ||||||||||||||||||||||||||
Calculating spinning eccentric GW templates | |||||||||||||||||||||||||||
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| > > | In the post-Newtonian formalism the spacetime is assumed to be split into two parts, the near and wave zones. The field equations for the perturbed Minkowski metric are solved in both regions. As a result of the calculations, the radiation field in the wave zone is expressed in terms of integrals over the source (the source multipole moments). For the special case of compact binary systems the source integrals are evaluated and the relative acceleration of the orbiting bodies is given e.g. in Kidder up to the leading order radiation reaction terms. We integrate these equations of motion and spin precession numerically with the 4th order Runge-Kutta method, and express the gravitational waveforms for spinning eccentric binaries from the general form of the radiation field. | ||||||||||||||||||||||||||
(Matyas Vasuth, Peter Csizmadia)
Implementing new templates, efficiency test | |||||||||||||||||||||||||||
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| < < | The calculated new waveforms are transformed into ninja format and are injected into the detector signal. We use the already existing template banks to see with what efficiency the new injections are discovered with the old non-spinning, circular waveforms. (Gergely Debreczeni) | ||||||||||||||||||||||||||
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| > > | The calculated new waveforms are transformed into ninja format and are injected into the detector signal. We use the already existing template banks to see with what efficiency the new injections are discovered with the old non-spinning, circular waveforms. (Gergely Debreczeni) | ||||||||||||||||||||||||||
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Revision 62009-09-08 - AndrasLaszlo
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| < < | Noise and Wiener-filter studies | ||||||||||||||||||||||||||
| > > | Noise and Wiener filter studiesIn case when the detector noise is not perfectly white, the optimal matched filtering is not realized by simply taking the cross-correlation of the signal pattern and the measured time series, but by correctly implementing the Wiener filter, depending also on the actual time series. We investigate the gain in signal to noise ratio when implementing the Wiener filter correctly. Our preferred approach is based on performing the Wiener filtering in time domain, using unbiased statistical estimators of the necessary correlation functions, and on the Neumann series expansion for deconvolution (for this, see J.Phys. A39 (2006) 13621). | ||||||||||||||||||||||||||
(Andras Laszlo)
Calculating spinning eccentric GW templates | |||||||||||||||||||||||||||
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Revision 52009-09-08 - GergelyDebreczeni
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| < < | The RMKI Budapest Group will participate in the search for burst sources and periodic sources of gravitational waves. More information and technical description of this activity is to be added to this page, soon. | ||||||||||||||||||||||||||
| > > | Data analysis activities of the RMKI Virgo Group | ||||||||||||||||||||||||||
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| < < | GRB searchesLinks | ||||||||||||||||||||||||||
| > > | Noise and Wiener-filter studies(Andras Laszlo)Calculating spinning eccentric GW templates(Matyas Vasuth, Peter Csizmadia)Implementing new templates, efficiency testThe calculated new waveforms are transformed into ninja format and are injected into the detector signal. We use the already existing template banks to see with what efficiency the new injections are discovered with the old non-spinning, circular waveforms. _ (Gergely.Debreczeni)_Links | ||||||||||||||||||||||||||
Revision 42009-03-03 - IstvanRacz
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Revision 32009-02-13 - GergelyDebreczeni
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| < < | The RMKI Budapest Group will participate in the search for burst sources and periodic sources of gravitational waves. More information and technical description of this activity is to be added to this page, soon. | ||||||||||||||||||||||||||
| > > | The RMKI Budapest Group will participate in the search for burst sources and periodic sources of gravitational waves. More information and technical description of this activity is to be added to this page, soon. | ||||||||||||||||||||||||||
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Revision 22008-11-23 - TWikiAdminUser
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Data analysis activitiesThe RMKI Budapest Group will participate in the search for burst sources and periodic sources of gravitational waves. More information and technical description of this activity is to be added to this page, soon. | |||||||||||||||||||||||||
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Revision 12008-11-19 - GergelyDebreczeni
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Data analysis activitiesThe RMKI Budapest Group will participate in the search for burst sources and periodic sources of gravitational waves. More information and technical description of this activity is to be added to this page, soon. -- GergelyDebreczeni - 19 Nov 2008 | |||||||
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