Block Normal A Change Point Analysis for Burst LIG块正常的变点分析突发LIGO.pptVIP

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2018-06-19 发布于福建
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Block Normal A Change Point Analysis for Burst LIG块正常的变点分析突发LIGO.ppt

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Block Normal A Change Point Analysis for Burst LIG块正常的变点分析突发LIGO

Block Normal: A Change Point Analysis for Burst Gravitational Waves Amber L. Stuver Center for Gravitational Wave Physics Penn State University Block Normal... What is it? How does it work? How well does it do? What’s next? What is a “Block Normal” Analysis? Seeks the onset of a GW signal by looking for a change in statistics of the detector output. Block: divide data into blocks where statistics are approximately constant Normal: characterizes statistics in block by mean and variance When a signal is present, the variance of the detector output must change (although the mean may not). Block Normal looks in an unprejudiced way at the data Assume nothing about GW properties: e.g. waveform, spectrum How Does it Work? Efficiency vs. False Alarm Rate1,024 Data Points Efficiency vs. False Alarm Rate16,384 Data Points What’s Next? Apply to S1 data Already part of LAL Investigate sensitivity to different kinds of bursts Mock data challenges Investigate utility as detector diagnostic New DMT monitor? Statistical Curves Picking Out Change Points LIGO Scientific Collaboration – Penn State University LIGO-G020310-00-Z This plot is the same as the last except that the data length on which ρ2 is calculated is 16,384 points. So, as is usual in signal detection, the longer the data we can integrate over, the better the signal to noise ratio. The effect here is quite obvious. BACKGROUND 1024 points, 10,000 iterations This slide just serves as a backup illustration in case anyone asks about the Monte Carlo simulations that determined the bounds on the value of ρ. BACKGROUND This slide just serves as an backup illustration of the effectiveness of the block normal analysis to pick out the index of the change point in the data in case anyone asks about it. Large errors occur near the end points of the data suggesting the need for overlapping successive data lengths. DCC # LIGO-G020310-00-Z Greeting Introduction of myself Statement of topic The detector output is largely noi