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Unformatted text preview: Einstein Telescope Mock Data Challenge Carl Rodriguez * Reed College, Portland, OR 97202 and Cardiff University, Cardiff, CF24 3YB, UK (Dated: August 12, 2009) Abstract: The Einstein Telescope (ET) is a proposed third generation gravitational wave interfer- ometer with a 10 fold increase in sensitivity over advanced detectors and a detection band from 1 Hz to 10 kHz. For binary neutron star inspirals (NS-NS), population density studies suggest anywhere from 10 5 to 10 6 sources per year within ETs detection horizon of z w 1. That, combined with an average chirp time of 6 days for the proposed detection band, suggests an average overlap of over 17,000 simultaneous signals. To test if current data analysis techniques can handle such significant numbers of signals, we design preliminary stages of a NS-NS inspiral data simulation similar to the LISA Mock Data Challenge. Using the restricted post-Newtonian waveform with a post-Newtonian phase out to 3.5, we generate two mock data sets using the proposed ET sensitivity curve with lower frequency cutoffs of 10 and 5 Hz, and the above population density. The details of the simulation will be discussed, as well as further improvements for the simulation. I. INTRODUCTION Gravitational Wave interferometry is a relatively new method for understanding the universe via the observa- tion of propagating ripples in spacetime. By measuring the interference from two phase locked detector arms, the strain produced on the detector by an incident grav- itational wave can be measured, providing an entirely new look into the state and structure of astrophysical phenomena. As gravitational waves are not absorbed or reflected, they can propagate without hindrance through- out the entire universe, yielding a view of objects previ- ously unavailable to conventional electromagnetic astron- omy . There are currently four gravitational wave interferom- eters in operation: the two detectors of the Laser Inter- ferometer Gravitational Observatory (LIGO), operating in Livingston, Louisiana and Hanford, Washington, the VIRGO detector, operating outside Pisa, Italy, the GEO 600 detector, operating outside Hanover, Germany, and the relatively new TAMA 300 detector, operating near Mitaka, Japan. These detectors are currently in their initial stage, with plans to upgrade LIGO and VIRGO to more advanced, second generation technology by the end of 2014. Once completed, Advanced LIGO and VIRGO will have sufficient range to detect several events per year, from binary neutron star inspirals (NS-NS) to gamma ray bursts, supernovae, black hole mergers and ring-downs, etc. With advanced detectors already slated for upgrades, plans have begun on the third generation of gravita- tional wave observatories. These detectors will use cut- ting edge technology, combined with instrumentation and data analysis techniques learned from first and second generation detectors to push to sensitivity levels far be- yond current planned detectors. One such detector, theyond current planned detectors....
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This note was uploaded on 12/15/2011 for the course PHY 2020 taught by Professor Staff during the Spring '08 term at University of Florida.
- Spring '08