gw detectors noise and sensitivity
DESCRIPTION
GW Detectors noise and sensitivity. LIGO detectors. Rep. Prog. Phys. 72 (2009) 076901 arXiv:0711.3041. Sensitivity progress. Rep. Prog. Phys. 72 (2009) 076901 arXiv:0711.3041. “Antenna pattern”. “peanut”. LIGO high frequency sensitivity. “FSR” (free spectral range) 37.5 kHz . - PowerPoint PPT PresentationTRANSCRIPT
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GW Detectors noise and sensitivity
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LIGO detectorsRep. Prog. Phys. 72 (2009) 076901 arXiv:0711.3041
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Sensitivity progress
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Rep. Prog. Phys. 72 (2009) 076901 arXiv:0711.3041
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“Antenna pattern”
“peanut”
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LIGO high frequency sensitivity
Class. Quantum Grav. 25 (2008) 184017
“FSR” (free spectral range) 37.5 kHz
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Antenna pattern at FSR
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Directional sensitivity
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LIGO calibration Nucl. Instrum. Meth. A624 (2010) 223 arXiv:1007.3973
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Enhanced LIGO detectors
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Squeezed Detectors
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Advanced LIGO/ Advanced Virgo
~10 times better, lower frequencies in bandInstallation in progress
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Initial vs Advanced LIGO
Simple pendulums become monolithic, quadruple pendulumswith better quality opticsPrototypes being tested, optics are polished
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Initial vs Advanced LIGOLasers become more powerful: 10W 200 WInstalled and being tested at LIGO Livingston.
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Initial vs Advanced LIGOSeismic isolation goes from passive to activeHAM SEI tested in S6Most chambers have now their “SEI” installed.
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More on Adv LIGO: LIGO magazine in www.ligo.org
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The Advanced GW Detector Network~2020GEO600Advanced LIGO
Hanford
Advanced LIGO Livingston
Advanced Virgo
LIGO-India?
KAGRA
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Other GW detectors
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Pulsar timing arrays
Image Courtesy of Michael Kramer
Nanograv residuals
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€
hc,min =σ
T 3 / 2 N pulsars
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Space detectors: LISA
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Online generators
http://www.gwoptics.org/processing/space_time_quest/
http://www.srl.caltech.edu/~shane/sensitivity/MakeCurve.html