GW Detectors noise and sensitivity

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Presentation transcript:

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 Class. Quantum Grav. 25 (2008) 184017

Antenna pattern at FSR

Directional sensitivity

LIGO calibration Nucl. Instrum. Meth. A624 (2010) 223 arXiv:1007.3973

Enhanced LIGO detectors Sensitivity equivalent to measuring the distance to the nearest star (Proxima Centauri, 4.22 light years distant) to better than 10 microns!

Squeezed Detectors

Advanced LIGO/ Advanced Virgo ~10 times better, lower frequencies in band Installation in progress

Initial vs Advanced LIGO Simple pendulums become monolithic, quadruple pendulums with better quality optics Prototypes being tested, optics are polished

Initial vs Advanced LIGO Lasers become more powerful: 10W  200 W Installed and being tested at LIGO Livingston.

Initial vs Advanced LIGO Seismic isolation goes from passive to active HAM SEI tested in S6 Most chambers have now their “SEI” installed.

More on Adv LIGO: LIGO magazine in www.ligo.org

The Advanced GW Detector Network~2020 Advanced LIGO Hanford GEO600 Advanced Virgo KAGRA LIGO-India? Advanced LIGO Livingston 19

Other GW detectors

Pulsar timing arrays Nanograv residuals Image Courtesy of Michael Kramer Nanograv residuals

Space detectors: LISA

Online generators http://www.srl.caltech.edu/~shane/sensitivity/MakeCurve.html http://www.gwoptics.org/processing/space_time_quest/