GW Detectors noise and sensitivity

LIGO detectorsRep. 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

Class. Quantum Grav. 25 (2008) 184017

“FSR” (free spectral range) 37.5 kHz

Antenna pattern at FSR

Directional sensitivity

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

Enhanced LIGO detectors

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Squeezed Detectors

Advanced LIGO/ Advanced Virgo

~10 times better, lower frequencies in bandInstallation in progress

Initial vs Advanced LIGO

Simple pendulums become monolithic, quadruple pendulumswith better quality opticsPrototypes being tested, optics are polished

Initial vs Advanced LIGOLasers become more powerful: 10W 200 WInstalled and being tested at LIGO Livingston.

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

1919

The Advanced GW Detector Network~2020GEO600Advanced LIGO

Hanford

Advanced LIGO Livingston

Advanced Virgo

LIGO-India?

KAGRA

Other GW detectors

Pulsar timing arrays

Image Courtesy of Michael Kramer

Nanograv residuals

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hc,min =σ

T 3 / 2 N pulsars

Space detectors: LISA

Online generators

http://www.gwoptics.org/processing/space_time_quest/

http://www.srl.caltech.edu/~shane/sensitivity/MakeCurve.html