Intro to LIGO Seismic Isolation Prebid meeting Gary

Intro to LIGO Seismic Isolation Pre-bid meeting Gary Sanders LIGO/Caltech Stanford, April 29, 2003 LIGO G 030246 -00 -M

May we record the meeting and distribute transcript to all? LIGO G 030246 -00 -M

General Relativity Einstein theorized that smaller masses travel toward larger masses, not because they are "attracted" by a mysterious force, but because the smaller objects travel through space that is warped by the larger object § Imagine space as a stretched rubber sheet. § A mass on the surface will cause a deformation. § Another mass dropped onto the sheet will roll toward that mass. LIGO G 030246 -00 -M 3

Gravitational Waves • a necessary consequence of Special Relativity with its finite speed for information transfer • time dependent gravitational fields come from the acceleration of masses and propagate away from their sources as a spacetime warpage at the speed of light gravitational radiation from binary inspiral of compact objects LIGO G 030246 -00 -M 4

Evidence for Gravitational Waves Neutron Binary System – Hulse & Taylor PSR 1913 + 16 -- Timing of pulsars Emission of gravitational waves 17 / sec · · ~ 8 hr Neutron Binary System • separated by 106 miles • m 1 = 1. 4 m ; m 2 = 1. 36 m ; e = 0. 617 Prediction from general relativity • spiral in by 3 mm/orbit • rate LIGO of change orbital period G 030246 -00 -M 5

Direct Detection Gravitational Wave Astrophysical Source Terrestrial detectors LIGO, GEO, TAMA, Virgo Detectors in space LISA LIGO G 030246 -00 -M 6

A New Window on the Universe Gravitational Waves will provide a new way to view the dynamics of the Universe LIGO G 030246 -00 -M 8

Astrophysical Sources of Gravitational Waves l Compact binary inspiral: “chirps” » NS-NS waveforms are well described » BH-BH need better waveforms » search technique: matched templates l Supernovae / GRBs: “bursts” » burst signals in coincidence with signals in electromagnetic radiation » Challenge to search for untriggered bursts l Pulsars in our galaxy: “periodic signals” » search for observed neutron stars (frequency, doppler shift) » all sky search (computing challenge) » r-modes l Cosmological Signals LIGO G 030246 -00 -M “stochastic background” 9

Terrestrial Interferometers free masses International network (LIGO, Virgo, GEO, TAMA) of suspended mass Michelson-type interferometers on earth’s surface detect distant astrophysical sources suspended test masses LIGO G 030246 -00 -M 10

The Laboratory Sites Laser Interferometer Gravitational-wave Observatory (LIGO) Hanford Observatory Livingston Observatory LIGO G 030246 -00 -M 11

LIGO Livingston Observatory LIGO G 030246 -00 -M 12

LIGO Hanford Observatory LIGO G 030246 -00 -M 13

LIGO Beam Tube 1. 2 m diameter - 3 mm stainless 50 km of weld LIGO G 030246 -00 -M l LIGO beam tube under construc l 65 ft spiral welded sections l girth welded in portable clean ro NO LEAKS !! 14

LIGO Vacuum Equipment LIGO G 030246 -00 -M 15

A LIGO Mirror Substrates: Si. O 2 25 cm Diameter, 10 cm thick Homogeneity < 5 x 10 -7 Internal mode Q’s > 2 x 106 Polishing Surface uniformity < 1 nm rms Radii of curvature matched < 3% Coating Scatter < 50 ppm Absorption < 2 ppm Uniformity <10 -3 LIGO G 030246 -00 -M 16

Core Optics installation and alignment LIGO G 030246 -00 -M 17

What Limits Sensitivity of Interferometers? 1. Seismic noise & vibration limit at low frequencies 2. Atomic vibrations (Thermal Noise) inside components limit at mid frequencies 3. Quantum nature of light (Shot Noise) limits at high frequencies 4. Myriad details of the lasers, electronics, etc. , can make problems above these levels LIGO G 030246 -00 -M 18

LIGO Sensitivity Livingston 4 km Interferometer May 2001 Jan 2003 LIGO G 030246 -00 -M 19

Advanced LIGO 2007 + • • Enhanced Systems laser suspension seismic isolation test mass Improvement factor in rate ~ 104 + narrow band optical configuration LIGO G 030246 -00 -M 20

Advanced LIGO Development Underway Multiple Suspensions Active Seismic Sapphire Optics Higher Power Laser LIGO G 030246 -00 -M 21