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Edit Comment Close Premium member Presentation Transcript Gravity Wave Detectors Riccardo DeSalvo - LIGO: Gravity Wave Detectors Riccardo DeSalvo - LIGO Gravity waves GW detectors Strain measurement, sensitivity Newtonian Noise How do we throw away your signal Rejection of Newtonian Noise Rejection of Seismic Noise Tidal rejection Items of cross pollination Gravity waves: Gravity waves Recipe to generate GW You throw a couple of solar masses in Tahoe lake You throw another couple of solar masses in Truckee city You let them orbit until the fall on each other The star-quake that ensues strains space-time and GW radiate outGravity waves: Gravity waves GW are quadrupolar, to conserve energy and impulse They deform ellipsoidally a set of masses arranged on a circle The amount of cyclic deformation on Earth for an inspiral in our galaxy is expected to be h~10-21How to detect GW: How to detect GW You suspend 4 heavy mirrors, each two separated by ~4 Km and arrange them in a L configuration You add a beam splitter at the corner and build a Michelson interferometer (with Fabry Perot light accumulators in the arms) The differential signal is the GW signal You make several for coincidence and triangulationSlide6: International network (LIGO, Virgo, GEO, TAMA) of suspended mass Michelson-type interferometers on earth’s surface detect distant astrophysical sources Terrestrial Interferometers suspended test masses free massesThe GW detectors: The GW detectors They are couple of large yard sticks laying on the ground Virgo, 3+3 Km, in the fields of Pisa It EU LIGO NW in the Hanford WA desert LIGO SE in the Livingston LA forestGW detectors as seismic sensors: GW detectors as seismic sensors They can detect soil strainDetecting Earth’s Tidal Strain: Detecting Earth’s Tidal StrainFuture generation of GW detectors: Future generation of GW detectors Next generation CLIO LCGT EGO CEGO Will be undergroundHow Small is 10-18 Meter?: How Small is 10-18 Meter?Can we measure 10-18 m: Can we measure 10-18 m We built the instruments It takes years to tune them up The LIGO commissioning is quite advanced Within a factor of 2 from design at 100 Hz Virgo 2 years behind, but coming soonWhat happens if you tune the detectors at lower frequency: What happens if you tune the detectors at lower frequency Comparing Advanced LIGO with an interferometer tuned at the lower frequency band When an interferometer is tuned below 30 Hz it starts being sensitive to Newtonian Noise (bifurcation on the left for b = 1 and b = 0.1)The Newtonian Noise problem: The Newtonian Noise problem The Newtonian Noise (also known as Gravity Gradient) is a limit energized by seismic waves that generates a wall with ~ f4 slope Changes of amplitude according to the local and dayly seismic activityReducing Newtonian Noise: Reducing Newtonian Noise NN derives from the varying rock density induced by seismic waves around the test mass It generates fluctuating gravitational forces indistinguishable from Gravity Waves It is composed of two parts, The movement of the rock surfaces or interfaces buffeted by the seismic waves The variations of rock density caused by the pressure waves NN reduction underground: NN reduction underground How to shape the environment’s surface to minimize NN? The dominant term of NN is the rock-to-air interface movement On the surface this edge is the flat surface of ground Ground surfaceNN reduction underground: NN reduction underground If the cavern housing the suspended test mass is shaped symmetrically along the beam line and around the test mass tilting and surface deformations, the dominant terms of NN, cancel out (with the exception of the longitudinal dipole moment, which can be measured and subtracted). NN reduction underground: NN reduction underground Pressure seismic waves induce fluctuating rock density around the test mass The result is also fluctuating gravitational forces on the test massNN reduction underground: NN reduction underground Larger caves induce smaller test mass perturbations The noise reduction is proportional to 1/r3 The longitudinal direction is more important =>elliptic caveNN reduction from size: NN reduction from size Reduction factor Cave radius [m] 5 Hz 10 Hz 20 Hz 40 Hz Calculation made for Centered Spherical Cave In rock salt beds Width LengthSlide25: Additionally deep rocks, if uniform, elastic, transmitting and non dissipative, can be measured with a small number of seismometers (or better density meters) to predict its seismic induced density fluctuations and subtract them from the test mass movements This subtraction is largely impeded on the surface by the fractal-like character of the rubble composing surface soil Contributions to NN: Contributions to NN Cave radius [m] Horizontal accelerometer on cave surface will gain a factor of 2 Three-directional 3D matrix of accelerometers or density meters needed for further subtraction Fraction of NN due to Surface Effects (balance from density waves)How do we get rid of your signal: How do we get rid of your signal We build seismic attenuation chains The initial part is variable All seismic attenuation systems end with alternating pendula and vertical springs LF Suspension and Seismic Isolation schematics: LF Suspension and Seismic Isolation schematics 10-20 meter pendula Between all stages 2-3 meter tall Pre-isolator In upper cave LF Vertical filters marionetta Composite Mirror Recoil massExamples of LF vertical springs: Examples of LF vertical springs A payload (1/3 t) is suspended from a pair (or a crown for larger payloads) of cantilever leaf springs. The vertical resonant frequency is reduced by radially compressing the leaf springs in antagonistic mode (Geometric Anti Springs)Movie (click to start): Movie (click to start) 150 mHz: 150 mHz Slide33: Spring tuning procedure, progressive radialcompressionSlide34: Attenuation performance of a GAS filter Acoustic coupling >100 HzGAS spring demonstration: GAS spring demonstration Next two movies (click to start) Watch the black flag on the wire supporting the payload Exciting the payload movement (gas spring main resonance) Applying an EarthquakeTidal Strain rejection: Tidal Strain rejection Reject common mode Tidal strain (<mHz) Clamp laser wavelength to common arm length Reject differential mode Tidal strain (<mHz) Track strain with top of attenuation chain All LF strain NOISE efficiently cancelled!How to recover strain signal: How to recover strain signal Below 50 mHz Compare wavelength with the reference cavity or with a suitably stabilized laser Keep track of the signal from the osition sensor at the top of the chain Above 50 mHz Install auxiliary interferometers between test masses and monuments Intrusive if precision below 10-8 m needed Items of common interest: Items of common interest Extracting signal from noise Template strategies, model based Extensive effort ongoing Signal and correlation extraction techniques Push Development of control techniques and digitalization techniques Oversampling techniques Cross timing techniquesItems of common interest: Items of common interest Can use seismic attenuation techniques developed for GW detection to characterize instruments, Dedicated pilot station in Firenze Geophysics interferometer in NapoliGW seismic attenuators for Geophysics: GW seismic attenuators for Geophysics TAMA-SAS, developed for the TAMA seismic attenuation upgrade, will equip its main mirrors implementing hierarchical controls and LF seismic attenuation like Virgo and Adv-LIGO One of these towers being modified for University of Firenze as a seismometer testing facility Three towers are being built for the Seismic Institute of the University of Napoli for a ground sensing interferometer You do not have the permission to view this presentation. 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granlibachen Herminia Download Post to : URL : Related Presentations : Share Add to Flag Embed Email Send to Blogs and Networks Add to Channel Uploaded from authorPOINTLite Insert YouTube videos in PowerPont slides with aS Desktop Copy embed code: (To copy code, click on the text box) Embed: URL: Thumbnail: WordPress Embed Customize Embed The presentation is successfully added In Your Favorites. Views: 92 Category: Entertainment License: All Rights Reserved Like it (0) Dislike it (0) Added: December 12, 2007 This Presentation is Public Favorites: 0 Presentation Description No description available. Comments Posting comment... By: carwaterguide.blogsp (42 month(s) ago) it's has review many sites like gas for free,run your car on water etc. http://carwaterguide.blogspot.com Saving..... Post Reply Close Saving..... Edit Comment Close Premium member Presentation Transcript Gravity Wave Detectors Riccardo DeSalvo - LIGO: Gravity Wave Detectors Riccardo DeSalvo - LIGO Gravity waves GW detectors Strain measurement, sensitivity Newtonian Noise How do we throw away your signal Rejection of Newtonian Noise Rejection of Seismic Noise Tidal rejection Items of cross pollination Gravity waves: Gravity waves Recipe to generate GW You throw a couple of solar masses in Tahoe lake You throw another couple of solar masses in Truckee city You let them orbit until the fall on each other The star-quake that ensues strains space-time and GW radiate outGravity waves: Gravity waves GW are quadrupolar, to conserve energy and impulse They deform ellipsoidally a set of masses arranged on a circle The amount of cyclic deformation on Earth for an inspiral in our galaxy is expected to be h~10-21How to detect GW: How to detect GW You suspend 4 heavy mirrors, each two separated by ~4 Km and arrange them in a L configuration You add a beam splitter at the corner and build a Michelson interferometer (with Fabry Perot light accumulators in the arms) The differential signal is the GW signal You make several for coincidence and triangulationSlide6: International network (LIGO, Virgo, GEO, TAMA) of suspended mass Michelson-type interferometers on earth’s surface detect distant astrophysical sources Terrestrial Interferometers suspended test masses free massesThe GW detectors: The GW detectors They are couple of large yard sticks laying on the ground Virgo, 3+3 Km, in the fields of Pisa It EU LIGO NW in the Hanford WA desert LIGO SE in the Livingston LA forestGW detectors as seismic sensors: GW detectors as seismic sensors They can detect soil strainDetecting Earth’s Tidal Strain: Detecting Earth’s Tidal StrainFuture generation of GW detectors: Future generation of GW detectors Next generation CLIO LCGT EGO CEGO Will be undergroundHow Small is 10-18 Meter?: How Small is 10-18 Meter?Can we measure 10-18 m: Can we measure 10-18 m We built the instruments It takes years to tune them up The LIGO commissioning is quite advanced Within a factor of 2 from design at 100 Hz Virgo 2 years behind, but coming soonWhat happens if you tune the detectors at lower frequency: What happens if you tune the detectors at lower frequency Comparing Advanced LIGO with an interferometer tuned at the lower frequency band When an interferometer is tuned below 30 Hz it starts being sensitive to Newtonian Noise (bifurcation on the left for b = 1 and b = 0.1)The Newtonian Noise problem: The Newtonian Noise problem The Newtonian Noise (also known as Gravity Gradient) is a limit energized by seismic waves that generates a wall with ~ f4 slope Changes of amplitude according to the local and dayly seismic activityReducing Newtonian Noise: Reducing Newtonian Noise NN derives from the varying rock density induced by seismic waves around the test mass It generates fluctuating gravitational forces indistinguishable from Gravity Waves It is composed of two parts, The movement of the rock surfaces or interfaces buffeted by the seismic waves The variations of rock density caused by the pressure waves NN reduction underground: NN reduction underground How to shape the environment’s surface to minimize NN? The dominant term of NN is the rock-to-air interface movement On the surface this edge is the flat surface of ground Ground surfaceNN reduction underground: NN reduction underground If the cavern housing the suspended test mass is shaped symmetrically along the beam line and around the test mass tilting and surface deformations, the dominant terms of NN, cancel out (with the exception of the longitudinal dipole moment, which can be measured and subtracted). NN reduction underground: NN reduction underground Pressure seismic waves induce fluctuating rock density around the test mass The result is also fluctuating gravitational forces on the test massNN reduction underground: NN reduction underground Larger caves induce smaller test mass perturbations The noise reduction is proportional to 1/r3 The longitudinal direction is more important =>elliptic caveNN reduction from size: NN reduction from size Reduction factor Cave radius [m] 5 Hz 10 Hz 20 Hz 40 Hz Calculation made for Centered Spherical Cave In rock salt beds Width LengthSlide25: Additionally deep rocks, if uniform, elastic, transmitting and non dissipative, can be measured with a small number of seismometers (or better density meters) to predict its seismic induced density fluctuations and subtract them from the test mass movements This subtraction is largely impeded on the surface by the fractal-like character of the rubble composing surface soil Contributions to NN: Contributions to NN Cave radius [m] Horizontal accelerometer on cave surface will gain a factor of 2 Three-directional 3D matrix of accelerometers or density meters needed for further subtraction Fraction of NN due to Surface Effects (balance from density waves)How do we get rid of your signal: How do we get rid of your signal We build seismic attenuation chains The initial part is variable All seismic attenuation systems end with alternating pendula and vertical springs LF Suspension and Seismic Isolation schematics: LF Suspension and Seismic Isolation schematics 10-20 meter pendula Between all stages 2-3 meter tall Pre-isolator In upper cave LF Vertical filters marionetta Composite Mirror Recoil massExamples of LF vertical springs: Examples of LF vertical springs A payload (1/3 t) is suspended from a pair (or a crown for larger payloads) of cantilever leaf springs. The vertical resonant frequency is reduced by radially compressing the leaf springs in antagonistic mode (Geometric Anti Springs)Movie (click to start): Movie (click to start) 150 mHz: 150 mHz Slide33: Spring tuning procedure, progressive radialcompressionSlide34: Attenuation performance of a GAS filter Acoustic coupling >100 HzGAS spring demonstration: GAS spring demonstration Next two movies (click to start) Watch the black flag on the wire supporting the payload Exciting the payload movement (gas spring main resonance) Applying an EarthquakeTidal Strain rejection: Tidal Strain rejection Reject common mode Tidal strain (<mHz) Clamp laser wavelength to common arm length Reject differential mode Tidal strain (<mHz) Track strain with top of attenuation chain All LF strain NOISE efficiently cancelled!How to recover strain signal: How to recover strain signal Below 50 mHz Compare wavelength with the reference cavity or with a suitably stabilized laser Keep track of the signal from the osition sensor at the top of the chain Above 50 mHz Install auxiliary interferometers between test masses and monuments Intrusive if precision below 10-8 m needed Items of common interest: Items of common interest Extracting signal from noise Template strategies, model based Extensive effort ongoing Signal and correlation extraction techniques Push Development of control techniques and digitalization techniques Oversampling techniques Cross timing techniquesItems of common interest: Items of common interest Can use seismic attenuation techniques developed for GW detection to characterize instruments, Dedicated pilot station in Firenze Geophysics interferometer in NapoliGW seismic attenuators for Geophysics: GW seismic attenuators for Geophysics TAMA-SAS, developed for the TAMA seismic attenuation upgrade, will equip its main mirrors implementing hierarchical controls and LF seismic attenuation like Virgo and Adv-LIGO One of these towers being modified for University of Firenze as a seismometer testing facility Three towers are being built for the Seismic Institute of the University of Napoli for a ground sensing interferometer