Advanced Detector Status Report and Future Scenarios Giles

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Advanced Detector Status Report and Future Scenarios Giles Hammond, University of Glasgow on behalf

Advanced Detector Status Report and Future Scenarios Giles Hammond, University of Glasgow on behalf of the LIGO Scientific Collaboration and the VIRGO Collaboration 3 rd October 2012 LIGO-G 1201050 ELi. TES meeting, Japan 1

Overview of the presentation • Worldwide network of detectors • Astrophysics with Advanced detectors

Overview of the presentation • Worldwide network of detectors • Astrophysics with Advanced detectors • Overview of the ongoing detector upgrades – GEO-HF – Advanced LIGO (a. LIGO) – Advanced VIRGO (Ad. V) • Incremental upgrades to the Advanced detectors • Summary and future prospects 2

Worldwide Detector Network LIGO Hanford (LHO) LIGO Livingston (LLO) GEO KAGRA VIRGO ACIGA

Worldwide Detector Network LIGO Hanford (LHO) LIGO Livingston (LLO) GEO KAGRA VIRGO ACIGA

Astrophysics with Advanced Detectors • The worldwide network is being upgraded to 2 nd

Astrophysics with Advanced Detectors • The worldwide network is being upgraded to 2 nd generation or “Advanced” status • A network allows source location for follow up observations =>Multimessenger astronomy INDIA/KAGRA/LIGO/VIRGO LIGO G 1000087 • • • The advanced detectors will provide the first detections of gravitational waves and open up a new, non-electromagnetic, window on the universe Multimessenger astronomy (e. g. EM/neutrino observation) will increase detection confidence and provide complementary information Expected event rates of several ten’s of neutron stars coalescences per year 4

Astrophysics with Advanced Detectors • • Fundamental test of general relativity=> measure the “speed

Astrophysics with Advanced Detectors • • Fundamental test of general relativity=> measure the “speed of gravity” and the polarisation of gravitational waves Confirm or rule out that the fireballs of gamma-ray burst events are powered by merging neutron star binaries Detect, for the first time, binary black holes and possibly provide the clue to the missing population of intermediate-mass black holes Measure the equation-of-state of ultra dense matter in neutron star cores and thereby help understand extremes of nuclear physics • Accurately measure the masses and spins of a number of neutron stars and black holes • Provide new tests of strong field gravity • Accurately measure the Hubble constant 5

Worldwide Detector Network >2010 LIGO India http: //gwic. ligo. org/ e. LIGO • LIGO

Worldwide Detector Network >2010 LIGO India http: //gwic. ligo. org/ e. LIGO • LIGO Advanced LIGO and Advanced VIRGO will result in a 10 distance increase => 1000 increase in volume • GEO-HF features a high frequency upgrade (>500 Hz) • KAGRA (LCGT) will be the first cryogenic detectors • LIGO India (2018) will significantly improve source location a. LIGO

Laser Interferometric Detectors seismic noise shot noise Need to measure length changes 10 -18

Laser Interferometric Detectors seismic noise shot noise Need to measure length changes 10 -18 m over 4 km baselines mirror thermal noise • Technologies required => Suspended optics (to reduce seismic noise) Ultra-high purity materials (to reduce thermal noise) High power solid state lasers (to reduce shot noise) 7

GEO-HF • • • GEO 600: the first detector to pioneer monolithic fused silica

GEO-HF • • • GEO 600: the first detector to pioneer monolithic fused silica suspensions and advanced interferometric techniques (signal recycling) GEO-HF upgrade will bridge the gap until longer baseline detectors will reach better sensitivities in the k. Hz range => ensuring continued network operation Pioneering techniques such as squeezed light 30 W laser Improved thermal compensation MSR Squeezed light Class. Quantum Grav. , 29, 065001, 2012 GEO monolithic suspension LIGO G 1200724 8

GEO-HF Hardware GEO squeezed light source Improved thermal compensation at beamsplitter LIGO G 1200724,

GEO-HF Hardware GEO squeezed light source Improved thermal compensation at beamsplitter LIGO G 1200724, H. Wittel, Ph. D thesis Squeezed light (laser appears 1. 5 x more powerful) Light entering interferometer through the output port 9

GEO-HF Hardware GEO squeezed light source Improved thermal compensation at beamsplitter LIGO G 1200724,

GEO-HF Hardware GEO squeezed light source Improved thermal compensation at beamsplitter LIGO G 1200724, H. Wittel, Ph. D thesis Squeezed light (laser appears 1. 5 x more powerful) Light entering interferometer through the output port 10

GEO-HF Hardware Squeezed light (laser appears 1. 5 x more powerful) Nature Physics, Vol.

GEO-HF Hardware Squeezed light (laser appears 1. 5 x more powerful) Nature Physics, Vol. 7, p. 962– 965, 2011 Light entering interferometer through the output port 11

Advanced LIGO (a. LIGO) • • Seismic isolation Dual (Signal and Power) recycled Fabry-Perot

Advanced LIGO (a. LIGO) • • Seismic isolation Dual (Signal and Power) recycled Fabry-Perot interferometer 40 kg test mass LIGO lab a. LIGO ring heater 180 W laser 4 km Suspension Power and Signal recycling Cavities LIGO M 060056 https: //www. advancedligo. mit. edu/ – Active seismic isolation – QUAD suspension – Fused silica lower stage – Thermal compensation (ring heater and CO 2 laser) 12

a. LIGO Hardware Active seismic isolation 10 isolation at 0. 16 m. Hz 1

a. LIGO Hardware Active seismic isolation 10 isolation at 0. 16 m. Hz 1 000 isolation at 10 Hz Actuate 180 W a. LIGO laser (97% in TEM 00) LIGO G 1200982 https: //www. advancedligo. mit. edu/ k b 13

a. LIGO Hardware Initial LIGO (10. 7 kg) Hydroxide catalysis bonding a. LIGO lower

a. LIGO Hardware Initial LIGO (10. 7 kg) Hydroxide catalysis bonding a. LIGO lower glass stage (40 kg) Ultra-low loss final stage for lowering thermal noise test mass CO 2 laser welding ( 34 cm) Mirrors are suspended from 7 isolation stages: – 1 external hydraulic actuator – 2 active isolation – QUAD (x 4) pendulum Class. Quantum Grav. , 29, 035003, 2012 Rev. Sci Instrum. , 82, 011301, 2011 Fibre pulling with a CO 2 laser 14

a. LIGO Installation Seismic isolation system Cartridge installation at LIGO Hanford Chamber cleaning QUAD

a. LIGO Installation Seismic isolation system Cartridge installation at LIGO Hanford Chamber cleaning QUAD Suspension at LIGO Hanford LIGO G 1200982 https: //ligoimages. mit. edu/ 15

a. LIGO Timeline a. LIGO design curves (LIGO G 1200982) LIGO G 1201105 •

a. LIGO Timeline a. LIGO design curves (LIGO G 1200982) LIGO G 1201105 • There is significant ongoing activity at the Hanford and Livingston sites • Currently conducting: – a 4 km long single arm at LHO (Hanford) – a vertex test at LLO (Livingston) comprising everything except end test masses • Installation complete date: LLO (May 2013) and LHO (September 2013) • Acceptance (2 -hour lock) date: LLO (April 2014) and LHO (May 2014) 16

a. LIGO Timeline LIGO M 060056 a. LIGO layout LIGO G 1201105 • There

a. LIGO Timeline LIGO M 060056 a. LIGO layout LIGO G 1201105 • There is significant ongoing activity at the Hanford and Livingston sites • Currently conducting: – a 4 km long single arm at LHO (Hanford) – a vertex test at LLO (Livingston) comprising everything except end test masses • Installation complete date: LLO (May 2013) and LHO (September 2013) • Acceptance (2 -hour lock) date: LLO (April 2014) and LHO (May 2014) 17

Advanced VIRGO • • Dual (Signal and Power) recycled Fabry-Perot interferometer 40 kg test

Advanced VIRGO • • Dual (Signal and Power) recycled Fabry-Perot interferometer 40 kg test masses VIRGO test mass Bizouard, MG 11, Berlin 2 100 W laser Vacuum system Power and Signal recycling Cavities https: //tds. ego-gw. it/ql/? c=8940, (VIR– 0128 A– 12) Fig 1. 1 – Multi-stage nested pendulums for low seismic attenuation – Fused silica lower stage – Thermal compensation (ring heater and CO 2 laser) 18

Advanced VIRGO Hardware G 1201017 • 100 W rod amplifiers under test (NICE) •

Advanced VIRGO Hardware G 1201017 • 100 W rod amplifiers under test (NICE) • Fused silica fibre pulling • Fused silica fibre puller/welder • 20 kg mirror for VIRGO+ (Ad. V is twice as thick) VIR-0312 A-12/LIGO-G 1201017 http: //www. fisica. unipg. it/vocca/MG 12. pdf 19

Advanced VIRGO Hardware • Compact 2 -stage isolator for auxiliary optics • a. VIRGO

Advanced VIRGO Hardware • Compact 2 -stage isolator for auxiliary optics • a. VIRGO mirror test stand • 6 stage “super attenuator” VIR-0312 A-12/LIGO-G 1201017 http: //csi. in 2 p 3. fr/CR-transparents/01%20 Flaminio_Plans%20 for%20 Advanced%20 Virgo. pdf 20

Advanced VIRGO Timeline Flaminio, MG 12 LIGO G 1201105 • The Advanced Virgo Technical

Advanced VIRGO Timeline Flaminio, MG 12 LIGO G 1201105 • The Advanced Virgo Technical Design Report was released in April 2012 • There is significant ongoing activity at the Cascina site • Installation/integration will be completed in the first half of 2015 • Commissioning will begin before the end of the installation – laser and input optics – 3 km cavity http: //csi. in 2 p 3. fr/CR-transparents/01%20 Flaminio_Plans%20 for%20 Advanced%20 Virgo. pdf 21

Upgrades to Advanced detectors • In 2011 the LIGO Scientific Collaboration initiated a study

Upgrades to Advanced detectors • In 2011 the LIGO Scientific Collaboration initiated a study of upgrade scenarios: – What R&D is needed over the next few years? – When do we need to be ready for the upgrades – Can we do the upgrades in an incremental way? – How much improvement is possible? • Three design teams (Red/Green/Blue) working on: – Room temperature upgrades – Cryogenic upgrades – Heavier (150 kg) test masses – New optical coatings – Low frequency subtraction of gravity – Alternative operating wavelengths (1064 nm vs 1550 nm) – Combined low/high frequency cold/warm interferometers: Xylophone configuration 22

LIGO-G 1200920 LIGO-G 1200031 LIGO-G 1200573 Upgrades to Advanced detectors 23

LIGO-G 1200920 LIGO-G 1200031 LIGO-G 1200573 Upgrades to Advanced detectors 23

LIGO-G 1200920 LIGO-G 1200031 LIGO-G 1200573 Upgrades to Advanced detectors • For more details

LIGO-G 1200920 LIGO-G 1200031 LIGO-G 1200573 Upgrades to Advanced detectors • For more details on KAGRA and ET please see the talks: • 12: 10 -12: 40: KAGRA project: status report (T. Kajita) • 14: 00 -14: 30 Einstein Telescope (ET) project (H. Lueck) • 14: 30 -15: 00 KAGRA and ET (K. Somiya) • Workpackage meetings 3 rd/4 th October 24

Summary • • There is a significant worldwide effort to install and commission the

Summary • • There is a significant worldwide effort to install and commission the hardware necessary for Advanced gravitational wave detectors Fused silica suspension, active seismic isolation and squeezed light are being used to improve sensitivity by a factor of 10 over the observing band of 10 Hz-10 k. Hz • Advanced network will be operational in 2014/2015 • Observing schedule for LSC detectors: • 2015: 3 month run with LLO/LHO at 60 Mpc range. Advanced VIRGO in commissioning at 40 Mpc with the opportunity to join the data run • 2016 -2017: 6 month run with LLO/LHO at 100 Mpc and Advanced VIRGO at 40 Mpc • 2017 -2018: 6 month run with LLO/LHO at 140 Mpc and Advanced VIRGO at 70 Mpc • 2019+: LLO/LHO at full sensitivity (200 Mpc) and Advanced VIRGO at 100 Mpc • 2022+: LLO/LHO, Advanced VIRGO and LIGO India at full sensitivity • From 2015 there is the opportunity for the Advanced detectors to open the gravitational wave window on the Universe. LIGO G 1201105 25