1. Advanced LIGO project status: getting ready to listen to the universe Giacomo Ciani for the LIGO Scientific Collaboration LIGO- G1401371

2. GW and laser interferometers Building and commissioning Advanced LIGO Near and far future in LIGO The GW detectors network Summary Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Overview 2

3. Who says GWs exist? – Predicted by General Relativity – Hulse-Taylor: indirect evidence by binary pulsar spin- down (Nobel Prize 1993) What are gravitational waves? – Ripple in space-time travelling at the speed of light Who creates GWs? – Mass distributions changing in a non-spherically symmetric way (e.g. binary systems) What is their effect? – Relative change in lengths orthogonal to propagation direction – The effect is VERY small: typical size Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 FAQs on gravitational waves 3

4. A whole orchestra on the stage Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 10 -9 Hz10 -4 Hz10 0 Hz10 3 Hz Relic radiation Cosmic Strings Supermassive BH Binaries BH and NS Binaries Binaries coalescences Extreme Mass Ratio Inspirals Supernovae Spinning NS 10 -16 Hz 4

5. And a microphone for everyone Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 10 -9 Hz10 -4 Hz10 0 Hz10 3 Hz Relic radiation Cosmic Strings Supermassive BH Binaries BH and NS Binaries Binaries coalescences Extreme Mass Ratio Inspirals Supernovae Spinning NS 10 -16 Hz Inflation Probe Pulsar timing Space detectorsGround interferometers 5

6. And a microphone for everyone Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 10 -9 Hz10 -4 Hz10 0 Hz10 3 Hz Relic radiation Cosmic Strings Supermassive BH Binaries BH and NS Binaries Binaries coalescences Extreme Mass Ratio Inspirals Supernovae Spinning NS 10 -16 Hz Inflation Probe Pulsar timing Space detectorsGround interferometers 6

7. LL P PD Inherently differential Broad band Long baseline Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Laser interferometers and GWs Laser “+” polarized GW propagating orthogonal to the screen Phase:  = 4  (L x – L y ) / ~  L Power: P PD = P BS sin 2  7

8. Caltech MIT Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Enhanced LIGO Laser 4 km Laser: 30W - 1064nm Output mode cleaner: Reject junk light to clean signal on photodetector DC Homodyne Readout 30kW Power Recycling Mirror: Enhances effective input power Input Mode Cleaner: Cleans the laser mode and stabilize the frequency Arm cavities: increase the number of photons probing the GW strain 8 2 Locations 3 interferometers

9. Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Enhanced LIGO performance Laser 4 km Laser: 30W - 1064nm Output mode cleaner: Reject junk light to clean signal on photodetector DC Homodyne Readout 30kW Power Recycling Cavity: enhances effective input power Input Mode Cleaner: Cleans the laser mode and stabilize the frequency Arm cavities: increase the number of photons probing the GW strain S6 – Enhanced LIGO best curve 9

10. Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Enhanced LIGO Laser 4 km Laser: 30W - 1064nm Output mode cleaner: Reject junk light to clean signal on photodetector DC Homodyne Readout 30kW Power Recycling Cavity: enhances effective input power Input Mode Cleaner: Cleans the laser mode and stabilize the frequency Arm cavities: increase the number of photons probing the GW strain S6 – Enhanced LIGO best curve 10

11. Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Data analysis and publications 11 S5/S6 data have produced more than 30 papers in the last 3 years: – See http://www.ligo.org/science/outreach.phphttp://www.ligo.org/science/outreach.php Several papers use joint data runs from LIGO and VIRGO Many of these papers involve other astronomy experiments/collaborations (multimessenger astronomy): – SWIFT – InterPlanetary Network – ANTARES – NINJA – Ground based optical, X-ray and radio telescopes – … S5 data has gone public: you can start you own search now! losc.ligo.org

12. Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Advanced LIGO design Input Laser MirrorsTopology ReadoutSensitivity Suspensions iLIGO 10W (10 kW arm) 10W (10 kW arm) 10 kg Power-Recycled Fabry-Perot Power-Recycled Fabry-Perot RF etherodyne 3 10 -23 Hz -1/2 Single pendulum (LF cutoff ~40 Hz) Single pendulum (LF cutoff ~40 Hz) aLIGO 180W (>700 kW arm) 180W (>700 kW arm) 40 kg Dual-Recycled Fabry-Perot Dual-Recycled Fabry-Perot DC homodyne 5 10 -24 Hz -1/2 (tunable) Quadruple pendulum (LF cutoff ~10 Hz) Quadruple pendulum (LF cutoff ~10 Hz) Seismic isolation Passive Active Design limited by fundamental noise: quantum, thermal Improvement at low frequency (from 40 to 10 Hz) 10x strain sensitivity  1000x observable volume (=rates) 12

13. The plan: staggered installation – LLO/LHO to build and commission different subsystem in parallel Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Building Advanced LIGO 13 Now!

14. The plan: staggered installation – LLO/LHO to build and commission different subsystem in parallel Installation now complete: – Livingston: May 2014 – Hanford: August 2014 Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Building Advanced LIGO 14 Now!

15. Test mass coating pattern The plan: staggered installation – LLO/LHO to build and commission different subsystem in parallel Installation now complete: – Livingston: May 2014 – Hanford: August 2014 Not without difficulties! – Cleanliness – Optical coatings – Vacuum system – … Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Building Advanced LIGO 15 Now! LHO ETMs in 532 nm and 1064 nm laser light

16. Commissioning work much faster than iLIGO: – Building on the experience of iLIGO – Better subsystems modeling and testing Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 The progress toward a science run 16

17. Commissioning work much faster than iLIGO: – Building on the experience of iLIGO – Better subsystems modeling and testing First full IFO lock at Livingston: May 27 th, 2014 Milestone 2+ hours full IFO lock May 29 th, 2014 Milestone 2+ hours full IFO lock May 29 th, 2014 Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 The progress toward a science run 17

18. Commissioning work much faster than iLIGO: – Building on the experience of iLIGO – Better subsystems modeling and testing First full IFO lock at Livingston: May 27 th, 2014 Milestone 2+ hours full IFO lock May 29 th, 2014 Milestone 2+ hours full IFO lock May 29 th, 2014 – Rapid improvement in the instrument noise (measured by NS-NS range) Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 The progress toward a science run 18

19. Commissioning work much faster than iLIGO: – Building on the experience of iLIGO – Better subsystems modeling and testing First full IFO lock at Livingston: May 27 th, 2014 Milestone 2+ hours full IFO lock May 29 th, 2014 Milestone 2+ hours full IFO lock May 29 th, 2014 – Rapid improvement in the instrument noise (measured by NS-NS range) LHO first full lock on December 3 rd, 2014 Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 The progress toward a science run Advanced LIGO broadband 19

20. DAC major transition glitch TM cleanliness issues at LHO TM Charging: – Fluctuating charge on Test Masses – Developing discharge system based on ionizer – But, charge comes back… ion pumps? Green light? Suspected parametric instability observed at LLO: – Interaction between laser field higher order modes and optics acoustic modes – Can induce resonances high enough to break IFO lock What’s coming next? Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Many challenges ahead 20

21. Engineering run (ER6) ongoing at LLO Working towards 2 hours full lock at Hanford Ongoing commissioning First coincident Engineering Run: early 2015? First coincident Observation Run: late 2015? Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 The near future Currently investigating loss (cleanliness?) issues We could be listening to the universe! 21

22. Will need to find a balance between commissioning and observation time A possible scenario: Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Balancing times 2015: > 3 month run, 40 - 80 Mpc Possible Detection 2015: > 3 month run, 40 - 80 Mpc Possible Detection 2016-17: > 6 month run, 80 - 120 Mpc Likely Detection 2016-17: > 6 month run, 80 - 120 Mpc Likely Detection 2017-18: > 9 month run, 120 - 170 Mpc Mulitple Detections 2017-18: > 9 month run, 120 - 170 Mpc Mulitple Detections Initial LIGO, 15 Mpc 22

23. Dec 19th, 2014 – CGC Conference in Fort Lauderdale23Giacomo Ciani for the LSC LIGO-G1401371 …and beyond R&D for (minor) upgrades to aLIGO (before 2020?): – Advanced (crystalline) optical coatings – squeezed light, filter cavities – longer suspensions Consolidating ideas and designs for major upgrades (using current facilities): – Cryogenics – silicon optics – 1550 nm lasers – Seismometers array for Newtonian noise subtraction – Straw man design study Brainstorming about next generation (new facilities needed) Photon Statistics  SNR ~ √P Laser Photon Statistics  SNR ~ 1/√P Laser Dissipative Dynamics

24. In the meanwhile around the world… Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 aLIGO Hanford ~2015 aLIGO Livingston ~2015 24

25. In the meanwhile around the world… Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 aLIGO Hanford ~2015 aLIGO Livingston ~2015 LIGO India 2022? 25

26. Proposal: move one of the two Hanford detectors to India – LIGO to provide detector components, assistance for installation and commissioning – India to provide infrastructures, personnel and operations Advantages: – Improved sky localization – Reduced downtime Status: – Site selection reduced to 3 (final recommendation expected by spring 2015) – National Science Board cleared NSF to approve the project – Installment of new government in India halted approval process (could resume before the end of the year) If everything goes well, LIGO India could come online in 2022 Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 LIGO India 26

27. In the meanwhile around the world… Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 aLIGO Hanford ~2015 aLIGO Livingston ~2015 AdVIRGO ~2016 LIGO India 2022? 27

28. Located in Italy Operated by European Consortium 3 km arm length Similar design to aLIGO: – unique SuperAttenuator suspensions Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Advanced VIRGO 28 Subsystems commissioning under way: Laser delivering 45W IMC locked June 2014 Construction end: fall 2015 Could be ready for science run in 2016

29. In the meanwhile around the world… Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 aLIGO Hanford ~2015 aLIGO Livingston ~2015 AdVIRGO ~2016 KAGRA 2020 LIGO India 2022? 29

30. Located in Kamioka mines, Japan 3 km arm length Pioneering in next generation technologies: – Underground – Cryogenics – Alternative materials Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Other detectors: KAGRA 30 Facilities almost completed Three stages plan iKAGRA (~4 Mpc) by 2016 Intermediate (~20 Mpc) by 2018 Final bKAGRA (140 Mpc) by 2020

31. In the meanwhile around the world… Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 aLIGO Hanford ~2015 aLIGO Livingston ~2015 AdVIRGO ~2016 GEO600 Now! KAGRA 2020 LIGO India 2022? 31

32. Locate in Hannover, Germany Part of the LIGO collaboration 600 m baseline – Limited sensitivity at low frequencies Very high duty cycle Pioneers advanced techniques: – Squeezing – Signal recycling – Thermal compensation – Automation – More… The only listener until 2015! Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Other detectors: GEO HF 32

33. In the meanwhile around the world… Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 aLIGO Hanford ~2015 aLIGO Livingston ~2015 AdVIRGO ~2016 GEO600 Now! KAGRA 2020 Increased detection confidence (coincidence runs) Reduced downtime Enhanced sky coverage Better and faster source localization More reliable source parameters estimation LIGO India 2022? 33

34. The initial generation of GW interferometer has been a success (despite no detection) Advanced LIGO is progressing fast towards goal sensitivity: – Could be listening to the GW sky in less than a year! Other advanced GW detectors around the world to join 1-2 years after We expect/hope to be doing full fledged GW astronomy by the end of the decade! Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Summary 34

35. Dec 19th, 2014 – CGC Conference in Fort Lauderdale35Giacomo Ciani for the LSC LIGO-G1401371

36. Additional slides

37. Who’s making noise? Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Laser Amplitude and frequency noise Residual gas Seismic noise Shot noise Radiation pressure 37

38. iLIGO strain sensitivity Dec 19th, 2014 – CGC Conference in Fort LauderdaleGiacomo Ciani for the LSC LIGO-G1401371 Seismic noise (displacement): mechanical vibration of the ground transmitted to the mirror through the pendulum chain Suspension thermal (displacement): thermal agitation induce noise in mirror motion Shot noise (detection): random arrival of photons creates noise at high frequencies 38