Advanced LIGO project status: getting ready to listen to the universe Giacomo Ciani for the LIGO...
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Transcript of Advanced LIGO project status: getting ready to listen to the universe Giacomo Ciani for the LIGO...
Advanced LIGO project status:getting ready to listen to the universe
Giacomo Cianifor the
LIGO Scientific Collaboration
LIGO- G1401371
2Giacomo Ciani for the LSC LIGO-G1401371
• 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 Lauderdale
Overview
3Giacomo Ciani for the LSC LIGO-G1401371
• 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 Lauderdale
FAQs on gravitational waves
ΔL/L ~ 10-21
Giacomo Ciani for the LSC LIGO-G1401371 4
A whole orchestra on the stage
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
10-9 Hz 10-4 Hz 100 Hz 103 Hz
Relic radiationCosmic Strings
Supermassive BH Binaries
BH and NS Binaries
Binaries coalescences
Extreme Mass RatioInspirals
Supernovae
Spinning NS
??
???
?
10-16 Hz
Giacomo Ciani for the LSC LIGO-G1401371 5
And a microphone for everyone
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
10-9 Hz 10-4 Hz 100 Hz 103 Hz
Relic radiationCosmic Strings
Supermassive BH Binaries
BH and NS Binaries
Binaries coalescences
Extreme Mass RatioInspirals
Supernovae
Spinning NS
??
???
?
10-16 HzInflation Probe Pulsar timing Space detectors Ground interferometers
Giacomo Ciani for the LSC LIGO-G1401371 6
And a microphone for everyone
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
10-9 Hz 10-4 Hz 100 Hz 103 Hz
Relic radiationCosmic Strings
Supermassive BH Binaries
BH and NS Binaries
Binaries coalescences
Extreme Mass RatioInspirals
Supernovae
Spinning NS
??
???
?
10-16 HzInflation Probe Pulsar timing Space detectors Ground interferometers
See Laleh Sadeghian talk right after this
See Guido Mueller talk on Sunday
7Giacomo Ciani for the LSC LIGO-G1401371
DL
P PD
• Inherently differential• Broad band• Long baseline
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Laser interferometers and GWs
Laser
“+” polarized GW propagating
orthogonal to the screen
Simulated action!Not a real
gravitational wave
Phase: f = 4p (Lx – Ly) /l ~ DLPower: PPD = PBS sin2f
8Giacomo Ciani for the LSC LIGO-G1401371
Caltech
MIT
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Enhanced LIGO
Laser
4 km4 km
Laser:30W - 1064nm
Output mode cleaner:Reject junk light to clean signal on photodetector
DC Homodyne Readout
30kW30kW
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
2 Locations3 interferometers
9Giacomo Ciani for the LSC LIGO-G1401371Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Enhanced LIGO performance
Laser
4 km4 km
Laser:30W - 1064nm
Output mode cleaner:Reject junk light to clean signal on photodetector
DC Homodyne Readout
30kW30kW
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
102
103
10-23
10-22
Frequency [Hz]
h(f)
[H
z-1/2
]
NS-NS range: 15->20 Mpc
S5 – Initial LIGO best c
urve
S6 – Enhanced LIGO best curve
10Giacomo Ciani for the LSC LIGO-G1401371Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Enhanced LIGO
Laser
4 km4 km
Laser:30W - 1064nm
Output mode cleaner:Reject junk light to clean signal on photodetector
DC Homodyne Readout
30kW30kW
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
102
103
10-23
10-22
Frequency [Hz]
h(f)
[H
z-1/2
]
Factor 2-3 improvement
at high frequencies.NS-NS range: 15->20 Mpc
S5 – Initial LIGO best c
urve
S6 – Enhanced LIGO best curve
SHUT DOWN Q4/2010
What have we been doing since?
11Giacomo Ciani for the LSC LIGO-G1401371Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Data analysis and publications
• S5/S6 data have produced more than 30 papers in the last 3 years:– See http://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
12Giacomo Ciani for the LSC LIGO-G1401371Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Advanced LIGO designInput Laser Mirrors Topology Readout SensitivitySuspensions
iLIGO 10W(10 kW arm) 10 kg Power-Recycled
Fabry-PerotRF
etherodyne 3 10-23 Hz-1/2Single pendulum(LF cutoff ~40 Hz)
aLIGO 180W(>700 kW arm) 40 kg Dual-Recycled
Fabry-PerotDC
homodyne5 10-24 Hz-1/2
(tunable)Quadruple pendulum
(LF cutoff ~10 Hz)
Seismic isolation
Passive
Active
Routine detection not certain, but plausible!
• Design limited by fundamental noise: quantum, thermal• Improvement at low frequency (from 40 to 10 Hz)• 10x strain sensitivity 1000x observable volume (=rates)
13Giacomo Ciani for the LSC LIGO-G1401371
• The plan: staggered installation– LLO/LHO to build and
commission different subsystem in parallel
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Building Advanced LIGONow!
14Giacomo Ciani for the LSC LIGO-G1401371
• 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 Lauderdale
Building Advanced LIGONow!
15Giacomo Ciani for the LSC LIGO-G1401371
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 Lauderdale
Building Advanced LIGONow!
LHO ETMsin 532 nm and
1064 nm laser light
16Giacomo Ciani for the LSC LIGO-G1401371
• Commissioning work much faster than iLIGO:– Building on the experience of iLIGO– Better subsystems modeling and testing
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
The progress toward a science run
17Giacomo Ciani for the LSC LIGO-G1401371
• Commissioning work much faster than iLIGO:– Building on the experience of iLIGO– Better subsystems modeling and testing
• First full IFO lock at Livingston: May 27th, 2014• Milestone 2+ hours full IFO lock May 29th, 2014
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
The progress toward a science run
18Giacomo Ciani for the LSC LIGO-G1401371
• Commissioning work much faster than iLIGO:– Building on the experience of iLIGO– Better subsystems modeling and testing
• First full IFO lock at Livingston: May 27th, 2014• Milestone 2+ hours full IFO lock May 29th, 2014
– Rapid improvement in the instrument noise (measured by NS-NS range)
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
The progress toward a science run
19Giacomo Ciani for the LSC LIGO-G1401371
• Commissioning work much faster than iLIGO:– Building on the experience of iLIGO– Better subsystems modeling and testing
• First full IFO lock at Livingston: May 27th, 2014• Milestone 2+ hours full IFO lock May 29th, 2014
– Rapid improvement in the instrument noise (measured by NS-NS range)
• LHO first full lock on December 3rd, 2014
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
The progress toward a science run
Advanced LIGO broadband
CALIBRATION IS PRELIMINARY
20Giacomo Ciani for the LSC LIGO-G1401371
• 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 Lauderdale
Many challenges ahead
21Giacomo Ciani for the LSC LIGO-G1401371
• 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 Lauderdale
The near future
Currently investigating loss (cleanliness?) issues
We could be listening to the universe!
22Giacomo Ciani for the LSC LIGO-G1401371
• Will need to find a balance between commissioning and observation time• A possible scenario:
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Balancing times
2015: > 3 month run, 40 - 80 MpcPossible Detection
2016-17: > 6 month run, 80 - 120 MpcLikely Detection
2017-18: > 9 month run, 120 - 170 MpcMulitple Detections
Initial LIGO, 15 Mpc
23Giacomo Ciani for the LSC LIGO-G1401371Dec 19th, 2014 – CGC Conference in Fort Lauderdale
…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 ~ √PLaser
Photon Statistics SNR ~ 1/√PLaser
DissipativeDynamics
Giacomo Ciani for the LSC LIGO-G1401371 24
In the meanwhile around the world…
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
aLIGO Hanford~2015
aLIGO Livingston~2015
Giacomo Ciani for the LSC LIGO-G1401371 25
In the meanwhile around the world…
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
aLIGO Hanford~2015
aLIGO Livingston~2015
LIGO India2022?
?
26Giacomo Ciani for the LSC LIGO-G1401371
• 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 2022Dec 19th, 2014 – CGC Conference in Fort Lauderdale
LIGO India
Giacomo Ciani for the LSC LIGO-G1401371 27
In the meanwhile around the world…
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
aLIGO Hanford~2015
aLIGO Livingston~2015
AdVIRGO~2016
LIGO India2022?
?
28Giacomo Ciani for the LSC LIGO-G1401371
• 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 Lauderdale
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
Giacomo Ciani for the LSC LIGO-G1401371 29
In the meanwhile around the world…
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
aLIGO Hanford~2015
aLIGO Livingston~2015
AdVIRGO~2016
KAGRA2020
LIGO India2022?
?
30Giacomo Ciani for the LSC LIGO-G1401371
• 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 Lauderdale
Other detectors: KAGRA
• Facilities almost completed
• Three stages plan• iKAGRA (~4 Mpc)
by 2016• Intermediate (~20
Mpc) by 2018• Final bKAGRA (140
Mpc) by 2020
Giacomo Ciani for the LSC LIGO-G1401371 31
In the meanwhile around the world…
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
aLIGO Hanford~2015
aLIGO Livingston~2015
AdVIRGO~2016
GEO600Now!
KAGRA2020
LIGO India2022?
?
32Giacomo Ciani for the LSC LIGO-G1401371
• 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 Lauderdale
Other detectors: GEO HF
Giacomo Ciani for the LSC LIGO-G1401371 33
In the meanwhile around the world…
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
aLIGO Hanford~2015
aLIGO Livingston~2015
AdVIRGO~2016
GEO600Now!
KAGRA2020
Increased detection confidence (coincidence runs)
Reduced downtime
Enhanced sky coverage Better and faster source localization
More reliable source parameters estimation
LIGO India2022?
?
34Giacomo Ciani for the LSC LIGO-G1401371
• 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 Lauderdale
Summary
35Giacomo Ciani for the LSC LIGO-G1401371Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Additional slides
Giacomo Ciani for the LSC LIGO-G1401371 37
Who’s making noise?
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Laser
Amplitude and frequency noise
Residual gas
Seismic noise
Shot noise
Radiation pressure
Giacomo Ciani for the LSC LIGO-G1401371 38
iLIGO strain sensitivity
Dec 19th, 2014 – CGC Conference in Fort Lauderdale
Size of anH nucleus!
NowInauguration First Lock Full Lock all IFO
4K strain noise
@150 Hz [Hz-1/2]
3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4
1999 2000 2001 2002 2003 2004 2005 2006
1 2 3 4
2007
1 2 3 4
2008
1 2 3 4
2009
1 2 3 4
2010
1 2 3 4
2011
Design Sensitivity
10-17 10-18 10-20 10-21 10-22 3x10-23
Enhanced LIGO
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