the future of virgo
TRANSCRIPT
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THE FUTURE OF VIRGOBEYOND ADVANCED DETECTORS
Gianluca GemmeINFN Genova
for the Virgo Collaboration
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GW150914
Riunione Direttori 28/04/2016 Gianluca Gemme 2
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DEVIATION OF PNCOEFFICIENTS FROM GR
Post Newtonian formalismPhase of the inspiral waveform -> power series in Nominal value predicted by GRAllow variation of the coefficients
-> Is the resulting waveformconsistent with data ?
No evidencefor violations of GR
arXiv:1602.03841Riunione Direttori 28/04/2016 Gianluca Gemme 3
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UPPER BOUND ONTHE GRAVITON MASS
If gravitational waves have a modified dispersion relationFindings : at 90 % confidence,
or equivalently
arXiv:1602.03841Riunione Direttori 28/04/2016 Gianluca Gemme 4
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WHAT ADVANCED DETECTORSWILL ACHIEVE?
Detections!− BBH, BNS, possibly stellar collapse
Measure the ratesA step forward in sensitivity is needed for having precise
characterization of the sources and for complementing EM observations(Astro)physical modelling would require a large sample of
events: different spins, mass ratiosNS structure characterization (if ellipticities not too low≥10-8): might need to go beyond 2G
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WHAT FUNDAMENTAL SCIENCE FOR 2G+/3G DETECTORS?
Extremes of physics− structure and dynamics of neutron stars (EoS)− physics of extreme gravity
Black holes through cosmic history− formation, evolution and growth of black holes and their
propertiesExplosive phenomena
− gamma ray bursts, gravitational collapse and supernovae, flaring and bursting neutron stars
All these will require many events at high SNR
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ADVANCED VIRGOWHAT NEXT?
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ADVANCED DETECTORSTIMELINE
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O1 O2 O3
Gianluca Gemme
LIGO
VIRGO
2015 2016 2017 2018 2019 2020 2021 2022 2023 2024 2025
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HOW MANY BBH MERGER IN FUTURE DATA?
arXiv:1602.03842Riunione Direttori 28/04/2016 Gianluca Gemme 9
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EXPECTATIONS FOR FUTURE RUNS
Probability of observing N > 0 (blue)N > 5 (green)N > 10 (red)N > 35 (purple) highly significant events, (FARs <1/century)as a function of surveyedtime-volume
2016-17 2017-182015
arXiv:1602.03842Riunione Direttori 28/04/2016 Gianluca Gemme 10
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ADV SENSITIVITY EVOLUTION
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PR, 25W. BNS range: 107 MpcDual rec., 125W, tuned SR. BNS range: 132 MpcDual rec., 125W detuned SR. BNS range: 145 MpcVirgo+ BNS range: 12 Mpc
Gianluca Gemme
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ADVANCED VIRGO: WHAT NEXT?
In the upcoming (~10) years our target is to maximize the scientific outcome of the detector− Need do maximize data taking− Need to minimize downtime
SHORT TERM (~2017-2021): towards design sensitivity− high power laser, signal recycling, frequency independent squeezing− R&D for gravity noise cancellation
MEDIUM TERM (~2021-2025):the best we can do in the current infrastructure − frequency dependent squeezing, gravity noise cancellation− better coatings, larger beams, heavier masses
LONG TERM (>2025)a new infrastructure− increased length (~10km), underground, cryogenics, laser wavelength, new
materials, topology, xylophone, …
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SHORT TERM(~2017-2021)towards design sensitivity
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INITIAL ADV SENSITIVITY
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BSN range ~100 Mpc
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REACHING ADVDESIGN SENSITIVITY
AdV baseline design− Signal recycling− High power laser− Tiltmeters (robustness at low
freq)Frequency independent
squeezing between O2–O3 (~2017-2018)− High frequency sensitivity
improvement− Intermediate step towards
frequency dependent squeezing
− Risk mitigation− Total investment ~1M€
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BNS range ~145 Mpc
Gianluca Gemme
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NEWTONIAN NOISE
16Credit M.Lorenzini
Virgo and advanced Virgo seismic filtering is already close to the top of the possible performancesGravity gradient noise bypasses the
seismic filtering
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NEWTONIAN NOISE IN ADV
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• NN noise could limit the AdV sensitivity during high seismic activity days
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REACHING ADVDESIGN SENSITIVITYAdV baseline design
− Signal recycling− High power laser− Tiltmeters (robustness at low
freq)Frequency independent
squeezing between O2–O3 (~2017-2018)− High frequency sensitivity
improvement− Intermediate step towards
frequency dependent squeezing
− Risk mitigation− Total investment ~1M€
R&D on NN− Site characterization− Coherent noise detection− Cost ~150k€
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BNS range ~145 Mpc
Gianluca Gemme
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MEDIUM TERM(~2021-2025)beyond design sensitivity……the best we can do in the current infrastructure
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FREQUENCY DEPENDENT SQUEEZING
𝜎𝜎~ 𝑃𝑃𝑐𝑐
𝜎𝜎~ �1 𝑃𝑃𝑐𝑐
Amplitude fluctuation
phase fluctuation
CREDIT: M. Punturo
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REALIZING A FREQUENCY-DEPENDENT SQUEEZE ANGLE
Filter cavitiesDifficulties
− Low losses−Highly detuned−Multiple cavities
• Conventional interferometers • Kimble, Levin, Matsko, Thorne, and Vyatchanin,
Phys. Rev. D 65, 022002 (2001).• Signal tuned interferometers
• Harms, Chen, Chelkowski, Franzen, Vahlbruch, Danzmann, and Schnabel, gr-qc/0303066 (2003).
filter cavities
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ADV+Quantum noise
− Frequency dependent squeezing(possibly after O3 ~2018-2019)
− Total investment ~2.5M€Newtonian noise
− NN cancellation ~350k€Thermal noise
− Installation of ‘better’ mirrors (lower loss, lower scatter; lower coating thermal noise)
− Increasing mirror mass (x2)− Larger beams− R&D ~1M€
Goal: 50% improvement in BNS horizon…clearly can keep us busy till 2025
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IMPROVING THE ROBUSTNESSANTHROPOGENIC NOISE REDUCTION
Moving machinery out of the experimental buildings (mainly HVAC equipment, pumps,…)
Improvement of air distributionduct paths
Already proposed in AdV –excluded for financial reasons
Cost estimate: ~500k€
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AdV uses marginally stablerecycling cavities
Potential problem @high laserpower and if larger beams areused (thermally inducedaberrations)
Upgrade of the thermalcompensation system
Long stable cavities proposed in AdV in 2010 and excluded for financial reasons
Not negligible impact on science
Long cavities: cost/time estimate (infrastructures, buildings, system) for 180m PR –80m SR ~8M€/two years
For TCS upgrade ~500k€/three years
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IMPROVING THE ROBUSTNESSCOPING WITH THERMALLY INDUCED ABERRATIONS
Gianluca Gemme
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LONG TERM (>2025)a new infrastructure
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EINSTEIN TELESCOPEDesign study of ET funded by the European Commission
under FP7− interest primarily focused on the Infrastructure rather than on the
detector and its technologies− The infrastructure should no limit the sensitivity of the future hosted
detectors • Size• Environmental noises
(seismic and NN)− ET absorbed and developed many
concepts in GW detectors:• Underground and cryo-compatible
facility, pioneered in Japan by CLIO and KAGRA
• Triangular geometry, concept used in LISA
• Xylophone configuration
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AdVET-D
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TIMELINE FOR THIRD GENERATION
Need to have a compelling argument – our data, and physics/astronomy customers, grow with time to motivate a ~bn € expense
Actions to be put in place:− Need to maintain the competences, renew and expand the INFN leadership− Need to attract partners at the National and European level (credibility, excellence)− ERIC@EGO is a fundamental tool
Timing:− Infrastructure: technical design must start now (ESFRI roadmap)− Site selection 2021-2022; construction starts 2023− Detector: timing may be limited by R&D bearing fruit, full-scale prototype tests,…
guess ~6 years from now− Detector: end-2022 review of concept - go-ahead mid-2023− Commissioning of new Observatory: end of next decade
Adequate funding for R&D is needed soon (motivated by the science to date). Ballpark figure ~200M€, globally
− Some actions already in place: IGRAINE, PIRE
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2020
2016
2017
2018
2019
2021
2022
2023
2024
2025
2026
2027
2028
2029
2030
2031
2032
AdV+ R&D
R&D Installation Commissioning Data taking Other
aLIGO A+A+/Voyager R&D
Voyager
Cosmic Explorer R&D CE site&detector installation
AdV AdV+
ESFRIRoadmap
ET R&DET Detector
Technical Design
ET Observatory & Detector funding
ET site construction - detector installation & commissioning
ET InfrastructureTechnical Design
KAGRA
LIGO India
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CONCLUSIONS Three-phase scenario
− Short term (~2017-2019) – well defined technologies. In some cases (squeezing) need to finalize design soon for the integration in the existing infrastructure
− Medium term (~2025) – R&D effort already started, needs to be finalized. Further detections will tell us where to concentrate our efforts
− Total investment ~5M€ (R&D for AdV+ partially preparatory for 3G)
− Long term (>2025) - some infrastructure requirements already established. Needs a focused, coordinated effort (worldwide) to finalize some key concepts:
• Topology• Underground/on surface• 3G Network/mixed 3G-2G• Working temperature/Materials• New technologies
− Coordinated R&D funding must start now: IGRAINE (Europe), PIRE (USA)• Need to attract partners at the National and European level (ERIC)
− Total investment ≥ 1B€ (~200M€ in R&D)
Vision document almost finalized with details on technical requirements, implementation timeline and cost
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