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Home , Einstein Telescope, GEO600, GW190412

The Einstein-Telescope Listening to the murmurs of the Universe (Status and Prospects)

Harald Lück AEI Hannover Max-Planck Institute for Gravitational physics Leibniz Universität Hannover, 17.3.2021 Institute for Gravitational physics Content

• Gravitational waves • What are we talking about? • What have we detected so far? • What do we intend to measure?

aLIGO + KAGRA • GW Detectors • How do they work? • What have we got? aLIGO+ INDIA AdV+ • How to improve? aLIGO + 3G south • ! In 1916 Einstein predicted Gravitational Waves as a consequence of his Theory of

The problem is:

∆퐿 2 퐺 푑2푄 1 ℎ = = 퐿 푐4 푑푡2 푑 with Gravitational waves are ripples 2퐺 = ퟏퟎ−ퟒퟒ푠2푘𝑔−1푚−1 in space and time caused by changing 푐4 gravitational fields How big is DL caused by a ?

Effect of a gravitational wave on a length of 4km

h = h10= -22

Gravitational waves C.Carreau propagate –

at the : ESA

and cause Credit measurable changes in the distance between objects

“Plus” polarization “Cross” polarization The Gravitational Wave Spectrum

Cosmic Strings BH and NS Binaries Supernovae

Relic radiation Extreme Mass Ratio Inspirals

Supermassive BH Binaries Binaries coalescences Spinning NS

10-16 Hz 10-9 Hz 10-4 Hz 100 Hz 103 Hz Probe Pulsar timing Space detectors Ground based

Source Giles Hammond: Adapted from M. Evans (LIGO G1300662-v4); adapted by H. Lück Working principle of a GW Detector:

Credit: MIT/Caltech LIGO Laboratory Lots of external disturbances

Power lines

Molecule Humans crossing Laser beam

Seismic disturbance Wind/Weather Thermal Bath Quantum Back-Action noise

Magnetic fields Planes Lightning The advanced GW Network

Advanced LIGO Hanford, GEO600, 2011 2015

Advanced LIGO INDIA, 2024 Advanced Virgo 2016 KAGRA 2018 Advanced LIGO Livingston, 2015 Sensitivity improvement LIGO <-> aLIGO

11 “Observation of THE Detection Gravitational Waves from a GW150914 Binary Merger” 14. September Detection of a 2015 transient signal in 09:50:45 UTC both advanced LIGO = 11:50:45 CEST detectors • Breakthrough Prize fundamental Physics 3M$ • Shaw Prize in Astronomy 1.2 M$ Preise • Gruber Cosmology Prize 0.5 M$ • Kalvi Prize 1 M$ • OSA team engineering award • Niedersächsische Staatspreis 25 k€ • Wissenschaftspreis Behrens Stiftung 30k€ • Körber Preis 0.75 M€ • Otto Hahn Preis 50 k€Nobel Preis 2017 !

Presidents Medal of Royal Society of Edinburgh LVK Observation runs

Median O3a: LHO: 108MPc (1.64xO2) LLO: 135 MPc (1.53xO2) Virgo: 45 MPc (1.73XO2) GW150914

https://arxiv.org/pdf/2010.14527.pdf GW170817: A Binary merger

Electromagnetic follow-up

Led to largest astronomical observation campaign Localisation by Trilateration

Virgo, Cascina, Italy

LIGO, Livingston, LA

LIGO, Hanford, WA Slide: Stefan Hild (modified) LVK Observation runs

Median O3a: LHO: 108MPc (1.64xO2) LLO: 135 MPc (1.53xO2) Virgo: 45 MPc (1.73XO2) GW150914

https://arxiv.org/pdf/2010.14527.pdf O4 („not before June 2022“) O3aO3a O3bO3b

Observing plans and public alerts: https://www.ligo.org/scientists/GWEMalerts.php

Gravitationswellendetektionen

G2001862/public

- https://dcc.ligo.org/LIGO Coalescing binaries observed so far O1 – O3a

150M⊙

plot/index.html -

NS? BH?

LIGO-P2000061-v14 https://ligo.northwestern.edu/media/mass Source: Detection Highlights from O3a GW190425 - 2nd Astrophys. J. Lett. 892, L3 (2020)

• Only measured by two detectors (LLO and Virgo) • Poorer localisation compared to GW170817 1.61-2.52 M⊙ • No EM counterpart found 1.12-1.68 M⊙ • Unexpectedly heavy pair: total mass of 3.4+0.3 -0.1 M⊙ is 5σ from galactic mean

Image: T. Dietrich (Nikhef), S. Ossokine, A. Buonanno (MPI for Gravitational Physics), W. Tichy (Florida Atlantic University) and the CoRe-collaboration

22 Slide from David Wu, AEI GW190412 & GW190814 – the “odd couples” Phys. Rev. D 102, 043015 (2020) Astrophys. J. Lett. 896, L44 (2020)

• First detections of a large GW190412 mass imbalance, mass 24.4 – 34.7 M⊙ ratio (q ~ 0.28 and 0.11) 7.4 – 10.1 M • First evidence of higher ⊙

order GW modes. Dominant Higher quadrupole order • Additional info from multipoles higher order modes GW190814 allowed better parameter 22.2 – 24.3 M constraints ⊙ • GW190814: what was the smaller object? 2.50 – 2.67 M⊙

Images: N. Fischer et al. Max Planck Institute for Gravitational Physics, Simulating eXtreme project 23 Slide from David Wu, AEI GW190521 – the “big fish” [1] Phys. Rev. Lett. 125, 101102 (2020) [2] • Most massive system observed: objects (1) 85 and 66 M⊙ • Remnant intermediate mass black hole - first direct observation of IMBH • One or both components in the pair instability mass gap (50 - 120 M⊙)

Image: LIGO/Caltech/MIT/R. Hurt (IPAC)

24 Slide from David Wu, AEI, modified Sensitivities of the 2nd Generation

aLIGO ET Advanced LIGO GEO600, 2011 Voyager CE Hanford, 2015

Advanced LIGO INDIA, 2024 Advanced Virgo KAGRA 2018 2016 Advanced LIGO Livingston, 2015

Infrastructure will reach an end of lifetime and a limit in performance (self noise, size) → New infrastructures Design Pläne

2008 – 2011 Increase size 4km → 10 km

Advanced LIGO ET

4 km

10 km Cosmic Explorer will have 40 km arms → gain a factor 10 w.r.t. advanced LIGO

3 Detektoren in Dreiecksanordnung rel. Längenänderung : DL/L = 2% Noise Budget (aLIGO example)

Noise Sources:

▪ High Frequencies  ShotHigh laser Noisepower/squeezing ▪ Mid Frequencies  ShotSqueezing noise, rad. press. Noise EURegio  Thermal noise of Coatings Meuse-Rhine Better coatings/ cryogenic operation ▪ Low frequencies  Rad.Low Laser press. Power noise  SeismicBetter suspensions  ThermalLonger suspensions suspension noise  Newtonian noise  ControlNew control noisesignals

LIGO-T1800044-v3 Sensitivities of the 2nd Generation

aLIGO ET Current aLIGO Advanced LIGO GEO600, 2011 Voyager CE Hanford, 2015

Advanced LIGO INDIA, 2024 Advanced Virgo KAGRA 2018 2016 10x Advanced LIGO Livingston, 2015 10x

Infrastructure will reach an end of lifetime and a limit in performance (self noise, size) → New infrastructures Challenge: Low Frequency improvement factor Newtonian Noise

▪ The Virgo suspension is almost good enough for filtering the seismic disturbances and keeping the mirrors quiet enough  A longer suspension is needed to improve filtering at low frequencies

 Newtonian Noise circumvents this isolation chain

→ Go underground SEISMIC WAVE

Credit M.Lorenzini ET - Xylophone Concept

ET - LF ET – HF 300 K low-power, cryogenic high-power, room-temperature ET-HF: low-frequency detector high-frequency detector • High power laser • High circulating light power • Thermal compensation • Large test masses • New coatings • Frequency dependent squeezing

ET-LF: 10 – 20 K • Cryogenics • Seismic suspensions • Silicon (Sapphire) test masses • Large test masses • New coatings • New laser wavelength • Frequency dependent squeezing, Filter cavities ET Xylophone Sensitivity

ET - HF ET - LF

ET-LF ET-HF

ET Total ET – LF Subdividing the ET - HF task Detector Subsystems

ETMy Cryo Cold Cooler Vacuum link Chain

Ly tank

ITMy Mirror suspension chain LASER sideview L displayed only x for one mirror PR ITMx ETMx for clarity SR Control Faraday IMC Faraday Isolator Filter Cavity Colours for subsystems: Isolator Core optics, coatings Light sources Plot(data) Squeezer Quantum Enhancements Auxiliary optics Computer OMC Sensing Sensing and Control PD Seismic Isolation & Suspensions Cryogenics Cosmic Explorer (USA) Oberirdisch Empfindlichkeit 10x advanced Det. 2 Phasen Sensitivities in the 3G era

aLIGO+ KAGRA

aLIGO+ INDIA AdV+

aLIGO +

3G south/ NEMO Reaching for the „whole universe“…

Horizon distance CBC Sources throughout the universe

Credit: E. Hall (MIT) Slide layout: Sheila Rowan, modified 3G Gravitational Wave Science

Sub-slides credit: B. Sathyaprakash, Dawn III Workshop, https://wiki.ligo.org/LSC/LIGOworkshop2017/WebHome Einstein Telescope Where are we? ESFRI Roadmap

Proposal submitted by: • Italy (Lead Country) • Netherlands • Belgium • Spain • Poland

40 Slide: Michele Punturo 2020 ET ESFRI Proposal: the consortium level

• The ET ESFRI consortium is composed by the institutions signing the ET consortium agreement (CA) • Very light CA at this level • 41 Institutions signed the ET consortium • The ET consortium is coordinated by INFN and Nikhef (Stan Bentvelsen, Antonio Zoccoli)

From LKV Sept2020, modified https://www.google.com/maps/d/edit?mid=1ljTBCqTyCmVncbYaeUVcpQA3udceyg2b&usp=sharing 41 Slide: Michele Punturo ESFRI Phases: 3G Enabling technologies development idea Design Sites qualification Preparatory Costs evaluation Implementation Building the ET collaboration ET Operation CDR Building ET consortium Raising Construction Raising initial funds funds

Site Decisi ET RI construction ESFRI proposal ESFRI on decision Opera ET detectors -tion construction RI operative TDR Pre-engineering studies ET Installation

Detector Operative TDR

2004 2010 2008 2018 2019 2020 2021 2022 2023 2024 2025 2026 2030 2032 2028

42 ET Governance Scheme (proposal) ET Boards

ESFRI Proposal: • The Instrument Science Board (ISB) • deliver the ET Technical Design Report (ET-TDR) for infrastructure and detectors • identify the missing technologies and suggest a (living) plan for R&D activities. first version ca. March 2021. • The Observational Science Board (OSB) • will detail the ET science case • will prepare the data analysis requirements • will indicate the computing requirements for ET • The Site Preparation Board (SPB) • will coordinate the effort on the site related activities • formulate the site specifications for Einstein Telescope • prepare the choice of the site for the Einstein Telescope observatory • The E-Infrastructures Board (EIB) -> Computing Infrastructure Board • will define the computing and storage resources, networking, local and distributed e-infrastructures • will study the computing models that can be adopted in ET and the synergies with the e-infrastructures available or expected in Europe in the next decade. • The Internal Finance Board (IFB) • will have the mandate to evaluate the financial needs • collecting and harmonizing the inputs received from the other technical boards • will suggest the funding tools needed to elaborate a financial strategy to be proposed to the Council. H. Lueck @ GWADW 2021 ISB: Instrument Science Board

44 Like to join the Einstein Telescope project?

Check out the website of the ISB Wiki.et-gw.eu/ISB/WelcomePage

and contact a working group chair or a division chair

They will assist you join the collaboration, where you can shape the next generation of gravitational wave observatories

45 OSB: Observational Science Board

Marica Branchesi - Michele Maggiore - Ed Porter

Synergies Fundamental Population MM Nuclear Transient Science Cosmology w. other Waveforms DA platform physics Studies observations physics GW Sources Potential GW observ.

Predictions of Synergies EoS of NSs in Predictions Waveforms Science Physics near BH Dark ET / high- population of with 2G+ isolated for relevant for potential for DA platform horizons energy astrophysical detector systems Supernovae ET various Dark matter origin detector EoS in NSs in Predictions Improvement of Tests of GR ET / optical Synergies configurations Estimation of binary for waveforms for Predictions of with CE, 3G cosmological systems magnetars BBH Exotic compact primordial BHs ET / radio Common tools objects parameters ET / Nucleo- Predictions Improvement of Synergies Modifications Stochastic neutrinos synthesis in for cosmic waveforms for with LISA of gravity at backgrounds of BNS mergers string bursts NSBH cosmological astrophysical scales origin Improvement of waveforms for Stochastic BNS background of cosmological origin

46 Site Candidates

Two candidate sites in • Italy and • The Netherlands EURegio Meuse-Rhine Both sites geologically and seismically suited. Investigations ongoing. Sardinia

47 Activities in the Euregio Meuse-Rhine

• A 250-m deep borehole has been drilled and is equipped with • Seismic data under acquisition and analysis • 3-5 more boreholes in 2021/22 • Extensive active and passive site characterisation with sensor arrays in 2021 • ET pathfinder lab under construction making good progress

“Site-selection criteria for the Einstein Telescope”, RSI 91, 094504 (2020) https://doi.org/10.1063/5.0018414

Site Preparation Board: Define common/comparable measurement methods 36/Panorama_heuvelland_Maurice_van_Bruggen.JPG https://upload.wikimedia.org/wikipedia/commons/3/ 49 Measurements in the Euregio Meuse-Rhine Data: https://www.fdsn.org/ne tworks/detail/3T_2020/

Terziet: Live data: http://www.orfeus- eu.org/data/odc/re altime/?network=N L&station=TERZ First three: on ground Lower three: down hole sensor Seismic noise at the Terziet site

ground level

noise reduction by a factor of 10,000 (day) & 200 (night) 250 m deep

soft top layer Ground conditions in South Limburg : ☺ Excellent damping on hard rock good for tunnel construction ☺ Sardinia Site Activities

Slide: Domenico D'Urso The Sos Enattos site

53 Slide: Domenico D'Urso Slide: Domenico D'Urso Measurement in Sardinia

Characterization of the Bitti and Onanì corners: Surface and underground seismic and environmental measurements will start soon

SarGrav surface lab SOE0 (surface)

integrated into the INGV seismometer network http://cnt.rm.ingv.it/en/instruments/station/SENA

SOE1, SOE2, SOE3 (-84m, -111m, -160m)

4 broadband seismometers, 3 short-period seismometers, 2 magnetometers, 54 1 tiltmeter distributed over underground and surface stations Credits to L. Naticchioni Measurement Results

➢ First year of seismic characterization measurements at Sos Enattos published (JPCS 1468, 2020, SRL https://doi.org/10.1785/0220200186): extremely low-noise conditions in the range 2-10Hz. SOE2 measurements are biased by the low-gain setting of the ACQ (compliant to the national monitoring program). @ EGO ➢ Preliminary sensitivity of Archimedes Prototype @ SOS Enattos balance (tiltmeter) (https://doi.org/10.1103/PhysRevD.90.022002) 6 × 10−11푟푎푑/ 퐻푧

−13 6 × 10 푟푎푑/ 퐻푧 55 Slide: Domenico D'Urso ET Community in Germany

ET activites are ramping up in several countries in Europe, e.g. in Germany Joint Research Activity of 17 university partners funded by BMBF

56 Einstein Telescope Infrastructure

https://www.youtube.com/watch?v=HJGVs6-wJG4

57 Check out the ISB page: https://wiki.et-gw.eu/ISB/WelcomePage and contact a working group chair to join the adventure ☺