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The Einstein Telescope project

The Einstein Telescope project. Michele Punturo INFN Perugia and EGO On behalf of the ET Design Study Team http://www.et-gw.eu/. The Einstein Telescope. The Einstein Telescope project aims to the realization of a third generation of GW observatory

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The Einstein Telescope project

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  1. The Einstein Telescope project Michele Punturo INFN Perugia and EGO On behalf of the ET Design Study Team http://www.et-gw.eu/ Einstein Telescope

  2. The Einstein Telescope • The Einstein Telescope project aims to the realization of a third generation of GW observatory • The Einstein Telescope project is currently in its conceptual design study phase, supported by the European Community FP7 with about 3M€ from May 2008 to July 2011. • The Einstein Telescope project aims to the realization of a third generation of GW observatory • The target of this design phase is to understand the feasibility of a new generation of GW observatory that will permit to gain one order of sensibility • The main deliverable, at the end of these 3 years, will be a conceptual design of such as infrastructure Einstein Telescope

  3. GW Astronomy ? • Current e.m. telescopes are mapping the Universe in all the wavelengths detectable from the Earth and from the space. • Gravitational wave telescopes, having a comparable sight distance, could complement the e.m. observation opening the GW astrophysics era • Thanks to the small interaction between graviton and the matter , GW are the best messenger to investigate the first instants of the Universe WMAP 408MHz Infrared visible g-ray X-ray GW ? GRB Einstein Telescope

  4. GW interferometer past evolution • Evolution of the GW detectors (Virgo example): Detection distance (a.u.) Proof of the working principle Upper Limit physics Commissioning & first runs Infrastructure realization and detector assembling Same infrastructure year Einstein Telescope 2003 2008

  5. GW interferometer present evolution First detection Initial astrophysics • Evolution of the GW detectors (Virgo example): Test of “advanced” techs UL physics Detection distance (a.u.) Advanced detectors Proof of the working principle Upper Limit physics enhanceddetectors Commissioning & first runs Infrastructure realization and detector assembling Same infrastructure Same infrastructure Same infrastructure year Einstein Telescope 2003 2008 2011 2017

  6. Precision Astrophysics Cosmology ? 3rd generation? Limit of the current infrastructures First detection Initial astrophysics • Evolution of the GW detectors (Virgo example): Test of “advanced” techs UL physics Detection distance (a.u.) Advanced detectors Proof of the working principle Upper Limit physics enhanceddetectors Commissioning & first runs Infrastructure realization and detector assembling Same infrastructure Same infrastructure Same infrastructure Same Infrastructure (20 years old for Virgo, even more for LIGO & GEO600) 2017 year Einstein Telescope 2003 2008 2011 2022

  7. Physics Beyond Advanced Detectors • GW detection is expected to occur in the advanced detectors. The 3rd generation will focus on observational aspects: • Astrophysics: • Measure in great detail the physical parameters of the stellar bodies composing the binary systems • NS-NS, NS-BH, BH-BH • Constrain the Equation of State of NS through the measurement • of the merging phase of BNS • of the NS stellar modes • of the gravitational continuous wave emitted by a pulsar NS • Contribute to solve the GRB enigma • Relativity • Compare the numerical relativity model describing the coalescence of intermediate mass black holes • Test General Relativity against other gravitation theories • Cosmology • Measure few cosmological parameters using the GW signal from BNS emitting also an e.m. signal (like GRB) • Probe the first instant of the universe and its evolution through the measurement of the GW stochastic background • Astro-particle: • Contribute to the measure the neutrino mass? • Constrain the graviton mass measurement Einstein Telescope

  8. Targets of the Design Study 2009 • Evaluate the science reaches of ET • Define the sensitivity and performance requirements • Site requirements • Infrastructures requirements • Fundamental and (main) technical noise requirements • Multiplicity requirements • Draft the observatory specs • Site candidates • Main infrastructures characteristics • Geometries • Size, L-Shaped or triangular • Topologies • Michelson, Sagnac, … • Technologies • Evaluate the (rough) cost of the infrastructure and of the observatory 2010 2011 Einstein Telescope

  9. Transversal Writing Team TWT EGO STAC (May 2010)

  10. How to go beyond the 2nd generation? 10-16 Seismic Newtonian Seismic Susp. Thermal h(f) [1/sqrt(Hz)] Quantum Thermal Quantum Mirror thermal 3rd generation ideal target 10-25 1 Hz 10 kHz Frequency [Hz] Einstein Telescope

  11. Stressing the current technologies • Obviously a certain improvement of the sensitivity of the advanced detectors could be achieved by stressing the “current” technologies: • High power lasers (1kW laser, shot noise reduction) • Larger mirrors and larger beams (lower thermal noise) • Better coatings (lower thermal noise, lower scattering) • But these aren’t the key elements justifying: • the transition 2nd 3rd generation • the need of a new infrastructure Einstein Telescope

  12. 3rd generation Technologies in ET • Injection of squeezed light states (where the phase noise in the ifo arms is lowered at the cost of the amplitude noise) permits to reduce HF noise • Higher order modes (LG33) resonating in the FP cavities permit to reduce the intermediate (thermal) noise effects • Cryogenic operative temperature (~10-20K) permits to suppress the thermal noise and improve the low and intermediate frequency sensitivity • New materials: Sapphire (LCGT), Silicon • New coatings Einstein Telescope

  13. Access the very low frequency • The most challenging requirement of a 3rd generation GW observatory is to access, as much as possible, the ~1-10Hz frequency range • The “enemy” to fight is the seismic noise, that acts on the test masses • Indirectly, through the suspension chain • Directly, through the so-called gravity gradient noise • Virgohas implemented a seismic filtering chain • The super attenuator (SA) • It has been evaluated (S. Braccini et al, 2010) to be compliant with the ET requirements, above 3Hz, if xseism<510-9/f2 m/Hz-1/2 and hSA~20m Einstein Telescope

  14. Underground site • Virgo SA filtering capabilities are compatible with the ET requirements from 3Hz, provided that xseims<5×10-9/f2 m/Hz½ (Kamioca underground site specs) • Surface wave GGN reduced going underground (G.Cella 2009) We need an underground site: new infrastructure! Measurements in Europe: BFO (Black Forest Observatory): -162m BRG (Berggieshübel seism Observatory): -36m GRFO (Graefenberg borehole station): -116m Einstein Telescope

  15. Credits: J.v.d.Brand Peterson’s High Noise Model Site Investigation Peterson’s Low Noise Model http://www.et-gw.eu/ Einstein Telescope

  16. The infrastructure • Pictorial view ~100 m Einstein Telescope

  17. The infrastructure • Full infrastructure realized • Initial detector(s)implementation • 1 detector (2 ITF) • Physics already possible in coincidence with the improved advanced detectors • Schematic view Credits: S. Hild • Progressive implementation • 2 detector (4 ITF) • Redundancy and cross-correlation • Full implementation • 3 detector (6 ITF) • Virtual interferometry • 2 polarizations reconstruction Einstein Telescope

  18. 2nd detector installation ET Timeline • The t0 depends on several constrains: • Readiness of the project (completion of the design studies) • Detection of GW in Advanced detectors (~2017?) • Formal decisions • … • We suppose to have a construction t0=2018, having a decision t0’=2016-2017 2016 2018 2020 2022 2024 Einstein Telescope

  19. ET Timeline ET Design ET Prep. phase ? ILIAS-next ? FP7 ET 2nd DS FP8 ASPERA-SAC, Apr2010

  20. ET Design Study: 2nd phase • We need maintain active the network between the scientists that currently are involved in ET, after the end of the DS • We need to pass from the conceptual design (“is it feasible?”) to the technical design (“how it should be realized?”) • Possibility to submit a new proposal to EU in 2010 • Who? • Enlarge the beneficiaries list • What? • Content of the proposal • Targets Einstein Telescope

  21. Conclusions • The Einstein Telescope project is concluding its first phase • We have been able to group a large community around a new idea • The effort and the continuity on this target must increase in the next years, although the advanced detectors realization will absorb a large fraction of the GW community resources • Other large research infrastructures are currently competing for the same budget Einstein Telescope

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