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![Page 1: Michele Punturo ET scientific Coordinator INFN Perugia and EGO On behalf of the ET design study team 1ET-Michele Punturo.](https://reader036.fdocuments.in/reader036/viewer/2022062417/551b9999550346a6148b63cc/html5/thumbnails/1.jpg)
The Einstein Telescope project: a 3rd generation gravitational wave observatory.
Michele PunturoET scientific CoordinatorINFN Perugia and EGO
On behalf of the ET design study team
http://www.et-gw.eu/
1ET-Michele Punturo
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E.M. Astronomy
visibleInfrared
408MHz WMAP
X-ray g-ray
GRB
Current e.m. telescopes are mapping almost the entire Universe
Keywords:Map it in all the accessible
wavelengthsSee as far as possible
Galaxy UDFy-38135539 in Ultra Deep Field image (Hubble Telescope) 13.1 Gly
2ET-Michele PunturoM. Trenti, Nature 467, 924–925 (21 October 2010)
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GW Astronomy ?
visibleInfrared
408MHz WMAP
X-ray g-ray
GRB
Enlarge as much as possible the frequency range of GW detectorsPulsar Timing Arrays
10-9-10-6 HzSpace based detectors
(LISA, DECIGO) 10-5-10-1 Hz
Ground based detectors 1-104Hz
Improve as much as possible the sensitivity to increase the detection volume (rate) and the observation SNR
3ET-Michele Punturo
GW ?
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Det
ectio
n di
stan
ce (
a.u.
)
GW interferometer past evolutionEvolution of the GW detectors (Virgo example):
2003
Infrastructure
realization and
detector assembling
2008
Sameinfrastructure
Proof of the working principle
Commissioning
& first ru
ns
4
ET
-Mic
he
le P
un
turo
year
Upper Limit physics
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GW interferometer present evolutionEvolution of the GW detectors (Virgo example):
2003
Infrastructure
realization and
detector assembling
2008
Sameinfrastructure
Proof of the working principle
Upper Limit physics
2011
enhanceddetectors
Sameinfrastructure
Test of “advanced” techsUL physics
2017
Sameinfrastructure
Advanced
detectors
First detection
Initial astrophysics
Commissioning
& first ru
ns
5
ET
-Mic
he
le P
un
turo
Det
ectio
n di
stan
ce (
a.u.
)
year
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Advanced detectors
6ET-Michele Punturo
Advanced detectors are, for example, promising:An increase of
the BNS detection distance up to 200 MPc
108 ly
Enhanced LIGO/Virgo+ Virgo/LIGO
Credit: R.Powell, B.Berger
Adv. Virgo/Adv. LIGO
Universe in 1 Gly
arXiv:1003.2480v2 [astro-ph.HE]
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3rd generation?Evolution of the GW detectors (Virgo example):
2003
Infrastructure
realization and
detector assembling
2008
Sameinfrastructure
Proof of the working principle
Upper Limit physics
2011
enhanceddetectors
Sameinfrastructure
Test of “advanced” techsUL physics
2017
Sameinfrastructure
Advanced
detectors
First detection
Initial astrophysics
2022
SameInfrastructure
(20 years old for Virgo, even more for LIGO & GEO600)
Commissioning
& first ru
ns
Precision Astrophysics
Cosmology ?
7
ET
-Mic
he
le P
un
turo
Det
ectio
n di
stan
ce (
a.u.
)
year
Limit of the current infrastructures
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Beyond Advanced Detectors GW detection is expected to occur in the advanced detectors. The 3rd generation should
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
8
ET-Michele Punturo
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Target Sensitivity
Target sensitivity of a new, 3rd generation “observatory” (the Einstein Telescope, ET) is the result of the trade off between several requirements
ET-Michele Punturo 9
1. Science targets2. Available technologies (detector realization)3. Infrastructure & site costs
1. Infrastructure & site costs2. Available technologies (detector realization)3. Science targets
As starting point of our studies we defined two rough requirements:Improvement by a factor 10 the advanced sensitivitiesAccess, as much as possible, to the 1-10Hz frequency range
Let see few of the new possibilities open by such as observatory
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Gamma Ray BurstsRecent satellite missions shown a series of explosive
events in the Universe generating a huge quantity of energy :GRB
ET-Michele Punturo 10
The origin of GRB is still unknown but some model has been developed
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BNS & GRB
ET-Michele Punturo 11
Simultaneous detection of GW from BNS and GRB by a specialized detector will allow:to solve the GRB enigmaUnderstand the Universe geometry (Cosmology)To measure the contribution of dark matter and dark
energy to the Universe model
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Supernova ExplosionsMechanism of the core-collapse SNe
still unclearShock Revival mechanism(s) after the
core bounce TBC
ET-Michele Punturo 12
GWs generated by a SNe should bring information from the inner massive part of the process and can constrains on the core-collapse mechanisms
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The Einstein TelescopeThe Einstein Telescope project is currently in its
conceptual design study phase, supported by the European Community FP7 from May 2008 to July 2011.
ET-Michele Punturo13
Participant Country
EGO ItalyFrance
INFN Italy
MPG Germany
CNRS France
University of Birmingham UK
University of Glasgow UK
Nikhef NL
Cardiff University UK
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ET beneficiaries
The ET beneficiaries are the core institutes of the GEO600 and Virgo collaborations
MTR-Brussels 14/12/2010 14
Participant Country
EGO ItalyFrance
INFN Italy
MPG Germany
CNRS France
University of Birmingham UK
University of Glasgow UK
Nikhef NL
Cardiff University UK
INFN (Istituto Nazionale di Fisica Nucleare) has a leading role in the definition of the seismic filtering design (WP2), cryogenics requirements (WP1-WP2) and seismic noise requirements (WP1)
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ET beneficiaries
The ET beneficiaries are the core institutes of the GEO600 and Virgo collaborations
MTR-Brussels 14/12/2010 15
Participant Country
EGO ItalyFrance
INFN Italy
MPG Germany
CNRS France
University of Birmingham UK
University of Glasgow UK
Nikhef NL
Cardiff University UK
MPG (Max-Planck-Institut für Gravitationsphysik) has a leading role in the definition of the QND technologies for the optical design (WP3) and an effective management support (WP5)
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ET beneficiaries
The ET beneficiaries are the core institutes of the GEO600 and Virgo collaborations
MTR-Brussels 14/12/2010 16
Participant Country
EGO ItalyFrance
INFN Italy
MPG Germany
CNRS France
University of Birmingham UK
University of Glasgow UK
Nikhef NL
Cardiff University UK
CNRS (Centre National de la Recherche Scientifique) has a leading role in the definition of the optics for ET (WP3) and contributes to the ET science case definition (WP4)
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ET beneficiaries
The ET beneficiaries are the core institutes of the GEO600 and Virgo collaborations
MTR-Brussels 14/12/2010 17
Participant Country
EGO ItalyFrance
INFN Italy
MPG Germany
CNRS France
University of Birmingham UK
University of Glasgow UK
Nikhef NL
Cardiff University UK
UNIBHAM (University of Birmingham) has a leading role in the definition of the optical design of ET (WP3) and contributes to the ET science case definition (WP4)
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ET beneficiaries
The ET beneficiaries are the core institutes of the GEO600 and Virgo collaborations
MTR-Brussels 14/12/2010 18
Participant Country
EGO ItalyFrance
INFN Italy
MPG Germany
CNRS France
University of Birmingham UK
University of Glasgow UK
Nikhef NL
Cardiff University UK
UNIGLASGOW (University of Glasgow) has a leading role in the definition of the overall sensitivity ET (WP3), to the suspension requirements (WP2) and to the science case definition (WP4)
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ET beneficiaries
The ET beneficiaries are the core institutes of the GEO600 and Virgo collaborations
MTR-Brussels 14/12/2010 19
Participant Country
EGO ItalyFrance
INFN Italy
MPG Germany
CNRS France
University of Birmingham UK
University of Glasgow UK
Nikhef NL
Cardiff University UK
VU (Nikhef) has a leading role in the definition of ET site requirements and specifications (WP1) and contributes to the science case definition (WP4)
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ET beneficiaries
The ET beneficiaries are the core institutes of the GEO600 and Virgo collaborations
MTR-Brussels 14/12/2010 20
Participant Country
EGO ItalyFrance
INFN Italy
MPG Germany
CNRS France
University of Birmingham UK
University of Glasgow UK
Nikhef NL
Cardiff University UK
CU (Cardiff University) has a leading role in the definition of ET science case (WP4)
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ET beneficiaries
The ET beneficiaries are the core institutes of the GEO600 and Virgo collaborations
MTR-Brussels 14/12/2010 21
Participant Country
EGO ItalyFrance
INFN Italy
MPG Germany
CNRS France
University of Birmingham UK
University of Glasgow UK
Nikhef NL
Cardiff University UK
EGO (European Gravitational Observatory), thanks to its expertise in the management of the Virgo site it has the (centralized) management (WP5) responsibility of the overall project and it collaborates to the definition of the ET infrastructures (WP1)
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Targets of the Design StudyEvaluate the science reaches of ETDefine the sensitivity and performance requirements
Site requirementsInfrastructures requirementsFundamental and (main) technical noise requirementsMultiplicity requirements
Draft the observatory specsSite candidatesMain infrastructures characteristicsGeometries
Size, L-Shaped or triangularTopologies
Michelson, Sagnac, …Technologies
Evaluate the (rough) cost of the infrastructure and of the observatory
ET-Michele Punturo 22
2009
2010
2011
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How ET goes beyond the 2nd generation?
ET-Michele Punturo 23
10-25
10-16
h(f
) [1
/sq
rt(H
z)]
Frequency [Hz]1 Hz 10 kHz
Seismic
Thermal Quantum
Seism
ic
NewtonianSusp. ThermalQuantum
Mirror thermal
3rd generation ideal target
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The ET ideaAdvanced Virgo will implement already most the cutting edge
technologies, but at the end it will be limited by the infrastructureObviously the realization of ET will push for an intense
technology developments in lasers, optics, mechanics , electronics, ..
ET-Michele Punturo 24
But, to go beyond the infrastructure limitation there are three possibilities:
1. Go in the space
2. Go on the Moon
3. Go underground !!!
LISA, DECIGO
Crazy (up to now)
LCGT, ET
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Seismology network
In ET we started the investigation using the support and the data of the ORFEUS* Network (>200 sites in Europe)
ET-Michele Punturo 25
* Observatories and Research Facilities for European Seismology
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ET-WP1: Site searchUnderground sites (mines, labs, …)Seismometer (Nikhef)
ET-Michele Punturo 26
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WP1: Site search:
Many sites visited in Europe
ET-Michele Punturo 27
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Underground Seismic noise Measurement
ET-Michele Punturo 28
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Day/Night variability vs population density
ET-Michele Punturo 29
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The infrastructureSchematic view
ET-Michele Punturo 30
Full infrastructure realized Initial detector(s)
implementation1 detector (2 ITF)Physics already
possible in coincidence with the improved advanced detectors
Progressive implementation 2 detector (4 ITF) Redundancy and cross-
correlation Full implementation3 detector (6 ITF)Virtual interferometry2 polarizations
reconstruction
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ET-Michele Punturo 31
Credits Martin Doets
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Complex infrastructureXylophone design and triangular geometry ask for a
complex hosting infrastructure
ET-Michele Punturo 32
The target of the ET project is, in fact, the realization in Europe of a fundamental Research Infrastructure that will host the Gravitational Wave observatory for decades, opening the GW precision astronomy and implementing the technical evolutions in the detectors composing the observatory
The realization of the infrastructure should be triggered by the first detection, but the implementation of the full observatory will be diluted in the years (modularity!)
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The ET project … an artistic view
ET-Michele Punturo 33
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“Political” achievementsET had a series of “political” important achievements:
Scientific initiative is back on this side of the OceanThe whole European GW community is coordinated by
EGO in a joint initiative The theoretical and Astrophysics community has been
involved in the ET design with reciprocal advantages ET science team is involving more than 220 scientists Some of them are not belonging to the 8 beneficiaries!!
ET-Michele Punturo 34
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ET Timeline
ET-Michele Punturo35
ET Design
ET Prep. phase?
FP7 FP8
ET needs to be in the ESFRI roadmap (2012 revision?)
ET needs to fill the gapET science
team needs a coordination
tool
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END
ET-Michele Punturo 36