Michele Punturo ET scientific Coordinator INFN Perugia and EGO On behalf of the ET design study team 1ET-Michele Punturo

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

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)

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 ?

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

GW interferometer present evolutionEvolution of the GW detectors (Virgo example):

2003

Infrastructure

realization and

detector assembling

2008

Sameinfrastructure


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

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]

http://arxiv.org/abs/1003.2480v2

3rd generation?Evolution of the GW detectors (Virgo example):

2003

Infrastructure

realization and

detector assembling

2008

Sameinfrastructure


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

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

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ET-Michele Punturo

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

Gamma Ray BurstsRecent satellite missions shown a series of explosive

events in the Universe generating a huge quantity of energy :GRB


The origin of GRB is still unknown but some model has been developed

BNS & GRB


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

Supernova ExplosionsMechanism of the core-collapse SNe

still unclearShock Revival mechanism(s) after the

core bounce TBC


GWs generated by a SNe should bring information from the inner massive part of the process and can constrains on the core-collapse mechanisms

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

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



Nikhef NL


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)

ET beneficiaries



Participant Country

EGO ItalyFrance

INFN Italy

MPG Germany

CNRS France



Nikhef NL


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)

ET beneficiaries



Participant Country

EGO ItalyFrance

INFN Italy

MPG Germany

CNRS France



Nikhef NL


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)

ET beneficiaries



Participant Country

EGO ItalyFrance

INFN Italy

MPG Germany

CNRS France



Nikhef NL


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)

ET beneficiaries



Participant Country

EGO ItalyFrance

INFN Italy

MPG Germany

CNRS France



Nikhef NL


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)

ET beneficiaries



Participant Country

EGO ItalyFrance

INFN Italy

MPG Germany

CNRS France



Nikhef NL


VU (Nikhef) has a leading role in the definition of ET site requirements and specifications (WP1) and contributes to the science case definition (WP4)

ET beneficiaries



Participant Country

EGO ItalyFrance

INFN Italy

MPG Germany

CNRS France



Nikhef NL


CU (Cardiff University) has a leading role in the definition of ET science case (WP4)

ET beneficiaries



Participant Country

EGO ItalyFrance

INFN Italy

MPG Germany

CNRS France



Nikhef NL


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)

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


2009

2010

2011

http://www.iconspedia.com/uploads/632613165.png



How ET goes beyond the 2nd generation?


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

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, ..


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

Seismology network

In ET we started the investigation using the support and the data of the ORFEUS* Network (>200 sites in Europe)


* Observatories and Research Facilities for European Seismology

ET-WP1: Site searchUnderground sites (mines, labs, …)Seismometer (Nikhef)


WP1: Site search:

Many sites visited in Europe


Underground Seismic noise Measurement


Day/Night variability vs population density


The infrastructureSchematic view


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


Credits Martin Doets

Complex infrastructureXylophone design and triangular geometry ask for a

complex hosting infrastructure


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!)

The ET project … an artistic view


“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 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

END


Documents

Michele Punturo ET scientific Coordinator INFN Perugia and EGO On behalf of the ET design study team 1ET-Michele Punturo