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Some ideas on ET1 site Adalberto Giazotto
INFN Pisa- EGO
Introduction
ET will be a network of detectors whose target is the systematic observation of the Universe by means of Gravitational Waves: i.e. GW astronomy.
GW astronomy implies, obviously, determination of GW sources celestial coordinates.
The most efficient and precise way of measuring source celestial coordinates is by means of GW event time of flight measurement. This method requires several interferometers well spaced around the Earth in the way of attaining the highest angular resolution.
4 well spaced ITF’s determine univocally GW source Celestial Coordinates.Per example angular resolution of the V-L network are :
Virgo-LIGODeclinazione: 4°30‘Ascensione retta: 3° 32‘ Courtesy Simona Birindelli
Virgo-LIGO-AIGODeclinazione: 2° 52‘Ascensione retta:1° 51‘ Courtesy Simona Birindelli
LIGO+AIGOLIGO
Correlation between detectors
Another reason for getting well separated ITF’s for ET is that this configuration has the lowest correlation between single network detectors.
For these reasons I refere to ET1 as the first of, at least, 4 interferometer which will form the ET network
ET a Global network of Detectors
Coherent Analysis: why?
-Sensitivity increase
-Source direction determination from time of flight differences
-Polarizations measurement
-Test of GW Theory and GW Physical properties
Astrophysical targets
- Far Universe expansion rate Measurement
-GW energy density in the Universe
-Knowledge of Universe at times close to Planck’s time
ET Sensitivity
Harald Lück
for the European Gravitational-Wave Community
TAMA 300
GEO600
LIGO
Virgo
AURIGA, NAUTILUS, EXPLORER
GW DETECTORS SENSITIVITY
Some exercise:Use of Superattenuators for ET
1) Inverted Pend. 40 mHz 2) 50 m tall mechanical filter chain
By assuming a seismic noise underground 10-
9m/sqrt(Hz)@1Hz, from theTF optimized at 1Hz we obtain h(1Hz)= 2.610-22/sqrt(Hz
~50 m
N 1 Hz 2 Hz --------------------------- {3, 1.6*10-7, 5.4*10-10} {4, 4.8*10-8, 3.3*10-11} {5, 2.6*10-8, 3.4*10-12} {6, 2.3*10-8, 6.7*10-12} {7, 2.1*10-8, 2.6*10-12}
Optimized at 1Hz
Courtesy G. Cella
Horizontal
ET sens.
2 HZ
Superattenuator
NEWTONIAN
Isolation in Vertical Direction
In Virgo, SA Vertical attenuation has been tuned to the horizontal one evaluated with length module of 1m.
Considering length module of 7m we obtain:
This frequency can be easily obtained both by tuning magnetic antispring or geometrical springs.
1
1 100.16 0.4
2 1m
gHz
L
7
1 100.16 0.2
2 7m
gHz
L
15-20 m diam.
10 km
10 km4k
300k
Tunnel standard
~100 m
15 m
clean room
10 km
10 km4k
300k
Tunnel standard
15-20 m
~100 m
15 m
clean room
Some exercise:Use of Superattenuators for ET
1) Inverted Pend. 40 mHz 2) 50 m tall mechanical filter chain
By assuming a seismic noise underground 10-8m/sqrt(Hz) @1Hz, from the TF optimized at 2Hz we obtain h(2Hz)=10-25/sqrt(Hz)<<10-22/sqrt(Hz)
N 1 Hz 2 Hz --------------------------- {3, 1.6*10-7, 5.4*10-10} {4, 4.8*10-8, 3.3*10-11} {5, 2.7*10-8, 3.3*10-12} {6, 2.8*10-8, 4.9*10-13} {7, 6.3*10-8, 1.0*10-13}
Optimized at 2 Hz
N 1 Hz 2 Hz --------------------------- {3, 1.6*10-7, 5.4*10-10} {4, 4.8*10-8, 3.3*10-11} {5, 2.6*10-8, 3.4*10-12} {6, 2.3*10-8, 6.7*10-12} {7, 2.1*10-8, 2.6*10-12}
Optimized at 1Hz
~50 m
Courtesy G. CellaCourtesy G. Cella