JRA3 STREGA - Introduction Geppo Cagnoli IGR – University of Glasgow ILIAS-GW Meeting, Orsay, 5 th -6 th Nov 2004
Jan 17, 2016
JRA3 STREGA - Introduction
Geppo CagnoliIGR – University of Glasgow
ILIAS-GW Meeting, Orsay, 5th-6th Nov 2004
ILIAS-GW Meeting, Orsay, 5th – 6th Nov 2004 2
10 0 10 910 6 [Hz]10 3
Bars and
Spheres
RF CavitiesInterferometers
Overview on GW detection
The expected strain of space is 10-22 Hz-1/2 or lower
ILIAS-GW Meeting, Orsay, 5th – 6th Nov 2004 3
Ultimate limits on GW detection
All the detectors are mainly limited by thermal noise
that causes fluctuations on position and shape of the
test masses Interferometers: thermal noise in mirrors and in suspension fibres
Bars/Spheres: thermal noise in the resonant elements
RF cavities: thermal noise in the cavity walls and in the e.m. field
ILIAS-GW Meeting, Orsay, 5th – 6th Nov 2004 4
STREGA Mission
Lower thermal noise 10 times with respect to the
second generation detectors
ILIAS-GW Meeting, Orsay, 5th – 6th Nov 2004 5
IFOS TH.NS BAND
Detectors Generations
1 10 100 1k 10kFrequency [Hz]
10 -22
10 -23
10 -24
10 -25
10 -19
10 -20
10 -21
h
[ H
z –1
/2 ]
GEO600
LIGOVIRGO
AURIGANAUTILUS
1ST GENERATION
FOR IFOS•STEEL SUSPENSIONS (APART GEO600)•ROOM TEMPERATURE
FOR RESONATORS•ALUMINIUM CYLINDERS•100mK < T < 4K
LIGO SCIENTIFIC RUN 3POSSIBLE DETECTION OF NS/NS MERGING
WITHIN THE LOCAL GROUPDISTANCE < 1.8 MPc
1ST GENERATION SHOULD REACH THE VIRGO CLUSTER AT 17MPc
ILIAS-GW Meeting, Orsay, 5th – 6th Nov 2004 6
Detectors Generations
1 10 100 1k 10kFrequency [Hz]
10 -22
10 -23
10 -24
10 -25
10 -19
10 -20
10 -21
h
[ H
z –1
/2 ]
GEO600
LIGOVIRGO
AURIGANAUTILUS
1ST GENERATION
FOR IFOS•STEEL SUSPENSIONS (APART GEO600)•ROOM TEMPERATURE
FOR RESONATORS•ALUMINIUM CYLINDERS•100mK < T < 4K
2ND GENERATION
FOR IFOS•SILICA SUSPENSIONS•HIGHER LASER POWER•ROOM TEMPERATURE
FOR RESONATORS•CuAl SPHERES• T < 100mK•BETTER READOUT
RF CAVITIES•1ST DETECTORSAD. LIGO
AD. VIRGO
MiniGRAIL
PACO
ILIAS-GW Meeting, Orsay, 5th – 6th Nov 2004 7
Detectors Generations
1 10 100 1k 10kFrequency [Hz]
10 -22
10 -23
10 -24
10 -25
10 -19
10 -20
10 -21
h
[ H
z –1
/2 ]
GEO600
LIGOVIRGO
AURIGANAUTILUS
1ST GENERATION
FOR IFOS•STEEL SUSPENSIONS (APART GEO600)•ROOM TEMPERATURE
FOR RESONATORS•ALUMINIUM CYLINDERS•100mK < T < 4K
2ND GENERATION
FOR IFOS•SILICA SUSPENSIONS•HIGHER LASER POWER•ROOM TEMPERATURE
FOR RESONATORS•CuAl SPHERES• T < 100mK•BETTER READOUT
RF CAVITIES•1ST DETECTORSAD. LIGO
AD. VIRGO
MiniGRAIL
PACO
EGO
DUAL
3RD GENERATION
FOR IFOS•SILICON MIRRORS•SILICON SUSPENSIONS•HIGHER LASER POWER•BETTER COATINGS•LOW TEMPERATURE
FOR RESONATORS•CRISTALLINE MATERIALS•DOUBLE RESONATORS• T < 10mK•SQL
Z = 1
ILIAS-GW Meeting, Orsay, 5th – 6th Nov 2004 8
… coming back on Earth3 Objectives for STREGA
1 Research on Materials Outcomes
- Selection or Development of the most suitable materials forMirrors, Suspensions and Resonant Masses
- Development of low losses Dielectric Coatings
- Investigation on Acoustic Emission caused by Cosmic Rays
ILIAS-GW Meeting, Orsay, 5th – 6th Nov 2004 9
… coming back on Earth3 Objectives for STREGA
2 Research on Cryogenics Outcomes
- Development of a cryogenic system for the interferometers with a low mechanical noise
- Design of a last stage suspension able to provide 1W of heat flow at ~5K
- Development of a low noise ultra cryogenic system (~10mK) for resonant detectors
ILIAS-GW Meeting, Orsay, 5th – 6th Nov 2004 10
… coming back on Earth3 Objectives for STREGA
3 Research on Thermal Noise Outcomes
- Development of facilities for the direct measurement of Thermo-elastic noise
- Development of facilities for the direct measurement of Photo-elastic noise
- Novel read-out configurations able to reduce the effect of thermal noise on the signal detected with resonant bars
ILIAS-GW Meeting, Orsay, 5th – 6th Nov 2004 11
Some Numbers
124 people of 25 different groups (subgroup of the Network) € 1794 per person per year
STREGA web page: http://www.ego-gw.it/ILIAS-GW/
STREGA has the largest number of deliverables among the ILIAS activities (15 in the first 18 months)
GOOD WORK !!