detection of gravitational waves - infnronga/slides_files/barishbo_8.pdfdetection of gravitational...
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![Page 1: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/1.jpg)
1
F Ronga Bologna October 2 2006
Introduction : gravitational waves
Acoustic Detectors
Laser Interferometers
Future Prospect
Summary and Conclusions
Detection of gravitational waves
Venerdì, 14 settembre 2012
![Page 2: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/2.jpg)
Last MACRO Meeting Gran Sasso January 2000
Venerdì, 14 settembre 2012
![Page 3: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/3.jpg)
Last MACRO Meeting Gran Sasso January 2000
Jack O’ MalleyVenerdì, 14 settembre 2012
![Page 4: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/4.jpg)
Gravitational Waves
€
∂ 2
∂x 2−1c 2
∂ 2
∂t 2⎛
⎝ ⎜
⎞
⎠ ⎟ hik = 0
€
h23 = h32h22 = −h33
€
hik <<1for weak field almost galilean metric with the addiction of a small terms
in absence of matter and in a transverse traceless gauge
This is the equation of transversal waves with velocity c
Venerdì, 14 settembre 2012
![Page 5: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/5.jpg)
Gravitational Waves
€
∂ 2
∂x 2−1c 2
∂ 2
∂t 2⎛
⎝ ⎜
⎞
⎠ ⎟ hik = 0
€
h23 = h32h22 = −h33
€
hik <<1for weak field almost galilean metric with the addiction of a small terms
in absence of matter and in a transverse traceless gauge
This is the equation of transversal waves with velocity c
In 1974 observed changes in the rotational velocity of the binary system PSR1913+16 (indirect evidence of gravitational waves)
Venerdì, 14 settembre 2012
![Page 6: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/6.jpg)
Gravitational Waves
€
∂ 2
∂x 2−1c 2
∂ 2
∂t 2⎛
⎝ ⎜
⎞
⎠ ⎟ hik = 0
€
h23 = h32h22 = −h33
€
hik <<1for weak field almost galilean metric with the addiction of a small terms
in absence of matter and in a transverse traceless gauge
This is the equation of transversal waves with velocity c
In 1974 observed changes in the rotational velocity of the binary system PSR1913+16 (indirect evidence of gravitational waves)
Importance of gravitational waves astronomy:
Universe is transparent only to gravitational waves and neutrinos!
Venerdì, 14 settembre 2012
![Page 7: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/7.jpg)
• neutron binary system PSR 1913+16 7 kpc from the earth
• period speeds up 35 sec from 1975 to 2004
• apparently loss is due to GW, agreement with general relativity at 0.1% level
• 1993 Nobel to Russel Taylor
Indirect evidence for GW emission
Venerdì, 14 settembre 2012
![Page 8: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/8.jpg)
Gravitational waves : some characteristic
1) 2 independent transversal quadrupolar components producing variations in the length ortogonally to the propagation axis
h+ hx
Detectors should measure ΔL
2) Invariance for 180o rotations. Electromagnetic waves 360o
/2
/2
Venerdì, 14 settembre 2012
![Page 9: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/9.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 10: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/10.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 11: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/11.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 12: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/12.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 13: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/13.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 14: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/14.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 15: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/15.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 16: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/16.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 17: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/17.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 18: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/18.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 19: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/19.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 20: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/20.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 21: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/21.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 22: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/22.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 23: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/23.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 24: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/24.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 25: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/25.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 26: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/26.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 27: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/27.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 28: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/28.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 29: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/29.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 30: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/30.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 31: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/31.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 32: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/32.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 33: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/33.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 34: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/34.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 35: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/35.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 36: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/36.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 37: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/37.jpg)
Two polarizations “+” and “x”The two independent polarization are shown in the following
example (bar and interferometer)
Testo
Detectors are sensitive to the polarization and to the angle of incidence
A measurement of the degree of circular polarization determines the inclination of a simple binary orbit.
To fully reconstruct a gravitational wave several cylinders/ interferometers are need or a spherical detector!
Venerdì, 14 settembre 2012
![Page 38: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/38.jpg)
Gravitational waves :production
very weak waves; needed big astrophysical object with large masses and quadrupolar mass distributions
€
GMR
⎛
⎝ ⎜
⎞
⎠ ⎟
€
1c 4
€
GMr
⎛
⎝ ⎜
⎞
⎠ ⎟
h ≤
Production upper limit:
Newtonian potential at the source of radius R
Newtonian potential at the detection distance r
Example
h ≤
10-21 for a neutron star R=10Km at 10Mparsec
Energy flux ≈0.3 watt/m2 (h=10-21,f=1KHz)
€
F =c 3
G116π
∂∂t
h+2 + hx
2( )
Venerdì, 14 settembre 2012
![Page 39: Detection of gravitational waves - INFNronga/Slides_files/BarishBo_8.pdfDetection of gravitational waves Venerdì, 14 settembre 2012. Last MACRO Meeting Gran Sasso January 2000 Venerdì,](https://reader036.vdocument.in/reader036/viewer/2022062602/5ec91ebc93cf98001f4e0865/html5/thumbnails/39.jpg)
Gravitational waves :production
very weak waves; needed big astrophysical object with large masses and quadrupolar mass distributions
€
GMR
⎛
⎝ ⎜
⎞
⎠ ⎟
€
1c 4
€
GMr
⎛
⎝ ⎜
⎞
⎠ ⎟
h ≤
Production upper limit:
Newtonian potential at the source of radius R
Newtonian potential at the detection distance r
Example
h ≤
10-21 for a neutron star R=10Km at 10Mparsec
Energy flux ≈0.3 watt/m2 (h=10-21,f=1KHz)
Quite large energy flux! bigger than the moon light, but very difficult to detect!
€
F =c 3
G116π
∂∂t
h+2 + hx
2( )
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Gravitational waves :production
very weak waves; needed big astrophysical object with large masses and quadrupolar mass distributions
€
GMR
⎛
⎝ ⎜
⎞
⎠ ⎟
€
1c 4
€
GMr
⎛
⎝ ⎜
⎞
⎠ ⎟
h ≤
Production upper limit:
Newtonian potential at the source of radius R
Newtonian potential at the detection distance r
Example
h ≤
10-21 for a neutron star R=10Km at 10Mparsec
Energy flux ≈0.3 watt/m2 (h=10-21,f=1KHz)
Quite large energy flux! bigger than the moon light, but very difficult to detect!
Current interferometers have sensitivity ~1 watt/m2 f=1KHz €
F =c 3
G116π
∂∂t
h+2 + hx
2( )
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Gravitational waves : frequency
€
f ≈ v2πR
€
ν 2 ≈GMR
€
f =12π
GMR3
The maximum emission frequency is related to the dimension and the mass of the astrophysical object
maximum
(virial teorem)
Current antennas are sensitive to f≈0.1-10Khz : could detect continuos waves produced in “small” objects as rotating neutron stars, merging of two neutron stars, and “burst sources’ (characteristic time 1 msec or less) as supernova explosions and black hole formation .sources of lower frequencies : space interferometers (LISA)
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Possible sources - earth detectors 1) “chirp” : merging of a binary system (like the Hulse Taylor). The signal start at low and end at high frequency. The Hulse Taylor end ~ 300 My. Binary system with two neutron star reference for the gravitational wave community
• signal can be computed accurately: we can detemine distance from the earth, masses of the bodies, orbital eccentricity and orbital inlclination. Over constraint : test of general relativity.
2) continous waves from a spinning neutron stars,needs a non-spherical pattern.Pulsar in our galaxy have 10-6 < ε< 10-4
9
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Possible sources - earth detectors 1) “chirp” : merging of a binary system (like the Hulse Taylor). The signal start at low and end at high frequency. The Hulse Taylor end ~ 300 My. Binary system with two neutron star reference for the gravitational wave community
• signal can be computed accurately: we can detemine distance from the earth, masses of the bodies, orbital eccentricity and orbital inlclination. Over constraint : test of general relativity.
2) continous waves from a spinning neutron stars,needs a non-spherical pattern.Pulsar in our galaxy have 10-6 < ε< 10-4
9
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Possible sources - earth detect.(cont)• supernovae (example of a “burst sources”) large uncertainties
in the calculations energy in GW from 10-2 (1970) to 10-9
(1995) to 10-4 (2006)• examples from one of the latest calculation (Ott et al PRL 96
2006)
10
bar nowbar quant lim
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Detectors1- laser inteferometer 2 - low temperature
cylinder
• Michelson interferometers: idea due to several independent peoples: Pirani (1956), Weber and Forward (Weber’s student) (~1960-72), Gerstenshtein and Pustovoit (1960-1972), Weiss(1972)
• first interferometer built by Forward at the Hughes Research Laboratories Sh ~ 2x10-16 Hz-1/2Venerdì, 14 settembre 2012
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J. Weber 1969
J. Weber and gravitational waves acoustic detectors
• Current acoustic detectors quite similar to the first detector due to J.Weber (1969) : aluminum cylinder and piezoelectric crystals.
• The major differences are in the bar temperature and in the extraction of the electric signal.
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J. Weber 1969
J. Weber and gravitational waves acoustic detectors
• Current acoustic detectors quite similar to the first detector due to J.Weber (1969) : aluminum cylinder and piezoelectric crystals.
• The major differences are in the bar temperature and in the extraction of the electric signal.
Weber published his results in Physical Review Letters (1969), claiming evidence for observation of gravitational waves based on coincident signals from two bars separated by 1000 km. Great excitement in the early 1970s : Beginning of the gravitational waves searches.
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Allegro, USA
Schenberg,Brazil
MiniGRAILThe Netherlands
ExplorerSwitzerland
Auriga, Italy
Nautilus, Italy
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SENSITIVITY OF PRESENT DETECTORS
TestoTesto
Improvement in sensitivity and bandwidth in the last couple of yearsbut interfometers have done a better job (Sh~10-22 @ 900 Hz)factor >10 possible at quantum limit
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rate[year –1]
search threshold
dashed region excluded with probability
> 95%
Burst search :expected performances of IGEC-2 Agreement for a joint search for gravitational waves based on our previous experience (IGEC
1997-2000)Participating groups: ALLEGRO, AURIGA and ROG (4 detectors). First search: time
coincidence search for bursts 2004 May → 2005 ,2006 Feb + …
Triple coincidences: < 1/100 years for SNR>5
Best guess on the achievable upper limit improvement by IGE-2 (Prodi Amaldi 2005)
1 month
1 year
IGEC-1 upper limit
0.01 solar mass in GW in a time <<1msec at the galactic center
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Interferometri nel mondo
TAMA
600 m
300 m
4 & 2 km
4 km 3km
Running Interferometers
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VIRGO/LIGO Time Line
NowInauguration
1999 2000 2001 2002 20033 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4
First Lock Full Lock all IFO
10-17 10-18 10-20
2004 20051 2 3 4 1 2 3 4 1 2 3 4
2006
S1 S4Science S2 RunsS3 S5
10-224K strain noise at 150 Hz [Hz-1/2]
HEPI at LLO
LIGO
LIGO
VIRGOInauguration Full Lock all IFO
10-21
10-21
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VIRGO/LIGO Time Line
NowInauguration
1999 2000 2001 2002 20033 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4
First Lock Full Lock all IFO
10-17 10-18 10-20
2004 20051 2 3 4 1 2 3 4 1 2 3 4
2006
S1 S4Science S2 RunsS3 S5
10-224K strain noise at 150 Hz [Hz-1/2]
2006
HEPI at LLO
LIGO
LIGO
VIRGOInauguration Full Lock all IFO
10-21
10-21
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LIGO/VIRGO noise budgetmain contributions:high frequency :laser shot noiselow frequency : seismic noise, suspension thermal
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LIGO/VIRGO noise budget
Virgo seismic
main contributions:high frequency :laser shot noiselow frequency : seismic noise, suspension thermal
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Interfermeters Science Run (LIGO, GEO and VIRGO
The fifth LIGO science run started in November 2005 S5 goal is to collect one year of triple coincidence data at
the design sensitivity Optimistic event rates: NS/NS ~3/year, BH/NS ~30/year
Nakar, Gal-Yam, Fox, astro-ph/0511254 Plan to reach the Crab pulsar spin down limit Expect to beat the Big-Bang Nucleosynthesis limit on
gravitational wave density in the LIGO band GEO interferometer joined the S5 run in January 2006. Virgo interferometer joined S5 this month (in the week
ends)
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Current detectors(design sensitivity for Virgo at low frequencies)
21
: Sensitivity for GEO – LIGO - Virgo – Explorer - Nautilus – Auriga, with levels of possible sources. The Pulsars points show SNR with respect to background noise of Virgo after one year of integration, for maximum amplitude of the emitted GW.
for maximum amplitude!realistic factor ~10-2
for eccentricity~10-6
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Future
In my opinion current run very important, future could change if gravitational waves will be discovered
If not discovered : proceed as soon as possible to the “advanced upgrade” of the LIGO,VIRGO, ...detectos on the earth
new space detector (LISA)
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LISA
R/D (LISA-PF 2009) LISA after 2015?Venerdì, 14 settembre 2012
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LISA
R/D (LISA-PF 2009) LISA after 2015?
• Optimized for low frequency 10-4 10-1 Hz
• Thousands of sources : galactic binaries like the Russel Taylor, ( gravitational wave noise!)
• more interesting black hole coalescence, stocastic noise...
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Conclusions
25
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• 4 alluminium cylindrical detectors are in “science” run sensitivity smaller than interferometers, but operation cost much smaller. Monitor during the interferometers upgrades
Conclusions
25
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• 4 alluminium cylindrical detectors are in “science” run sensitivity smaller than interferometers, but operation cost much smaller. Monitor during the interferometers upgrades
• LIGO, GEO interferometers, scientific run for >1 year. VIRGO at the end of the commissioning. VIRGO run at the end of the year.
Conclusions
25
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• 4 alluminium cylindrical detectors are in “science” run sensitivity smaller than interferometers, but operation cost much smaller. Monitor during the interferometers upgrades
• LIGO, GEO interferometers, scientific run for >1 year. VIRGO at the end of the commissioning. VIRGO run at the end of the year.
• Non zero probability to detect G.W. NOW !
Conclusions
25
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• 4 alluminium cylindrical detectors are in “science” run sensitivity smaller than interferometers, but operation cost much smaller. Monitor during the interferometers upgrades
• LIGO, GEO interferometers, scientific run for >1 year. VIRGO at the end of the commissioning. VIRGO run at the end of the year.
• Non zero probability to detect G.W. NOW !
Conclusions
25
• In August 2004 Ladbrokes, the British betting firm, opened a book on the chances of LIGO seeing gravitational waves before 2010. They initially set the odds at 500:1 but business was so brisk that within a week the odds had fallen to 6:1and then to 3:1 before Ladbrokes closed the book!
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The End
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F Ronga Torino Febbraio 2004
Misura rumore Browniano
T da termometri ~ 0.1 Kelvin
Nautilus 1998
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August 30, 2006 G060488
Triple Coincidence Accumulation
100%
~ 45%
~ 61%
Expect to collect one year of triple coincidence data by summer-fall 2007
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LIGO
29
LIGO-G060363-00-Z
S2
S1
S4 projected
Excluded 90% CL
S5 projected
Rate
Lim
it (e
vent
s/da
y)
Upper Limits
! No GW bursts detected through S4
" set limit on rate vs signal strength.
Lower amplitude limits
from lower detector noise
Lower rate
limits from
longer
observation
times
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Virgo /Ligo Noise budgetmain contributions:high frequency :laser shot noiselow frequency : mirror pendolum noise, newtonian noise, seismic noise
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Burst search : IGEC1 results Phys.Rev.D68:022001,2003
31
rate[year –1]
search threshold
dashed region excluded with probability
> 95%
0.02 solar mass in GW at the Galactic center
LIGO/TAMA e-Print Archive: gr-qc/0505029
10!20
10!19
10!18
10!17
10!1
100
101
Signal Amplitude (Hz!1/2
)
90%
Rate
Uppe
r Lim
it (da
y!1) LIGO!only (S1)
LIGO!only (S2)
TAMA!only (DT9)
LIGO!TAMA (S2/DT8)
Comparison of the search sensitivity with the interferometers could be done in several different ways (due to the different sensitivity band) hrss= is the root sum square of h.Assumed a Gaussian waveform τ=0.1 msec:
Note the different h units!
gr-qc/0507081
95%
CL
uppe
r lim
it
€
h(t) = hrss2πτ 2⎛
⎝ ⎜
⎞
⎠ ⎟ 1/ 4
e−t 2
τ 2
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Cosmic ray showers detection (Nautilus 1998)
• interesting to study the detector performances and to understand the cosmic rays backgrounds
• In Nautilus at T=130 mKelvin unexpected events of very large energy probably related to the superconductivity
32
Large energy events expected if hadrons are in the shower, butrate much larger than expected.
In the runs at temperature T >1 Kelvin rate of big events lower
To solve this question: RAP experimenton a particle beam Quintieri’s talk this afternoon
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Burst search with bar (optimized for length<<1 msec).
Background estimate of triple coincidence on the common observation time (130 days) by 107 time shifts
With a detection threshold of 5.5 stdev on AURIGA the FA rate goes down to 1 per century
FALSE ALARM RATE vs DETECTION THRESHOLD(AU-EX-NA PRELIMINARY) Testo
• In the past : some excess in the coincidences between tow detectors (Explorer and Nautilus)with small statistical significance• Now in progress a search with better detectors and at least a triple coincidenceNow in progress
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F Ronga Torino Febbraio 2004
Example of a cylindrical resonant detector: Nautilus (the first cooled at 100 mK)
Liquid Helium
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F Ronga Torino Febbraio 2004
Example of a cylindrical resonant detector: Nautilus (the first cooled at 100 mK)
Liquid Helium
Al 2036 bar 2300 Kg L=3 m r=0.3m
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F Ronga Torino Febbraio 2004
Example of a cylindrical resonant detector: Nautilus (the first cooled at 100 mK)
Liquid Helium
Al 2036 bar 2300 Kg L=3 m r=0.3m
Cross section : 2 aluminum shields, container for helium 2000 liters, dilution refrigerator with 3He 4He mixture
Venerdì, 14 settembre 2012
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F Ronga Torino Febbraio 2004
Example of a cylindrical resonant detector: Nautilus (the first cooled at 100 mK)
Liquid Helium
Al 2036 bar 2300 Kg L=3 m r=0.3m
Cross section : 2 aluminum shields, container for helium 2000 liters, dilution refrigerator with 3He 4He mixture
Mechanical suspension: shields are suspended in a chains and copper wire around the bar 260 db @ 1 Khz
Venerdì, 14 settembre 2012
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Sources : Gravitational waves from big bang
• from big bang : microway radiation, relic particles and gravitational radiation
• searched usually correlating the signal of two antennas optimal distance~
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Virgo “superattenuator”
• seismic noise better reduction (low fequency limitation)
• 10 years development
7.3
met
ri
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Measurement of differential deformations of two nested resonators
Intermediate GW broadband
Dual: Main Concept
5.0 kHz
π Phase difference
The inner resonator is driven below frequency
The outer resonator is driven above resonance
Two detectors studied Molibdenum 16.4 tonsSiC(ceramic) 62.2 tons Phys Rev D 68
102004
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LISA• Each S/C carries 2
lasers, 2 telescopes, 2 test masses
• Local lasers phase-locked
• Lasers on distant S/C phase-locked to incoming light
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Advanced resonant
Complementare agli Esperimenti Terrestri
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Bar as cosmic ray and particle detector
41
• first cosmic ray detection in NAUTILUS (1998) T=0.1 K, unexpected big signals, probably due to the superconductivity
Upper limit using Standord data
-----T=2-4 K-------------------
T=0.1K
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To reach the standard quantum limit and to become comparable to the current
interferometers:
Mechanical oscillatorMass M
Temperature TQuality factor Q
Resonant frequency fr
TransducerEnergy conversion coefficient
β
Amplifiernoise temperature Tn
L0 Li
x
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To reach the standard quantum limit and to become comparable to the current
interferometers:
Mechanical oscillatorMass M
Temperature TQuality factor Q
Resonant frequency fr
TransducerEnergy conversion coefficient
β
Amplifiernoise temperature Tn
L0 Li
Thermal noise
€
σ x =kT
2πf0M
x
Venerdì, 14 settembre 2012
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To reach the standard quantum limit and to become comparable to the current
interferometers:
Mechanical oscillatorMass M
Temperature TQuality factor Q
Resonant frequency fr
TransducerEnergy conversion coefficient
β
Amplifiernoise temperature Tn
L0 Li
Amplifier noiseTn=VnIn/k
Thermal noise
€
σ x =kT
2πf0M
x
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To reach the standard quantum limit and to become comparable to the current
interferometers:
Mechanical oscillatorMass M
Temperature TQuality factor Q
Resonant frequency fr
TransducerEnergy conversion coefficient
β
Amplifiernoise temperature Tn
L0 Li
Amplifier noiseTn=VnIn/k
Thermal noise
€
σ x =kT
2πf0M
x
Large Mass, Low T, High Qtechnology ~ ok
Venerdì, 14 settembre 2012
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To reach the standard quantum limit and to become comparable to the current
interferometers:
Mechanical oscillatorMass M
Temperature TQuality factor Q
Resonant frequency fr
TransducerEnergy conversion coefficient
β
Amplifiernoise temperature Tn
L0 Li
Amplifier noiseTn=VnIn/k
Thermal noise
€
σ x =kT
2πf0M
x
increase β and the quality of the electrical oscillatortechnologic improvement
Large Mass, Low T, High Qtechnology ~ ok
Venerdì, 14 settembre 2012
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To reach the standard quantum limit and to become comparable to the current
interferometers:
Mechanical oscillatorMass M
Temperature TQuality factor Q
Resonant frequency fr
TransducerEnergy conversion coefficient
β
Amplifiernoise temperature Tn
L0 Li
Amplifier noiseTn=VnIn/k
Thermal noise
€
σ x =kT
2πf0M
x
increase β and the quality of the electrical oscillatortechnologic improvement
Large Mass, Low T, High Qtechnology ~ ok
Squid: technologic improvement
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Sources : Wide frequency range
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Sources : Wide frequency range
43
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Sources : Wide frequency range
A chirping system is a GW standard candle: if positionis known, distance can be
inferred.
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Sources : Wide frequency range
A chirping system is a GW standard candle: if positionis known, distance can be
inferred.
2 x 100 M BHs coalesce in 1 yr from ~ 0.1 Hz
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NS-NS Inspiral Range Improvement (LIGO)
Time progression since the start of S5
HistogramDesign Goal
Commissioningbreaks
Stuck ITMY opticat LLO
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