François BONDU (Observatoire de la Côte d'Azur) mail

The Gravitational Wave Detector Virgo

2 lectures:November  9th, 10th 2006

(last update of this page : 2006, Nov. 10th)


I.                   Target spectral resolution and fundamental noise sources (also c.f. J.Y. Vinet course here, Virgo reference here)

a.       Laser frequency noise

b.      Photon shot noise

c.       Thermal noise of test masses

d.      Thermal noise of pendulum

II.                Mirror suspension and control

a.       Passive attenuation of seismic noise

b.      Feedback loops

c.       Interferometer longitudinal degrees of freedom control

d.      Interferometer angular degrees of freedom control

III.             Optical performances

a.       The Fabry-Perot cavity in practice

b.      Mirror metrology

c.       Optical simulation

d.      In-situ metrology

IV.             Virgo history and performances

a.       Design

b.      Virgo systems

c.       Commissioning

d.      Actual performances (see also talks of M.-A. Bizouard, E. Chassande-Mottin, B. Mours, A. Viceré, J-Y Vinet here)

e.       2008/2009: Virgo+

f.       2013: Advanced VIRGO

g.      Other detectors: LIGO, Advanced LIGO, GEO, TAMA, LCGT, ACIGA.





The Virgo large mirrors: a challenge for low loss coatings, The Virgo collaboration, Class. Quantum Grav. 21 (2004) S935-S945

Measurement of the Virgo superattenuator performance for seismic noise suppression, Review of Scientific Instruments, Vol. 12, No. 9 (2001), pp 3643-3652

The Virgo status”, The Virgo collaboration, Class. Quant. Grav. 23 No 19 (2006) S635-S642



Other G.W. detection experiments:

LIGO (U.S.A.):

ACIGA (Australia):

GEO 600 (Germany/U.K.):

TAMA (Japan):

Advanced LIGO:


Fabry-Perot cavities:

“A taste of Fabry and Perot’s discoveries”, Ph. Amram and Y. Georgelin, Physica Scripta. Vol. T86, 76-82, 2000