Titre : 
Characterization of the high frequency response of laser interferometer gravitational wave detectors 
Type de document : 
texte imprimÃ© 
Auteurs : 
William E. Butler (1975....), Auteur ; Adrian C. Melissinos, Directeur de thÃ¨se 
Editeur : 
Rochester, New York [USA] : University of Rochester. Department of physics and astronomy 
AnnÃ©e de publication : 
2004 
Importance : 
1 vol. (XX175 p.) 
PrÃ©sentation : 
fig., ill. 
Format : 
30 cm 
ISBN/ISSN/EAN : 
PPN 237431904 
Note gÃ©nÃ©rale : 
Phd thesis : Doctor of philosophy : Rochester, New York [USA] : University of Rochester. Department of physics and astronomy : june 2004 
Langues : 
Anglais (eng) 
Tags : 
Rayonnement gravitationnel  ThÃ¨ses et Ã©crits acadÃ©miques InterfÃ©romÃ©trie InterfÃ©romÃ¨tres laser VIRGO (interfÃ©romÃ¨tre) LIGO (interfÃ©romÃ¨tre) LISA (interfÃ©romÃ¨tre) Traitement du signal Gravitational waves  Thesis Gravitational waves  Measurement  Instruments Interferometry Laser interferometers LIGO (interferometer) LISA [Laser Interferometer Space Antenna] Signal processing 
Index. dÃ©cimale : 
535.4 Dispersion, interférence, diffraction de la lumière 
RÃ©sumÃ© : 
This thesis describes a search for a stochastic background of gravitational waves at high frequency, 37.52 kHz. At this frequency the separation between the available instruments excludes the use of a correlation technique. Instead I rely on the spectral response of the LASER interferometer to isolate a possible signal from the underlying noise. This research was carried out at the LIGO (LASER Interferometer Gravitational Observatory) located in Hanford, WA and within the LIGO Scientific Collaboration (LSC). Chapter 1 serves as a general introduction to the present state of the search for gravitational waves (GW). I discuss the indirect observation of gravitational radiation as well as the expected sources for GW and their characteristics. I also discuss possible future developments, in particular the Advanced LIGO instruments and the LASER Interferometer Space Antenna (LISA). The characteristics of the large LASER interferometers, layout, terminology and necessary formulae are developed in Chapter 2. To carry out the proposed search it is essential that the frequency response of the interferometer be thoroughly understood, including possible noise sources. This was the subject of a series of experimental investigations using sideband injection and mirror excitations to characterize the IFO response in the region of the first free spectral range, which is at 37.52 kHz. The results of these experiments as well as their theoretical model are presented in Chapter 3. Contributions to the spectrum from mechanical noise are investigated in Chapter 4, and compared to the expected contribution thermal excitation. The results of my search are based on data obtained during the third science run of LIGO (S3) and are presented in Chapter 5. I show that a signal such as expected from a stochastic gravitational wave background is manifest in the data and compare it to the expected noise signal. This allows me to postulate a limit on a possible stochastic background. I also discuss further possible high sensitivity measurements at these high frequencies. 
Note de contenu : 
Bibliographie p. 157165 (74 rÃ©f.) 
Characterization of the high frequency response of laser interferometer gravitational wave detectors [texte imprimÃ©] / William E. Butler (1975....), Auteur ; Adrian C. Melissinos, Directeur de thÃ¨se .  Rochester, New York (USA)Â : University of Rochester. Department of physics and astronomy, 2004 .  1 vol. (XX175 p.) : fig., ill. ; 30 cm. ISSN : PPN 237431904 Phd thesis : Doctor of philosophy : Rochester, New York [USA] : University of Rochester. Department of physics and astronomy : june 2004 Langues : Anglais ( eng)
Tags : 
Rayonnement gravitationnel  ThÃ¨ses et Ã©crits acadÃ©miques InterfÃ©romÃ©trie InterfÃ©romÃ¨tres laser VIRGO (interfÃ©romÃ¨tre) LIGO (interfÃ©romÃ¨tre) LISA (interfÃ©romÃ¨tre) Traitement du signal Gravitational waves  Thesis Gravitational waves  Measurement  Instruments Interferometry Laser interferometers LIGO (interferometer) LISA [Laser Interferometer Space Antenna] Signal processing 
Index. dÃ©cimale : 
535.4 Dispersion, interférence, diffraction de la lumière 
RÃ©sumÃ© : 
This thesis describes a search for a stochastic background of gravitational waves at high frequency, 37.52 kHz. At this frequency the separation between the available instruments excludes the use of a correlation technique. Instead I rely on the spectral response of the LASER interferometer to isolate a possible signal from the underlying noise. This research was carried out at the LIGO (LASER Interferometer Gravitational Observatory) located in Hanford, WA and within the LIGO Scientific Collaboration (LSC). Chapter 1 serves as a general introduction to the present state of the search for gravitational waves (GW). I discuss the indirect observation of gravitational radiation as well as the expected sources for GW and their characteristics. I also discuss possible future developments, in particular the Advanced LIGO instruments and the LASER Interferometer Space Antenna (LISA). The characteristics of the large LASER interferometers, layout, terminology and necessary formulae are developed in Chapter 2. To carry out the proposed search it is essential that the frequency response of the interferometer be thoroughly understood, including possible noise sources. This was the subject of a series of experimental investigations using sideband injection and mirror excitations to characterize the IFO response in the region of the first free spectral range, which is at 37.52 kHz. The results of these experiments as well as their theoretical model are presented in Chapter 3. Contributions to the spectrum from mechanical noise are investigated in Chapter 4, and compared to the expected contribution thermal excitation. The results of my search are based on data obtained during the third science run of LIGO (S3) and are presented in Chapter 5. I show that a signal such as expected from a stochastic gravitational wave background is manifest in the data and compare it to the expected noise signal. This allows me to postulate a limit on a possible stochastic background. I also discuss further possible high sensitivity measurements at these high frequencies. 
Note de contenu : 
Bibliographie p. 157165 (74 rÃ©f.) 
