A Xylophone Configuration for a third Generation Gravitational Wave Detector Export

@article{citeulike:4866692, abstract = {Achieving the demanding sensitivity and bandwidth, envisaged for third generation gravitational wave (GW) observatories, is extremely challenging with a single broadband interferometer. Very high optical powers (Megawatts) are required to reduce the quantum noise contribution at high frequencies, while the interferometer mirrors have to be cooled to cryogenic temperatures in order to reduce thermal noise sources at low frequencies. To resolve this potential conflict of cryogenic test masses with high thermal load, we present a conceptual design for a 2-band xylophone configuration for a third generation GW observatory, composed of a high-power, high-frequency interferometer and a cryogenic low-power, low-frequency instrument. Featuring inspiral ranges of 3200Mpc and 38000Mpc for binary neutron stars and binary black holes coalesences, respectively, we find that the potential sensitivity of xylophone configurations can be significantly wider and better than what is possible in a single broadband interferometer.}, archivePrefix = {arXiv}, author = {Hild, Stefan and Chelkowski, Simon and Freise, Andreas and Franc, Janyce and Morgado, Nazario and Flaminio, Raffaele and Desalvo, Riccardo}, citeulike-article-id = {4866692}, citeulike-linkout-0 = {http://arxiv.org/abs/0906.2655}, citeulike-linkout-1 = {http://arxiv.org/pdf/0906.2655}, day = {15}, eprint = {0906.2655}, keywords = {interferometers}, month = {Jun}, posted-at = {2009-06-16 07:50:57}, priority = {2}, title = {A Xylophone Configuration for a third Generation Gravitational Wave Detector}, url = {http://arxiv.org/abs/0906.2655}, year = {2009} }

TY - JOUR ID - citeulike:4866692 L3 - citeulike-article-id:4866692 N2 - Achieving the demanding sensitivity and bandwidth, envisaged for third generation gravitational wave (GW) observatories, is extremely challenging with a single broadband interferometer. Very high optical powers (Megawatts) are required to reduce the quantum noise contribution at high frequencies, while the interferometer mirrors have to be cooled to cryogenic temperatures in order to reduce thermal noise sources at low frequencies. To resolve this potential conflict of cryogenic test masses with high thermal load, we present a conceptual design for a 2-band xylophone configuration for a third generation GW observatory, composed of a high-power, high-frequency interferometer and a cryogenic low-power, low-frequency instrument. Featuring inspiral ranges of 3200Mpc and 38000Mpc for binary neutron stars and binary black holes coalesences, respectively, we find that the potential sensitivity of xylophone configurations can be significantly wider and better than what is possible in a single broadband interferometer. TI - A Xylophone Configuration for a third Generation Gravitational Wave Detector KW - interferometers AU - Hild, Stefan AU - Chelkowski, Simon AU - Freise, Andreas AU - Franc, Janyce AU - Morgado, Nazario AU - Flaminio, Raffaele AU - Desalvo, Riccardo PY - 2009/Jun/15/ UR - http://arxiv.org/abs/0906.2655 ER -