Stanford Program in Support of LIGO

近100年前，爱因斯坦的广义相对论预言了引力波，但由于所需的极端敏感性，引力波尚未被探测到。潜在来源的例子包括相互作用的黑洞、合并的致密双星系统、恒星崩塌和脉冲星。激光干涉仪引力波天文台(LIGO)是为了测量引力波在时空结构中产生的应变而建造的。然而，最初的版本足够敏感，只能看到进入宇宙的一条捷径。随着最近的升级完成，高级LIGO将很快投入运行，灵敏度是LIGO的十倍。当它达到设计灵敏度时，它应该能够探测到远至室女座星系团的引力波源，并启动引力波天文学，作为宇宙的一个新窗口。斯坦福大学在开发LIGO等探测器技术方面有一个强大的多学科项目。参与者包括机械、电气和控制工程师、物理学家和材料研究人员。该计划为未来的科学家和工程师提供本科和研究生水平的培训；它将基础科学研究与科学教育相结合；它还开发和资助向更广泛的社区提供信息和教育的外展计划。斯坦福大学从事LIGO计划引力波探测的研究和开发。将开发改进的地震隔离和对准系统平台，以便在目前地面振动限制灵敏度的低频下实现更高的灵敏度。光学研究仍将是一个活跃的研究领域，以降低非晶态光学涂层中由热驱动的机械波动造成的噪声，目前预计这将限制Advanced LIGO在其最敏感的频段约1000赫兹的灵敏度。对非晶态涂层的原子结构的研究将侧重于更好地理解导致机械损失的微观机制，这将导致过多的热噪声。拟议研究的主旨是降低风险并促进高级LIGO的成功，并使引力波天文学的开启成为可能。

Gravitational waves were predicted almost 100 years ago in Einstein's General Theory of Relativity, but they have not yet been detected due to the extreme sensitivity required. Examples of potential sources include interacting black holes, coalescing compact binary stellar systems, stellar collapses, and pulsars. The Laser Interferometer Gravitational-wave Observatory (LIGO) was built to measure strains in the fabric of space-time that are produced by gravitational waves. However, the initial version was sensitive enough to see only a short way into the Cosmos. With completion of a recent upgrade, Advanced LIGO will soon become operational with ten times the sensitivity of LIGO. When it reaches design sensitivity, it should be able to detect gravity wave sources as far away as the Virgo cluster of galaxies and launch gravitational wave astronomy as a new window on the Universe. Stanford has a strong, multidisciplinary program in developing the technology for detectors such as LIGO. Participants include mechanical, electrical and control engineers, physicists and materials researchers. The program provides training for future scientists and engineers at both the undergraduate and graduate levels; it integrates basic scientific research with scientific education; and it develops and funds outreach programs that inform and educate the broader community.Stanford is engaged in research and development on gravitational wave detection for the LIGO program. Improved seismic isolation and alignment system platforms will be developed to enable higher sensitivity at low frequencies where ground vibrations currently limit sensitivity. Studies of the optics will remain an active area of research to reduce noise from thermally-driven mechanical fluctuations in their amorphous optical coatings, which is now predicted to limit the sensitivity of Advanced LIGO in its most sensitive frequency band around 1000 Hz. Investigations of the atomic structure of the amorphous coatings will focus on a better understanding of the microscopic mechanisms that cause mechanical loss, which results in excess thermal noise. The thrust of the proposed research is to reduce risk and facilitate the success of Advanced LIGO, and to enable an opening of gravitational wave astronomy.