Operation and Enhancement of the LSU Gravitational Wave Observatory

WPC ' 2 B P Z Courier 10cpi #| x x @ 8；X @信头- HP Laserjet II HPLASER2。PRS x @, t 0# lX @ 2 Z L $ #| x BOND - HP Laserjet II HPLASERJ。PRS x @， t 0# BmX @ Courier 10cpi行打印机16.67cpi 2 x F ' ^ 2 x x x, x @ 8；X @ t j, H H H, H | @；我提出了一种新型探测器的建议，这种探测器有望灵敏得多。路易斯安那州立大学的探测器已经观测了2年。LSU的引力物理小组将继续进行一项研究计划，其目标是探测引力波的短爆发。该方案包括三个部分：1)继续使用LSU棒状引力波天线进行观测；2)提高其灵敏度；3)准备一种新型探测器的详细设计，这种探测器的灵敏度有望大大提高。路易斯安那州立大学的探测器已经观测了2年。它对短脉冲的灵敏度是目前任何地方的任何探测器所能获得的最好的（平均爆发引力应变2 '噪声是6 × 10 19），并且可能足以探测到来自我们星系内超新星的引力波。路易斯安那州立大学的研究小组将继续操作他们的探测器，直到他们准备好提高其灵敏度。数据交换和搜索与任何其他运行的探测器的一致性将继续进行。路易斯安那州立大学的研究小组还将研究一种接近球形的新型探测器，即截断二十面体引力波天线（TIGA）。他们已经公布了计算结果，预测TIGA探测器的能量灵敏度比等效的条形天线提高56倍。TIGA系统可以由几个不同频率的全方位探测器组成，所有这些探测器都被设计成相互配合并与激光干涉引力（LIGO）配合工作。路易斯安那州立大学的研究小组将继续他们的计划，通过在TIGA原型上进行实验测量来验证理论预测。路易斯安那州立大学重力物理小组将与其他美国共振质量探测器小组合作，承担引力波探测器TIGA系统的详细设计。这项合作研究工作的目标是，在1995年1月以前，为该系统连同世界上所有其他引力波探测器的建造和操作，制定一份详细的设计和计划。＊＊＊

WPC` 2 B P Z Courier 10cpi #| x x @ 8 ; X @ LETTERHEAD - HP Laserjet II HPLASER2.PRS x @ , t 0# lX @ 2 Z L $ #| x BOND - HP Laserjet II HPLASERJ.PRS x @ , t 0# BmX @ Courier 10cpi Line Printer 16.67cpi 2 X F ` ^ 2 x x x , x @ 8 ; X @ t j , H H H , H | @ ; @ iled proposal for a new type of detector which promises to be much more sensitive. The LSU detector has been observing for 2 years. Its sensitivity to short b 9311731 Hamilton The LSU gravitational physics group will continue with a program of research which has the goal of detecting a short burst of gravitational waves. The program has three parts: 1) continued observation with the LSU bar type gravitational wave antenna, 2) improvement of its sensitivity; and 3) preparation of a detailed design for a new type of detector which promises to be much more sensitive. The LSU detector has been observing for 2 years. Its sensitivity to short bursts is now the best ever obtained by any detector anywhere (average burst gravitational strain 2 ` noise is 6x10 19 ), and is probably sufficient to detect the gravitational waves from a supernova within our galaxy. The LSU group will continue to operate their detector, until they are ready to improve its sensitivity. Data exchange and searches for coincidences with any other detectors operational will continue. The LSU group will also investigate a new type of detector with a nearly spherical shape, the Truncated Icosahedral Gravitational wave Antenna, or TIGA. They have already published calculati ons that predict a 56 fold increase in energy sensitivity for a TIGA detector, compared to the equivalent bar type antenna. A TIGA system could consist of several omni directional detectors at different frequencies, all designed to work in coincidence with each other and with the Laser Interferometer Gravitational (LIGO). The LSU group will continue its program to verify the theoretical predictions by experimental measurement on a prototype TIGA. In collaboration with other U.S. resonant mass detector groups, the LSU gravitational physics group will undertake the detailed design of a TIGA system of gravitational wave detectors. The goal of the collaborative research effort will be the production, by January of 1995, of a detailed design and a plan for the construction and operation of the system in conjunction with all other gravitational wave detectors in the world. ***