Third-generation gravitational wave observatories will extend the lower frequency limit of the observation band toward 2 Hz, where new sources of gravitational waves, in particular intermediate-mass black holes (IMBH), will be detected. In this frequency region, seismic noise will play an important role, mainly through the so-called Newtonian noise, i.e., the gravity-mediated coupling between ground motion and test mass displacements. The signal lifetime of such sources in the detector is of the order of tens of seconds. In order to determine whether a candidate site to host the Einstein Telescope observatory is particularly suitable to observe such sources, it is necessary to estimate the probability distributions that, in the characteristic time scale of the signal, the sensitivity of the detector is not perturbed by Newtonian noise. In this paper, a first analysis is presented, focused on the Sos Enattos site (Sardinia, Italy), a candidate to host the Einstein Telescope. Starting from a long data set of seismic noise, this distribution is evaluated considering both the presently designed triangular ET configuration and also the classical ”L” configuration.

第三代重力波观测站将把观测频带的下限扩展到2 Hz，在那里将检测到新的重力波源，特别是中间质量黑洞（IMBH）。在这个频率区域中，地震噪声将起重要作用，主要是通过所谓的牛顿噪声，即地面运动与测试质量位移之间的重力作用耦合。检测器中此类源的信号寿命约为数十秒。为了确定容纳爱因斯坦望远镜天文台的候选站点是否特别适合于观测此类源，有必要估计概率分布，该分布在信号的特征时间标度中不会干扰检测器的灵敏度。牛顿噪声。在本文中，我们将对以爱因斯坦望远镜的候选地Sos Enattos站点（意大利撒丁岛）为中心进行首次分析。从地震噪声的长数据集开始，在考虑当前设计的三角ET配置和经典“ L”配置的情况下评估此分布。