GW number count can be used as a novel tracer of the large scale structure (LSS) in the luminosity distance space (LDS), just like galaxies in the redshift space. It is possible to obtain the $D_L-D_A$ duality relation with clustering effect. However, the peculiar velocity dispersion error of the host galaxy and the foreground lensing magnification will contaminate the GW luminosity distance measurement, and will degrade the GW clustering from a spectroscopic-like data down to a photometric-like data. In this paper, we investigate how these LSS induced distance errors modify our cosmological parameter precision inferred from the LDS clustering for the Big Bang Observatory (BBO) and the Einstein Telescope (ET). We forecast the parameter estimation errors on the angular diameter distance $D_A$, luminosity distance space Hubble parameter $H_L$ and structure growth rate $f_L{\sigma }_8$ with a Fisher matrix method. We find that for BBO, it is possible to constrain the cosmological parameters with a relative error of $10^{-3}$ to $10^{-2}$ below $D_L<5$ Gpc. The velocity dispersion error is dominant in the low luminosity distance range, while the lensing magnification error is the bottleneck in the large luminosity distance range. To reduce the lensing error, we assumed two different delensing efficiencies, namely 50% (optimistic) and 10% (conservative). Even with the optimistic assumption, the fractional error increased to $O\left(1\right)$ at luminosity distance $D_L=25$ Gpc. The results for ET are similar as those from BBO. Due to the GW source number in ET is less than that from BBO, the corresponding results also get a bit worse.

GW 数计数可以用作光度距离空间 (LDS) 中大尺度结构 (LSS) 的新型示踪剂，就像红移空间中的星系一样。有可能获得${丁}_{\mathrm{大号}}-{丁}_A$与聚类效应的二元关系。然而，宿主星系特有的速度色散误差和前景透镜放大率会污染 GW 光度距离测量，并将 GW 聚类从类光谱数据退化为类光度数据。在本文中，我们研究了这些 LSS 引起的距离误差如何修改我们从大爆炸天文台 (BBO) 和爱因斯坦望远镜 (ET) 的 LDS 聚类推断出的宇宙学参数精度。我们预测角直径距离的参数估计误差${丁}_A$, 光度距离空间哈勃参数$H_{\mathrm{大号}}$和结构增长率$F_{\mathrm{大号}}{\sigma }_{\mathrm{8个}}$使用 Fisher 矩阵方法。我们发现对于 BBO，可以用相对误差来约束宇宙学参数$\mathrm{1个}{0}^{-\mathrm{3个}}$到$\mathrm{1个}{0}^{-\mathrm{2个}}$以下${丁}_{\mathrm{大号}}<\mathrm{5个}$GPC。速度色散误差在低光度距离范围内占主导地位，而透镜放大误差是大光度距离范围内的瓶颈。为了减少透镜误差，我们假设了两种不同的脱透镜效率，即 50%（乐观）和 10%（保守）。即使采用乐观的假设，分数误差也会增加到$欧\left(\mathrm{1个}\right)$在光度距离${丁}_{\mathrm{大号}}=25$GPC。ET 的结果与 BBO 的结果相似。由于 ET 中的 GW 源数小于 BBO 中的 GW 源数，相应的结果也变得更差。