The kinetic Sunyaev-Zel’dovich effect is a secondary CMB temperature anisotropy that provides a powerful probe of the radial-velocity field of matter distributed across the Universe. This velocity field is reconstructed by combining high-resolution CMB measurements with galaxy survey data, and it provides an unbiased tracer of matter perturbations in the linear regime. In this paper, we show how this measurement can be used to probe primordial non-Gaussianity of the local type, particularly focusing on the trispectrum amplitude ${\tau }_{\mathrm{NL}}$, as may arise in a simple two-field inflation model that we provide by way of illustration. Cross-correlating the velocity-field-derived matter distribution with the biased large-scale galaxy density field allows one to measure the scale-dependent bias factor with sample variance cancellation. We forecast that a configuration corresponding to CMB-S4 and VRO results in a sensitivity of ${\sigma }_{f_{\mathrm{NL}}}\approx 0.59$ and ${\sigma }_{{\tau }_{\mathrm{NL}}}\approx 1.5$. These forecasts predict improvement factors of 10 and 195 for ${\sigma }_{f_{\mathrm{NL}}}$ and ${\sigma }_{{\tau }_{\mathrm{NL}}}$, respectively, over the sensitivity using VRO data alone, without internal sample variance cancellation. Similarly, for a configuration corresponding to DESI and SO, we forecast a sensitivity of ${\sigma }_{f_{\mathrm{NL}}}\approx 3.1$ and ${\sigma }_{{\tau }_{\mathrm{NL}}}\approx 69$, with improvement factors of 2 and 5, respectively, over the use of the DESI data set in isolation. We find that a high galaxy number density and large survey volume considerably improve our ability to probe the amplitude of the primordial trispectrum for the multifield model considered.

中文翻译：

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来自动力学 Sunyaev-Zel'dovich 断层扫描的原始三谱

动力学 Sunyaev-Zel'dovich 效应是一种次级 CMB 温度各向异性，它为分布在整个宇宙中的物质径向速度场提供了强有力的探测。该速度场是通过将高分辨率 CMB 测量与星系调查数据相结合来重建的，它提供了线性状态下物质扰动的无偏示踪剂。在本文中，我们展示了如何使用这种测量来探测局部类型的原始非高斯性，特别关注三谱幅度${\tau }_{\mathrm{荷兰}}$, as may arise in a simple two-field inflation model that we provide by way of illustration. Cross-correlating the velocity-field-derived matter distribution with the biased large-scale galaxy density field allows one to measure the scale-dependent bias factor with sample variance cancellation. We forecast that a configuration corresponding to CMB-S4 and VRO results in a sensitivity of ${\sigma }_{f_{\mathrm{NL}}}\approx 0.59$ and ${\sigma }_{{\tau }_{\mathrm{NL}}}\approx 1.5$. These forecasts predict improvement factors of 10 and 195 for ${\sigma }_{f_{\mathrm{NL}}}$ and ${\sigma }_{{\tau }_{\mathrm{NL}}}$, respectively, over the sensitivity using VRO data alone, without internal sample variance cancellation. Similarly, for a configuration corresponding to DESI and SO, we forecast a sensitivity of ${\sigma }_{f_{\mathrm{NL}}}\approx 3.1$ and ${\sigma }_{{\tau }_{\mathrm{NL}}}\approx 69$，与单独使用 DESI 数据集相比，改进因子分别为 2 和 5。我们发现，对于所考虑的多场模型，高星系数密度和大测量体积显着提高了我们探测原始三谱振幅的能力。