We present the 3-dimensional intrinsic alignment power spectra between the projected 2d galaxy shape/spin and the 3d tidal field across 0.1<k/<60 using cosmological hydrodynamical simulation, Illustris-TNG300, at redshifts ranging from 0.3 to 2. The shape-tidal field alignment increases with galaxy mass and the linear alignment coefficient A_IA, defined with respect to the primordial tidal field, is found to have weak redshift dependence. We also show a promising detection of the shape/spin-tidal field alignments for stellar mass limited samples and a weak or almost null signal for star-forming galaxies for the TNG300 volume, ∼ 0.01(h^-1 Gpc)³. We further study the morphology and environmental dependence of the intrinsic alignment power spectra. The shape of massive disk- and spheroid-galaxies tend to align with the tidal field. The spin of low mass disks (and spheroids at low redshifts) tend to be parallel with the tidal field, while the spin of massive spheroids and disks tend to be perpendicular to tidal field. The shape and spin of massive centrals align with the tidal field at both small and large scales. Satellites show a radial alignment within the one-halo term region, and low mass satellites have an intriguing alignment signal in the two-halo term region. We also forecast a feasibility to measure the intrinsic alignment power spectrum for spectroscopic and imaging surveys such as Subaru HSC/PFS and DESI. Our results thus suggest that galaxy intrinsic alignment can be used as a promising tool for constraining the galaxy formation models.

我们使用宇宙学流体动力学模拟 Illustris-TNG300，在 0.1<k/<60 范围内呈现投影的 2d 星系形状/自旋和 3d 潮汐场之间的 3维固有对齐功率谱，红移范围为 0.3 到 2。潮汐场对齐随着星系质量的增加而增加，并且发现相对于原始潮汐场定义的线性对齐系数 A _{IA具有较弱的红移依赖性。}我们还展示了对恒星质量有限样本的形状/自旋潮汐场对齐的有希望的检测以及对于 TNG300 体积的恒星形成星系的微弱或几乎为零的信号，~ 0.01(h ^-1 Gpc) ³. 我们进一步研究了固有对齐功率谱的形态和环境依赖性。大质量盘状星系和球状星系的形状往往与潮汐场对齐。低质量圆盘（和低红移球体）的自旋倾向于与潮汐场平行，而大质量球体和圆盘的自旋倾向于垂直于潮汐场。大质量中心的形状和自旋在小尺度和大尺度上都与潮汐场一致。卫星在单晕项区域内显示出径向对准，而低质量卫星在双晕项区域内具有有趣的对准信号。我们还预测了测量光谱和成像调查（如斯巴鲁 HSC/PFS 和 DESI）的内在对准功率谱的可行性。