论文标题
关于在罗马太空望远镜的红移$ z> 7.6 $处的巴属声学振荡测量的可能性
On the possibility of Baryon Acoustic Oscillation measurements at redshift $z>7.6$ with the Roman Space Telescope
论文作者
论文摘要
Nancy Grace Roman太空望远镜（RST），其视野和高灵敏度将使高红移的宇宙学大规模结构成为可能。我们调查了在RedShifts $ z> 7.6 $中检测到Baryon声学振荡（BAO）的可能性。我们将数据中的数据与GigaparSec-Scale尺度外边缘模拟和斑驳的电离模型结合使用的数据，以创建模拟的lyman-Alpha排放线的模型，以创建模型的电动机，以创建模拟的高纬度调查GRISM数据。我们测量了模拟目录中星系的单极子，并适合BAO功能。我们发现，对于$ l = 7 \ times 10^{ - 17} \ {\ rm erg/s/cm}^{2} $的线通量，$5σ$检测限制当前设计的$5σ$检测限，BAO功能可部分检测（在四个调查中分析了四个分析的Quadrants中的四个分析）。在角直径距离到$ z = 7.7 $的结果均方根误差为7.9 $ \％$。如果我们将检测灵敏度提高了两个因子（即$ l = 3.5 \ times 10^{ - 17} \ {\ rm erg/s/s/cm}^{2} $），则距离错误将减少到$ 1.4 \％$。我们警告说，还有更多的因素尚待建模，包括灰尘遮挡，由于层次间介质引起的阻尼机翼和低红移闯入者。如果这些问题不会强烈影响结果，或者不同的观察技术（例如使用多条线）可以减轻它们，则可能能够将角直径距离限制为高红移宇宙。
The Nancy Grace Roman Space Telescope (RST), with its field of view and high sensitivity will make surveys of cosmological large-scale structure possible at high redshifts. We investigate the possibility of detecting Baryon Acoustic Oscillations (BAO) at redshifts $z>7.6$ for use as a standard ruler. We use data from the hydrodynamic simulation \textsc{BlueTides} in conjunction with the gigaparsec-scale Outer Rim simulation and a model for patchy reionization to create mock RST High Latitude Survey grism data for Lyman-alpha emission line selected galaxies at redshifts $z=7.4$ to $z=10$, covering 2280 square degrees. We measure the monopoles of galaxies in the mock catalogues and fit the BAO features. We find that for a line flux of $L = 7\times 10^{-17} \ {\rm erg/s/cm}^{2}$, the $5 σ$ detection limit for the current design, the BAO feature is partially detectable (measured in three out of four survey quadrants analysed independently). The resulting root mean square error on the angular diameter distance to $z=7.7$ is 7.9$\%$. If we improve the detection sensitivity by a factor of two (i.e. $L = 3.5\times 10^{-17} \ {\rm erg/s/cm}^{2}$), the distance error reduces to $1.4\%$. We caution that many more factors are yet to be modelled, including dust obscuration, the damping wing due to the intergalactic medium, and low redshift interlopers. If these issues do not strongly affect the results, or different observational techniques (such as use of multiple lines) can mitigate them, RST or similar instruments may be able to constrain the angular diameter distance to the high redshift Universe.
