论文标题
IMF与ELT和MICADO I研究的未来：本地宇宙作为已解决的IMF实验室
The Future of IMF studies with the ELT and MICADO I: The local Universe as a resolved IMF laboratory
论文作者
论文摘要
目标。在这项工作中，我们旨在估算Micado在ELT的最低恒星质量，并且在恒星密度和距离的情况下将能够可靠地检测到。我们还表明，可以发挥关键作用的工具效应，并报告与ELT本地宇宙中IMF研究可以访问的年轻群集的数量。 方法。我们使用Simcado（Micado相机的仪器模拟器包装）来生成56个密集的恒星区域的观测，其密度与年轻恒星簇的岩心相似。我们将群集场放置在距地球8 kpc和5 mpc之间的距离，这意味着核心密度从10^2到10^5 stars arcsec^-2，并确定了每个恒星场通过点范围函数（PSF）拟合光度法的最低可靠观察到的质量。 结果。我们的结果表明，<10^3星的恒星密度很容易通过Micado解析。对于密度<10^3 stars arcsec^-2的簇，大麦芽云中最低的可靠观察质量将约为0.1 msun。 Micado将能够访问Magellanic Clouds中所有密集的年轻恒星簇的核心的恒星内容，从而使IMF的峰值和形状在银河系外的详细范围内进行了详细的研究。在2 MPC的距离下，所有具有M> 2 MSUN的星星将在<10^4星ArcSec^-2的田地中解析，从而使IMF的高质量端在所有星系中都可以在所有星系中进行研究，包括NGC300。
Aims. In this work we aim to estimate the lowest stellar mass that MICADO at the ELT will be able to reliably detect given a stellar density and distance. We also show that instrumental effects that will play a critical role, and report the number of young clusters that will be accessible for IMF studies in the local Universe with the ELT. Methods. We used SimCADO, the instrument simulator package for the MICADO camera, to generate observations of 56 dense stellar regions with densities similar to the cores of young stellar clusters. We placed the cluster fields at distances between 8 kpc and 5 Mpc from the Earth, implying core densities from 10^2 to 10^5 stars arcsec^-2, and determined the lowest reliably observable mass for each stellar field through point-spread function (PSF) fitting photometry. Results. Our results show that stellar densities of <10^3 stars arcsec^-2 will be easily resolvable by MICADO. The lowest reliably observable mass in the Large Magellanic Cloud will be around 0.1 Msun for clusters with densities <10^3 stars arcsec^-2. MICADO will be able to access the stellar content of the cores of all dense young stellar clusters in the Magellanic Clouds, allowing the peak and shape of the IMF to be studied in great detail outside the Milky Way. At a distance of 2 Mpc, all stars with M > 2 Msun will be resolved in fields of <10^4 stars arcsec^-2 , allowing the high-mass end of the IMF to be studied in all galaxies out to and including NGC300.
