EDGE-INFERNO：模拟暗弱矮星系中每一颗可观测恒星及其对分辨恒星测光巡天的影响
EDGE-INFERNO: Simulating every observable star in faint dwarf galaxies and their consequences for resolved-star photometric surveys
AI总结：
针对暗弱矮星系观测仅见亮星的问题，提出EDGE-INFERNO放大宇宙学模拟，解析追踪所有可观测恒星，首次预测约10万恒星的颜色-星等图与空间分布，揭示结构参数测量偏差及小样本散粒噪声影响，提升矮星系数据解释的稳健性。
摘要：
对暗弱矮星系数据的解释因观测仅局限于最明亮的恒星而变得具有挑战性。我们提出了一项重大改进来应对这一挑战，通过开展放大宇宙学模拟，解析所有质量大于$0.5\\,{\rm M}_{\odot}$的单个恒星的演化，从而在哈勃时间内显式追踪所有可观测恒星。我们首次直接从其宇宙学初始条件出发，预测了四个暗弱（$M_{\star} \approx 10^5 \\, \\,{\rm M}_{\odot}$）矮星系中约$100,000$颗恒星的可观测颜色-星等图及其空间分布。在所有情况下，模拟都预测出具有多分量的复杂光分布轮廓，这意味着对结构参数的典型观测测量可能使总V波段星等看起来比模拟估计值暗多达0.5等。此外，当仅能观测到少量（$\lessapprox100$）恒星时，颜色-星等图实现产生的散粒噪声所引入的不确定性与总体星等、半光半径和平均铁丰度测量中的总体散布相当。利用完全自洽的质量增长、恒星形成和化学增丰历史来估计这些不确定性，为更稳健地解释矮星系数据铺平了道路。
英文摘要：
Interpretation of data from faint dwarf galaxies is made challenging by observations limited to only the brightest stars. We present a major improvement to tackle this challenge by undertaking zoomed cosmological simulations that resolve the evolution of all individual stars more massive than $0.5\,{\rm M}_{\odot}$, thereby explicitly tracking all observable stars for the Hubble time. For the first time, we predict observable color-magnitude diagrams and the spatial distribution of $\approx 100,000$ stars within four faint ($M_{\star} \approx 10^5 \, \,{\rm M}_{\odot}$) dwarf galaxies directly from their cosmological initial conditions. In all cases, simulations predict complex light profiles with multiple components, implying that typical observational measures of structural parameters can make total V-band magnitudes appear up to 0.5 mag dimmer compared to estimates from simulations. Furthermore, when only small ($\lessapprox100$) numbers of stars are observable, shot noise from realizations of the color-magnitude diagram introduces uncertainties comparable to the population scatter in, e.g., total magnitude, half-light radius, and mean iron abundance measurements. Estimating these uncertainties with fully self-consistent mass growth, star formation and chemical enrichment histories paves the way for more robust interpretation of dwarf galaxy data.
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