基于聚类的红移高星系暗物质晕质量分配：方法、验证及其在JWST中的应用
Clustering-based halo mass assignment for high-redshift galaxies: method, validation, and application to JWST
浏览论文内容
中文总结 AI 辅助
提出基于聚类的高红移星系暗物质晕质量分配方法，经模拟验证，应用于JWST样本，提供稳健经验校准的晕质量，有助于约束再电离期星系形成。
中文摘要 AI 辅助
我们提出了一种基于聚类的方法来推断高红移星系的暗物质晕质量，并使用COLIBRE模拟结合HOMA经验模型进行了验证，该模型假设恒星形成与暗物质晕吸积率成正比，并根据JWST观测进行了校准。我们的方法将恒星质量分箱中的星系两点相关函数与参考暗物质晕聚类进行匹配，在最优径向范围0.5 < r_p/cMpc < 1.0内建立了恒星-暗物质晕质量关系。与真实暗物质晕质量的验证显示偏差极小，在体积低至(50 cMpc)^3、红移至z=12的情况下，散射低于0.3 dex，即使对于测光数据也是如此。使用原生COLIBRE星族进行的交叉验证表明，该方法对不同星系-暗物质晕模型具有鲁棒性。巡天体积主导误差预算：场间聚类振幅的变化对于测光（光谱）样本可达3（2）倍，转化为暗物质晕质量的0.3-0.5 dex不确定性。按恒星形成率、颜色和年龄等属性对样本进行分割可减轻组装偏差，这相对于丰度匹配具有关键优势。应用于JWST（JADES）在z=6和10的样本，对于M_UV < -17的星系，得到的暗物质晕质量为log M_h/M_sun = 10.52_{-0.21}^{+0.12}和9.91_{-0.34}^{+0.19}，线性偏差分别为b_h = 4.2_{-0.41}^{+0.26}和7.7_{-1.16}^{+0.77}。当前数据无法区分恒星形成模型。我们的Roman Deep Tier预测表明，在z=10时，对于M_UV < -21的星系，推断的暗物质晕质量在爆发式和非爆发式模型之间相差0.5 dex，但预期的星系对数量限制了约束能力。我们的框架提供了稳健且经验校准的暗物质晕质量，这对于解释JWST观测和约束再电离期间的星系形成至关重要。
英文摘要
We present a clustering-based method for inferring halo masses of high-redshift galaxies, validated using the COLIBRE simulations combined with the HOMA empirical model, which assumes star formation to be proportional to halo accretion rate and is calibrated to JWST observations. Our approach matches the two-point correlation function of galaxies in stellar mass bins to reference halo clustering, establishing the stellar-to-halo mass relation over an optimal radial range 0.5 < r_p/cMpc < 1.0. Validation against true halo masses shows minimal bias, with scatter below 0.3 dex for volumes down to (50 cMpc)^3 and redshifts to z=12, even for photometric data. Cross-validation using the native COLIBRE population shows that the method is robust to the different galaxy-halo prescriptions. Survey volume dominates the error budget: field-to-field variations in the clustering amplitude vary by factors of 3 (2) for photometric (spectroscopic) samples, translating to 0.3-0.5 dex uncertainty in halo masses. Splitting the sample by properties such as SFR, colour, and age mitigates assembly bias, offering a key advantage over abundance matching. Application to JWST (JADES) samples at z=6 and 10 yields halo masses of log M_h/M_sun = 10.52_{-0.21}^{+0.12} and 9.91_{-0.34}^{+0.19} for M_UV < -17 galaxies, with linear biases of b_h = 4.2_{-0.41}^{+0.26} and 7.7_{-1.16}^{+0.77}, respectively. Current data cannot distinguish between star formation models. Our Roman Deep Tier forecasts indicate that at z=10, the inferred halo masses for M_UV < -21 galaxies differ by 0.5 dex between bursty and non-bursty models, but the expected number of pairs limits the constraining power. Our framework provides robust, empirically-calibrated halo masses essential for interpreting JWST observations and constraining galaxy formation during reionization.
发表机构
- University of Cambridge（剑桥大学）
- Leiden University（莱顿大学）
机构由 AI 辅助整理，请以论文原文为准。
