Clustering with JWST: Constraining galaxy host halo masses, satellite quenching efficiencies, and merger rates at z = 4−10
Clustering with JWST: Constraining galaxy host halo masses, satellite quenching efficiencies, and merger rates at z = 4−10
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DOI：
10.1093/mnras/staa324
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发表时间：
2019-07
影响因子：
4.8
通讯作者：
R. Endsley;P. Behroozi;D. Stark;C. Williams;B. Robertson;M. Rieke;S. Gottlöber;G. Yepes
中科院分区：
文献类型：
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作者：
R. Endsley;P. Behroozi;D. Stark;C. Williams;B. Robertson;M. Rieke;S. Gottlöber;G. Yepes
星系聚类测量可用于约束星系演化的许多方面，包括星系宿主晕质量、卫星猝灭效率和合并率。我们利用经验模型（宇宙机器）生成的模拟星系样本来模拟 z ∼ 4-10 处的 JWST 星系聚类测量。我们还采用计划为第 1 周期计划的 NIRCam 和 NIRSpec 联合保证时间观测计划的勘测足迹和典型深度，以生成现实的 JWST 勘测实现并模拟高红移星系选择完整性。我们发现，在 z ∼ 4-10 处，星系团的显着性为 ≳5σ。对于 z ∼ 4-10 处的微弱 (−18 ≳ $\mathit {M}_{\mathrm{UV}}^{ }$ ≳ −19) 星系，第 1 周期角聚类测量产生的晕质量精度将为 ∼0.2 dex，对于明亮星系 ($\mathit {M}_{\mathrm{UV}}^{ }$ ∼ −20) z ∼ 4–7 处的星系。通过消除偶然投影和低红移污染物，超过 ∼150 arcmin2 的专用光谱跟踪可以将这些精度提高 ∼0.1 dex。因此，未来的 JWST 观测将为再电离时期的恒星-晕质量关系提供第一个约束，并实质上阐明这种关系在 z > 4 时如何演化。我们还发现，JWST 将在 z ∼ 4-8 处识别出 ~1000 颗单独的卫星，从而能够对超出当前可用数据 (z ≲ 2) 的卫星淬灭演化进行强有力的测试。最后，我们发现 JWST 观测可以测量 z ∼ 4-8 处星系主要合并对分数的演化，不确定性为 ∼0.1-0.2 dex。这样的测量将有助于确定合并对进入再电离时代恒星质量积累的相对作用。
Galaxy clustering measurements can be used to constrain many aspects of galaxy evolution, including galaxy host halo masses, satellite quenching efficiencies, and merger rates. We simulate JWST galaxy clustering measurements at z ∼ 4–10 by utilizing mock galaxy samples produced by an empirical model, the universemachine. We also adopt the survey footprints and typical depths of the planned joint NIRCam and NIRSpec Guaranteed Time Observation program planned for Cycle 1 to generate realistic JWST survey realizations and to model high-redshift galaxy selection completeness. We find that galaxy clustering will be measured with ≳5σ significance at z ∼ 4–10. Halo mass precisions resulting from Cycle 1 angular clustering measurements will be ∼0.2 dex for faint (−18 ≳ $\mathit {M}_{\mathrm{UV}}^{ }$ ≳ −19) galaxies at z ∼ 4–10 as well as ∼0.3 dex for bright ($\mathit {M}_{\mathrm{UV}}^{ }$ ∼ −20) galaxies at z ∼ 4–7. Dedicated spectroscopic follow-up over ∼150 arcmin2 would improve these precisions by ∼0.1 dex by removing chance projections and low-redshift contaminants. Future JWST observations will therefore provide the first constraints on the stellar–halo mass relation in the epoch of reionization and substantially clarify how this relation evolves at z > 4. We also find that ∼1000 individual satellites will be identifiable at z ∼ 4–8 with JWST, enabling strong tests of satellite quenching evolution beyond currently available data (z ≲ 2). Finally, we find that JWST observations can measure the evolution of galaxy major merger pair fractions at z ∼ 4–8 with ∼0.1–0.2 dex uncertainties. Such measurements would help determine the relative role of mergers to the build-up of stellar mass into the epoch of reionization.