Feedback-free starbursts at cosmic dawn. Observable predictions for JWST

Zhaozhou Li, A. Dekel, Kartick C. Sarkar, Han Aung, M. Giavalisco, Nir Mandelker, S. Tacchella
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Abstract

We extend the analysis of a physical model within the standard cosmology that robustly predicts a high star-formation efficiency (SFE) in massive galaxies at cosmic dawn due to feedback-free starbursts (FFBs). This model implies an excess of bright galaxies at $z 10$ compared to the standard models based on the low SFE at later epochs, an excess that is indicated by JWST observations. Here we provide observable predictions of galaxy properties based on the analytic FFB scenario. These can be compared with simulations and JWST observations. We use the model to approximate the SFE as a function of redshift and mass, assuming a maximum SFE of $ max 1$ in the FFB regime. From this, we derive the evolution of the galaxy mass and luminosity functions as well as the cosmological evolution of stellar and star-formation densities. We then predict the star-formation history (SFH), galaxy sizes, outflows, gas fractions, metallicities, and dust attenuation, all as functions of mass and redshift in the FFB regime. The major distinguishing feature of the model is the occurrence of FFBs above a mass threshold that declines with redshift. The luminosities and star formation rates in bright galaxies are predicted to be in excess of extrapolations of standard empirical models and standard cosmological simulations, an excess that grows from $z 9$ to higher redshifts. The FFB phase of $ is predicted to show a characteristic SFH that fluctuates on a timescale of $ The stellar systems are compact ($ at $z 10$ and declining with $z$). The galactic gas consists of a steady wind driven by supernovae from earlier generations, with high outflow velocities FWHM low gas fractions ($<\!0.1$), low metallicities ($ and low dust attenuation UV 0.5$ at $z 10$ and declining with $z$). We make tentative comparisons with current JWST observations for initial insights, anticipating more complete and reliable datasets for detailed quantitative comparisons in the future. The FFB predictions are also offered in digital form.
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宇宙黎明时的无反馈星爆。对 JWST 的可观测预测
我们对标准宇宙学中的一个物理模型的分析进行了扩展,该模型有力地预测了大质量星系在宇宙黎明时由于无反馈星爆(FFBs)而产生的高恒星形成效率(SFE)。与基于后期低恒星形成效率的标准模型相比,该模型意味着在$z 10$的明亮星系过多,JWST的观测结果也表明了这一点。在这里,我们提供了基于解析FFB方案的星系性质的可观测预测。我们假定在FFB体系中SFE的最大值为$ max 1$,并利用该模型将SFE近似为红移和质量的函数。由此,我们得出了星系质量和光度函数的演变,以及恒星密度和恒星形成密度的宇宙学演变。然后,我们预测恒星形成历史(SFH)、星系大小、外流、气体分数、金属性和尘埃衰减,所有这些都是 FFB 系统中质量和红移的函数。该模型的主要特征是出现质量阈值以上的 FFB,而质量阈值随着红移的减小而减小。据预测,明亮星系的光度和恒星形成率将超过标准经验模型和标准宇宙学模拟的推断值,而且从 $z 9$ 到更高的红移,这种超量会越来越大。据预测,$的FFB阶段将显示出一种特征性的SFH,其波动的时间尺度为$ 恒星系统是紧凑的($在$z 10$时,随着$z$的增大而减小)。银河气体由前代超新星驱动的稳定风组成,具有高外流速度(FWHM)、低气体分数($<\!0.1$)、低金属性($)和低尘埃衰减(UV 0.5$,在$z 10$时,随$z$的增大而减小)。我们将与目前的 JWST 观测结果进行初步比较,以获得初步认识,并期待将来有更完整可靠的数据集来进行详细的定量比较。FFB 预测也以数字形式提供。
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