arXiv 2007.098532020-07astro-ph.GA

星系形成模拟中（亚）毫米选择星系的物理性质和演化

Physical properties and evolution of (Sub-)millimeter selected galaxies in the galaxy formation simulation Shark

Claudia del P. Lagos, Elisabete da Cunha, Aaron S. G. Robotham, Danail Obreschkow, Francesco Valentino, Seiji Fujimoto, Georgios E. Magdis, Rodrigo Tobar

备注：: Final version accepted for publication in MNRAS. 28 pages, 22 of main text and figures
DOI：: 10.1093/mnras/staa2861

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摘要：

本文在Shark半解析星系形成模型中，对亚毫米选择星系的性质进行了深入的研究。与观测值比较，在波长（λ）0.6- 2 mm处的预测数和在波长（λ）0.1- 2 mm处的红移分布符合得很好。在明亮的一端（> 1 mJy），鲨鱼星系是合并和盘不稳定的混合体。这些星系显示出一个堆叠的FUV到FIR光谱，与观测结果一致。我们预测，目前的光学/近红外巡天足够深，可以探测到z<5的明亮（> 1 mJy）λ =0.85- 2 mm的选定星系，但太浅，无法探测到更高红移的对应星系。詹姆斯·韦伯太空望远镜10,000年的巡天应该能探测到$S_{\rm 0.85mm}>0.01$ mJy星系的所有对应物。我们预测SMG的磁盘贡献显着（可忽略不计）的休息帧UV（IR）。我们研究了0<z1 <6 evolution of the intrinsic properties of >mJy λ =0.85- 2 mm的选择星系，发现它们的：（i）恒星质量为$>10^{10.2}M_{\odot}$，其中2 mm的质量跟踪质量最大的星系（$>10^{11}M_{\odot}$）;（ii）比恒星形成率（SFR）略高于主序（MS）（~3- 10倍）;（iii）宿主晕质量为$\gtrsim 10^{12.3}M_{\odot}$，2 mm星系追踪最大质量的晕（原星系团）;（iv）SMG比MS星系具有更低的尘埃质量（$\approx 10^{8}M_{\odot}$），更高的尘埃温度（$\approx 40-45$ K）和更高的静止框架V带衰减（>1.5）;（v）大小随红移而减小，从z=1时的4kpc到z=4时的<1 kpc;（vi）$S_{\rm 0.85mm}>1$ mJy源的一氧化碳线光谱在4->3处达到峰值。最后，我们研究了SMG对0<z<10的分子气体和宇宙SFR密度的贡献，发现> 1 mJy的源在z>3和z>5的贡献分别可以忽略不计，这表明目前的观测已经揭示了大部分恒星形成在0<z<10。

英文摘要：

We thoroughly explore the properties of (sub)-millimeter (mm) selected galaxies (SMGs) in the Shark semi-analytic model of galaxy formation. Compared to observations, the predicted number counts at wavelengths (lambda) 0.6-2mm and redshift distributions at 0.1-2mm, agree well. At the bright end (>1mJy), Shark galaxies are a mix of mergers and disk instabilities. These galaxies display a stacked FUV-to-FIR spectrum that agrees well with observations. We predict that current optical/NIR surveys are deep enough to detect bright (>1mJy) lambda=0.85-2mm-selected galaxies at z<5, but too shallow to detect counterparts at higher redshift. A James Webb Space Telescope 10,000s survey should detect all counterparts for galaxies with $S_{\rm 0.85mm}>0.01$mJy. We predict SMG's disks contribute significantly (negligibly) to the rest-frame UV (IR). We investigate the 0<z<6 evolution of the intrinsic properties of >1mJy lambda=0.85-2mm-selected galaxies finding their: (i) stellar masses are $>10^{10.2}M_{\odot}$, with the 2mm ones tracing the most massive galaxies ($>10^{11}M_{\odot}$); (ii) specific star formation rates (SFR) are mildly (~3-10x) above the main sequence (MS); (iii) host halo masses are $\gtrsim 10^{12.3}M_{\odot}$, with 2mm galaxies tracing the most massive halos (proto-clusters); (iv) SMGs have lower dust masses ($\approx 10^{8}M_{\odot}$), higher dust temperatures ($\approx 40-45$K) and higher rest-frame V-band attenuation (>1.5) than MS galaxies; (v) sizes decrease with redshift, from 4kpc at z=1 to <1kpc at z=4; (vi) the Carbon Monoxide line spectra of $S_{\rm 0.85mm}>1$mJy sources peak at 4->3. Finally, we study the contribution of SMGs to the molecular gas and cosmic SFR density at 0<z<10, finding that >1mJy sources make a negligible contribution at z>3 and z>5, respectively, suggesting current observations have unveiled the majority of the star formation at 0<z<10.

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