论文标题
Galaxy形成鲨鱼中（亚）毫米选择星系的物理特性和（亚）毫米选择的星系的演变
Physical properties and evolution of (Sub-)millimeter selected galaxies in the galaxy formation simulation Shark
论文作者
论文摘要
我们彻底探讨了（sub） - 千分表（mm）选定星系（SMG）在星系形成的半分析模型中的特性。与观察结果相比，在波长（lambda）0.6-2mm和0.1-2mm的红移分布处的预测数量计数很好。在明亮的端（> 1MJY），鲨鱼星系是合并和磁盘不稳定性的混合体。这些星系显示出堆叠的fuv-to-fir频谱，与观察结果很好。我们预测，当前的光学/NIR调查足够深，可以检测到Z <5的明亮（> 1MJY）lambda = 0.85-2mm选择的星系，但也太浅了，无法在较高的红移下检测对应物。詹姆斯·韦伯（James Webb）太空望远镜10,000S调查应检测出$ s _ {\ rm 0.85mm}> 0.01 $ mjy的星系的所有对应物。我们预测SMG的磁盘会对其余框架（IR）的贡献显着（可忽略）。我们调查了> 1MJy lambda = 0.85-2mm选择的星系的0 <z <6的0 <z <6的演变，找到了它们：（i）恒星质量为$> 10^{10.2} m _ {\ odot} $，带有2mm的最大质量（$> 10^}}} {11}} {11} {11} {11} {11 {11} {11} {11} {11} {11} {11} { （ii）特定的恒星形成速率（SFR）在主序列（MS）上方的温和（〜3-10x）中； （iii）主机光环质量为$ \ gtrsim 10^{12.3} m _ {\ odot} $，有2mm的星系可追踪最大的晕孔（proto-clusters）； （iv）SMG的尘埃质量较低（$ \ of 10^{8} m _ {\ odot} $），较高的灰尘温度（$ \ $ \约40-45 $ k）和比MS星系更高的REST F-BAND衰减（> 1.5）； （v）随着红移的尺寸减小，从z = 1的4kpc降低到z = 4时的<1kpc; （vi）$ s _ {\ rm 0.85mm}> 1 $ mjy源在4-> 3的峰值的一氧化碳线光谱。最后，我们研究了SMG在0 <z <10时对分子气体和宇宙SFR密度的贡献，发现> 1MJY的来源在z> 3和z> 5时分别贡献了可忽略的贡献，这表明当前的观察结果已在0 <z <10处公布了大部分星形形成。
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.
