论文标题
高$ z $星系的调查：Serra模拟
A survey of high-$z$ galaxies: SERRA simulations
论文作者
论文摘要
我们介绍了Serra，这是一套缩放的高分辨率（$ \ sim 10 \，\ rm PC $）宇宙学模拟，包括非平衡化学和狂热的辐射转移。输出后处理以得出Galaxy UV+FIR连续性和发射线的性能。将结果与可用的多波长数据进行比较，以限制高红移$ 6 \ Lessim Z \ Lessim Z \ Lessim 15 $星系的物理特性（例如恒星形成率，恒星/气体/尘埃，金属性）。这份旗舰纸重点介绍了$ z = 7.7 $子样本，包括202个带有恒星质量的星系$ 10^7 m_ \ odot \ odot \ simsim m_ \ star \ star \ lyseSim 5 \ times 10^{10} {10} m_ \ odot $，以及特定的星形构造范围从$ {\ rm sssfr} \ sim sssfr} \ sim 100 \ sim { gyr}^{ - 1} $在年轻的低质量星系中为$ \ sim 10 \，{\ rm gyr}^{ - 1} $，用于较老的，大型的。在此红移时，Serra星系通常是爆发的，即它们位于Schmidt-Kennicutt关系上方，其因子$κ__s= 3.03^{+4.9} _ { - 1.8} $，与[OIII]和[CIII]和[CII] EMITTERS的最新发现一致。它们还显示相对较大的$ {\ rm irx} = l _ {\ rm fir}/l _ {\ rm UV} $值，因为它们的紧凑/块状形态有效地阻止了恒星UV的亮度。请注意，该结论可能会受到分子云水平上空间分辨率不足的影响。我们确认早期星系位于标准$ \ rm [CII] -SFR $关系上；他们观察到的$ l _ {\ rm [oiii]}/l _ {\ rm [cii]} \ simeq 1-10 $比率可以由一部分Serra星系复制，而无需顶部高度的IMF和/或Anomalous C/O c/o Bruncantances。 [oi]线强度与本地浓度相似，使Alma High-$ z $检测具有挑战性但可行（$ \ sim 6 \，\ rm hr $，sfr $ 50 \，m_ \ odot \，{\ rm yr yr yr yr}^{ - 1} $）。
We introduce SERRA, a suite of zoom-in high-resolution ($\sim 10\,\rm pc$) cosmological simulations including non-equilibrium chemistry and on-the-fly radiative transfer. The outputs are post-processed to derive galaxy UV+FIR continuum and emission line properties. Results are compared with available multi-wavelength data to constrain the physical properties (e.g., star formation rates, stellar/gas/dust mass, metallicity) of high-redshift $6 \lesssim z \lesssim 15$ galaxies. This flagship paper focuses on the $z=7.7$ sub-sample, including 202 galaxies with stellar mass $10^7 M_\odot \lesssim M_\star \lesssim 5\times 10^{10}M_\odot$, and specific star formation ranging from ${\rm sSFR} \sim 100\,{\rm Gyr}^{-1}$ in young, low-mass galaxies to $\sim 10\,{\rm Gyr}^{-1}$ for older, massive ones. At this redshift, SERRA galaxies are typically bursty, i.e. they are located above the Schmidt-Kennicutt relation by a factor $κ_s = 3.03^{+4.9}_{-1.8}$, consistent with recent findings for [OIII] and [CII] emitters at high-$z$. They also show relatively large ${\rm IRX} = L_{\rm FIR}/L_{\rm UV}$ values as a result of their compact/clumpy morphology effectively blocking the stellar UV luminosity. Note that this conclusion might be affected by insufficient spatial resolution at the molecular cloud level. We confirm that early galaxies lie on the standard $\rm [CII]-SFR$ relation; their observed $L_{\rm [OIII]}/L_{\rm [CII]} \simeq 1-10$ ratios can be reproduced by a part of the SERRA galaxies without the need of a top-heavy IMF and/or anomalous C/O abundances. [OI] line intensities are similar to local ones, making ALMA high-$z$ detections challenging but feasible ($\sim 6\,\rm hr$ for a SFR of $50\,M_\odot\,{\rm yr}^{-1}$).
