Zooming on the internal structure of $z\simeq 6$ galaxies

Abstract

We present zoom-in, AMR, high-resolution ($\simeq 30$ pc) simulations of high-redshift ($z\simeq 6$) galaxies with the aim of characterizing their internal properties and interstellar medium. Among other features, we adopt a star formation model based on a physically-sound molecular hydrogen prescription, and introduce a novel scheme for supernova feedback, stellar winds and dust-mediated radiation pressure. In the zoom-in simulation the target halo hosts "Dahlia", a galaxy with a stellar mass $M_{\ast }=1.6\times 10^{10}$M${}_{\odot }$, representative of a typical $z\sim 6$ Lyman Break Galaxy. Dahlia has a total H2 mass of $10^{8.5}$M${}_{\odot }$, that is mainly concentrated in a disk-like structure of effective radius $\simeq 0.6$ kpc and scale height $\simeq 200$ pc. Frequent mergers drive fresh gas towards the center of the disk, sustaining a star formation rate per unit area of $\simeq 15$M${}_{\odot }$ yr${}^{-1}$ kpc${}^{-2}$. The disk is composed by dense ($n\gtrsim 25$ cm${}^{-3}$), metal-rich ($Z\simeq 0.5$ Z${}_{\odot }$) gas, that is pressure-supported by radiation. We compute the $158\mu$m [CII] emission arising from {Dahlia}, and find that $\simeq 95\%$ of the total [CII] luminosity ($L_{[CII]}\simeq 10^{7.5}$ L${}_{\odot }$) arises from the H2 disk. Although $30\%$ of the CII mass is transported out of the disk by outflows, such gas negligibly contributes to [CII] emission, due to its low density ($n\lesssim 10$ cm${}^{-3}$) and metallicity ($Z\lesssim 10^{-1}$Z${}_{\odot }$). Dahlia is under-luminous with respect to the local [CII]-SFR relation; however, its luminosity is consistent with upper limits derived for most $z\sim 6$ galaxies.

arXiv comment21 pages, 11 figures, 3 tables

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