The impact of chemistry on the structure of high-z galaxies

Abstract

To improve our understanding of high-z galaxies we study the impact of H${}_2$ chemistry on their evolution, morphology and observed properties. We compare two zoom-in high-resolution (30 pc) simulations of prototypical $M_{\star }\sim 10^{10}{\mathrm{M}}_{\odot }$ galaxies at $z=6$. The first, "Dahlia", adopts an equilibrium model for H${}_2$ formation, while the second, "Althæa", features an improved non-equilibrium chemistry network. The star formation rate (SFR) of the two galaxies is similar (within 50\%), and increases with time reaching values close to 100 ${\mathrm{M}}_{\odot }/\mathrm{yr}$ at $z=6$. They both have SFR-stellar mass relation consistent with observations, and a specific SFR of $\simeq 5{\mathrm{Gyr}}^{-1}$. The main differences arise in the gas properties. The non-equilibrium chemistry determines the H$\to$ H${}_2$~transition to occur at densities $>300{cm}^{-3}$, i.e. about 10 times larger than predicted by the equilibrium model used for Dahlia. As a result, Althæa features a more clumpy and fragmented morphology, in turn making SN feedback more effective. Also, because of the lower density and weaker feedback, Dahlia sits $3\sigma$ away from the Schmidt-Kennicutt relation; Althæa, instead nicely agrees with observations. The different gas properties result in widely different observables. Althæa outshines Dahlia by a factor of 7 (15) in [CII]~$157.74\mu \mathrm{m}$ (H${}_2$~$17.03\mu \mathrm{m}$) line emission. Yet, Althæa is under-luminous with respect to the locally observed [CII]-SFR relation. Whether this relation does not apply at high-z or the line luminosity is reduced by CMB and metallicity effects remains as an open question.

18 pages, 13 Figures 1 Table, accepted for publication in MNRAS

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