%0 Generic %1 pallottini2016zooming %A Pallottini, A. %A Ferrara, A. %A Gallerani, S. %A Vallini, L. %A Maiolino, R. %A Salvadori, S. %D 2016 %K galaxy high redshift simulation zoom %T Zooming on the internal structure of $z\simeq6$ galaxies %U http://arxiv.org/abs/1609.01719 %X We present zoom-in, AMR, high-resolution ($30$ pc) simulations of high-redshift ($z 6$) 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 $M_*=1.6\times 10^10$M$_ødot$, representative of a typical $z6$ Lyman Break Galaxy. Dahlia has a total H2 mass of $10^8.5$M$_ødot$, that is mainly concentrated in a disk-like structure of effective radius $0.6$ kpc and scale height $200$ pc. Frequent mergers drive fresh gas towards the center of the disk, sustaining a star formation rate per unit area of $15 $M$_ødot$ yr$^-1$ kpc$^-2$. The disk is composed by dense ($n 25$ cm$^-3$), metal-rich ($Z 0.5 $ Z$_ødot$) gas, that is pressure-supported by radiation. We compute the $158\mu$m CII emission arising from Dahlia, and find that $95\%$ of the total CII luminosity ($L_CII\simeq10^7.5$ L$_ødot$) 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 ($n 10$ cm$^-3$) and metallicity ($Z10^-1$Z$_ødot$). Dahlia is under-luminous with respect to the local CII-SFR relation; however, its luminosity is consistent with upper limits derived for most $z\sim6$ galaxies.

@misc{pallottini2016zooming, 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 $M_*=1.6\times 10^{10}$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 ($L_{[CII]}\simeq10^{7.5}$ 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 $z\sim6$ galaxies.}, added-at = {2016-09-08T10:22:34.000+0200}, author = {Pallottini, A. and Ferrara, A. and Gallerani, S. and Vallini, L. and Maiolino, R. and Salvadori, S.}, biburl = {https://www.bibsonomy.org/bibtex/213000cd6ffe29003792c3d47b816b1bc/miki}, description = {[1609.01719] Zooming on the internal structure of $z\simeq6$ galaxies}, interhash = {89ecd4e52b91004cf45baef3e5b8041d}, intrahash = {13000cd6ffe29003792c3d47b816b1bc}, keywords = {galaxy high redshift simulation zoom}, note = {cite arxiv:1609.01719Comment: 20 pages, 11 figures, submitted to MNRAS}, timestamp = {2016-09-08T10:22:34.000+0200}, title = {Zooming on the internal structure of $z\simeq6$ galaxies}, url = {http://arxiv.org/abs/1609.01719}, year = 2016 }