Physical properties and evolution of (Sub-)millimeter selected galaxies in the galaxy formation simulation Shark

Claudia del P. Lagos; Elisabete da Cunha; Aaron S. G. Robotham; Danail Obreschkow; Francesco Valentino; Seiji Fujimoto; Georgios E. Magdis; Rodrigo Tobar

doi:10.1093/mnras/staa2861

paper

Physical properties and evolution of (Sub-)millimeter selected galaxies in the galaxy formation simulation Shark

arXiv:2007.09853 · doi:10.1093/mnras/staa2861

Abstract

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 $S_{0.85mm} > 0.01$ 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 $> 1 0^{10.2} M_{⊙}$ , with the 2mm ones tracing the most massive galaxies ( $> 1 0^{11} M_{⊙}$ ); (ii) specific star formation rates (SFR) are mildly (~3-10x) above the main sequence (MS); (iii) host halo masses are $≳ 1 0^{12.3} M_{⊙}$ , with 2mm galaxies tracing the most massive halos (proto-clusters); (iv) SMGs have lower dust masses ( $\approx 1 0^{8} M_{⊙}$ ), 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 $S_{0.85mm} > 1$ 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.

arXiv commentFinal version accepted for publication in MNRAS. 28 pages, 22 of main text and figures

Physical properties and evolution of (Sub-)millimeter selected galaxies in the galaxy formation simulation Shark

Abstract

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