Essential physics of early galaxy formation

作者: Pratika Dayal , Andrea Ferrara , James S. Dunlop , Fabio Pacucci

DOI: 10.1093/MNRAS/STU1848

关键词: Disc galaxyGalaxy formation and evolutionPhysicsStar formationAstrophysicsActive galactic nucleusGalaxyGalaxy mergerAstronomyElliptical galaxyStellar mass

摘要: We present a theoretical model embedding the essential physics of early galaxy formation (z ≃ 5-12) based on single premise that any can form stars with maximal limiting efficiency provides enough energy to expel all remaining gas, quenching further star formation. This simple idea is implemented into merger-tree-based semi-analytical utilizes two mass and redshift-independent parameters capture key supernova feedback in ejecting gas from low- haloes, tracks resulting impact subsequent growth more massive systems via halo mergers accretion. Our shows that: (i) smallest haloes (halo Mh ≤ 1010 M☉) build up their by accretion intergalactic medium; (ii) bulk powering larger (Mh ≥ 1011.5 brought merging progenitors; (iii) faint-end UV luminosity function slope evolves according α = -1.75 log z - 0.52. In addition, (iv) stellar mass-to-light ratio well fitted functional M* -0.38MUV 0.13 + 2.4, which we use evolving compare observations. end census cosmic density (SMD) across galaxies magnitudes over range -23 MUV -11 spanning redshifts 5 < 12; (v) while currently detected LBGs contain ≈50 per cent (10 cent) total SMD at (8), James Webb Space Telescope will detect 25 9.5.

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