HI gas in disk and dwarf galaxies in the view of SAMs Fu Jian (富坚) Shanghai Astronomical Observatory, CAS fujian@shao.ac.cn 2018-06-18 KIAA Forum on Gas in Galaxies Peking University

Galaxies in cosmological simulations Semi-analytic models L-Galaxies, GALFORM Hydrodynamic Simulations EAGLE, Illustris, Horizon-AGN Describe baryonic processes based on dark matter N-body simulation Simulating dark matter and baryonic matter at the same time

The newest version of L-Galaxies SAMs L-Galaxies SAMs developed by Munich group Public version Henriques et al. (2015) http://galformod.mpa- garching.mpg.de/public/LGalaxies/ Main branches Radial resolved models of HI and H2 gas components (Fu et al. 2013) Chemical abundance models for different elements (Yates et al. 2014) Cold gas stripping process and star formation quenching by ram pressure (Luo et al. 2016)

The radial resolved disks and radial profiles HI-H2-HII transition prescriptions 1: Krumholz et al. 2009; Mckee & Krumholz 2010 2: Pressure related H2 fraction recipe (B&R 2006) 3: Molecular-atomic-ionized gas (Gnedin& Kravtsov 2011) H2 proportional star formation law Exponential infalling gas

The chemical enrichment models Two types of supernovae and AGBs instead of IRA (Chabrier03 IMF) Results of 11 elements in IMF (H He C N O Ne Mg Si S Ca Fe) Pristine gas for original infall: 75% H and 25% He

Radial resolved disks with chemical enrichments Radial bins array, star formation history, metallicity arrays A lot more memory and time consumption —— options can be switched off —— still a lot faster that hydrodynamic simulation

Dark matter halo for L-Galaxies Millennium II Simulation Millennium Simulation For the observations of HI and H2 these years, modelers try to describe Based on n-body simulation Aquarius Simulation

The L-Galaxies models on ELUCID haloes ELUCID simulation (Wang, Mo, Yang et al. 2014) Reconstruct the initial density field according to local universe Same to the data structure of Millennium Simulation ELUCID项目-利用再构造初始密度场研究近邻宇宙。 •由中科大、上海交大、清华大学等多方合作。 •可以精确再现宇宙演化历史，精确度较其他方法提高2-3倍。 •依赖完备的星系群列表信息

similar in different types of galaxies Radial profiles for HI gas Size-mass relation of HI disks Wang et al. 2016 HI-H2 transition similar in different types of galaxies

21cm flux and velocity profiles of HI disks W50 fpeak The line profile of a model HI disk with constant circular velocity

HI Mass functions at z=0 Models based on Aquarius haloes (Grcevich & Putman 2009) Models based on ELUCID halos predict low HIMF at low HI mass end Models based on Aquarius haloes 4 MW satellites with HI detected within 280 kpc (HIPASS)

Redshift evolution of HI gas in the models

The mock catalogue for HI survey FAST telescope Frequency (L-band) 1050-1450 MHz Number of beams 19 Dish diameter 300 m Survey region -14°~+66°

Light-cones algorithms Discrete redshift snapshots continuous redshift random tiling Periodic box consistent space Kitzbichler & White 2006; Blaizot et al. 2005

Galaxy cluster numbers for FAST HI gas survey based on models

Conclusions Models on ELUCID haloes can fit the HIMF from ALFALFA to very low mass end, which is very sensitive to the physical processes in low mass satellites, e.g SN feedback, ram pressure stripping Our models predict a lot of gas rich low mass dark galaxies, which may offer opportunities for future HI 21cm survey in nearby by galaxies by FAST and SKA-1 The size-mass correlation of HI gas can be extended to very low mass range (MHI~107M☉), which means the prescription between HI and H2 should be similar in different types of galaxies 21cm mock catalogue show more HI rich clusters can be detected at z>1 Thank you!