@article{3cc1f47687a3440395afb815b74e0972,
title = "Comparison of cosmological simulations and deep submillimetre galaxy surveys",
abstract = "Recent progress in submillimetre surveys by single-dish telescopes allows us to further challenge the consistency between cosmological simulations and observations. In particular, we compare our simulations that include dust formation and destruction with the recent SCUBA-2 surveys ('STUDIES') by putting emphases on basic observational properties of dust emission such as dust temperature, size of infrared (IR)-emitting region, IR luminosity function, and IRX-β relation. After confirming that our models reproduce the local galaxy properties, we examine the STUDIES sample at z ≈ 1-4, finding that the simulation reproduces the aforementioned quantities except for the z ≳ 2 IR luminosity function at the massive end (∼1013 L☉). This means that the current simulation correctly reproduces the overall scaling between the size and luminosity (or star formation rate) of dusty region, but lacks extreme starburst phenomena at z ≳ 2. We also discuss extinction curves and possible active galactic nucleus contribution.",
keywords = "Dust: extinction, Galaxies: ISM, Galaxies: evolution, Galaxies: formation, Methods: numerical",
author = "Shohei Aoyama and Hiroyuki Hirashita and Lim, {Chen Fatt} and Chang, {Yu Yen} and Wang, {Wei Hao} and Kentaro Nagamine and Hou, {Kuan Chou} and Ikkoh Shimizu and Chung, {Hui Hsuan} and Lee, {Chien Hsiu} and Zheng, {Xian Zhong}",
note = "Funding Information: We are grateful to C.-Y. Chiang for useful discussions and comments regarding the AGN fraction in high-redshift galaxies. We thank C.-C. Chen, T. Goto, T. Hashimoto, and I. Smail for useful comments. We acknowledge the STUDIES team and the JCMT for the observational data. We are grateful to V. Springel for providing us with the original version of GADGET-3 code. Numerical computations were carried out on Cray XC50 at the Center for Computational Astrophysics, National Astronomical Observatory of Japan and XL at the Theoretical Institute for Advanced Research in Astrophysics (TIARA) in Academia Sinica. HH thanks the Ministry of Science and Technology for support through grant MOST 105-2112-M-001-027-MY3 and MOST 107-2923-M-001-003-MY3 (RFBR 18-52-52-006). CFL, YYC, and WHW are supported by the Ministry of Science and Technology through grant MOST 105-2112-M-001-029-MY3. KN and IS acknowledge the support from the JSPS KAKENHI Grant Number JP17H01111. KN acknowledges the travel support from the Kavli IPMU, World Premier Research Center Initiative (WPI), where part of this work was conducted. Publisher Copyright: {\textcopyright} 2019 The Author(s).",
year = "2019",
month = apr,
day = "1",
doi = "10.1093/mnras/stz021",
language = "English",
volume = "484",
pages = "1852--1864",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",
number = "2",
}