TY - JOUR
T1 - The distribution and physical properties of high-redshift [OIII] emitters in a cosmological hydrodynamics simulation
AU - Moriwaki, Kana
AU - Yoshida, Naoki
AU - Shimizu, Ikkoh
AU - Harikane, Yuichi
AU - Matsuda, Yuichi
AU - Matsuo, Hiroshi
AU - Hashimoto, Takuya
AU - Inoue, Akio K.
AU - Tamura, Yoichi
AU - Nagao, Tohru
N1 - Funding Information:
The authors thank the anonymous referee for providing us with many insightful comments. This research was supported by the Munich Institute for Astro-and Particle Physics (MIAPP) of the DFG cluster of excellence ‘Origin and Structure of the Universe’. KM has been supported by Advanced Leading Graduate Course for Photon Science (ALPS) of the University of Tokyo. IS, YH, YM, AKI, and YT acknowledge JSPS KAKENHI grant numbers 26247022, 17H01111 (IS), 16J03329 (YH), 17H04831, 17KK0098 (YM), 17H01114 (AKI), and 17H06130 (YT). TH, AKI, and YT acknowledge the NAOJ ALMA Scientific Research grant numbers 2016-01A (TH, AKI) and 2018-09B (YT).
PY - 2018/11/21
Y1 - 2018/11/21
N2 - Recent observations with the Atacama Large Millimeter/submillimeter Array (ALMA) detected far-infrared emission lines such as the [OIII] 88μm line from galaxies at z ~ 7-9. We use a cosmological simulation of galaxy formation to study the physical properties of [O III] 88μm emitters. In a comoving volume of 50 h-1 Mpc on a side, we locate 34 galaxies with stellar masses greater than 108 M⊙ at z = 9, and more than 270 such galaxies at z = 7. We calculate the [O III] 88μm luminosities (LOIII,88) by combining a physical model of HII regions with emission line calculations using the photoionization code CLOUDY.We show that the resulting LOIII,88, for a given star formation rate, is slightly higher than predicted from the empirical relation for local galaxies, and is consistent with recent observations of galaxies at redshifts 7-9. Bright [O III] emitters with LOIII,88 > 108 L⊙ have star formation rates higher than 3M⊙ yr-1, and the typical metallicity is ~0.1Z⊙. The galaxies are hosted by dark matter haloes with masses greater than 1011M⊙. We propose to use the [OIII] 5007Å line, to be detected by James Webb Space Telescope, to study the properties of galaxies whose [OIII] 88 μm line emission has been already detected with ALMA.
AB - Recent observations with the Atacama Large Millimeter/submillimeter Array (ALMA) detected far-infrared emission lines such as the [OIII] 88μm line from galaxies at z ~ 7-9. We use a cosmological simulation of galaxy formation to study the physical properties of [O III] 88μm emitters. In a comoving volume of 50 h-1 Mpc on a side, we locate 34 galaxies with stellar masses greater than 108 M⊙ at z = 9, and more than 270 such galaxies at z = 7. We calculate the [O III] 88μm luminosities (LOIII,88) by combining a physical model of HII regions with emission line calculations using the photoionization code CLOUDY.We show that the resulting LOIII,88, for a given star formation rate, is slightly higher than predicted from the empirical relation for local galaxies, and is consistent with recent observations of galaxies at redshifts 7-9. Bright [O III] emitters with LOIII,88 > 108 L⊙ have star formation rates higher than 3M⊙ yr-1, and the typical metallicity is ~0.1Z⊙. The galaxies are hosted by dark matter haloes with masses greater than 1011M⊙. We propose to use the [OIII] 5007Å line, to be detected by James Webb Space Telescope, to study the properties of galaxies whose [OIII] 88 μm line emission has been already detected with ALMA.
KW - Galaxies: ISM
KW - Galaxies: evolution
KW - Galaxies: high-redshift
UR - http://www.scopus.com/inward/record.url?scp=85054073809&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=85054073809&partnerID=8YFLogxK
U2 - 10.1093/mnrasl/sly167
DO - 10.1093/mnrasl/sly167
M3 - Article
AN - SCOPUS:85054073809
VL - 481
SP - L84-L88
JO - Monthly Notices of the Royal Astronomical Society: Letters
JF - Monthly Notices of the Royal Astronomical Society: Letters
SN - 1745-3933
IS - 1
ER -