Investigating the physical properties of galaxies in the Epoch of Reionization with MIRI/JWST spectroscopy
journal contributionposted on 2019-09-18, 17:18 authored by J Alvarez-Marquez, L Colina, R Marques-Chaves, D Ceverino, A Alonso-Herrero, K Caputi, M Garcia-Marin, A Labiano, O Le Fevre, HU Norgaard-Nielsen, G Ostlin, PG Perez-Gonzalez, JP Pye, TV Tikkanen, PP van der Werf, F Walter, GS Wright
The James Webb Space Telescope (JWST) will provide deep imaging and spectroscopy for sources at redshifts above 6, covering the entire Epoch of Reionization (EoR, 6 < z < 10), and enabling the detailed exploration of the nature of the different sources during the first 1 Gyr of the history of the Universe. The Medium Resolution Spectrograph (MRS) of the mid-IR Instrument (MIRI) will be the only instrument on board JWST able to observe the brightest optical emission lines Hα and [OIII]0.5007 μm at redshifts above 7 and 9, respectively, providing key insights into the physical properties of sources during the early phases of the EoR. This paper presents a study of the Hα fluxes predicted by state-of-the-art FIRSTLIGHT cosmological simulations for galaxies at redshifts of 6.5–10.5, and its detectability with MIRI. Deep (40 ks) spectroscopic integrations with MRS will be able to detect (signal-to-noise ratio > 5) EoR sources at redshifts above 7 with intrinsic star formation rates (SFR) of more than 2 M⊙ yr−1, and stellar masses above 4–9 × 107 M⊙. These limits cover the upper end of the SFR and stellar mass distribution at those redshifts, representing ∼6% and ∼1% of the predicted FIRSTLIGHT population at the 6.5–7.5 and 7.5–8.5 redshift ranges, respectively. In addition, the paper presents realistic MRS simulated observations of the expected rest-frame optical and near-infrared spectra for some spectroscopically confirmed EoR sources recently detected by ALMA as [OIII]88 μm emitters. The MRS simulated spectra cover a wide range of low metallicities from about 0.2–0.02 Z⊙, and different [OIII]88 μm/[OIII]0.5007 μm line ratios. The simulated 10 ks MRS spectra show S/N in the range of 5–90 for Hβ, [OIII]0.4959,0.5007 μm, Hα and HeI1.083 μm emission lines of the currently highest spectroscopically confirmed EoR (lensed) source MACS1149-JD1 at a redshift of 9.11, independent of metallicity. In addition, deep 40 ksec simulated spectra of the luminous merger candidate B14-65666 at 7.15 shows the MRS capabilities of detecting, or putting strong upper limits on, the weak [NII]0.6584 μm, [SII]0.6717,0.6731 μm, and [SIII]0.9069,0.9532 μm emission lines. These observations will provide the opportunity of deriving accurate metallicities in bright EoR sources using the full range of rest-frame optical emission lines up to 1 μm. In summary, MRS will enable the detailed study of key physical properties such as internal extinction, instantaneous star formation, hardness of the ionizing continuum, and metallicity in bright (intrinsic or lensed) EoR sources.
The authors gratefully thank the referee for the constructive comments and recommendations that helped to improve the quality of the paper, and the EC MIRI test team and MIRISim developers for providing a great and useful tool, the MIRI instrument simulator (MIRISim). The authors also acknowledge the STScI and the developer team of the official JWST calibration pipeline. This work was supported by the Spanish Ministry for Science, Innovation and Universities project number ESP2017-83197. D.C. acknowledges the Gauss Center for Supercomputing for funding this project by providing computing time on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre (Project ID: pr92za). D.C. is supported by the state of BadenWürttemberg through bwHPC. D.C. is a DAWN fellow. A.L. acknowledges funding from the Comunidad de Madrid, Spain, under Atracción de Talento Investigador Grant 2017-T1/TIC-5213. J.P.P. and T.V.T. acknowledge financial support from UK Space Agency grants. A.A.-H. acknowledges support from the Spanish Ministry of Science, Innovation and Universities through grants AYA2015-64346-C2-1-P and PGC2018-094671-B-I00, which were party funded by the FEDER program and from CSIC grant PIE201650E36. K.I.C. acknowledges funding from the European Research Council through the award of the Consolidator Grant ID 681627-BUILDUP
CitationAstronomy and Astrophysics, 2019, 629, A9
Author affiliation/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy
- VoR (Version of Record)