Investigating the physical properties of galaxies in the Epoch of Reionization with MIRI/JWST spectroscopy

dc.contributor.authorÁlvarez González, J.
dc.contributor.authorColina, L.
dc.contributor.authorMarqués Chaves, R.
dc.contributor.authorPérez González, Pablo Guillermo
dc.date.accessioned2023-06-17T13:33:33Z
dc.date.available2023-06-17T13:33:33Z
dc.date.issued2019-08-23
dc.description© ESO 2019. 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.
dc.description.abstractThe 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 Mꙩ yr^(−1), and stellar masses above 4–9 × 10^(7) Mꙩ. 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 Zꙩ, 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.
dc.description.departmentDepto. de Física de la Tierra y Astrofísica
dc.description.facultyFac. de Ciencias Físicas
dc.description.refereedTRUE
dc.description.sponsorshipUnión Europea. H2020
dc.description.sponsorshipMinisterio de Ciencia e Innovación (MICINN)/FEDER
dc.description.sponsorshipComunidad de Madrid
dc.description.sponsorshipConsejo Superior de Investigaciones Científicas (CSIC)
dc.description.sponsorshipGauss Center for Supercomputing on the GCS Supercomputer SuperMUC at Leibniz Supercomputing Centre
dc.description.sponsorshipState of BadenWürttemberg
dc.description.sponsorshipUK Space Agency
dc.description.statuspub
dc.eprint.idhttps://eprints.ucm.es/id/eprint/57609
dc.identifier.doi10.1051/0004-6361/201935594
dc.identifier.issn1432-0746
dc.identifier.officialurlhttp://dx.doi.org/10.1051/0004-6361/201935594
dc.identifier.relatedurlhttps://www.aanda.org/
dc.identifier.urihttps://hdl.handle.net/20.500.14352/13752
dc.journal.titleAstronomy & Astrophysics
dc.language.isoeng
dc.publisherEDP Sciencies
dc.relation.projectIDBUILDUP (681627)
dc.relation.projectID(ESP2017-83197; AYA2015-64346-C2-1-P; PGC2018-094671-B-I00)
dc.relation.projectID2017-T1/TIC-5213
dc.relation.projectIDPIE201650E36
dc.relation.projectIDpr92za
dc.relation.projectIDbwHPC
dc.rights.accessRightsopen access
dc.subject.cdu52
dc.subject.keywordStar-forming galaxies
dc.subject.keywordEmission-line
dc.subject.keywordO-III
dc.subject.keywordRedshift
dc.subject.keywordFeedback
dc.subject.keywordAlpha
dc.subject.keywordDust
dc.subject.ucmAstrofísica
dc.titleInvestigating the physical properties of galaxies in the Epoch of Reionization with MIRI/JWST spectroscopy
dc.typejournal article
dc.volume.number629
dspace.entity.typePublication
relation.isAuthorOfPublicationa57c0327-fab0-44e0-9b9c-24b1f7081391
relation.isAuthorOfPublication.latestForDiscoverya57c0327-fab0-44e0-9b9c-24b1f7081391
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