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

Álvarez-Márquez, J., Colina, L., Marques-Chaves, R., Ceverino, D., Alonso-Herrero, A., Caputi, K., et al. (2019). Investigating the physical properties of galaxies in the Epoch of Reionization with MIRI/JWST spectroscopy. Astronomy and Astrophysics, 629.

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Datensatz-Permalink: https://hdl.handle.net/21.11116/0000-0005-D1FA-5 Versions-Permalink: https://hdl.handle.net/21.11116/0000-0005-D1FB-4
Genre: Zeitschriftenartikel

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externe Referenz:
https://ui.adsabs.harvard.edu/abs/2019A&A...629A...9A (beliebiger Volltext)
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 Urheber:
Álvarez-Márquez, J.1, Autor
Colina, L.1, Autor
Marques-Chaves, R.1, Autor
Ceverino, D.1, Autor
Alonso-Herrero, A.1, Autor
Caputi, K.1, Autor
García-Marín, M.1, Autor
Labiano, A.1, Autor
Le Fèvre, O.1, Autor
Norgaard-Nielsen, H. U.1, Autor
Östlin, G.1, Autor
Pérez-González, P. G.1, Autor
Pye, J. P.1, Autor
Tikkanen, T. V.1, Autor
van der Werf, P. P.1, Autor
Walter, F.1, Autor
Wright, G. S.1, Autor
Affiliations:
1Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners, ou_2421692              

Inhalt

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Schlagwörter: galaxies: high-redshift galaxies: formation galaxies: evolution infrared: galaxies telescopes Astrophysics - Astrophysics of Galaxies
 Zusammenfassung: 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 HŒ± and [OIII]0.5007 Œºm 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 HŒ± 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‚òâ yr-1, and stellar masses above 4-9 107 M‚òâ. 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 Œºm emitters. The MRS simulated spectra cover a wide range of low metallicities from about 0.2-0.02 Z‚òâ, and different [OIII]88 Œºm/[OIII]0.5007 Œºm line ratios. The simulated 10 ks MRS spectra show S/N in the range of 5-90 for HŒ≤, [OIII]0.4959,0.5007 Œºm, HŒ± and HeI1.083 Œºm 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 Œºm, [SII]0.6717,0.6731 Œºm, and [SIII]0.9069,0.9532 Œºm 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 Œºm. 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.

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 Datum: 2019
 Publikationsstatus: Erschienen
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Titel: Astronomy and Astrophysics
Genre der Quelle: Zeitschrift
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Ort, Verlag, Ausgabe: -
Seiten: - Band / Heft: 629 Artikelnummer: - Start- / Endseite: - Identifikator: -