Details

Autor(en) / Beteiligte

• Rinaldi, P.
• Caputi, K. I.
• Costantin, L.
• Gillman, S.
• Iani, E.
• Pérez-González, P. G.
• Östlin, G.
• Colina, L.
• Greve, T. R.
• Noorgard-Nielsen, H. U.
• Wright, G. S.
• Alonso-Herrero, A.
• Álvarez-Márquez, J.
• Eckart, A.
• García-Marín, M.
• Hjorth, J.
• Ilbert, O.
• Kendrew, S.
• Labiano, A.
• Le Fèvre, O.
• Pye, J.
• Tikkanen, T.
• Walter, F.
• van der Werf, P.
• Ward, M.
• Annunziatella, M.
• Azzollini, R.
• Bik, A.
• Boogaard, L.
• Bosman, S. E. I.
• Gómez, A. Crespo
• Jermann, I.
• Langeroodi, D.
• Melinder, J.
• Meyer, R. A.
• Moutard, T.
• Peissker, F.
• Topinka, M.
• van Dishoeck, E.
• Güdel, M.
• Henning, Th
• Lagage, P.-O.
• Ray, T.
• Vandenbussche, B.
• Waelkens, C.
• Navarro-Carrera, R.
• Kokorev, V.

Titel

MIDIS: Strong (Hβ+[O iii]) and Hα Emitters at Redshift z ≃ 7–8 Unveiled with JWST NIRCam and MIRI Imaging in the Hubble eXtreme Deep Field

Ist Teil von

• The Astrophysical journal, 2023-08, Vol.952 (2), p.143

Ort / Verlag

Philadelphia: The American Astronomical Society

Erscheinungsjahr

2023

Link zum Volltext

Quelle

Free E-Journal (出版社公開部分のみ）

Beschreibungen/Notizen

• Abstract We make use of JWST medium-band and broadband NIRCam imaging, along with ultradeep MIRI 5.6 μ m imaging, in the Hubble eXtreme Deep Field to identify prominent line emitters at z ≃ 7–8. Out of a total of 58 galaxies at z ≃ 7–8, we find 18 robust candidates (≃31%) for (H β + [O iii ]) emitters, based on their enhanced fluxes in the F430M and F444W filters, with EW 0 (H β +[O iii ]) ≃87–2100 Å. Among these emitters, 16 lie in the MIRI coverage area and 12 exhibit a clear flux excess at 5.6 μ m, indicating the simultaneous presence of a prominent H α emission line with EW 0 (H α ) ≃200–3000 Å. This is the first time that H α emission can be detected in individual galaxies at z > 7. The H α line, when present, allows us to separate the contributions of H β and [O iii ] to the (H β +[O iii ]) complex and derive H α -based star formation rates (SFRs). We find that in most cases [O iii ]/H β > 1. Instead, two galaxies have [O iii ]/H β < 1, indicating that the NIRCam flux excess is mainly driven by H β . Most prominent line emitters are very young starbursts or galaxies on their way to/from the starburst cloud. They make for a cosmic SFR density log 10 ( ρ SFR H α / ( M ⊙ yr − 1 Mpc − 3 ) ) ≃ − 2.35 , which is about a quarter of the total value ( log 10 ( ρ SFR tot / ( M ⊙ yr − 1 Mpc − 3 ) ) ≃ − 1.76 ) at z ≃ 7–8. Therefore, the strong H α emitters likely had a significant role in reionization.