MIDIS: The Relation between Strong (Hβ + [O iii]) Emission, Star Formation, and Burstiness around the Epoch of Reionization

Autor(en): K. I. Caputi, P. Rinaldi, E. Iani, P. G. Pérez-González, G. Ostlin, L. Colina, T. R. Greve, H. U. Norgaard-Nielsen, G. S. Wright, J. Álvarez-Márquez, A. Eckart, J. Hjorth, A. Labiano, O. Le Fèvre, F. Walter, P. van der Werf, L. Boogaard, L. Costantin, A. Crespo Gómez, S. Gillman, I. Jermann, D. Langeroodi, J. Melinder, F. Peissker, M. Gudel, Th Henning, P. O. Lagage, T. P. Ray
Abstrakt: We investigate the properties of strong (Hβ + [O iii]) emitters before and after the end of the “Epoch of Reionization” from z = 8 to z = 5.5. We make use of ultradeep JWST/NIRCam imaging in the parallel field (P2) of the MIRI Deep Imaging Survey (MIDIS) in the Hubble eXtreme Deep Field (H-XDF), in order to select prominent (Hβ + [O iii]) emitters (with rest-frame equivalent width (EW₀) ≳ 100 Å) at z = 5.5-7, based on their flux density enhancement in the F356W band with respect to the spectral energy distribution continuum. We complement our selection with other (Hβ + [O iii]) emitters from the literature at similar and higher (z = 7−8) redshifts. We find (nonindependent) anticorrelations between EW₀(Hβ + [O iii]) and both galaxy stellar mass and age, in agreement with previous studies, and a positive correlation with specific star formation rate (sSFR). On the SFR-M ^⋆ plane, the (Hβ + [O iii]) emitters populate both the star formation main sequence and the starburst region, which become indistinguishable at low stellar masses ( log 10 ( M ⋆ ) < 7.5 ). We find tentative evidence for a nonmonotonic relation between EW₀(Hβ + [O iii]) and SFR, such that both parameters correlate with each other at SFR ≳ 1 M _⊙ yr⁻¹, while the correlation flattens out at lower SFRs. This suggests that low metallicities producing high EW₀(Hβ + [O iii]) could be important at low SFR values. Interestingly, the properties of the strong emitters and other galaxies (33% and 67% of our z = 5.5-7 sample, respectively) are similar, including, in many cases, high sSFR. Therefore, it is crucial to consider both emitters and nonemitters to obtain a complete picture of the cosmic star formation activity around the Epoch of Reionization.
Organisation(en): Institut für Astrophysik
Externe Organisation(en): University of Groningen, University of Copenhagen, European Space Astronomy Centre (ESA), Oskar Klein Centre, Technical University of Denmark (DTU), The Royal Observatory, Edinburgh, Universität zu Köln, Aix-Marseille Université, Max-Planck-Institut für Astronomie, Leiden University, Eidgenössische Technische Hochschule Zürich, Université Paris Saclay, Dublin Institute for Advanced Studies
Journal: Astrophysical Journal
Band: 969
Anzahl der Seiten: 10
ISSN: 0004-637X
DOI: https://doi.org/10.3847/1538-4357/ad4eb2
Publikationsdatum: 07-2024
Peer-reviewed: Ja
ÖFOS 2012: 103003 Astronomie, 103004 Astrophysik
ASJC Scopus Sachgebiete: Astronomy and Astrophysics, Space and Planetary Science
Link zum Portal: https://ucrisportal.univie.ac.at/de/publications/9a35e404-3002-4281-a0f1-e564ee772b7d

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