@article{afc86195d9054326bfc971ef6c995a3c,
title = "CEERS Key Paper. VI. JWST/MIRI Uncovers a Large Population of Obscured AGN at High Redshifts",
abstract = "Mid-infrared (mid-IR) observations are powerful in identifying heavily obscured active galactic nuclei (AGN) that have weak emission in other wavelengths. Data from the Mid-Infrared Instrument (MIRI) on board the James Webb Space Telescope provides an excellent opportunity to perform such studies. We take advantage of the MIRI imaging data from the Cosmic Evolution Early Release Science Survey to investigate the AGN population in the distant universe. We estimate the source properties of MIRI-selected objects by utilizing spectral energy distribution (SED) modeling, and classify them into star-forming galaxies (SFs), SF-AGN mixed objects, and AGN. The source numbers of these types are 433, 102, and 25, respectively, from four MIRI pointings covering ∼9 arcmin2. The sample spans a redshift range of ≈0-5. We derive the median SEDs for all three source types, respectively, and publicly release them. The median MIRI SED of AGN is similar to the typical SEDs of hot dust-obscured galaxies and Seyfert 2s, for which the mid-IR SEDs are dominated by emission from AGN-heated hot dust. Based on our SED-fit results, we estimate the black hole accretion density (BHAD; i.e., total BH growth rate per comoving volume) as a function of redshift. At z < 3, the resulting BHAD agrees with the X-ray measurements in general. At z > 3, we identify a total of 27 AGN and SF-AGN mixed objects, leading to that our high-z BHAD is substantially higher than the X-ray results (∼0.5 dex at z ≈ 3-5). This difference indicates MIRI can identify a large population of heavily obscured AGN missed by X-ray surveys at high redshifts.",
author = "G. Yang and Caputi, {K. I.} and C. Papovich and {Arrabal Haro}, P. and Bagley, {M. B.} and P. Behroozi and Bell, {E. F.} and L. Bisigello and V. Buat and D. Burgarella and Y. Cheng and Cleri, {N. J.} and R. Dav{\'e} and M. Dickinson and D. Elbaz and Ferguson, {H. C.} and Finkelstein, {S. L.} and Grogin, {N. A.} and Hathi, {N. P.} and M. Hirschmann and Holwerda, {B. W.} and M. Huertas-Company and Hutchison, {T. A.} and E. Iani and Kartaltepe, {J. S.} and A. Kirkpatrick and Kocevski, {D. D.} and Koekemoer, {A. M.} and V. Kokorev and Larson, {R. L.} and Lucas, {R. A.} and P{\'e}rez-Gonz{\'a}lez, {P. G.} and P. Rinaldi and L. Shen and Trump, {J. R.} and {De La Vega}, A. and Yung, {L. Y.A.} and Zavala, {J. A.}",
note = "Funding Information: We thank the referee for helpful feedback that improved this work. We acknowledge the hard work of our colleagues in the CEERS collaboration and everyone involved in the JWST mission. G.Y., K.I.C., and E.I. acknowledge funding from the Netherlands Research School for Astronomy (NOVA). K.I.C. and V.K. acknowledge funding from the Dutch Research Council (NWO) through the award of the Vici Grant VI.C.212.036. C.P. thanks Marsha and Ralph Schilling for generous support of this research. T.A.H. is supported by an appointment to the NASA Postdoctoral Program (NPP) at NASA Goddard Space Flight Center, administered by Oak Ridge Associated Universities under contract with NASA. This work acknowledges support from the NASA/ESA/CSA James Webb Space Telescope through the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-03127. Support for program No. JWST-ERS01345 was provided through a grant from the STScI under NASA contract NAS5-03127. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via doi: 10.17909/agda-2w34 . STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS526555. Support to MAST for these data is provided by the NASA Office of Space Science via grant NAG57584 and by other grants and contracts. Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",
year = "2023",
month = jun,
doi = "10.3847/2041-8213/acd639",
language = "English",
volume = "950",
journal = "Astrophysical Journal Letters",
issn = "2041-8205",
publisher = "IOP PUBLISHING LTD",
number = "1",
}