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Larson, Rebecca L.; Finkelstein, Steven L.; Kocevski, Dale D.; Hutchison, Taylor A.; Trump, Jonathan R.; Arrabal Haro, Pablo; Bromm, Volker; Cleri, Nikko J.; Dickinson, Mark; Fujimoto, Seiji; Kartaltepe, Jeyhan S.; Koekemoer, Anton M.; Papovich, Casey; Pirzkal, Nor; Tacchella, Sandro; Zavala, Jorge A.; Bagley, Micaela; Behroozi, Peter; Champagne, Jaclyn B.; Cole, Justin W.; Jung, Intae; Morales, Alexa M.; Yang, Guang; Zhang, Haowen; Zitrin, Adi; Amorín, Ricardo O.; Burgarella, Denis; Casey, Caitlin M.; Chávez Ortiz, Óscar A.; Cox, Isabella G.; Chworowsky, Katherine; Fontana, Adriano; Gawiser, Eric; Grazian, Andrea; Grogin, Norman A.; Harish, Santosh; Hathi, Nimish P.; Hirschmann, Michaela; Holwerda, Benne W.; Juneau, Stéphanie; Leung, Gene C. K.; Lucas, Ray A.; McGrath, Elizabeth J.; Pérez-González, Pablo G.; Rigby, Jane R.; Seillé, Lise-Marie; Simons, Raymond C.; de la Vega, Alexander; Weiner, Benjamin J.; Wilkins, Stephen M.; Yung, L. Y. Aaron
Astrophysical journal. Letters, 08/2023, Letnik: 953, Številka: 2Journal Article
Abstract We report the discovery of an accreting supermassive black hole at z = 8.679. This galaxy, denoted here as CEERS_1019, was previously discovered as a Ly α -break galaxy by Hubble with a Ly α redshift from Keck. As part of the Cosmic Evolution Early Release Science (CEERS) survey, we have observed this source with JWST/NIRSpec, MIRI, NIRCam, and NIRCam/WFSS and uncovered a plethora of emission lines. The H β line is best fit by a narrow plus a broad component, where the latter is measured at 2.5 σ with an FWHM ∼1200 km s −1 . We conclude this originates in the broadline region of an active galactic nucleus (AGN). This is supported by the presence of weak high-ionization lines (N V, N IV, and C III), as well as a spatial point-source component. The implied mass of the black hole (BH) is log ( M BH / M ⊙ ) = 6.95 ± 0.37, and we estimate that it is accreting at 1.2 ± 0.5 times the Eddington limit. The 1–8 μ m photometric spectral energy distribution shows a continuum dominated by starlight and constrains the host galaxy to be massive (log M/M ⊙ ∼9.5) and highly star-forming (star formation rate, or SFR ∼ 30 M ⊙ yr −1 ; log sSFR ∼ − 7.9 yr −1 ). The line ratios show that the gas is metal-poor ( Z / Z ⊙ ∼ 0.1), dense ( n e ∼ 10 3 cm −3 ), and highly ionized (log U ∼ − 2.1). We use this present highest-redshift AGN discovery to place constraints on BH seeding models and find that a combination of either super-Eddington accretion from stellar seeds or Eddington accretion from very massive BH seeds is required to form this object.
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