Suppression of black-hole growth by strong outflows at redshifts 5.8-6.6.

Autor: Bischetti M; INAF - Osservatorio Astronomico di Trieste, Trieste, Italy. manuela.bischetti@inaf.it., Feruglio C; INAF - Osservatorio Astronomico di Trieste, Trieste, Italy.; IFPU - Institute for Fundamental Physics of the Universe, Trieste, Italy., D'Odorico V; INAF - Osservatorio Astronomico di Trieste, Trieste, Italy.; IFPU - Institute for Fundamental Physics of the Universe, Trieste, Italy.; Scuola Normale Superiore, Pisa, Italy., Arav N; Department of Physics, Virginia Tech, Blacksburg, VA, USA., Bañados E; Max-Planck-Institut für Astronomie, Heidelberg, Germany., Becker G; Department of Physics & Astronomy, University of California, Riverside, CA, USA., Bosman SEI; Max-Planck-Institut für Astronomie, Heidelberg, Germany., Carniani S; Scuola Normale Superiore, Pisa, Italy., Cristiani S; INAF - Osservatorio Astronomico di Trieste, Trieste, Italy., Cupani G; INAF - Osservatorio Astronomico di Trieste, Trieste, Italy., Davies R; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, Australia.; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australian Capital Territory, Australia., Eilers AC; MIT Kavli Institute for Astrophysics and Space Research, Cambridge, MA, USA., Farina EP; Max Planck Institut für Astrophysik, Garching bei München, Germany., Ferrara A; Scuola Normale Superiore, Pisa, Italy., Maiolino R; Kavli Institute for Cosmology, University of Cambridge, Cambridge, UK., Mazzucchelli C; European Southern Observatory, Vitacura, Chile., Mesinger A; Scuola Normale Superiore, Pisa, Italy., Meyer RA; Max-Planck-Institut für Astronomie, Heidelberg, Germany., Onoue M; Max-Planck-Institut für Astronomie, Heidelberg, Germany., Piconcelli E; INAF - Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy., Ryan-Weber E; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, Australia.; ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Canberra, Australian Capital Territory, Australia., Schindler JT; Max-Planck-Institut für Astronomie, Heidelberg, Germany., Wang F; Department of Astronomy, University of Arizona, Tucson, AZ, USA., Yang J; Steward Observatory, University of Arizona, Tucson, AZ, USA., Zhu Y; Department of Physics & Astronomy, University of California, Riverside, CA, USA., Fiore F; INAF - Osservatorio Astronomico di Trieste, Trieste, Italy.; IFPU - Institute for Fundamental Physics of the Universe, Trieste, Italy.
Jazyk: angličtina
Zdroj: Nature [Nature] 2022 May; Vol. 605 (7909), pp. 244-247. Date of Electronic Publication: 2022 May 11.
DOI: 10.1038/s41586-022-04608-1
Abstrakt: Bright quasars, powered by accretion onto billion-solar-mass black holes, already existed at the epoch of reionization, when the Universe was 0.5-1 billion years old 1 . How these black holes formed in such a short time is the subject of debate, particularly as they lie above the correlation between black-hole mass and galaxy dynamical mass 2,3 in the local Universe. What slowed down black-hole growth, leading towards the symbiotic growth observed in the local Universe, and when this process started, has hitherto not been known, although black-hole feedback is a likely driver 4 . Here we report optical and near-infrared observations of a sample of quasars at redshifts 5.8 ≲ z ≲ 6.6. About half of the quasar spectra reveal broad, blueshifted absorption line troughs, tracing black-hole-driven winds with extreme outflow velocities, up to 17% of the speed of light. The fraction of quasars with such outflow winds at z ≳ 5.8 is ≈2.4 times higher than at z ≈ 2-4. We infer that outflows at z ≳ 5.8 inject large amounts of energy into the interstellar medium and suppress nuclear gas accretion, slowing down black-hole growth. The outflow phase may then mark the beginning of substantial black-hole feedback. The red optical colours of outflow quasars at z ≳ 5.8 indeed suggest that these systems are dusty and may be caught during an initial quenching phase of obscured accretion 5 .
(© 2022. The Author(s), under exclusive licence to Springer Nature Limited.)
Databáze: MEDLINE
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