First Results from the JWST Early Release Science Program Q3D: Powerful Quasar-driven Galactic Scale Outflow at z = 3

Andrey Vayner, Nadia L. Zakamska, Yuzo Ishikawa, Swetha Sankar, Dominika Wylezalek, David S.N. Rupke, Sylvain Veilleux, Caroline Bertemes, Jorge K. Barrera-Ballesteros, Hsiao Wen Chen, Nadiia Diachenko, Andy D. Goulding, Jenny E. Greene, Kevin N. Hainline, Fred Hamann, Timothy Heckman, Sean D. Johnson, Hui Xian Grace Lim, Weizhe Liu, Dieter LutzNora Lützgendorf, Vincenzo Mainieri, Ryan McCrory, Grey Murphree, Nicole P.H. Nesvadba, Patrick Ogle, Eckhard Sturm, Lillian Whitesell

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Abstract

Quasar-driven galactic outflows are a major driver of the evolution of massive galaxies. We report observations of a powerful galactic-scale outflow in a z = 3 extremely red and intrinsically luminous (L bol ≃ 5 × 1047erg s−1) quasar SDSSJ1652 + 1728 with the Near-infrared Spectrograph on board JWST. We analyze the kinematics of rest-frame optical emission lines and identify the quasar-driven outflow extending out to ∼10 kpc from the quasar with a velocity offset of (v r = ± 500 km s−1) and high velocity dispersion (FWHM = 700-2400 km s−1). Due to JWST’s unprecedented surface brightness sensitivity in the near-infrared, we unambiguously show that the powerful high velocity outflow in an extremely red quasar encompasses a large swath of the host galaxy’s interstellar medium. Using the kinematics and dynamics of optical emission lines, we estimate the mass outflow rate—in the warm ionized phase alone—to be at least 2300 ± 1400 M yr−1. We measure a momentum flux ratio between the outflow and the quasar accretion disk of ∼1 on a kpc scale, indicating that the outflow was likely driven in a relatively high (>1023cm−2) column density environment through radiation pressure on dust grains. We find a coupling efficiency between the bolometric luminosity of the quasar and the outflow of 0.1%, matching the theoretical prediction of the minimum coupling efficiency necessary for negative quasar feedback. The outflow has sufficient energetics to drive the observed turbulence seen in shocked regions of the quasar host galaxy, which are likely directly responsible for prolonging the time that it takes for gas to cool efficiently.

Original languageEnglish (US)
Article number126
JournalAstrophysical Journal
Volume960
Issue number2
DOIs
StatePublished - Jan 1 2024

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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