The Astrophysical Journal (Jan 2025)
First Results from the JWST Early Release Science Program Q3D: The Fast Outflow in a Red Quasar at z = 0.44
- Weizhe Liu,
- Sylvain Veilleux,
- Swetha Sankar,
- David S. N. Rupke,
- Nadia L. Zakamska,
- Dominika Wylezalek,
- Andrey Vayner,
- Caroline Bertemes,
- Yuzo Ishikawa,
- Yu-Ching Chen,
- Jenny E. Greene,
- Timothy Heckman,
- Guilin Liu,
- Hsiao-Wen Chen,
- Dieter Lutz,
- Sean D. Johnson,
- Nicole P. H. Nesvadba,
- Patrick Ogle,
- Nadiia Diachenko,
- Andy D. Goulding,
- Kevin N. Hainline,
- Fred Hamann,
- Hui Xian Grace Lim,
- Nora Lützgendorf,
- Vincenzo Mainieri,
- Ryan McCrory,
- Grey Murphree,
- Lu Shen,
- Eckhard Sturm,
- Lillian Whitesell
Affiliations
- Weizhe Liu
- ORCiD
- Steward Observatory, University of Arizona , 933 N. Cherry Avenue, Tucson, AZ 85721, USA ; [email protected]
- Sylvain Veilleux
- ORCiD
- Department of Astronomy and Joint Space-Science Institute, University of Maryland , College Park, MD 20742, USA
- Swetha Sankar
- ORCiD
- Department of Physics and Astronomy, Bloomberg Center, Johns Hopkins University , Baltimore, MD 21218, USA
- David S. N. Rupke
- ORCiD
- Department of Physics, Rhodes College , Memphis, TN 38112, USA
- Nadia L. Zakamska
- ORCiD
- Department of Physics and Astronomy, Bloomberg Center, Johns Hopkins University , Baltimore, MD 21218, USA; Institute for Advanced Study , Princeton, NJ 08540, USA
- Dominika Wylezalek
- ORCiD
- Zentrum für Astronomie der Universität Heidelberg , Astronomisches Rechen-Institut, Mönchhofstr 12-14, D-69120 Heidelberg, Germany
- Andrey Vayner
- ORCiD
- IPAC, California Institute of Technology , 1200 E. California Boulevard, Pasadena, CA 91125, USA
- Caroline Bertemes
- ORCiD
- Zentrum für Astronomie der Universität Heidelberg , Astronomisches Rechen-Institut, Mönchhofstr 12-14, D-69120 Heidelberg, Germany
- Yuzo Ishikawa
- ORCiD
- Department of Physics and Astronomy, Bloomberg Center, Johns Hopkins University , Baltimore, MD 21218, USA
- Yu-Ching Chen
- ORCiD
- Department of Physics and Astronomy, Bloomberg Center, Johns Hopkins University , Baltimore, MD 21218, USA
- Jenny E. Greene
- ORCiD
- Department of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08544, USA
- Timothy Heckman
- ORCiD
- Department of Physics and Astronomy, Bloomberg Center, Johns Hopkins University , Baltimore, MD 21218, USA
- Guilin Liu
- ORCiD
- CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China , Hefei, Anhui 230026, People’s Republic of China; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of China
- Hsiao-Wen Chen
- ORCiD
- Department of Astronomy & Astrophysics, The University of Chicago , 5640 South Ellis Avenue, Chicago, IL 60637, USA
- Dieter Lutz
- ORCiD
- Max-Planck-Institut für Extraterrestrische Physik , Gießenbachstraße 1, D-85748 Garching, Germany
- Sean D. Johnson
- ORCiD
- Department of Astronomy, University of Michigan , Ann Arbor, MI 48109, USA
- Nicole P. H. Nesvadba
- ORCiD
- Université de la Côte d’Azur , Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, CS 34229, Nice cedex 4 F-06304, France
- Patrick Ogle
- ORCiD
- Space Telescope Science Institute , 3700, San Martin Drive, Baltimore, MD 21218, USA
- Nadiia Diachenko
- ORCiD
- Department of Physics and Astronomy, Bloomberg Center, Johns Hopkins University , Baltimore, MD 21218, USA
- Andy D. Goulding
- ORCiD
- Department of Astrophysical Sciences, Princeton University , 4 Ivy Lane, Princeton, NJ 08544, USA
- Kevin N. Hainline
- ORCiD
- Steward Observatory, University of Arizona , 933 North Cherry Avenue, Tucson, AZ 85721, USA
- Fred Hamann
- Department of Physics & Astronomy, University of California, Riverside , Riverside, CA 92521, USA
- Hui Xian Grace Lim
- Department of Physics, Rhodes College , Memphis, TN 38112, USA
- Nora Lützgendorf
- ORCiD
- European Space Agency, Space Telescope Science Institute , Baltimore, MD, USA
- Vincenzo Mainieri
- ORCiD
- European Southern Observatory , Karl-Schwarzschild-Straße 2, D-85748 Garching bei München, Germany
- Ryan McCrory
- Department of Physics, Rhodes College , Memphis, TN 38112, USA
- Grey Murphree
- ORCiD
- Department of Physics, Rhodes College , Memphis, TN 38112, USA; Institute for Astronomy, University of Hawai’i , Honolulu, HI 96822, USA
- Lu Shen
- ORCiD
- Department of Physics and Astronomy, Texas A&M University , College Station, TX 77843-4242, USA; George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University , College Station, TX 77843-4242, USA
- Eckhard Sturm
- ORCiD
- Max-Planck-Institut für Extraterrestrische Physik , Gießenbachstraße 1, D-85748 Garching, Germany
- Lillian Whitesell
- Department of Physics, Rhodes College , Memphis, TN 38112, USA
- DOI
- https://doi.org/10.3847/1538-4357/ada772
- Journal volume & issue
-
Vol. 980,
no. 1
p. 31
Abstract
Quasar feedback may play a key role in the evolution of massive galaxies. The dust-reddened quasar F2M110648.35+480712 at z = 0.4352 is one of the few cases at its redshift that exhibits powerful quasar feedback through bipolar outflows. Our new observation with the integral field unit mode of the Near-infrared Spectrograph on board JWST opens a new window to examine this spectacular outflow through the Pa α emission line with ~3× better spatial resolution than previous work. The morphology and kinematics of the Pa α nebula confirm the existence of a bipolar outflow extending on a scale of ∼17 × 14 kpc and with a velocity reaching ∼1100 km s ^−1 . The higher spatial resolution of our new observation leads to more reliable measurements of outflow kinematics. Considering only the spatially resolved outflow and assuming an electron density of 100 cm ^−2 , the mass, momentum, and kinetic energy outflow rates are ∼50–210 M _⊙ yr ^−1 , ∼(0.3–1.7) × 10 ^36 dynes (∼14%–78% of the quasar photon momentum flux), and ∼(0.16–1.27) × 10 ^44 erg s ^−1 (∼0.02%–0.20% of the quasar bolometric luminosity), respectively. The local instantaneous outflow rates generally decrease radially. We infer that the quasar is powerful enough to drive the outflow, while stellar processes cannot be overlooked as a contributing energy source. The mass outflow rate is ∼0.4–1.5 times the star formation rate, and the ratio of kinetic energy outflow rate to the quasar bolometric luminosity is comparable to the minimum value required for negative quasar feedback in simulations. This outflow may help regulate the star formation activity within the system to some extent.
Keywords
