Galactic-scale Feedback Observed in the 3C 298 Quasar Host Galaxy
Abstract
We present high angular resolution multiwavelength data of the 3C 298 radio-loud quasar host galaxy (z = 1.439) taken using the W.M. Keck Observatory OSIRIS integral field spectrograph (IFS) with adaptive optics, the Atacama Large Millimeter/submillimeter Array (ALMA), the Hubble Space Telescope (HST) WFC3, and the Very Large Array (VLA). Extended emission is detected in the rest-frame optical nebular emission lines Hβ, [O III], Hα, [N II], and [S II], as well as in the molecular lines CO (J = 3−2) and (J = 5−4). Along the path of the relativistic jets of 3C 298, we detect conical outflows in ionized gas emission with velocities of up to 1700 km s^(-1) and an outflow rate of 450–1500 M⊙ yr^(-1) extended over 12 kpc. Near the spatial center of the conical outflow, CO (J = 3−2) emission shows a molecular gas disk with a rotational velocity of ±150 km s^(-1) and total molecular mass (M_H2) of 6.6 ± 0.36 x 10^9 M⊙. On the blueshifted side of the molecular disk, we observe broad extended emission that is due to a molecular outflow with a rate of 2300 M⊙ yr^(-1) and depletion timescale of 3 Myr. We detect no narrow Hα emission in the outflow regions, suggesting a limit on star formation of 0.3 M⊙ yr^(-1) kpc^(-2). Quasar-driven winds are evacuating the molecular gas reservoir, thereby directly impacting star formation in the host galaxy. The observed mass of the supermassive black hole is 10^(9.37-9.56) M⊙, and we determine a dynamical bulge mass of M_(bulge) = 1-1.7 x 1-^(10) R/1.6 kpc M⊙. The bulge mass of 3C 298 lies 2–2.5 orders of magnitude below the expected value from the local galactic bulge—supermassive black hole mass (M_(bulge)-M_(BH)) relationship. A second galactic disk observed in nebular emission is offset from the quasar by 9 kpc, suggesting that the system is an intermediate-stage merger. These results show that galactic-scale negative feedback is occurring early in the merger phase of 3C 298, well before the coalescence of the galactic nuclei and assembly on the local M_(bulge)-M_(BH) relationship.
Additional Information
© 2017 The American Astronomical Society. Received 2017 September 11; revised 2017 November 3; accepted 2017 November 15; published 2017 December 20. The authors wish to thank Randy Campbell and Jim Lyke for their assistance at the telescope in acquiring the Keck OSIRIS data sets. We also appreciate valuable discussions with Dusan Keres and the constructive comments made by the anonymous referee. The data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This paper makes use of the following ALMA data: ADS/JAO.ALMA[2013.1.01359.S]. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC, and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive (Program GO13023) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. A portion of the research was conducted at The Dunlap Institute for Astronomy and Astrophysics that is funded through an endowment established by the David Dunlap family and the University of Toronto. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Facilities: Keck (OSIRIS-LGSAO) - , ALMA (Band 4 and 6) - Atacama Large Millimeter Array, HST(WFC3) - Hubble Space Telescope satellite, VLA - Very Large Array. Software: Scipy: (Jones et al. 2001), CASA: (McMullin et al. 2007), OSIRIS Data Reduction Pipeline: (Lyke et al. 2017), Matplotlib (Hunter 2007).Attached Files
Published - Vayner_2017_ApJ_851_126.pdf
Submitted - 1709.03510.pdf
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Additional details
- Eprint ID
- 83976
- Resolver ID
- CaltechAUTHORS:20171220-101806680
- W. M. Keck Foundation
- NAS 5-26555
- NASA
- David Dunlap Family
- University of Toronto
- NASA/JPL/Caltech
- Created
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2017-12-20Created from EPrint's datestamp field
- Updated
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2021-11-15Created from EPrint's last_modified field