An AGN with an Ionized Gas Outflow in a Massive Quiescent Galaxy in a Protocluster at z = 3.09

Creators: Kubo, Mariko; Umehata, Hideki; Matsuda, Yuichi; Kajisawa, Masaru; Steidel, Charles C.; Yamada, Toru; Tanaka, Ichi; Hatsukade, Bunyo; Tamura, Yoichi; Nakanishi, Kouichiro; Kohno, Kotaro; Lee, Kianhong; Matsuda, Keiichi; Ao, Yiping; Nagao, Tohru; Yun, Min S.

Abstract

We report the detection of an ionized gas outflow from an X-ray active galactic nucleus hosted in a massive quiescent galaxy in a protocluster at z = 3.09 (J221737.29+001823.4). It is a type-2 QSO with broad (W_80 > 1000 km s^(−1)) and strong (log(L[OIII]/erg s^(−1)) ≈ 43.4) [O III]λλ 4959,5007 emission lines detected by slit spectroscopy in three-position angles using Multi-Object Infra-Red Camera and Spectrograph (MOIRCS) on the Subaru telescope and the Multi-Object Spectrometer For Infra-Red Exploration (MOSFIRE) on the Keck-I telescope. In the all slit directions, [O III] emission is extended to ∼15 physical kpc and indicates a powerful outflow spreading over the host galaxy. The inferred ionized gas mass outflow rate is 22 ± 3 M_⊙ yr^(−1). Although it is a radio source, according to the line diagnostics using Hβ, [O II], and [O III], photoionization by the central QSO is likely the dominant ionization mechanism rather than shocks caused by radio jets. On the other hand, the spectral energy distribution of the host galaxy is well characterized as a quiescent galaxy that has shut down star formation several hundred Myr ago. Our results suggest a scenario that QSOs are powered after the shutdown of the star formation and help complete the quenching of massive quiescent galaxies at high redshift.

Additional Information

This work has been supported by JSPS KAKENHI Grant Nos. 20K14530, 21H044902 (MK), 17K14252, 20H01953 (HU), 19H00697, 20H01949 (TN), 17H06130 (YT and KK). This work has been also supported by a US National Science Foundation (NSF) grant AST-2009278 (CCS). This work has been also supported by NAOJ ALMA Scientific Research Grant Numbers 2018-09B (YT) The spectroscopic data 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 observations were carried out within the framework of the Subaru-Keck/Subaru-Gemini time exchange program, which is operated by the National Astronomical Observatory of Japan. The Ks -band image was collected with nuMOIRCS at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We are honored and grateful for the opportunity of observing the Universe from Maunakea, which has the cultural, historical, and natural significance in Hawaii. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00162.S, ADS/JAO.ALMA#2016.1.00580.S, ADS/JAO.ALMA #2017.1.01332.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The F814W-band image is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

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Resource type: Journal Article
Publisher: American Astronomical Society
Published in: Astrophysical Journal, 935(2), 89, ISSN: 0004-637X.