The Astrophysical Journal (Jan 2025)
The MBH–M∗ Relation up to z ∼ 2 through Decomposition of COSMOS-Web NIRCam Images
- Takumi S. Tanaka,
- John D. Silverman,
- Xuheng Ding,
- Knud Jahnke,
- Benny Trakhtenbrot,
- Erini Lambrides,
- Masafusa Onoue,
- Irham Taufik Andika,
- Angela Bongiorno,
- Andreas L. Faisst,
- Steven Gillman,
- Christopher C. Hayward,
- Michaela Hirschmann,
- Anton Koekemoer,
- Vasily Kokorev,
- Zhaoxuan Liu,
- Georgios E. Magdis,
- Alvio Renzini,
- Caitlin Casey,
- Nicole E. Drakos,
- Maximilien Franco,
- Ghassem Gozaliasl,
- Jeyhan Kartaltepe,
- Daizhong Liu,
- Henry Joy McCracken,
- Jason Rhodes,
- Brant Robertson,
- Sune Toft
Affiliations
- Takumi S. Tanaka
- ORCiD
- Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan ; [email protected]; Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study , The University of Tokyo, Kashiwa, Chiba 277-8583, Japan; Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo , Kashiwa, Chiba 277-8583, Japan
- John D. Silverman
- ORCiD
- Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan ; [email protected]; Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study , The University of Tokyo, Kashiwa, Chiba 277-8583, Japan; Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo , Kashiwa, Chiba 277-8583, Japan; Center for Astrophysical Sciences, Department of Physics & Astronomy, Johns Hopkins University , Baltimore, MD 21218, USA
- Xuheng Ding
- ORCiD
- Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan ; [email protected]; Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study , The University of Tokyo, Kashiwa, Chiba 277-8583, Japan; Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo , Kashiwa, Chiba 277-8583, Japan; School of Physics and Technology, Wuhan University , Wuhan 430072, People’s Republic of China
- Knud Jahnke
- ORCiD
- Max-Planck-Institut für Astronomie , Königstuhl 17, D-69117 Heidelberg, Germany
- Benny Trakhtenbrot
- ORCiD
- School of Physics and Astronomy, Tel Aviv University , Tel Aviv 69978, Israel
- Erini Lambrides
- ORCiD
- NASA-Goddard Space Flight Center , Code 662, Greenbelt, MD, 20771, USA
- Masafusa Onoue
- ORCiD
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study , The University of Tokyo, Kashiwa, Chiba 277-8583, Japan; Kavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People’s Republic of China
- Irham Taufik Andika
- ORCiD
- Technical University of Munich , TUM School of Natural Sciences, Department of Physics, James-Franck-Str. 1, D-85748 Garching, Germany; Max-Planck-Institut für Astrophysik , Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany
- Angela Bongiorno
- ORCiD
- INAF–Osservatorio Astronomico di Roma , Via Frascati 33, I-00078, Monte Porzio Catone, Italy
- Andreas L. Faisst
- ORCiD
- Caltech/IPAC , 1200 E. California Boulevard, Pasadena, CA 91125, USA
- Steven Gillman
- ORCiD
- Cosmic Dawn Center (DAWN) , Denmark; DTU Space , Technical University of Denmark, Elektrovej, Building 328, 2800, Kgs. Lyngby, Denmark
- Christopher C. Hayward
- ORCiD
- Center for Computational Astrophysics , Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USA
- Michaela Hirschmann
- ORCiD
- Institute for Physics , Laboratory for Galaxy Evolution and Spectral Modelling, EPFL, Observatoire de Sauverny, Chemin Pegasi 51, 1290 Versoix, Switzerland
- Anton Koekemoer
- ORCiD
- Space Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USA
- Vasily Kokorev
- ORCiD
- Kapteyn Astronomical Institute, University of Groningen , P.O. Box 800, NL-9700AV Groningen, The Netherlands
- Zhaoxuan Liu
- ORCiD
- Department of Astronomy, Graduate School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo, 113-0033, Japan ; [email protected]; Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study , The University of Tokyo, Kashiwa, Chiba 277-8583, Japan; Center for Data-Driven Discovery, Kavli IPMU (WPI), UTIAS, The University of Tokyo , Kashiwa, Chiba 277-8583, Japan
- Georgios E. Magdis
- ORCiD
- Cosmic Dawn Center (DAWN) , Denmark; DTU-Space, Technical University of Denmark , Elektrovej 327, DK2800 Kgs. Lyngby, Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, Denmark
- Alvio Renzini
- ORCiD
- Osservatorio Astronomico di Padova , Vicolo dell’Osservatorio 5, Padova, I-35122, Italy
- Caitlin Casey
- ORCiD
- Cosmic Dawn Center (DAWN) , Denmark; The University of Texas at Austin , 2515 Speedway Boulevard Stop C1400, Austin, TX 78712, USA
- Nicole E. Drakos
- ORCiD
- Department of Physics and Astronomy, University of Hawaii , Hilo, 200 W Kawili Street, Hilo, HI 96720, USA
- Maximilien Franco
- ORCiD
- The University of Texas at Austin , 2515 Speedway Boulevard Stop C1400, Austin, TX 78712, USA
- Ghassem Gozaliasl
- ORCiD
- Department of Computer Science, Aalto University , PO Box 15400, Espoo, FI-00 076, Finland; Department of Physics, Faculty of Science, University of Helsinki , 00014-Helsinki, Finland
- Jeyhan Kartaltepe
- ORCiD
- Laboratory for Multiwavelength Astrophysics, School of Physics and Astronomy, Rochester Institute of Technology , 84 Lomb Memorial Drive, Rochester, NY 14623, USA
- Daizhong Liu
- ORCiD
- Max-Planck-Institut für extraterrestrische Physik , Gießenbachstraße 1, 85748 Garching b. München, Germany
- Henry Joy McCracken
- ORCiD
- Institut d’Astrophysique de Paris , UMR 7095, CNRS, and Sorbonne Universit’e, 98 bis boulevard Arago, F-75014 Paris, France
- Jason Rhodes
- ORCiD
- Jet Propulsion Laboratory, California Institute of Technology , 4800 Oak Grove Drive, Pasadena, CA 91001, USA
- Brant Robertson
- ORCiD
- Department of Astronomy and Astrophysics, University of California , Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA
- Sune Toft
- ORCiD
- Cosmic Dawn Center (DAWN) , Denmark; Niels Bohr Institute, University of Copenhagen , Jagtvej 128, DK-2200 Copenhagen N, Denmark
- DOI
- https://doi.org/10.3847/1538-4357/ad9d0a
- Journal volume & issue
-
Vol. 979,
no. 2
p. 215
Abstract
Our knowledge of relations between supermassive black holes and their host galaxies at z ≳ 1 is still limited, even though being actively sought out to z ∼ 6. Here, we use the high resolution and sensitivity of JWST to measure the host galaxy properties for 107 X-ray-selected type-I active galactic nuclei (AGNs) at 0.68 < z < 2.5 with rest-frame optical/near-infrared imaging from COSMOS-Web and PRIMER. Black hole masses ( $\mathrm{log}\left({M}_{{\rm{BH}}}/{M}_{\odot }\right)\sim 6.9-9.6$ ) are available from previous spectroscopic campaigns. We extract the host galaxy components from four NIRCam broadband images and the Hubble Space Telescope/Advanced Camera for Surveys F814W image by applying a 2D image decomposition technique. We detect the host galaxy for ∼90% of the sample after subtracting the unresolved AGN emission. With host photometry free of AGN emission, we determine the stellar mass of the host galaxies to be $\mathrm{log}\left({M}_{* }/{M}_{\odot }\right)\sim 9.5-11.6$ through spectral energy distribution fitting and measure the evolution of the mass relation between SMBHs and their host galaxies. Considering selection biases and measurement uncertainties, we find that the M _BH / M _* ratio evolves as ${\left(1+z\right)}^{0.4{8}_{-0.62}^{+0.31}}$ thus remains essentially constant or exhibits mild evolution up to z ∼ 2.5. We also see an amount of scatter ( ${\sigma }_{\mu }=0.3{0}_{-0.13}^{+0.14}$ ), similar to the local relation and consistent with low- z studies, and a noncausal cosmic assembly history where mergers contribute to the statistical averaging toward the local relation is still feasible. We highlight improvements to come with larger samples from JWST and, particularly, Euclid, which will exceed the statistical power of current wide and deep surveys.
Keywords
