Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics
We conduct a study of the gas kinematics of two quasar host galaxies at z ≳ 6 traced by the [C ii ] emission line using the Atacama Large Millimeter/submillimeter Array. By combining deep observations at both low and high resolution, we recover the diffuse emission, resolve its structure, and measu...
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2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ada145 |
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| author | Qinyue Fei John D. Silverman Seiji Fujimoto Ran Wang Luis C. Ho Manuela Bischetti Stefano Carniani Michele Ginolfi Gareth Jones Roberto Maiolino Wiphu Rujopakarn N. M. Förster Schreiber Juan M. Espejo Salcedo L. L. Lee |
| author_facet | Qinyue Fei John D. Silverman Seiji Fujimoto Ran Wang Luis C. Ho Manuela Bischetti Stefano Carniani Michele Ginolfi Gareth Jones Roberto Maiolino Wiphu Rujopakarn N. M. Förster Schreiber Juan M. Espejo Salcedo L. L. Lee |
| author_sort | Qinyue Fei |
| collection | DOAJ |
| description | We conduct a study of the gas kinematics of two quasar host galaxies at z ≳ 6 traced by the [C ii ] emission line using the Atacama Large Millimeter/submillimeter Array. By combining deep observations at both low and high resolution, we recover the diffuse emission, resolve its structure, and measure the rotation curves from the inner region of the galaxy to its outskirts using DysmalPy and ^3D Barolo . Assuming that both galaxies exhibit disk rotation driven by the gravitational potential of the galaxy, we find that the best-fit disk models have a V _rot / σ ≈ 2 and inferred circular velocities out to ∼6–8 kpc scales, well beyond the likely stellar distribution. We then determine the mass profiles of each component (stars, gas, dark matter) with priors on the baryon and dark matter properties. We find relatively large dark matter fractions within their effective radii ( f _DM ( R < R _e ) = ${0.61}_{-0.08}^{+0.08}$ and ${0.53}_{-0.23}^{+0.20}$ , respectively), which are significantly larger than those extrapolated from lower redshift studies and remain robust under different input parameters verified by Monte Carlo simulations. The large f _DM ( R < R _e ) corresponds to halo masses of ∼10 ^12.5 −10 ^12.8 M _⊙ , thus representative of the most massive halos at these redshifts. Notably, while the masses of these supermassive black holes (SMBHs) are approximately 1 dex higher than the low-redshift relationship with stellar mass, the closer alignment of SMBH and halo masses with a local relationship may indicate that the early formation of these SMBHs is linked to their dark matter halos, providing insights into the coevolution of galaxies and black holes in the early Universe. |
| format | Article |
| id | doaj-art-7320aaa28286487e9b4d6a7f8610adaa |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-7320aaa28286487e9b4d6a7f8610adaa2025-02-05T16:00:37ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198018410.3847/1538-4357/ada145Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas KinematicsQinyue Fei0https://orcid.org/0000-0001-7232-5355John D. Silverman1https://orcid.org/0000-0002-0000-6977Seiji Fujimoto2https://orcid.org/0000-0001-7201-5066Ran Wang3https://orcid.org/0000-0003-4956-5742Luis C. Ho4Manuela Bischetti5https://orcid.org/0000-0002-4314-021XStefano Carniani6https://orcid.org/0000-0002-6719-380XMichele Ginolfi7https://orcid.org/0000-0002-9122-1700Gareth Jones8https://orcid.org/0000-0002-0267-9024Roberto Maiolino9https://orcid.org/0000-0002-4985-3819Wiphu Rujopakarn10https://orcid.org/0000-0002-0303-499XN. M. Förster Schreiber11https://orcid.org/0000-0003-4264-3381Juan M. Espejo Salcedo12https://orcid.org/0000-0001-6703-4676L. L. Lee13https://orcid.org/0000-0001-7457-4371Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI) , UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo, Chiba, 277-8583, Japan; Department of Astronomy, School of Physics, Peking University , Beijing 100871, People’s Republic of China; Kavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People’s Republic of ChinaKavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI) , UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo, Chiba, 277-8583, Japan; Department of Astronomy, School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan; Center for Data-Driven Discovery, Kavli PMU (WPI), UTIAS, The University of Tokyo , Kashiwa,Chiba 277-8583, Japan; Center for Astrophysical Sciences, Departmentof Physics & Astronomy, Johns Hopkins University , Baltimore, MD 21218, USADepartment of Astronomy, The University of Texas at Austin , Austin,TX, USADepartment of Astronomy, School of Physics, Peking University , Beijing 100871, People’s Republic of China; Kavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People’s Republic of ChinaDepartment of Astronomy, School of Physics, Peking University , Beijing 100871, People’s Republic of China; Kavli Institute for Astronomy and Astrophysics, Peking University , Beijing 100871, People’s Republic of ChinaDipartimento di Fisica, Universitá di Trieste , Sezione di Astronomia, Via G.B. Tiepolo 11, I-34131 Trieste, Italy; INAF—Osservatorio Astronomico di Trieste , Via G. B. Tiepolo 11, I–34131 Trieste, ItalyScuola Normale Superiore , Piazza dei Cavalieri 7, I-56126 Pisa, ItalyDipartimento di Fisica e Astronomia, Università di Firenze , Via G. Sansone 1, I-50019, Sesto F.no (Firenze), Italy; INAF–Osservatorio Astrofisico di Arcetri , Largo E. Fermi 5, I-50125, Florence, ItalyCavendish Laboratory, University of Cambridge , 19 J. J. Thomson Avenue, Cambridge CB3 0HE, UK; Kavli Institute for Cosmology, University of Cambridge , Madingley Road, Cambridge CB3 0HA, UKCavendish Laboratory, University of Cambridge , 19 J. J. Thomson Avenue, Cambridge CB3 0HE, UK; Kavli Institute for Cosmology, University of Cambridge , Madingley Road, Cambridge CB3 0HA, UK; Department of Physics & Astronomy, University College London , GowerStreet, London WC1E 6BT, UKNational Astronomical Research Institute of Thailand , Don Kaeo, Mae Rim, Chiang Mai 50180, Thailand; Department of Physics, Faculty of Science, Chulalongkorn University , 254 Phayathai Road, Pathumwan, Bangkok 10330, ThailandMax-Planck-Institut für extraterrestrische Physik (MPE) , Giessenbachstr. 1, D-85748 Garching, GermanyMax-Planck-Institut für extraterrestrische Physik (MPE) , Giessenbachstr. 1, D-85748 Garching, GermanyMax-Planck-Institut für extraterrestrische Physik (MPE) , Giessenbachstr. 1, D-85748 Garching, GermanyWe conduct a study of the gas kinematics of two quasar host galaxies at z ≳ 6 traced by the [C ii ] emission line using the Atacama Large Millimeter/submillimeter Array. By combining deep observations at both low and high resolution, we recover the diffuse emission, resolve its structure, and measure the rotation curves from the inner region of the galaxy to its outskirts using DysmalPy and ^3D Barolo . Assuming that both galaxies exhibit disk rotation driven by the gravitational potential of the galaxy, we find that the best-fit disk models have a V _rot / σ ≈ 2 and inferred circular velocities out to ∼6–8 kpc scales, well beyond the likely stellar distribution. We then determine the mass profiles of each component (stars, gas, dark matter) with priors on the baryon and dark matter properties. We find relatively large dark matter fractions within their effective radii ( f _DM ( R < R _e ) = ${0.61}_{-0.08}^{+0.08}$ and ${0.53}_{-0.23}^{+0.20}$ , respectively), which are significantly larger than those extrapolated from lower redshift studies and remain robust under different input parameters verified by Monte Carlo simulations. The large f _DM ( R < R _e ) corresponds to halo masses of ∼10 ^12.5 −10 ^12.8 M _⊙ , thus representative of the most massive halos at these redshifts. Notably, while the masses of these supermassive black holes (SMBHs) are approximately 1 dex higher than the low-redshift relationship with stellar mass, the closer alignment of SMBH and halo masses with a local relationship may indicate that the early formation of these SMBHs is linked to their dark matter halos, providing insights into the coevolution of galaxies and black holes in the early Universe.https://doi.org/10.3847/1538-4357/ada145High-redshift galaxiesQuasarsGalaxy kinematicsGalaxy dark matter halos |
| spellingShingle | Qinyue Fei John D. Silverman Seiji Fujimoto Ran Wang Luis C. Ho Manuela Bischetti Stefano Carniani Michele Ginolfi Gareth Jones Roberto Maiolino Wiphu Rujopakarn N. M. Förster Schreiber Juan M. Espejo Salcedo L. L. Lee Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics The Astrophysical Journal High-redshift galaxies Quasars Galaxy kinematics Galaxy dark matter halos |
| title | Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics |
| title_full | Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics |
| title_fullStr | Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics |
| title_full_unstemmed | Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics |
| title_short | Assessing the Dark Matter Content of Two Quasar Host Galaxies at z ∼ 6 through Gas Kinematics |
| title_sort | assessing the dark matter content of two quasar host galaxies at z ∼ 6 through gas kinematics |
| topic | High-redshift galaxies Quasars Galaxy kinematics Galaxy dark matter halos |
| url | https://doi.org/10.3847/1538-4357/ada145 |
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