Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program
We assess the dark matter halo masses of luminous active galactic nuclei (AGNs) over the redshift range 0.2–1.2 using galaxy–galaxy lensing based on imaging data from the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). We measure the weak lensing signal of a sample of 48,907 AGNs constructed u...
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IOP Publishing
2024-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ad86b5 |
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| author | Wentao Luo John D. Silverman Surhud More Andy Goulding Hironao Miyatake Takahiro Nishimichi Chiaki Hikage Lalitwadee Kawinwanichakij Junyao Li Qinxun Li Xiangchong Li Elinor Medezinski Masamune Oguri Taira Oogi Cristobal Sifon |
| author_facet | Wentao Luo John D. Silverman Surhud More Andy Goulding Hironao Miyatake Takahiro Nishimichi Chiaki Hikage Lalitwadee Kawinwanichakij Junyao Li Qinxun Li Xiangchong Li Elinor Medezinski Masamune Oguri Taira Oogi Cristobal Sifon |
| author_sort | Wentao Luo |
| collection | DOAJ |
| description | We assess the dark matter halo masses of luminous active galactic nuclei (AGNs) over the redshift range 0.2–1.2 using galaxy–galaxy lensing based on imaging data from the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). We measure the weak lensing signal of a sample of 48,907 AGNs constructed using HSC and Wide-field Infrared Survey Explorer photometry. As expected, we find that the lensing mass profile of total AGN sample is consistent with that of massive galaxies ( $\mathrm{log}({M}_{* }/{h}^{-2}{M}_{\odot })\sim $ 10.61). Surprisingly, the lensing signal remains unchanged when the AGN sample is split into four host galaxy stellar mass bins. Specifically, we find that the excess surface density of AGNs residing in galaxies with high stellar masses significantly differs from that of the control sample. We further fit a halo occupation distribution model to the data to infer the posterior distribution of parameters including the average halo mass. We find that the characteristic halo mass of the full AGN population lies near the knee ( $\mathrm{log}({M}_{{\rm{h}}}/{h}^{-1}{M}_{\odot })=12.0$ ) of the stellar-to-halo mass relation (SHMR). Illustrative of the results given above, the halo masses of AGNs residing in host galaxies with high stellar masses (i.e., above the knee of the SHMR) fall below the calibrated SHMR while the halo masses of the low stellar mass sample are more consistent with the established SHMR. These results indicate that massive halos with a higher clustering bias tend to suppress AGN activity, probably due to the lack of available gas. |
| format | Article |
| id | doaj-art-12aa4b3a963c4e8d8a689dd16a5bd06b |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-12aa4b3a963c4e8d8a689dd16a5bd06b2025-01-27T16:37:14ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-0197715910.3847/1538-4357/ad86b5Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic ProgramWentao Luo0https://orcid.org/0000-0003-1297-6142John D. Silverman1https://orcid.org/0000-0002-0000-6977Surhud More2https://orcid.org/0000-0002-2986-2371Andy Goulding3https://orcid.org/0000-0003-4700-663XHironao Miyatake4Takahiro Nishimichi5https://orcid.org/0000-0002-9664-0760Chiaki Hikage6Lalitwadee Kawinwanichakij7https://orcid.org/0000-0003-4032-2445Junyao Li8https://orcid.org/0000-0002-1605-915XQinxun Li9Xiangchong Li10https://orcid.org/0000-0003-2880-5102Elinor Medezinski11https://orcid.org/0000-0001-7007-2358Masamune Oguri12https://orcid.org/0000-0003-3484-399XTaira Oogi13Cristobal Sifon14Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cn; Department of Astronomy, School of Physical Sciences, University of Science and Technology of China , Hefei, Anhui 230026, People’s Republic of ChinaInstitute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cn; Department of Astronomy, School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, JapanInstitute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cn; IUCAA, Post Bag 4 Ganeshkhind, Savitribai Phule Pune University Campus , Pune 411 007, IndiaDepartment of Astrophysical Sciences, Peyton Hall Princeton University , 08544 NJ, USAInstitute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cn; Institute for Advanced Research, Nagoya University , Nagoya 464-8601, Japan; Division of Physics and Astrophysical Science, Graduate School of Science, Nagoya University , Nagoya 464-8602, JapanInstitute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cn; Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University , Kyoto 606-8502, JapanInstitute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cnInstitute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cnInstitute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cn; Department of Astronomy, School of Physical Sciences, University of Science and Technology of China , Hefei, Anhui 230026, People’s Republic of ChinaDepartment of Physics and Astronomy, University of Utah , INSCC, Salt Lake City, UT 84102, USAInstitute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cnDepartment of Astrophysical Sciences, Peyton Hall Princeton University , 08544 NJ, USAInstitute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cn; Research Center for the Early Universe, University of Tokyo , Tokyo 113-0033, Japan; Department of Physics, University of Tokyo , Tokyo 113-0033, JapanInstitute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), UTIAS, Tokyo Institutes for Advanced Study, University of Tokyo , Chiba 277-8583, Japan ; wtluo@ustc.edu.cnPhysics Institute, Pontificia Universidad Católica de Valparaíso , Valparaíso 2340025, ChileWe assess the dark matter halo masses of luminous active galactic nuclei (AGNs) over the redshift range 0.2–1.2 using galaxy–galaxy lensing based on imaging data from the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP). We measure the weak lensing signal of a sample of 48,907 AGNs constructed using HSC and Wide-field Infrared Survey Explorer photometry. As expected, we find that the lensing mass profile of total AGN sample is consistent with that of massive galaxies ( $\mathrm{log}({M}_{* }/{h}^{-2}{M}_{\odot })\sim $ 10.61). Surprisingly, the lensing signal remains unchanged when the AGN sample is split into four host galaxy stellar mass bins. Specifically, we find that the excess surface density of AGNs residing in galaxies with high stellar masses significantly differs from that of the control sample. We further fit a halo occupation distribution model to the data to infer the posterior distribution of parameters including the average halo mass. We find that the characteristic halo mass of the full AGN population lies near the knee ( $\mathrm{log}({M}_{{\rm{h}}}/{h}^{-1}{M}_{\odot })=12.0$ ) of the stellar-to-halo mass relation (SHMR). Illustrative of the results given above, the halo masses of AGNs residing in host galaxies with high stellar masses (i.e., above the knee of the SHMR) fall below the calibrated SHMR while the halo masses of the low stellar mass sample are more consistent with the established SHMR. These results indicate that massive halos with a higher clustering bias tend to suppress AGN activity, probably due to the lack of available gas.https://doi.org/10.3847/1538-4357/ad86b5Active galaxiesWeak gravitational lensing |
| spellingShingle | Wentao Luo John D. Silverman Surhud More Andy Goulding Hironao Miyatake Takahiro Nishimichi Chiaki Hikage Lalitwadee Kawinwanichakij Junyao Li Qinxun Li Xiangchong Li Elinor Medezinski Masamune Oguri Taira Oogi Cristobal Sifon Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program The Astrophysical Journal Active galaxies Weak gravitational lensing |
| title | Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program |
| title_full | Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program |
| title_fullStr | Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program |
| title_full_unstemmed | Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program |
| title_short | Dark Matter Halos of Luminous Active Galactic Nuclei from Galaxy–Galaxy Lensing with the HSC Subaru Strategic Program |
| title_sort | dark matter halos of luminous active galactic nuclei from galaxy galaxy lensing with the hsc subaru strategic program |
| topic | Active galaxies Weak gravitational lensing |
| url | https://doi.org/10.3847/1538-4357/ad86b5 |
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