Clustering of z~6.6 Quasars and [O III] Emitters Constrains Host Halo Masses and Duty Cycles in 25 ASPIRE Fields
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2026
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| author | Huang, Jiamu Hennawi, Joseph Pizzati, Elia Wang, Feige Yang, Jinyi Champagne, Jaclyn B. Fan, Xiaohui Bañados, Eduardo Jin, Xiangyu Kakiichi, Koki Meyer, Romain A. Sun, Fengwu Wu, Yunjing Zhang, Haowen Mazzucchelli, Chiara Eilers, Anna-Christina Pudoka, Maria Zhang, Huanian Schindler, Jan-Torge Schaller, Matthieu Schaye, Joop Snyder, Ben Kang, Yi Onorato, Silvia |
| author_facet | Huang, Jiamu Hennawi, Joseph Pizzati, Elia Wang, Feige Yang, Jinyi Champagne, Jaclyn B. Fan, Xiaohui Bañados, Eduardo Jin, Xiangyu Kakiichi, Koki Meyer, Romain A. Sun, Fengwu Wu, Yunjing Zhang, Haowen Mazzucchelli, Chiara Eilers, Anna-Christina Pudoka, Maria Zhang, Huanian Schindler, Jan-Torge Schaller, Matthieu Schaye, Joop Snyder, Ben Kang, Yi Onorato, Silvia |
| contents | We use data from the JWST ASPIRE Wide Field Slitless Spectroscopy (WFSS) program to measure the auto-correlation function of [O,{\sc iii}] emitters at 5.3$<z<$7.0 and the quasar--[O,{\sc iii}] emitter cross-correlation around 25 ASPIRE quasars (6.51$<z<$6.82; $\langle z\rangle=6.6$). We use synthetic source injection to calibrate the selection function, which we combine with the large-volume FLAMINGO-10k simulation (2.8,cGpc box) to construct realistic mock observations. Our simulation-based approach captures nonlinear structure growth and scale-dependent bias on small scales and derives covariance matrices that include cosmic variance. The clustering yields correlation lengths of $r_0^{\rm GG}=4.7^{+0.4}{-0.5},h^{-1}$,cMpc for the [O,{\sc iii}] auto-correlation with fixed slope $γ{\rm GG}=1.8$, and $r_0^{\rm QG}=8.7^{+0.8}{-0.9},h^{-1}$,cMpc for the quasar--[O,{\sc iii}] cross-correlation with $γ{\rm QG}=2.0$. We infer $\log(M_{h,{\rm min}}^{[{\rm O,III}]}/M_\odot)=10.5^{+0.1}{-0.1}$ for [O,{\sc iii}] emitters and $\log(M{h,{\rm min}}^{\rm QSO}/M_\odot)=12.1^{+0.3}{-0.4}$ for quasars. These imply duty cycles of $2.5^{+1.0}{-0.8}$,per,cent for [O,{\sc iii}] emitters and $0.3^{+4.0}{-0.3}$,per,cent for quasars, corresponding to UV-bright lifetimes of $t{\rm Q}=2.6^{+30}_{-2.5}$,Myr (less than 10,per,cent of a Salpeter $e$-folding time). The results indicate that the observed UV-luminous phase contributes little to total SMBH growth, placing tight constraints on early black-hole formation. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2602_04974 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Clustering of z~6.6 Quasars and [O III] Emitters Constrains Host Halo Masses and Duty Cycles in 25 ASPIRE Fields Huang, Jiamu Hennawi, Joseph Pizzati, Elia Wang, Feige Yang, Jinyi Champagne, Jaclyn B. Fan, Xiaohui Bañados, Eduardo Jin, Xiangyu Kakiichi, Koki Meyer, Romain A. Sun, Fengwu Wu, Yunjing Zhang, Haowen Mazzucchelli, Chiara Eilers, Anna-Christina Pudoka, Maria Zhang, Huanian Schindler, Jan-Torge Schaller, Matthieu Schaye, Joop Snyder, Ben Kang, Yi Onorato, Silvia Astrophysics of Galaxies We use data from the JWST ASPIRE Wide Field Slitless Spectroscopy (WFSS) program to measure the auto-correlation function of [O,{\sc iii}] emitters at 5.3$<z<$7.0 and the quasar--[O,{\sc iii}] emitter cross-correlation around 25 ASPIRE quasars (6.51$<z<$6.82; $\langle z\rangle=6.6$). We use synthetic source injection to calibrate the selection function, which we combine with the large-volume FLAMINGO-10k simulation (2.8,cGpc box) to construct realistic mock observations. Our simulation-based approach captures nonlinear structure growth and scale-dependent bias on small scales and derives covariance matrices that include cosmic variance. The clustering yields correlation lengths of $r_0^{\rm GG}=4.7^{+0.4}{-0.5},h^{-1}$,cMpc for the [O,{\sc iii}] auto-correlation with fixed slope $γ{\rm GG}=1.8$, and $r_0^{\rm QG}=8.7^{+0.8}{-0.9},h^{-1}$,cMpc for the quasar--[O,{\sc iii}] cross-correlation with $γ{\rm QG}=2.0$. We infer $\log(M_{h,{\rm min}}^{[{\rm O,III}]}/M_\odot)=10.5^{+0.1}{-0.1}$ for [O,{\sc iii}] emitters and $\log(M{h,{\rm min}}^{\rm QSO}/M_\odot)=12.1^{+0.3}{-0.4}$ for quasars. These imply duty cycles of $2.5^{+1.0}{-0.8}$,per,cent for [O,{\sc iii}] emitters and $0.3^{+4.0}{-0.3}$,per,cent for quasars, corresponding to UV-bright lifetimes of $t{\rm Q}=2.6^{+30}_{-2.5}$,Myr (less than 10,per,cent of a Salpeter $e$-folding time). The results indicate that the observed UV-luminous phase contributes little to total SMBH growth, placing tight constraints on early black-hole formation. |
| title | Clustering of z~6.6 Quasars and [O III] Emitters Constrains Host Halo Masses and Duty Cycles in 25 ASPIRE Fields |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2602.04974 |