Arita, J.Kashikawa, N.Matsuoka, Y.He, W.Ito, K.Liang, Y.Ishimoto, R.Yoshioka, T.Takeda, Y.Iwasawa, KazushiOnoue, M.Toba, Y.Imanishi, M.2025-01-312025-01-3120230004-637Xhttps://hdl.handle.net/2445/218358We present, for the first time, dark matter halo (DMH) mass measurement of quasars at z ∼ 6 based on a clustering analysis of 107 quasars. Spectroscopically identified quasars are homogeneously extracted from the Hyper Suprime-Cam Strategic Survey Program wide layer over 891 deg2. We evaluate the clustering strength by three different autocorrelation functions: projected correlation function, angular correlation function, and redshift–space correlation function. The DMH mass of quasars at z ∼ 6 is evaluated as with the bias parameter b = 20.8 ± 8.7 by the projected correlation function. The other two estimators agree with these values; though, each uncertainty is large. The DMH mass of quasars is found to be nearly constant ∼1012.5h−1M⊙ throughout cosmic time, suggesting that there is a characteristic DMH mass where quasars are always activated. As a result, quasars appear in the most massive halos at z ∼ 6, but in less extreme halos thereafter. The DMH mass does not appear to exceed the upper limit of 1013h−1M⊙, which suggests that most quasars reside in DMHs with across most of the cosmic time. Our results supporting a significant increasing bias with redshift are consistent with the bias evolution model with inefficient active galactic nucleus feedback at z ∼ 6. The duty cycle (fduty) is estimated as 0.019 ± 0.008 by assuming that DMHs in some mass interval can host a quasar. The average stellar mass is evaluated from stellar-to-halo mass ratio as, which is found to be consistent with [C ii] observational results.1 p.application/pdfeng(c) American Astronomical Society, 2023QuàsarsForats negres (Astronomia)GalàxiesQuasarsBlack holes (Astronomy)Galaxiesinfo:eu-repo/semantics/article7538962025-01-31info:eu-repo/semantics/openAccess