High Star Formation Rates of Low Eddington Ratio Quasars at $z\gtrsim 6$

Abstract

Recent simulation studies suggest that the supermassive black hole (SMBH) growth in the early universe may precede the prolonged intense star formation within its host galaxy, instead of quasars appearing after the obscured dusty star formation phase. If so, high-redshift quasars with low Eddington ratios (${\lambda }_{\mathrm{Edd}}$) would be found in actively star-forming hosts with a star formation rate (SFR) of $>100M_{\odot }$ yr${}^{-1}$. We present the sub-mm observations of IMS J2204+0112, a faint quasar with a quasar bolometric luminosity of $L_{\mathrm{bol}}=4.2\times 10^{12}{L}_{\odot }$ and a low ${\lambda }_{\mathrm{Edd}}$ of only 0.1 at $z\sim 6$, carried out with the Atacama Large Millimeter/submillimeter Array (ALMA). From its sub-mm fluxes, we measure the rest-frame far-infrared (FIR) luminosity of $L_{\mathrm{FIR}}=(3$--$4)\times 10^{12}{L}_{\odot }$. Interestingly, the derived host galaxy's SFR is $\sim 500$--$700M_{\odot }$ yr${}^{-1}$, an order of magnitude higher than those of the $L_{\mathrm{bol}}$-matched $z\gtrsim 6$ quasars with high ${\lambda }_{\mathrm{Edd}}$. Similar FIR excesses are also found for five $z\gtrsim 6$ low-${\lambda }_{\mathrm{Edd}}$ quasars (${\lambda }_{\mathrm{Edd}}<0.2$) in the literature. We show that the overall SFR, $M_{\mathrm{BH}}$, and ${\lambda }_{\mathrm{Edd}}$ distributions of these and other sub-mm-detected quasars at $z\gtrsim 6$ can be explained with the evolutionary track of high-redshift quasars in a simulation study where low ${\lambda }_{\mathrm{Edd}}$ and high SFR quasars are expected at the end of the SMBH growth. This suggests that the nuclear activities of the low ${\lambda }_{\mathrm{Edd}}$, high $L_{\mathrm{FIR}}$ quasars are on the brink of being turned off, while their host galaxies continue to form the bulk of their stars at SFR $>100M_{\odot }$ yr${}^{-1}$.

arXiv comment15 pages, 7 figures, 3 tables. Accepted for publication in ApJ

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