Merging gas-rich galaxies that harbor low-luminosity twin quasars at z = 6.05: a promising progenitor of the most luminous quasars
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| Autori principali: | , , , , , , , , , , , , , , , , , |
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| Natura: | Preprint |
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2024
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| author | Izumi, Takuma Matsuoka, Yoshiki Onoue, Masafusa Strauss, Michael A. Umehata, Hideki Silverman, John D. Nagao, Tohru Imanishi, Masatoshi Kohno, Kotaro Toba, Yoshiki Iwasawa, Kazushi Nakanishi, Kouichiro Sawamura, Mahoshi Fujimoto, Seiji Kikuta, Satoshi Kawaguchi, Toshihiro Aoki, Kentaro Goto, Tomotsugu |
| author_facet | Izumi, Takuma Matsuoka, Yoshiki Onoue, Masafusa Strauss, Michael A. Umehata, Hideki Silverman, John D. Nagao, Tohru Imanishi, Masatoshi Kohno, Kotaro Toba, Yoshiki Iwasawa, Kazushi Nakanishi, Kouichiro Sawamura, Mahoshi Fujimoto, Seiji Kikuta, Satoshi Kawaguchi, Toshihiro Aoki, Kentaro Goto, Tomotsugu |
| contents | We present ALMA [CII] 158 $μ$m line and underlying far-infrared (FIR) continuum emission observations ($0''.57 \times 0''.46$ resolution) toward a quasar-quasar pair system recently discovered at $z = 6.05$ (Matsuoka et al. 2024). The quasar nuclei (C1 and C2) are faint ($M_{\rm 1450} \gtrsim -23$ mag), but we detect very bright [CII] emission bridging the 12 kpc between the two objects and extending beyond them (total luminosity $L_{\rm [CII]} \simeq 6 \times 10^9~L_\odot$). The [CII]-based total star formation rate of the system is $\sim 550~M_\odot$ yr$^{-1}$ (IR-based dust-obscured SFR is $\sim 100~M_\odot$ yr$^{-1}$), with a [CII]-based total gas mass of $\sim 10^{11}~M_\odot$. The dynamical masses of the two galaxies are large ($\sim 9 \times 10^{10}~M_\odot$ for C1 and $\sim 5 \times 10^{10}~M_\odot$ for C2). There is a smooth velocity gradient in [CII], indicating that these quasars are a tidally interacting system. We identified a dynamically distinct, fast [CII] component around C1: detailed inspection of the line spectrum there reveals the presence of a broad wing component, which we interpret as the indication of fast outflows with a velocity of $\sim 600$ km s$^{-1}$. The expected mass loading factor of the outflows, after accounting for multiphase gas, is $\gtrsim 2-3$, which is intermediate between AGN-driven and starburst-driven outflows. Hydrodynamic simulations in the literature predicted that this pair will evolve to a luminous ($M_{\rm 1450} \lesssim -26$ mag), starbursting ($\gtrsim 1000~M_\odot$ yr$^{-1}$) quasar after coalescence, one of the most extreme populations in the early universe. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_02468 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Merging gas-rich galaxies that harbor low-luminosity twin quasars at z = 6.05: a promising progenitor of the most luminous quasars Izumi, Takuma Matsuoka, Yoshiki Onoue, Masafusa Strauss, Michael A. Umehata, Hideki Silverman, John D. Nagao, Tohru Imanishi, Masatoshi Kohno, Kotaro Toba, Yoshiki Iwasawa, Kazushi Nakanishi, Kouichiro Sawamura, Mahoshi Fujimoto, Seiji Kikuta, Satoshi Kawaguchi, Toshihiro Aoki, Kentaro Goto, Tomotsugu Astrophysics of Galaxies We present ALMA [CII] 158 $μ$m line and underlying far-infrared (FIR) continuum emission observations ($0''.57 \times 0''.46$ resolution) toward a quasar-quasar pair system recently discovered at $z = 6.05$ (Matsuoka et al. 2024). The quasar nuclei (C1 and C2) are faint ($M_{\rm 1450} \gtrsim -23$ mag), but we detect very bright [CII] emission bridging the 12 kpc between the two objects and extending beyond them (total luminosity $L_{\rm [CII]} \simeq 6 \times 10^9~L_\odot$). The [CII]-based total star formation rate of the system is $\sim 550~M_\odot$ yr$^{-1}$ (IR-based dust-obscured SFR is $\sim 100~M_\odot$ yr$^{-1}$), with a [CII]-based total gas mass of $\sim 10^{11}~M_\odot$. The dynamical masses of the two galaxies are large ($\sim 9 \times 10^{10}~M_\odot$ for C1 and $\sim 5 \times 10^{10}~M_\odot$ for C2). There is a smooth velocity gradient in [CII], indicating that these quasars are a tidally interacting system. We identified a dynamically distinct, fast [CII] component around C1: detailed inspection of the line spectrum there reveals the presence of a broad wing component, which we interpret as the indication of fast outflows with a velocity of $\sim 600$ km s$^{-1}$. The expected mass loading factor of the outflows, after accounting for multiphase gas, is $\gtrsim 2-3$, which is intermediate between AGN-driven and starburst-driven outflows. Hydrodynamic simulations in the literature predicted that this pair will evolve to a luminous ($M_{\rm 1450} \lesssim -26$ mag), starbursting ($\gtrsim 1000~M_\odot$ yr$^{-1}$) quasar after coalescence, one of the most extreme populations in the early universe. |
| title | Merging gas-rich galaxies that harbor low-luminosity twin quasars at z = 6.05: a promising progenitor of the most luminous quasars |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2405.02468 |