Discovery of merging twin quasars at z = 6.05
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| Main Authors: | , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866913341251780608 |
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| author | Matsuoka, Yoshiki Izumi, Takuma Onoue, Masafusa Strauss, Michael A. Iwasawa, Kazushi Kashikawa, Nobunari Akiyama, Masayuki Aoki, Kentaro Arita, Junya Imanishi, Masatoshi Ishimoto, Rikako Kawaguchi, Toshihiro Kohno, Kotaro Lee, Chien-Hsiu Nagao, Tohru Silverman, John D. Toba, Yoshiki |
| author_facet | Matsuoka, Yoshiki Izumi, Takuma Onoue, Masafusa Strauss, Michael A. Iwasawa, Kazushi Kashikawa, Nobunari Akiyama, Masayuki Aoki, Kentaro Arita, Junya Imanishi, Masatoshi Ishimoto, Rikako Kawaguchi, Toshihiro Kohno, Kotaro Lee, Chien-Hsiu Nagao, Tohru Silverman, John D. Toba, Yoshiki |
| contents | We report the discovery of two quasars at a redshift of $z$ = 6.05, in the process of merging. They were serendipitously discovered from the deep multi-band imaging data collected by the Hyper Suprime-Cam (HSC) Subaru Strategic Program survey. The quasars, HSC $J$121503.42$-$014858.7 (C1) and HSC $J$121503.55$-$014859.3 (C2), both have luminous ($>$10$^{43}$ erg s$^{-1}$) Ly$α$ emission with a clear broad component (full width at half maximum $>$1000 km s$^{-1}$). The rest-frame ultraviolet (UV) absolute magnitudes are $M_{1450} = -23.106 \pm 0.017$ (C1) and $-22.662 \pm 0.024$ (C2). Our crude estimates of the black hole masses provide $\log (M_{\rm BH}/M_\odot) = 8.1 \pm 0.3$ in both sources. The two quasars are separated by 12 kpc in projected proper distance, bridged by a structure in the rest-UV light suggesting that they are undergoing a merger. This pair is one of the most distant merging quasars reported to date, providing crucial insight into galaxy and black hole build-up in the hierarchical structure formation scenario. A companion paper will present the gas and dust properties captured by Atacama Large Millimeter/submillimeter Array observations, which provide additional evidence for and detailed measurements of the merger and also demonstrate that the two sources are not gravitationally-lensed images of a single quasar. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2405_02465 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Discovery of merging twin quasars at z = 6.05 Matsuoka, Yoshiki Izumi, Takuma Onoue, Masafusa Strauss, Michael A. Iwasawa, Kazushi Kashikawa, Nobunari Akiyama, Masayuki Aoki, Kentaro Arita, Junya Imanishi, Masatoshi Ishimoto, Rikako Kawaguchi, Toshihiro Kohno, Kotaro Lee, Chien-Hsiu Nagao, Tohru Silverman, John D. Toba, Yoshiki Astrophysics of Galaxies We report the discovery of two quasars at a redshift of $z$ = 6.05, in the process of merging. They were serendipitously discovered from the deep multi-band imaging data collected by the Hyper Suprime-Cam (HSC) Subaru Strategic Program survey. The quasars, HSC $J$121503.42$-$014858.7 (C1) and HSC $J$121503.55$-$014859.3 (C2), both have luminous ($>$10$^{43}$ erg s$^{-1}$) Ly$α$ emission with a clear broad component (full width at half maximum $>$1000 km s$^{-1}$). The rest-frame ultraviolet (UV) absolute magnitudes are $M_{1450} = -23.106 \pm 0.017$ (C1) and $-22.662 \pm 0.024$ (C2). Our crude estimates of the black hole masses provide $\log (M_{\rm BH}/M_\odot) = 8.1 \pm 0.3$ in both sources. The two quasars are separated by 12 kpc in projected proper distance, bridged by a structure in the rest-UV light suggesting that they are undergoing a merger. This pair is one of the most distant merging quasars reported to date, providing crucial insight into galaxy and black hole build-up in the hierarchical structure formation scenario. A companion paper will present the gas and dust properties captured by Atacama Large Millimeter/submillimeter Array observations, which provide additional evidence for and detailed measurements of the merger and also demonstrate that the two sources are not gravitationally-lensed images of a single quasar. |
| title | Discovery of merging twin quasars at z = 6.05 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2405.02465 |