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An ultraluminous quasar with a twelve-billion-solar-mass black hole at redshift 6.30

机译：一种超发光类星体，在红移6.30处具有120亿太阳能质量的黑洞

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摘要

6到7之间的宇宙红移值代表着星际介质从中性状态向完全电离转变的一个时间段。在这篇论文中,Xue-Bing Wu等人报告了在红移值z=6.30处一个超明亮类星体的发现,其可见光和近红外亮度要比以前所知的红移值为6的类星体大数倍。根据近红外光谱数据,作者估计与此相关黑洞的质量大约为120亿个太阳质量,这与通过假设存在一个"埃丁顿极限吸积率"(向外作用的辐射力与向内作用的引力处于平衡状态时的吸积率)所推导出的130亿个太阳质量是一致的。作为红移值为z=6处迄今已知最明亮的类星体,该天体对于研究宇宙再电离时期末大质量黑洞周围的星系形成来说将是一个有用的资源。%So far, roughly 40 quasars with redshifts greater than z = 6 have been discovered. Each quasar contains a black hole with a mass of about one billion solar masses (10~9 M_☉). The existence of such black holes when the Universe was less than one billion years old presents substantial challenges to theories of the formation and growth of black holes and the coevolution of black holes and galaxies. Here we report the discovery of an ultraluminous quasar, SDSS J010013.02+280225.8, at redshift z = 6.30. It has an optical and near-infrared luminosity a few times greater than those of previously known z＞6 quasars. On the basis of the deep absorption trough on the blue side of the Lyman-a emission line in the spectrum, we estimate the proper size of the ionized proximity zone associated with the quasar to be about 26 million light years, larger than found with other z ＞ 6.1 quasars with lower luminosities16. We estimate (on the basis of a near-infrared spectrum) that the black hole has a mass of〜1.2 × 10~(10) M_☉, which is consistent with the 1.3 × 10~(10) M_☉ derived by assuming an Eddington-limited accretion rate.
机译：6到7之间的宇宙红移值代表着星际介质从中性状态向完全电离转变的一个时间段。在这篇论文中,Xue-Bing Wu等人报告了在红移值z=6.30处一个超明亮类星体的发现,其可见光和近红外亮度要比以前所知的红移值为6的类星体大数倍。根据近红外光谱数据,作者估计与此相关黑洞的质量大约为120亿个太阳质量,这与通过假设存在一个"埃丁顿极限吸积率"(向外作用的辐射力与向内作用的引力处于平衡状态时的吸积率)所推导出的130亿个太阳质量是一致的。作为红移值为z=6处迄今已知最明亮的类星体,该天体对于研究宇宙再电离时期末大质量黑洞周围的星系形成来说将是一个有用的资源。%So far, roughly 40 quasars with redshifts greater than z = 6 have been discovered. Each quasar contains a black hole with a mass of about one billion solar masses (10~9 M_☉). The existence of such black holes when the Universe was less than one billion years old presents substantial challenges to theories of the formation and growth of black holes and the coevolution of black holes and galaxies. Here we report the discovery of an ultraluminous quasar, SDSS J010013.02+280225.8, at redshift z = 6.30. It has an optical and near-infrared luminosity a few times greater than those of previously known z＞6 quasars. On the basis of the deep absorption trough on the blue side of the Lyman-a emission line in the spectrum, we estimate the proper size of the ionized proximity zone associated with the quasar to be about 26 million light years, larger than found with other z ＞ 6.1 quasars with lower luminosities16. We estimate (on the basis of a near-infrared spectrum) that the black hole has a mass of〜1.2 × 10~(10) M_☉, which is consistent with the 1.3 × 10~(10) M_☉ derived by assuming an Eddington-limited accretion rate.

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  • 来源
    《Nature》 |2015年第7540期|512-515a3|共5页
  • 作者

    Xue-Bing Wu; Feige Wang; Xiaohui Fan; Weimin Yi; Wenwen Zuo; Fuyan Bian; Linhua Jiang; Ian D. McGreer; Ran Wang; Jinyi Yang; Qian Yang; David Thompson; Yuri Beletsky;

  • 作者单位

    Department of Astronomy, School of Physics, Peking University, Beijing 100871, China, Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China;

    Department of Astronomy, School of Physics, Peking University, Beijing 100871, China, Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China;

    Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China, Steward Observatory, University of Arizona, Tucson, Arizona 85721-0065, USA;

    Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, China, University of Chinese Academy of Sciences, Beijing 100049, China, Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011, China;

    Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China;

    Mount Stromlo Observatory, Research School of Astronomy and Astrophysics, Australian National University, Weston Creek, Australian Capital Territory 2611, Australia;

    Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China;

    Steward Observatory, University of Arizona, Tucson, Arizona 85721-0065, USA;

    Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China;

    Department of Astronomy, School of Physics, Peking University, Beijing 100871, China, Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China;

    Department of Astronomy, School of Physics, Peking University, Beijing 100871, China, Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China;

    Large Binocular Telescope Observatory, University of Arizona, Tucson, Arizona 85721, USA;

    Las Campanas Observatory, Carnegie Institution of Washington, Colina el Pino, Casilla 601, La Serena, Chile;

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