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Wind from the black-hole accretion disk driving a molecular outflow in an active galaxy

机译：来自黑洞积积盘的风驱动活跃星系中的分子流出

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摘要

本期封面所示为从其核心区域有强大的大规模物质外流的一个星系，是艺术家的一个想rn象图。Francesco Tombesi等人报告，他们在 IRAS F11119+3257(一个附近的(z = 0.189)、在光学上被归为1-型的、其中有强大分子外流的超亮红外星系)的X-射线光谱中检测到了具有温和相对论速度的强大吸积盘风(accretion-disk wind)。这些风的能量状况与认为"活动星系核"风能提供将能量转移到星际介质的一个高效方式的观点相一致，并且支持认为这种风影响超大质量黑洞和它们主星系演化的理论。封面图片：ESA/ATG medialab。%Powerful winds driven by active galactic nuclei are often thought to affect the evolution of both supermassive black holes and their host galaxies, quenching star formation and explaining the close relationship between black holes and galaxies. Recent observations of large-scale molecular outflows in ultraluminous infrared galaxies support this quasar-feedback idea, because they directly trace the gas from which stars form. Theoretical models suggest that these outflows originate as energy-conserving flows driven by fast accretion-disk winds. Proposed connections between large-scale molecular outflows and accretion-disk activity in ultraluminous galaxies were incomplete because no accretion-disk wind had been detected. Conversely, studies of powerful accretion-disk winds have until now focused only on X-ray observations of local Seyfert galaxies and a few higher-redshift quasars. Here we report observations of a power-fill accretion-disk wind with a mildly relativistic velocity (a quarter that of light) in the X-ray spectrum of IRAS F11119+3257, a nearby (redshift 0.189) optically classified type 1 ultraluminous infrared galaxy hosting a powerful molecular outflow. The active galactic nucleus is responsible for about 80 per cent of the emission,with a quasar-like luminosity of 1.5 × 10~(46) ergs per second. The energetics of these two types of wide-angle outflows is consistent with the energy-conserving mechanism that is the basis of the quasar feedback in active galactic nuclei that lack powerful radio jets (such jets are an alternative way to drive molecular outflows).
机译：本期封面所示为从其核心区域有强大的大规模物质外流的一个星系，是艺术家的一个想rn象图。Francesco Tombesi等人报告，他们在 IRAS F11119+3257(一个附近的(z = 0.189)、在光学上被归为1-型的、其中有强大分子外流的超亮红外星系)的X-射线光谱中检测到了具有温和相对论速度的强大吸积盘风(accretion-disk wind)。这些风的能量状况与认为"活动星系核"风能提供将能量转移到星际介质的一个高效方式的观点相一致，并且支持认为这种风影响超大质量黑洞和它们主星系演化的理论。封面图片：ESA/ATG medialab。%Powerful winds driven by active galactic nuclei are often thought to affect the evolution of both supermassive black holes and their host galaxies, quenching star formation and explaining the close relationship between black holes and galaxies. Recent observations of large-scale molecular outflows in ultraluminous infrared galaxies support this quasar-feedback idea, because they directly trace the gas from which stars form. Theoretical models suggest that these outflows originate as energy-conserving flows driven by fast accretion-disk winds. Proposed connections between large-scale molecular outflows and accretion-disk activity in ultraluminous galaxies were incomplete because no accretion-disk wind had been detected. Conversely, studies of powerful accretion-disk winds have until now focused only on X-ray observations of local Seyfert galaxies and a few higher-redshift quasars. Here we report observations of a power-fill accretion-disk wind with a mildly relativistic velocity (a quarter that of light) in the X-ray spectrum of IRAS F11119+3257, a nearby (redshift 0.189) optically classified type 1 ultraluminous infrared galaxy hosting a powerful molecular outflow. The active galactic nucleus is responsible for about 80 per cent of the emission,with a quasar-like luminosity of 1.5 × 10~(46) ergs per second. The energetics of these two types of wide-angle outflows is consistent with the energy-conserving mechanism that is the basis of the quasar feedback in active galactic nuclei that lack powerful radio jets (such jets are an alternative way to drive molecular outflows).

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  • 来源
    《Nature》 |2015年第7544期|436-438q2|共4页
  • 作者

    F. Tombesi; M. Melendez; S. Veilleux; J. N. Reeves; E. Gonzalez-Alfonso; C. S. Reynolds;

  • 作者单位

    X-ray Astrophysics Laboratory, NASA/Goddard Space FlightCenter,Greenbelt,Maryland 20771;

    USA,Department of Astronomy and CRESST, University of Maryland,College Park, Maryland 20742, USA;

    Department of Astronomy and CRESST, University of Maryland,College Park, Maryland 20742, USA;

    Department of Astronomy and CRESST, University of Maryland,College Park, Maryland 20742, USA,Joint Space Science Institute, University of Maryland, College Park, Maryland 20742, USA;

    Astro physics Group, School of Physical and Geographical Sciences, Keele University, Keele, Staffordshire ST5 5BG, UK,Center for Space Science and Technology, University of Maryland Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA;

    Universidad de Alcala, Departamento de Fisica y Matematicas, Campus Universitario, E-28871 Alcala de Henares, Madrid, Spain;

    Department of Astronomy and CRESST, University of Maryland,College Park, Maryland 20742, USA,Joint Space Science Institute, University of Maryland, College Park, Maryland 20742, USA;

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