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A dust-parallax distance of 19 megaparsecs to the supermassive black hole in NGC 4151

机译：到NGC 4151中超大质量黑洞的尘埃视差距离为19 megaparsecs

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摘要

本星系群中的Seyfert星系NGC 4151，更具体来说是其活动星系核(AGN),已成为一个有用的宇宙学工具。正如各种不同方法所推断的那样，该星系，还有与其类似的星系NGC3227，都具有使其在校正AGN中黑洞质量方面有用的特性。然而，有效校正需要距NGC 4151的准确距离，而此前这个数据一直没有。这项研究报告了根据对NGC 4151的热尘埃发射区的观测结果得出的一个新的尘埃视差距离。这个19兆秒差距的新数值表明，该星系中央黑洞的质量与以前的估计值相比增加了 1.4倍，也为其中的黑洞质量提供了一个相应的修正。%The active galaxy NGC 4151 has a crucial role as one of only two active galactic nuclei for which black hole mass measurements based on emission line reverberation mapping can be calibrated against other dynamical techniques. Unfortunately, effective calibration requires accurate knowledge of the distance to NGC 4151, which is not at present available. Recently reported distances range from 4 to 29 megaparsecs. Strong peculiar motions make a redshift-based distance very uncertain, and the geometry of the galaxy and its nucleus prohibit accurate measurements using other techniques. Here we report a dust-parallax distance to NGC 4151 of 19.0_(-2.6)~(+2.4) megaparsecs. The measurement is based on an adaptation of a geometric method that uses the emission line regions of active galaxies8. Because these regions are too small to be imaged with present technology, we use instead the ratio of the physical and angular sizes of the more extended hot-dust emission as determined from time delays10 and infrared interferometry. This distance leads to an approximately 1.4-fold increase in the dynamical black hole mass, implying a corresponding correction to emission line reverberation masses of black holes if they are calibrated against the two objects with additional dynamical masses.
机译：本星系群中的Seyfert星系NGC 4151，更具体来说是其活动星系核(AGN),已成为一个有用的宇宙学工具。正如各种不同方法所推断的那样，该星系，还有与其类似的星系NGC3227，都具有使其在校正AGN中黑洞质量方面有用的特性。然而，有效校正需要距NGC 4151的准确距离，而此前这个数据一直没有。这项研究报告了根据对NGC 4151的热尘埃发射区的观测结果得出的一个新的尘埃视差距离。这个19兆秒差距的新数值表明，该星系中央黑洞的质量与以前的估计值相比增加了 1.4倍，也为其中的黑洞质量提供了一个相应的修正。%The active galaxy NGC 4151 has a crucial role as one of only two active galactic nuclei for which black hole mass measurements based on emission line reverberation mapping can be calibrated against other dynamical techniques. Unfortunately, effective calibration requires accurate knowledge of the distance to NGC 4151, which is not at present available. Recently reported distances range from 4 to 29 megaparsecs. Strong peculiar motions make a redshift-based distance very uncertain, and the geometry of the galaxy and its nucleus prohibit accurate measurements using other techniques. Here we report a dust-parallax distance to NGC 4151 of 19.0_(-2.6)~(+2.4) megaparsecs. The measurement is based on an adaptation of a geometric method that uses the emission line regions of active galaxies8. Because these regions are too small to be imaged with present technology, we use instead the ratio of the physical and angular sizes of the more extended hot-dust emission as determined from time delays10 and infrared interferometry. This distance leads to an approximately 1.4-fold increase in the dynamical black hole mass, implying a corresponding correction to emission line reverberation masses of black holes if they are calibrated against the two objects with additional dynamical masses.

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  • 来源
    《Nature》 |2014年第7528期|528-530B1|共4页
  • 作者

    Sebastian F. Hoenig; Darach Watson; Makoto Kishimoto; Jens Hjorth;

  • 作者单位

    Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30,2100 Copenhagen O, Denmark,School of Physics & Astronomy, University of Southampton, Southampton SO17 1BJ, UK;

    Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30,2100 Copenhagen O, Denmark;

    Department of Physics, Faculty of Science, Kyoto Sangyo University, Kamigamo-motoyama, Kita-ku, Kyoto 603-8555, Japan;

    Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30,2100 Copenhagen O, Denmark;

  • 收录信息 美国《科学引文索引》(SCI);美国《工程索引》(EI);美国《生物学医学文摘》(MEDLINE);美国《化学文摘》(CA);
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