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A clumpy and anisotropic galaxy halo at redshift 1 from gravitational-arc tomography

机译：引力弧层析成像在红移1处的块状各向异性银河晕

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摘要

Every star-forming galaxy has a halo of metal-enriched gas that extends out to at least 100 kiloparsecs(1-3), as revealed by the absorption lines that this gas imprints on the spectra of background quasars(4). However, quasars are sparse and typically probe only one narrow beam of emission through the intervening galaxy. Close quasar pairs(5-7) and gravitationally lensed quasars(8-11) have been used to circumvent this inherently one-dimensional technique, but these objects are rare and the structure of the circumgalactic medium remains poorly constrained. As a result, our understanding of the physical processes that drive the recycling of baryons across the lifetime of a galaxy is limited(12,13). Here we report integral-field (tomographic) spectroscopy of an extended background source-a bright, giant gravitational arc. We can thus coherently map the spatial and kinematic distribution of Mg II absorption-a standard tracer of enriched gas-in an intervening galaxy system at redshift 0.98 (around 8 billion years ago). Our gravitational-arc tomography unveils a dumpy medium in which the absorption strength decreases with increasing distance from the galaxy system, in good agreement with results for quasars. Furthermore, we find strong evidence that the gas is not distributed isotropically. Interestingly, we detect little kinematic variation over a projected area of approximately 600 square kiloparsecs, with all line-of-sight velocities confined to within a few tens of kilometres per second of each other. These results suggest that the detected absorption originates from entrained recycled material, rather than in a galactic outflow.
机译：每个吸收恒星的星系都有一个富含金属的气体晕圈，该晕圈至少延伸到100千帕秒（1-3），吸收线表明该气体会印在背景类星体的光谱上（4）。但是，类星体稀疏，通常仅探测穿过中间星系的一束窄光束。近距离类星体对（5-7）和引力透镜类星体（8-11）已被用来规避这种固有的一维技术，但是这些物体很少见，并且绕银河系介质的结构仍然受限制。结果，我们对在银河系整个生命周期中驱动重子循环的物理过程的理解是有限的（12,13）。在这里，我们报告了扩展的背景源（明亮的巨大引力弧）的积分场（层析）光谱。因此，我们可以在红移0.98（大约80亿年前）插入星系系统中，将Mg II吸收（富气的标准示踪剂）的Mg II吸收的空间和运动分布连贯地绘制出来。我们的引力弧线层析成像技术揭示了一种稀疏介质，该介质的吸收强度会随着距星系系统距离的增加而降低，这与类星体的结果非常吻合。此外，我们发现有力的证据表明气体不是各向同性的。有趣的是，在大约600平方千米的投影面积上，我们发现运动学变化很小，所有视线速度都限制在每秒几十公里的范围内。这些结果表明，检测到的吸收来自夹带的再循环材料，而不是银河系外流。

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  • 来源
    《Nature》 |2018年第7693期|493-496|共4页
  • 作者

    Lopez Sebastian; Tejos Nicolas; Ledoux Cedric; Felipe Barrientos L.; Sharon Keren; Rigby Jane R.; Gladders Michael D.; Bayliss Matthew B.; Pessa Ismael;

  • 作者单位

    Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile;

    Pontificia Univ Catolica Valparaiso, Inst Fis, Valparaiso 4059, Chile;

    European Southern Observ, Alonso Cordova 3107,Casilla 19001, Santiago 19, Chile;

    Pontificia Univ Catolica Chile, Inst Astrofis, Vicuna Mackenna 4860, Santiago, Chile;

    Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA;

    NASA Goddard Space Flight Ctr, Observat Cosmol Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA;

    Univ Chicago, Dept Astron & Astrophys, 5640 South Ellis Ave, Chicago, IL 60637 USA|Univ Chicago, Kavli Inst Cosmol Phys, 5640 South Ellis Ave, Chicago, IL 60637 USA;

    MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA;

    Pontificia Univ Catolica Chile, Inst Astrofis, Vicuna Mackenna 4860, Santiago, Chile;

  • 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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