Diffuse Lyα haloes around Lyα emitters at z=3: do dark matter distributions determine the Lyα spatial extents?

DOI DOI PDF 被引用文献26件 参考文献44件 オープンアクセス
  • Y. Matsuda
  • T. Yamada
    Astronomical Institute, Graduate School of Science; Tohoku University; Aramaki, Aoba-ku; Sendai; 980-8578; Japan
  • T. Hayashino
    Research Center for Neutrino Science, Graduate School of Science; Tohoku University; Sendai; 980-8578; Japan
  • R. Yamauchi
    Research Center for Neutrino Science, Graduate School of Science; Tohoku University; Sendai; 980-8578; Japan
  • Y. Nakamura
  • N. Morimoto
    Astronomical Institute, Graduate School of Science; Tohoku University; Aramaki, Aoba-ku; Sendai; 980-8578; Japan
  • M. Ouchi
    Institute for Cosmic Ray Research; University of Tokyo; Kashiwa; 277-8582; Japan
  • Y. Ono
    Department of Astronomy, Graduate School of Science; University of Tokyo; Tokyo; 113-0033; Japan
  • M. Umemura
    Center for Computational Sciences; University of Tsukuba; Tsukuba; 305-8577; Japan
  • M. Mori
    Center for Computational Sciences; University of Tsukuba; Tsukuba; 305-8577; Japan

書誌事項

タイトル別名
  • Lyα haloes at z = 3
公開日
2012-08-13
資源種別
journal article
DOI
  • 10.1111/j.1365-2966.2012.21143.x
  • 10.48550/arxiv.1204.4934
公開者
Oxford University Press (OUP)

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説明

Using stacks of Ly-a images of 2128 Ly-a emitters (LAEs) and 24 protocluster UV-selected galaxies (LBGs) at z=3.1, we examine the surface brightness profiles of Ly-a haloes around high-z galaxies as a function of environment and UV luminosity. We find that the slopes of the Ly-a radial profiles become flatter as the Mpc-scale LAE surface densities increase, but they are almost independent of the central UV luminosities. The characteristic exponential scale lengths of the Ly-a haloes appear to be proportional to the square of the LAE surface densities (r(Lya) \propto Sigma(LAE)^2). Including the diffuse, extended Ly-a haloes, the rest-frame Ly-a equivalent width of the LAEs in the densest regions approaches EW_0(Lya) ~ 200 A, the maximum value expected for young (< 10^7 yr) galaxies. This suggests that Ly-a photons formed via shock compression by gas outflows or cooling radiation by gravitational gas inflows may partly contribute to illuminate the Ly-a haloes; however, most of their Ly-a luminosity can be explained by photo-ionisation by ionising photons or scattering of Ly-a photons produced in HII regions in and around the central galaxies. Regardless of the source of Ly-a photons, if the Ly-a haloes trace the overall gaseous structure following the dark matter distributions, it is not surprising that the Ly-a spatial extents depend more strongly on the surrounding Mpc-scale environment than on the activities of the central galaxies.

7 pages, 4 figures, accepted for publication in MNRAS

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