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Near-infrared measurements of kinematics in infrared bright galaxies.

机译：红外明亮星系中运动学的近红外测量。

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摘要

I have developed techniques to utilize the deep sharp 2.3 {dollar}mu{dollar}m CO stellar absorption bandhead to measure stellar kinematics in galaxies. The motivation for this stems from the high optical obscuration often found in starforming galaxies, which can be partially circumvented by moving the observations into the low extinction regime of the near-infrared. The choice of the CO bandhead comes from its shape, as it sharp bandedge is very sensitive to motions of the stars, and its depth, as it is as deep as all other non-CO absorption features in the 2-2.3 {dollar}mu{dollar}m wavelength range. Thus, spectra with moderate signal-to-noise can be used to determine stellar kinematics in the near-infrared. I present two techniques for measuring kinematics with this molecular bandhead.; Using these techniques, I have studied two such galaxies, M82 and NGC 6240. In M82, a small nearby starburst galaxy, I have spatially resolved both the ionized and shock gas kinematics as well as the stellar kinematics, revealing a complex system containing old stars, young stars, and gas which may become new stars. Unlike previous studies of this system, I have shown in the central {dollar}r < 30spprimespprime{dollar} the older underlying bulge contributes {dollar}approx{dollar}1/5 of the total K luminosity, and must be accounted for when modeling the star formation. In NGC 6240, I have measured the stellar kinematics. In this more distant and more luminous system, the situation is even more extreme, with the K-light being dominated solely by the old bulge population. By studying these two galaxies that bracket the range of luminosities found in starbursting sources, I have shown that, at least in these sources, one must have an understanding of the kinematics of these galaxies in order to accurately determine how important the old stellar population is to their near-infrared luminosity. This ratio of old to young stars is curtail to modeling the star formation in these systems.
机译：我已经开发出了利用深达2.3 {μm}μm的CO恒星吸收带头来测量星系中恒星运动学的技术。造成这种现象的原因是星状星系中经常出现的高度光学遮蔽性，可以通过将观测值移至近红外的低消光状态来部分规避。 CO带状头的选择取决于其形状，因为其锋利的带状边缘对恒星的运动非常敏感，深度也与2-2.3 {dollar} mu中所有其他非CO吸收特征一样深{m} m波长范围。因此，具有中等信噪比的光谱可用于确定近红外的恒星运动学。我介绍了两种利用该分子带头测量运动学的技术。使用这些技术，我研究了两个这样的星系，即M82和NGC6240。在附近的一个小型星爆星系M82中，我在空间上解析了电离气体和冲击气体运动学以及恒星运动学，揭示了一个包含旧恒星的复杂系统，年轻的恒星和可能成为新恒星的气体。与以前对该系统的研究不同，我在中央{dol} r <30spprimespprime {dollar}中显示，较老的基础凸起贡献了总K光度的{dollar}约{dollar} 1/5，在建模时必须考虑恒星形成。在NGC 6240中，我测量了恒星运动学。在这个更遥远，更发光的系统中，情况更加极端，K灯仅由老的凸起人群控制。通过研究包围星爆源中发现的光度范围的这两个星系，我已经表明，至少在这些源中，人们必须了解这些星系的运动学，才能准确地确定旧星体的重要性。他们的近红外光度。老恒星与年轻恒星的比率减少了对这些系统中恒星形成进行建模的时间。

著录项

  • 作者

    Gaffney, Niall Ives.;

  • 作者单位

    The University of Texas at Austin.;

  • 授予单位 The University of Texas at Austin.;
  • 学科 Physics Astronomy and Astrophysics.
  • 学位 Ph.D.
  • 年度 1996
  • 页码 192 p.
  • 总页数 192
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类 天文学;
  • 关键词

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