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2011/11/07

Galactic Astronomy 銀河物理学特論 I Lecture 1-5: Dependence of Galaxy Properties on Environment Seminar: Park et al. 2007, ApJ, 658, 898 Lecture:. 2011/11/07. Before SDSS:

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2011/11/07

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  1. Galactic Astronomy銀河物理学特論 ILecture 1-5: Dependence of Galaxy Properties on EnvironmentSeminar: Park et al. 2007, ApJ, 658, 898 Lecture: 2011/11/07

  2. Before SDSS: The composition of the galaxy luminosity function vary from field to clusters of galaxies. E/S0 is more common in the cluster region. (Need to note that Virgo cluster is relatively spiral-rich cluster). Binggeli et al. 1988, ARAA, 26, 509

  3. Environmental Effects ? • Nature (生まれ)? • In high-density region, galaxies are formed earlier than low-density region due to the higher background density level. In such region, elliptical galaxies are preferentially formed ? • Nurture (育ち) ? • Galaxies are formed as disk galaxies at first, afterthat, in high-density region, galaxies are transformed to elliptical galaxies ? • Interaction between galaxies ? • Merging or interaction ?High-speed interaction (Harassment) ? • Ram-pressure stripping by hot intra-cluster gas • S0 galaxies as anemic (貧血) spiral ? Effect of “local” density field to “global” density field

  4. Early SDSS: Using the large database of SDSS, morphological composition of galaxies can be examined as a function of galaxy density. Morphological classification of galaxies are done with concentration parameter (C) etc. Abrupt change of the composition found only in the very high density region = core of clusters. Goto et al. 2003, MNRAS, 346, 601

  5. Galaxy “harassment” in a simulated cluster of galaxies ? In the high density region, the relative movement of the galaxies have large velocity difference and the dynamical effect of one interaction between galaxies may be small. But the number of such encounter is large in such region and cumulative effect can make a big impact on the galaxy properties. Such effect is called galaxy “harassment”. The green clouds in the figure represent stars from a “galaxy” spread by many encounters. Moore et al. 1999, MNRAS, 304, 465

  6. Examples in Virgo cluster : Ram pressure stripping ? HI gas observation of galaxies in the Virgo cluster region revealed gas structure with long tail. The contour of the figure shows the X-ray flux representing the column density of the hot intra cluster gas. The direction of the tailes are against the core of the cluster. Chung et al. 2007, ApJ, 659, L115

  7. Virgo cluster: Interaction with cold gas of galaxy and hot gas of cluster ? Pfrommer et al. 2010, Nature, 6, 520

  8. Clustering of galaxies: Auto-correlation function Auto-correlation function of galaxies determined from the SDSS database. The correlation function is explained with two components, 1) correlation between dark matter halos and 2) correlation between galaxies inside one dark halo. One-halo term: Correlation between galaxies inside same halo Two-halo term: Correlation between dark-matter halos Zehavi et al. 2004, ApJ, 608, 16

  9. “Classical” evolution of galaxies in clusters : Butcher-Oemler effect The fraction of blue galaxies in clusters increasing with the redshift. The scatter of the fraction is large and it is difficult to define the same “population” of clusters. Van Dokkum, 2000, ApJ, 541, 95 Buther & Oemler , 1984, ApJ, 285, 426

  10. “Classical” evolution of galaxies in clusters : Butcher-Oemler effect For example, the fraction of blue galaxies depends on the shape of the clusters of galaxies. The shape is though to reflect the “relaxation” level of the structure. Smail et al. 1998, MNRAS, 293, 124

  11. “Classical” evolution of galaxies in clusters : Butcher-Oemler effect The morphological mixture of galaxies also vary with redshift. The fraction of early-type galaxies decreases with redshift. Van Dokkum, 2000, ApJ, 541, 95

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