1 / 4

Spin Distribution of Galaxies in Clusters Masanori Iye(NAOJ)

Spin Distribution of Galaxies in Clusters Masanori Iye(NAOJ). Structure formation in the Universe #CMB, SDSS, 2dF, CDM simulations=> density distribution #Yet no serious observational/theoretical works on the origin of vorticity of galaxies Revive the “origin of spiral structure” issue

candice-bowers
Télécharger la présentation

Spin Distribution of Galaxies in Clusters Masanori Iye(NAOJ)

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Spin Distribution of Galaxies in ClustersMasanori Iye(NAOJ) • Structure formation in the Universe #CMB, SDSS, 2dF, CDM simulations=> density distribution #Yet no serious observational/theoretical works on the origin of vorticity of galaxies • Revive the “origin of spiral structure” issue => FMOS gives a new insight on this problem: • Method: Offset spectroscopy to probe statistical analysis on internal kinematics + orientation, axis ratio: *1st MOS on centers, *2nd 3rd MOS with major axis offset Start with nearby clusters => distant clusters *MOIRCS slit are suited for individual studies. FMOS needed for cluster studies. M.Iye@FMOS SWS, Kyoto, 14/1/04

  2. All spirals are trailing? Conspiracy of S/Z, +/－ , Near/Far defines spin vector & trailing/leading completely. (1) S/Z , or (2) Near/Far & +/－ => gives the sign of the line of sight component (spin parity) of galaxies. S Z Far Near Near Far _ + + _ M.Iye@FMOS SWS, Kyoto, 14/1/04

  3. Spin parity conservation. Spin sum tend to be zero rather than random binomial distribution for groups ? (Yamagata et al.1989) M.Iye@FMOS SWS, Kyoto, 14/1/04

  4. Spin distribution in clusters: Pancake, Tidal torque, Primordial whirl… *Surely, orbital mixing adds complication.... M.Iye@FMOS SWS, Kyoto, 14/1/04

More Related