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SUMMARY:Dwarf early-type galaxies in the Coma and Virgo clusters: dynamica
 l masses\, kinematically-decoupled cores\, stellar populations
DTSTART;VALUE=DATE-TIME:20230323T143000Z
DTEND;VALUE=DATE-TIME:20230323T143200Z
DTSTAMP;VALUE=DATE-TIME:20240704T115756Z
UID:indico-contribution-280@meetings.aip.de
DESCRIPTION:Speakers: Kirill Grishin (Astroparticule et Cosmologie)\nGalax
 y clusters are the largest gravitationally bound structures in the Univers
 e. Numerical simulations provide detailed scenarios on how they assemble a
 nd evolve over the lifetime of the Universe\, but observational evidences 
 supporting these predictions are still elusive. Galaxy populations in near
 by clusters are dominated by dwarf stellar systems\, and the number of the
 se galaxies continues to grow over time even at the present epoch.\nOver t
 he last 4 years\, using MMT Binospec we collected a rich spectroscopic dat
 aset\, which comprises over 250 dwarf early-type galaxies in three massive
  nearby clusters: Coma (D=99 Mpc)\, Abell 2147 (D=165 Mpc)\, and Abell 168
  (D=193 Mpc). We have also reduced and analyzed spectra of dwarf galaxies 
 in the Virgo cluster (D=16.5 Mpc) publicly available in the Keck\, Gemini\
 , and VLT data archives. For every galaxy we have a spatially resolved opt
 ical spectrum reaching 1-2 half-light radii from its center. By analyzing 
 these data\, we studied their internal properties\, such as stellar kinema
 tics (rotation\, velocity dispersion)\, ages and chemical composition of t
 heir stars (e.g. to estimate when the star formation was quenched)\, and p
 erform Jeans dynamical modelling\, which yields dark matter content and dy
 namical masses. Profiles of radial velocity for a dozen of dEs in the Coma
  cluster demonstrate quite large kinematically decoupled cores suggestive 
 of relatively recent mergers\, which were experienced by these galaxies. W
 e discuss several various scenarios of dE galaxy formation and evolution b
 ased on their dynamical masses\, stellar population properties\, internal 
 dynamics and position within the host clusters and put them in corresponde
 nce with different dE sub-classes. With these data we can directly test th
 e applicability of the abundance matching to galaxies in clusters in the 3
 e8-5e9 MSun range in stellar mass.\n\nhttps://meetings.aip.de/event/20/con
 tributions/280/
LOCATION:Haus H\, Telegrafenberg
URL:https://meetings.aip.de/event/20/contributions/280/
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