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SUMMARY:Disrupted vs survived dwarf galaxies in cosmological simulations
DTSTART;VALUE=DATE-TIME:20230321T090300Z
DTEND;VALUE=DATE-TIME:20230321T090500Z
DTSTAMP;VALUE=DATE-TIME:20241114T092420Z
UID:indico-contribution-250@meetings.aip.de
DESCRIPTION:Speakers: Sergey Khoperskov (AIP)\nSince the chemical abundanc
 es of stars are the fossil records of the physical conditions in galaxies\
 , they provide the key information for recovering the assembly history of 
 galaxies. In this work\, we explore the chemo-chrono-kinematics of accrete
 d and survived dwarf galaxies by analyzing six M31/MW analogues from the H
 ESTIA suite of cosmological hydrodynamics zoom-in simulations of the Local
  Group. We found that accreted stellar haloes\, including individual debri
 s\, reveal abundance gradients in the E-Lz space\, where the most metal-ri
 ch stars have formed in the inner parts of the disrupted systems before th
 e merger and mainly contribute to the central regions of the hosts. Theref
 ore\, we suggest that abundance measurements in the inner MW will allow to
  constrain better the parameters of building blocks of the MW stellar halo
 . We found that the merger debris are chemically distinct from the survive
 d dwarf galaxies\; however\, the mergers debris have abundances expected f
 or stars originating from dwarfs that had their star formation activity qu
 enched at early times. Using the data from the APOGEE spectroscopic survey
  we also explore some other similarities between satellite galaxies and ac
 creted stellar halo of the MW.\n\nhttps://iaus379.aip.de/event/20/contribu
 tions/250/
LOCATION:Haus H\, Telegrafenberg
URL:https://iaus379.aip.de/event/20/contributions/250/
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