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Elliptical galaxies/stellar halos connection

Published online by Cambridge University Press:  14 May 2020

Magda Arnaboldi Open the ORCID record for Magda Arnaboldi [Opens in a new window] ,
Claudia Pulsoni ,
Ortwin Gerhard  and
the ePN.S team
Magda Arnaboldi
Affiliation:
European Southern Observatory, K. Schwarzschild Str. 2, DE-85748, Garching, Germany email: marnabol@eso.org
Claudia Pulsoni
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, DE-85748 Garching, Germany emails: cpulsoni@mpe.mpg.de, gerhard@mpe.mpg.de Excellence Cluster Universe, Boltzmannstrasse 2, DE-85748, Garching, Germany
Ortwin Gerhard
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse, DE-85748 Garching, Germany emails: cpulsoni@mpe.mpg.de, gerhard@mpe.mpg.de
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Abstract

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Cosmological simulations predict that early-type galaxies (ETGs) are the results of extended mass accretion histories. The latter are characterized by different numbers of mergers, mergers’ mass ratios and gas fractions, and timing. Depending on the sequence and nature of these mergers that follow the first phase of the in-situ star formation, these accretion histories may lead to ETGs that have low or high mass halos, and that rotate fast or slow. Since the stellar halos maintain the fossil records of the events that led to their formation, a discontinuity may be in place between the inner regions of ETGs and their outer halos, because the time required for the halos’ stars to exchange their energies and momenta is very long compared with the age of these systems. Exquisite deep photometry and extended spectroscopy for significant samples of ETGs are then used to quantify the occurrence and significance of such a transition in the galaxies’ structural and kinematical parameters. Once this transition radius is measured, its dependency with the effective radius of the galaxies’ light distribution and total stellar masses can be investigated. Such correlations can then be compared with the predictions of accreted, i.e. ex-situ vs. in-situ components from cosmological simulations to validate such models.

Keywords

ISM: planetary nebulae: generalgalaxies: elliptical and lenticular, cDevolutionhalosindividual: NGC 5866kinematics and dynamics
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S353: Galactic Dynamics in the Era of Large Surveys , June 2019 , pp. 233 - 238
Copyright
© International Astronomical Union 2020

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