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From evolved stars to the formation and evolution of galaxies

Published online by Cambridge University Press:  09 June 2023

Hamidreza Mahani ,
Atefeh Javadi Open the ORCID record for Atefeh Javadi [Opens in a new window] ,
Jacco Th. van Loon ,
Habib Khosroshahi ,
Elham Saremi ,
Roya Hamedani Golshan ,
Mahdieh Navabi ,
Seyed Azim Hashemi ,
Mahtab Gholami  and
Sima Taefi Aghdam
Hamidreza Mahani
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran, 19568-36613, Iran email: mahani@ipm.ir
Atefeh Javadi
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran, 19568-36613, Iran email: mahani@ipm.ir
Jacco Th. van Loon
Affiliation:
Lennard-Jones Laboratories, Keele University, ST5 5BG, UK
Habib Khosroshahi
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran, 19568-36613, Iran email: mahani@ipm.ir
Elham Saremi
Affiliation:
Instituto de Astrof’ısica de Canarias, C/ V’ıa L’actea s/n, 38205 La Laguna, Tenerife, Spain Departamento de Astrof‘?sica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain
Roya Hamedani Golshan
Affiliation:
Physikalisches Institut der Universität zu Köln, Zülpicher Str. 77, D-50937 Köln, Germany
Mahdieh Navabi
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran, 19568-36613, Iran email: mahani@ipm.ir
Seyed Azim Hashemi
Affiliation:
Department of Physics and Astronomy, University of California Riverside, CA 92521, The USA
Mahtab Gholami
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran, 19568-36613, Iran email: mahani@ipm.ir
Sima Taefi Aghdam
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran, 19568-36613, Iran email: mahani@ipm.ir
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Abstract

Due to observational constraints, our detailed knowledge of stellar populations, formation, and evolution of galaxies is limited to a few dozen galaxies located in the Local Group. The Local Group of galaxies offers a unique opportunity to construct the formation histories and probe the structure and dynamics of many dwarf galaxies surrounding the Milky Way and Andromeda and of isolated dwarf galaxies. In this regard, we monitored the majority of galaxies in the Local Group, including the M33 galaxy and satellites galaxies surrounding the Milky Way and Andromeda galaxy, as well as isolated dwarf galaxies. We identified stellar populations and based on light curve analysis, the cool evolved stars pulsating in the fundamental mode were identified. In this paper, first, we will present the results we obtained for SFH and dust production rate in individual galaxies separately to answer how different types of galaxies have been formed and evolved over cosmic time. Then, we will discuss whether the mass return from dusty evolved stars can provide enough gas reservoirs to sustain the star formation or even rejuvenate the dwarf galaxy, as some seem to harbor relatively young stars.

Keywords

stars: AGB and post-AGBstars: carbonstars: mass-losssupergiantsgalaxies: evolution
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S373: Resolving the Rise and Fall of Star Formation in Galaxies , August 2021 , pp. 264 - 267
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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