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Spatial variation of the star formation history in the disc of M31 galaxy using evolved stars

Published online by Cambridge University Press:  09 June 2023

Maryam Torki
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran, 19568-36613, Iran email: [email protected]
Mahdieh Navabi
Affiliation:
Physics Department, University of Surrey, Guildford, GU2 7XH, United Kingdon
Atefeh Javadi
Affiliation:
School of Astronomy, Institute for Research in Fundamental Sciences (IPM), Tehran, 19568-36613, Iran email: [email protected]
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Abstract

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The rate of star formation (SFR) is one of the important quantities that helps to study galaxies’ evolutionary path. In fact, measuring the SFR during the life of the Universe shows us how galaxies have acquired their metallicity and star mass. In this regard, the galaxies of the Local Group give us a great opportunity to study the connection between different stellar populations and galaxy evolution. In this paper, we use the Long-Period variable stars to estimate the radial star formation in the disc of the M31 galaxy. These stars are powerful instruments to achieve this goal. They reach their peak luminosity and coldest state at the final point of their evolution. Also, there is a directly related between their mass and luminosity, so using stellar evolution theoretical models, we construct the mass function and hence the star formation history (SFH). In the disc of M31, we see an increase in the rate of star formation and a decrease in the age of stars in the outer parts. These results predict the inside-out growth well.

Type
Poster Paper
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

References

Gogarten et al. 2010, APJ, 712, 854 10.1088/0004-637X/712/2/858CrossRefGoogle Scholar
Hamedani Golshan, R. et al. 2017, MNRAS, 466, 1764 10.1093/mnras/stw3174CrossRefGoogle Scholar
Hashemi, S.A. et al. 2019, MNRAS, 483, 4751 10.1093/mnras/sty3450CrossRefGoogle Scholar
Javadi, A. et al. 2011a, ASPC, 445, 497 Google Scholar
Javadi, A. et al. 2011b, MNRAS, 414, 3394 10.1111/j.1365-2966.2011.18638.xCrossRefGoogle Scholar
Javadi, A. et al. 2017, MNRAS, 464, 2103 10.1093/mnras/stw2463CrossRefGoogle Scholar
Marigo, P. et al., 2017, ApJ, 835, 19 10.3847/1538-4357/835/1/77CrossRefGoogle Scholar
Mould, J., et al. 2004, ApJ, 154, 623 10.1086/422875CrossRefGoogle Scholar
Navabi, M. et al. 2020, Proc.conf. Stars and their Variability Observed from Space, 383, 385Google Scholar
Navabi, M. et al. 2021, ApJ, 910, 127 10.3847/1538-4357/abdec1CrossRefGoogle Scholar
Rezaeikh, S. et al. 2014, MNRAS, 445, 2214 Google Scholar
Saremi, E. et al. 2019, Proceedings of IAU Symposium, 339, 336 Google Scholar
Saremi, E. et al. 2020, ApJ, 894, 135 10.3847/1538-4357/ab88a2CrossRefGoogle Scholar
Saremi, E. et al. 2021, ApJ, 923, 164 10.3847/1538-4357/ac2d96CrossRefGoogle Scholar
Sick et al. 2014, Proceedings of IAU Symposium, 311, 82 10.1017/S1743921315003440CrossRefGoogle Scholar
Torki, M. et al. 2019, Proceedings of IAU Symposium, 343, 512 10.1017/S1743921318007275CrossRefGoogle Scholar
Torki, M. et al. 2023, IAU Symposium, 362, 353 Google Scholar
Williams, B. F. et al. 2009, APJ, 695, L15 10.1088/0004-637X/695/1/L15CrossRefGoogle Scholar