Hostname: page-component-cd9895bd7-8ctnn Total loading time: 0 Render date: 2024-12-25T05:13:52.004Z Has data issue: false hasContentIssue false
  • English
  • Français

Milky Way’s structure based on thousands of Cepheids and RR Lyrae stars from OGLE

Published online by Cambridge University Press:  14 May 2020

Pawel Pietrukowicz Open the ORCID record for Pawel Pietrukowicz [Opens in a new window]
Pawel Pietrukowicz*
Affiliation:
Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warszawa, Poland email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Classical Cepheids and RR Lyrae-type variable stars are widely-used tracers of young (< 300 Myr) and old (> 10 Gyr) stellar populations, respectively. These stars also serve as distance indicators allowing for Galactic structure studies. Robust detection of pulsating variables requires precise and relatively frequent observations over several years. Recently, the OGLE survey has discovered nearly 1,300 new genuine classical Cepheids and 15,000 RR Lyrae stars along the southern Galactic plane. Here, we present the picture of the Milky Way’s thin disk drawn with the Cepheids and the view of the Galactic old population that emerges from the set of known RR Lyrae stars.

Keywords

Galaxy: structurestars: variables: Cepheidsstars: variables: RR Lyrae
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. 1 - 5
Copyright
© International Astronomical Union 2020

References

Abuter, R., Amorim, A., Anugu, N., et al. 2018, A&A, 615, L15Google Scholar
Cao, L., Mao, S., Nataf, D., Rattenbury, N. J., & Gould, A. 2013, MNRAS, 434, 59510.1093/mnras/stt1045CrossRefGoogle Scholar
Iwanek, P., Soszyński, I., Skowron, J., et al. 2019, ApJ, 879, 11410.3847/1538-4357/ab23f6CrossRefGoogle Scholar
Mróz, I., Udalski, A., Skowron, D. M., et al. 2018, ApJL, 870, L1010.3847/2041-8213/aaf73fCrossRefGoogle Scholar
Pietrukowicz, P., Dziembowski, W. A., Mróz, P., et al. 2013, AcA, 63, 379Google Scholar
Pietrukowicz, P., Kozowski, S., Skowron, J., et al. 2015, ApJ, 811, 11310.1088/0004-637X/811/2/113CrossRefGoogle Scholar
Skowron, D. M., Skowron, J., Mróz, P., et al. 2019, Science, 365, 47810.1126/science.aau3181CrossRefGoogle Scholar
Soszyński, I., Udalski, A., Szymański, M. K., et al. 2014, AcA, 64, 177Google Scholar
Soszyński, I., Udalski, A., Szymański, M. K., et al. 2015, AcA, 65, 297Google Scholar
Udalski, A., Szymański, M., & Szymański, G. 2015, AcA, 65, 1Google Scholar
Udalski, A., Soszyński, I., Pietrukowicz, P., et al. 2018, AcA, 68, 315Google Scholar
Vallée, J. P. 2017, The Astronomical Review, 13, 11310.1080/21672857.2017.1379459CrossRefGoogle Scholar