The VMC survey – XXXIV. Morphology of stellar populations in the Magellanic Clouds

Author:

El Youssoufi Dalal1ORCID,Cioni Maria-Rosa L1ORCID,Bell Cameron P M1ORCID,Rubele Stefano2,Bekki Kenji3ORCID,de Grijs Richard456ORCID,Girardi Léo2ORCID,Ivanov Valentin D78ORCID,Matijevic Gal1,Niederhofer Florian1ORCID,Oliveira Joana M9ORCID,Ripepi Vincenzo10ORCID,Subramanian Smitha11,van Loon Jacco Th9ORCID

Affiliation:

1. Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany

2. Osservatorio Astronomico di Padova, INAF Vicolo dell’Osservatorio 5, I-35122 Padova, Italy

3. ICRAR, M468, University of Western Australia, 35 Stirling Hwy, 6009 Crawley, Western Australia, Australia

4. Department of Physics and Astronomy, Macquarie University, Balaclava Road, Sydney, NSW 2109, Australia

5. Centre for Astronomy, Astrophysics and Astrophotonics, Macquarie University, Balaclava Road, Sydney, NSW 2109, Australia

6. International Space Science Institute–Beijing, 1 Nanertiao, Zhongguancun, Hai Dian District, Beijing 100190, China

7. European Southern Observatory, Karl-Schwarzschild-Str 2, D-85748 Garching bei München, Germany

8. European Southern Observatory, Ave. Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile

9. Lennard-Jones Laboratories, School of Chemical and Physical Sciences, Keele University, Staffordshire ST5 5BG, UK

10. INAF – Osservatorio Astronomico di Capodimonte, via Moiariello 16, I-80131 Naples, Italy

11. Indian Institute of Astrophysics, Koramangala II Block, Bangalore 560034, India

Abstract

ABSTRACT The Magellanic Clouds are nearby dwarf irregular galaxies whose morphologies show different properties when traced by different stellar populations, making them an important laboratory for studying galaxy morphologies. We study the morphology of the Magellanic Clouds using data from the Visible and Infrared Survey Telescope for Astronomy survey of the Magellanic Clouds system. We used about 10 and 2.5 million sources across an area of ∼105 and ∼42 deg2 towards the Large and Small Magellanic Cloud (LMC and SMC), respectively. We estimated median ages of stellar populations occupying different regions of the near-infrared (J − Ks, Ks) colour–magnitude diagram. Morphological maps were produced and detailed features in the central regions were characterized for the first time with bins corresponding to a spatial resolution of 0.13 kpc (LMC) and 0.16 kpc (SMC). In the LMC, we find that main-sequence stars show coherent structures that grow with age and trace the multiple spiral arms of the galaxy, star-forming regions become dimmer as we progress in age, while supergiant stars are centrally concentrated. Intermediate-age stars, despite tracing a regular and symmetrical morphology, show central clumps and hints of spiral arms. In the SMC, young main-sequence stars depict a broken bar. Intermediate-age populations show signatures of elongation towards the Magellanic Bridge that can be attributed to the LMC–SMC interaction ∼200 Myr ago. They also show irregular central features suggesting that the inner SMC has also been influenced by tidal interactions.

Funder

Science and Technology Facilities Council

European Research Council

Horizon 2020

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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1. The ALPINE-ALMA [C ii] survey: characterization of spatial offsets in main-sequence galaxies at z ∼ 4–6;Monthly Notices of the Royal Astronomical Society;2024-05-31

2. Spatiotemporal map of star clusters in the Magellanic Clouds using Gaia: synchronized peaks and radial shrinkage of cluster formation;Monthly Notices of the Royal Astronomical Society;2024-01-10

3. Kinematics of stellar substructures in the small magellanic cloud;Monthly Notices of the Royal Astronomical Society;2023-05-04

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