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UVIT study of the MAgellanic clouds (U-SMAC). II. a far-uv catalog of the small magellanic cloud: morphology and kinematics of young stellar population

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dc.contributor.author Hota, Sipra
dc.contributor.author Subramaniam, A
dc.contributor.author Nayak, Prasanta K
dc.contributor.author Subramanian, S
dc.date.accessioned 2024-12-17T06:38:53Z
dc.date.available 2024-12-17T06:38:53Z
dc.date.issued 2024-12-02
dc.identifier.citation The Astronomical Journal, Vol. 168, No. 6, 255 en_US
dc.identifier.issn 1538-3881
dc.identifier.uri http://hdl.handle.net/2248/8619
dc.description Open Access en_US
dc.description Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI
dc.description.abstract The Small Magellanic Cloud (SMC) is an irregular dwarf galaxy that has recently undergone an interaction with the Large Magellanic Cloud. The young massive stars in the SMC formed in the disturbed low-metallicity environment are important targets in astrophysics. We present a catalog of ∼76,800 far-ultraviolet (FUV) sources toward the SMC detected using the Ultra Violet Imaging Telescope onboard AstroSat. We created an FUV catalog with ∼62,900 probable SMC members which predominantly comprise main-sequence, giant, and subgiant stars. We selected four young populations (Young 1, Young 2, Young 3, and Blue Loop (BL) stars) identified from the Gaia optical color–magnitude diagram to study the morphology and kinematics of the young SMC using this catalog. We detect a clumpy morphology with a broken bar, a shell-like structure, and the inner SMC Wing for the four stellar populations. The eastern region and the northeastern regions are mainly populated by Young 1, 2, and 3 stars. The central region predominantly has the Young 2 and 3 populations, whereas the SW has BL stars, and Young 2 and 3 stars. The 2D kinematic study using proper motion (PM) reveals that Young 2 and 3 populations show two kinematically distinct subpopulations with low and high PM dispersion, whereas the Young 1 and BL stars show two kinematically distinct populations with low dispersion. Our analysis points to a kinematic disturbance along the R.A. direction for stars younger than ∼150 Myr located in the eastern region, with no significant disturbance along the decl. en_US
dc.language.iso en en_US
dc.publisher American Astronomical Society en_US
dc.relation.uri https://doi.org/10.3847/1538-3881/ad7de2
dc.rights © 2024. The Author(s).
dc.subject Magellanic Clouds en_US
dc.subject Galaxy photometry en_US
dc.subject Ultraviolet astronomy en_US
dc.subject Galaxy evolution en_US
dc.title UVIT study of the MAgellanic clouds (U-SMAC). II. a far-uv catalog of the small magellanic cloud: morphology and kinematics of young stellar population en_US
dc.type Article en_US


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