| Name: | Sipra Hota |
| Affiliation: | Indian Institute of Astrophysics |
| Conference ID: | ASI2025_29 |
| Title: | Morphology and kinematics of young population in the Small Magellanic Cloud: Insights from UVIT/AstroSat |
| Authors: | Sipra Hota 1,2, Annapurni Subramaniam 1, Prasanta K. Nayak 3, Smitha Subramanian 1 |
| Authors Affiliation: | 1 Sipra Hota, Annapurni Subramaniam, Smitha Subramanian Affiliation (Indian Institute of Astrophysics, 2nd Block, Koramangala, Bangalore-560034, India)
2 Sipra Hota Affiliation (Pondicherry University, R.V.Nagar, Kalapet, Puducherry-605014, India)
3 Prasant K. Nayak Affiliation (Institute of Astrophysics, Pontificia Universidad Cat´olica de Chile, Av. Vicu˜na MacKenna 4860, Santiago 7820436, Chile4) |
| Mode of Presentation: | Poster |
| Abstract Category: | Galaxies and Cosmology |
| Abstract: | The Small Magellanic Cloud (SMC) is one of the nearest gas-rich dwarf satellite galaxies, on its first passage around the Milky Way (MW). Its evolution is significantly influenced by interactions with the Large Magellanic Cloud (LMC) and the MW, particularly due to its much smaller dynamical mass compared to these larger galaxies. The SMC is characterized by active star formation in a metal-poor environment, and studying the SMC in the ultraviolet (UV) band is crucial for understanding its recent evolution amid these interactions. In this work, we present a catalog of ∼ 76,800 far-ultraviolet (FUV) sources observed towards the SMC using the Ultra Violet Imaging Telescope (UVIT) onboard AstroSat. From these observations, we compiled a catalog of ∼ 62,900 probable SMC members, which are primarily main-sequence, giant, and subgiant stars. We identified four young stellar populations (Young 1 (Y1), Young 2 (Y2), Young 3 (Y3), and Blue Loop (BL) stars) from the Gaia optical color-
magnitude diagram to investigate the morphology and kinematics of the young population of SMC. These populations reveal a clumpy morphology characterized by a broken bar, a shell-like structure, and the inner SMC Wing. A two-dimensional kinematic analysis using proper motion (PM) data reveals that the Y2 and Y3 populations consist of two kinematically distinct sub-populations with low and high PM dispersion. In contrast, the Y1 and BL stars display two distinct groups with low PM
dispersion. Notably, a kinematic disturbance is observed in the Right Ascension direction for stars younger than approximately 150 Myr in the eastern region, while no significant disturbance is detected along the declination. These findings provide valuable insights into models of LMC-SMC interaction. |
