Chayan Mondal
S.N. Bose National Centre for Basic Sciences, Institute of Astronomy and Astrophysics, Academia Sinica, Indian Institute of Technology Kharagpur, Inter-University Centre for Astronomy and Astrophysics
About
I am Chayan Mondal, currently working as an Assistant Professor at the S. N. Bose National Centre for Basic Sciences (SNBNCBS), Kolkata, India. I completed my PhD at the Indian Institute of Astrophysics, Bangalore. After completing my PhD, I served as a postdoctoral fellow at the Inter-University Center for Astronomy and Astrophysics (IUCAA) in Pune, India. I have been exploring different aspects of galaxy deep fields using multi-wavelength photometric and spectroscopic observations. Primarily, we are using the FUV and NUV imaging of the AstroSat/UVIT to produce deep UV images of some selected HST deep fields. The two primary fields that we have been working on are AstroSat UV Deep Field South (AUDFs) and north (AUDFn), which respectively cover the HST GOODS-S and GOODS-N fields. I am leading the research on the AUDFn field with an inclination to understand: (i) the evolution of dust in galaxies with cosmic time, (ii) do different galaxies at different times follow the same attenuation law?, (iii) the nature of dusty star-forming galaxies at higher redshift, (iv) lyman continuum leaking galaxies at intermediate redshifts.
From IUCAA, I moved to the Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Taipei, Taiwan, with the ASIAA Distinguished Post Doctoral Fellowship. At ASIAA, I am collaborating with the ASIAA Dusty galaxy group to explore more about the nature and evolution of interstellar dust in galaxies. Currently, I am investigating emissions from the Polycyclic Aromatic Hydrocarbon (PAH) dust molecules using the JWST MIRI observations. The primary goal is to understand how energetic UV photons from young stars can regulate the heating or destruction of PAHs in galaxies.
Apart from the deep fields, I also study selected nearby galaxies to understand various aspects of star formation and galaxy evolution. Some of the key questions that I try to explore are: (i) what regulates star formation in massive spiral and low-mass dwarf galaxies? (ii) how do the external and internal environments affect the evolution of a galaxy? (iii) can galaxies retain their structural component after going through a collision or merger?
Employment
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S.N. Bose National Centre for Basic Sciences Assistant Professor2025 - Present
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Institute of Astronomy and Astrophysics, Academia Sinica Distinguished Postdoctoral Fellow2024 - 2025
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Inter-University Centre for Astronomy and Astrophysics Post doctoral Fellow2021 - 2024
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Indian Institute of Astrophysics PhD student2015 - 2020
Education
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Indian Institute of Technology Kharagpur Master student2012 - 2014
Projects & Funding
Projects & funding information is unavailable.
Publications (33)
- Investigating the Young Stellar Populations and Hierarchies in Nearby Galaxies with the UVIT. II. Presenting the Properties of ∼25,000 UV-detected Star-forming Clumps Save
- An FUV-optical Approach for Studying Hierarchical Star Formation in Nearby Galaxies with UVIT Save
- Cloud-scale Star Formation and Gas Scaling Relations in the Milky Way Save
- Unveiling a Population of Strong Galaxy–Galaxy Lensed, Faint Dusty Star-forming Galaxies Save
- GNHeII J1236+6215: A He II λ1640 Emitting and Potentially LyC Leaking Galaxy at z = 2.9803 Unveiled through JWST and Keck Observations Save
- Discovery of a kinematically distinct component in the central region of the collisional ring galaxy AM0644-741 Save
- GNHeII J1236+6215: A He II $λ$1640 emitting and potentially LyC leaking galaxy at $z$ = 2.9803 unveiled through JWST & Keck observations Save
- The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region Save
- Simultaneous Far-ultraviolet and Near-ultraviolet Observations of T Tauri Stars with UVIT/AstroSat: Probing the Accretion Process in Young Stars Save
- The AstroSat UV Deep Field North: The IRX–β Relation for the UV-selected Galaxies at z ∼ 0.5−0.7 Save