Name: Amrutha S
Affiliation: IIA
Conference ID : ASI2022_591
Authors : Amrutha S, Dr. Mousumi Das, Jyoti Yadav
Abstract Type: Poster
Abstract Category : Extragalactic Astronomy
Abstract : Dwarf galaxies (M < 1010 Msun) are the most abundant systems in the Universe. They are characterized by smaller sizes and shallower gravitational potentials compared to more massive galaxies. These properties make it difficult for them to retain dense gas and hence form stars. Although a large fraction of dwarfs are low luminosity and fall in the low surface brightness (LSB) galaxy class, a significant fraction are a star forming dwarf galaxies. They can be broadly classified as dwarf spirals and irregular galaxies. These star forming dwarf galaxies (SFDGs) are characterized by low mass, low chemical abundances, high gas masses, and dark matter (DM) content. They also have different subclasses based on their morphology. Our study is aimed at characterizing and comparing the star formation in dwarf spirals and irregulars using UVIT observations. As UVIT has a high spatial resolution (~1.2”), it is possible to study the star forming complexes (SFCs) in nearby dwarf galaxies. We have extracted the SFCs, derived their areas, star formation rates, and their distributions in the galaxy disks. We compared this distribution within our sample and also with more massive galaxies which are already studied using UVIT. We compared these results for dwarf spirals and dwarf irregulars to see how star formation is different in different types of dwarfs. In this poster we present some preliminary results of our study - for the dwarf spiral NGC4136 and the irregular galaxy UGC7608.