Unravelling multi-temperature dust populations in the dwarf galaxy Holmberg II
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The product under consideration is a scientific study titled "Unravelling multi-temperature dust populations in the dwarf galaxy Holmberg II." This study aims to investigate the dust populations in the dwarf galaxy Holmberg II, which is known for its complex star formation history. The authors employ a multi-wavelength approach to analyze the dust properties and temperature distribution in the galaxy. The study provides valuable insights into the physical processes that govern the evolution of galaxies and the role of dust in star formation. The findings of this study have significant implications for our understanding of the formation and evolution of galaxies.
Abstract
Introduction
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Holmberg II – a dwarf galaxy in the nearby M81 group – is a very informative source of distribution of gas and dust in the interstellar discs. High-resolution observations in the infrared (IR) allows us to distinguish isolated star-forming regions, photodissociation (PDR) and HII regions, remnants of supernovae (SNe) explosions and, as such, can provide information about more relevant physical processes. In this paper we analyse dust emission in the wavelength range 4.5 to 160 𝜇m using the data from IR space observatories at 27 different locations across the galaxy. We observe that the derived spectra can be represented by multiple dust populations with different temperatures, which are found to be independent of their locations in the galaxy. By comparing the dust temperatures with the far ultraviolet (FUV) intensities observed by the UVIT instrument onboard AstroSat, we find that for locations showing a 100 𝜇m peak, the temperature of cold (20 to 30 K) dust grains show a dependence on the FUV intensities, while such a dependence is not observed for the other locations. We believe that the approach described here can be a good tool in revealing different dust populations in other nearby galaxies with available high spatial resolution data.