Radial properties of dust in galaxies: Comparison between observations and isolated galaxy simulations

Understand

We study the importance of several processes that influence the evolution of dust and its grain size distribution on spatially resolved scales in nearby galaxies.

• Here, we compiled several multi-wavelength observations for the nearby galaxies NGC628(M74), NGC5457(M101), NGC598(M33), and NGC300.
• We applied spatially resolved spectral energy distribution fitting to the latest iteration of infrared data to get constraints on the galaxy dust masses and the small-to-large grain abundance ratio.
• For comparison, we took the radial profiles of the stellar mass and gas mass surface density for NGC628 combined with its metallicity gradient in the literature to calibrate a single-galaxy simulation using the GADGET4-OSAKA code.