Speaker
Description
Understanding the star formation processes in galaxies is fundamental to unravelling the mysteries of galaxy evolution. This research focuses on evaluating the accuracy and correlation of three generally used star formation rate (SFR) indicators, which are the ultraviolet (UV) emission, far-infrared emission, and 1.4 GHz non-thermal radio continuum. From the Herschel Astrophysical Terahertz Large Area Survey, specifically the first data release, a sample of 852 spiral galaxies was analysed, covering a wide range of 70 to 350-micron flux ratios. To analyse the complete Spectral Energy Distribution for each of the 852 sources from UV to 1.4 GHz radio continuum, the Code Investigating GALaxy Emission fitting code was employed to derive physical properties and assess the fraction of UV light absorbed by dust, the total far-infrared emission, the star formation rate and the mass of young and old stars. Correlations between different SFR indicators were examined to identify variations and potential biases introduced by different modelling approaches. Preliminary results suggest that the accuracy of far-infrared-based SFR estimates improves when accounting for the different dust emission components, leading to a better characterisation of the star formation contribution to the far-infrared emission. Results also show a tight correlation between far-infrared and radio emissions, confirming the effectiveness of radio synchrotron emission as a dust-unbiased diagnostic for measuring star formation rates. However, the correlation analysis of SFR indicators reveals systematic differences, highlighting the need for refined calibrations. These findings contribute to improving SFR measurements and provide insights into the role of dust in star-forming galaxies.
| Stream | Science or Engineering |
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