Abstract
We analyzed the star formation surface density (ΣSFR) between the global and H ii regions in a sample of 69 low surface brightness galaxies (LSBGs) and 68 star-forming (SF) galaxies using data from the Hα images. The conventional global ΣSFR, which is defined as the star formation rate (SFR) divided by the area of the global galaxy, may not accurately describe the star formation activity in LSBGs due to the lower number of H ii regions compared to SF galaxies. To address this, we divide the global galaxy into two regions, the H ii region and the diffuse region, and then study the ΣSFR in each region. Our results show that both the SFR and area of the H ii regions in LSBGs are lower than those in SF galaxies, resulting in the H ii region’s ΣSFR (SFR/area) being slightly lower in LSBGs than in SF galaxies by 0.28 dex, although the global ΣSFR is at least an order of magnitude lower in LSBGs than in SF galaxies. Furthermore, a significant difference exists between the global and H ii regions in ΣSFR. In LSBGs, ΣSFR increased by 0.80 dex from the global region to the H ii region, while SF galaxies demonstrate a 0.54 dex increase, highlighting the crucial aspect of carefully selecting an appropriate aperture for ΣSFR calculations.
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