Disc scalelength refers to a parameter that describes the distribution of stars within a disk galaxy, influencing its mass distribution based on a specific mass-to-light (M/L) ratio. While the term is commonly used in astrophysical research, it lacks a precise, universally accepted definition, leading to some ambiguity among researchers. The concept can vary in interpretation, particularly when discussing specific measurements like "2.5 scale lengths." Despite extensive searches, definitive explanations remain elusive, highlighting a gap in clarity for a term frequently encountered in academic literature. Overall, the discussion emphasizes the need for a clearer understanding of disc scalelength in the context of galaxy formation studies.