Description
Intensity mapping has emerged as one of the most promising techniques to probe the large-scale structure of the Universe across both high and low redshifts, offering new insights into its fundamental properties. The standard model of cosmology is grounded in the cosmological principle, which assumes homogeneity and isotropy on large scales. Homogeneity, in particular, can be tested through the measurement of the homogeneity scale—the scale beyond which the Universe becomes statistically homogeneous. In this work, we propose the first estimator of the homogeneity scale using intensity mapping. We generate a set of lognormal simulations in the redshift range 0.15 < z < 0.45, assuming a 40 arcmin beam width, MeerKLASS thermal noise levels, and foregrounds simulated with PySM. These maps will be cleaned using the GNILC method to mitigate foreground contamination. Preliminary tests of the estimator on full-sky maps containing only the cosmological signal show good agreement with theoretical predictions, demonstrating that our method reliably recovers the expected homogeneity scale. These results lay the groundwork for future applications in more realistic scenarios that include instrumental effects and foregrounds.
