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We investigate how different galaxy properties - luminosities in u, g, r, J,K-bands, stellar mass, star formation rate and specific star formation ratetrace the environment in the local universe. We also study the effect of surveyflux limits on galaxy clustering measurements. We measure the two-pointcorrelation function (2pCF) and marked correlation functions (MCFs) using theaforementioned properties as marks. We use nearly stellar-mass-complete galaxysample in the redshift range 0.1 < z < 0.16 from the Galaxy And Mass Assembly(GAMA) survey with a flux limit of r < 19.8. Further, we impose a brighter fluxlimit of r < 17.8 to our sample and repeat the measurements to study how thisaffects galaxy clustering analysis. We compare our results to measurements fromthe Sloan Digital Sky Survey (SDSS) with flux limits of r < 17.8 and r < 16.8.We show that the stellar mass is the best tracer of galaxy environment, theK-band luminosity being a good substitute, although such a proxy sample missesclose pairs of evolved, red galaxies. We also confirm that the u-bandluminosity is a good, but not a perfect proxy of star formation rate in thecontext of galaxy clustering. We observe an effect of the survey flux limit onclustering studies - samples with a higher flux limit (smaller magnitude) misssome information about close pairs of starburst galaxies.

Galaxy and Mass Assembly (GAMA): Tracing galaxy environment using the marked correlation function