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We investigate the evolution of star formation rates (SFRs), stellar masses,and M/L$_{3.4 \mu m}$ ratios of brightest cluster galaxies (BCGs) in the COSMOSsurvey since z ~ 1 to determine the contribution of star formation to thegrowth-rate of BCG stellar mass over time. Through the spectral energydistribution (SED) fitting of the GALEX, CFHT, Subaru, Vista, Spitzer, andHerschel photometric data available in the COSMOS2015 catalog, we estimate thestellar mass and SFR of each BCG. We use a modified version of the iSEDfitpackage to fit the SEDs of our sample with both stellar and dust emissionmodels, as well as constrain the impact of star formation history assumptionson our results. We find that in our sample of COSMOS BCGs, star formationevolves similarly to that in BCGs in samples of more massive galaxy clusters.However, compared to the latter, the magnitude of star formation in our sampleis lower by ~ 1 dex. Additionally, we find an evolution of BCG baryonicmass-to-light ratio (M/L$_{3.4 \mu m}$) with redshift which is consistent witha passively aging stellar population. We use this to build upon Wen et al.'s(2013) low-redshift $\nu$L$_{3.4 \mu m}$-M$_{Stellar}$ relation, quantifying acorrelation between $\nu$L$_{3.4 \mu m}$ and M$_{Stellar}$ to z ~ 1. Bycomparing our results to BCGs in Sunyaev-Zel'dovich and X-ray-selected samplesof galaxy clusters, we find evidence that the normalization of star formationevolution in a cluster sample is driven by the mass range of the sample and maybe biased upwards by cool cores.

Stellar Mass and 3.4 $\mu$m M/L Ratio Evolution of Brightest Cluster Galaxies in COSMOS since z ~ 1.0