Synthetic photometry of OB star clusters with stochastically sampled IMFs*analysis of models and HST observations

We present a pilot library of synthetic NUV, U, B, V, and I photometry of star clusters with stochastically sampled IMFs and ionized gas for initial masses, Mi = 103, 104, and 105 M; t = 1, 3, 4, and 8 Myr; Z = 0.014 and Z = 0.002; and log(US) = -2 and -3. We compare the library with predictions from deteinistic models and observations of isolated low-mass (<104 M) star clusters with co-spatial compact H ii regions. The clusters are located in NGC 7793, one of the nearest galaxies observed as part of the HST LEGUS and Hα-LEGUS surveys. (1) For model magnitudes that only account for the stars*(a) the residual |deteinistic mag - median stochastic mag| can be ≥0.5 mag, even for Mi = 105 M; and (b) the largest spread in stochastic magnitudes occurs when Wolf-Rayet stars are present. (2) For Mi = 105 M*(a) the median stochastic mag with gas can be >1.0 mag more luminous than the median stochastic magnitude without gas; and (b) nebular emission lines can contribute with $gt 50{{ per cent}}$ and $gt 30{{ per cent}}$ to the total emission in the V and I bands, respectively. (3) Age-dating OB-star clusters via deteinistic tracks in the U-B versus V-I plane is highly uncertain at Z = 0.014 for Mi 103 M and Z = 0.002 for Mi 103-105 M. (4) For low-mass clusters, the V-band extinction derived with stochastic models significantly depends on the value of log(US). (5) The youngest clusters tend to have higher extinction. (6) The majority of clusters have lti-peaked age PDFs. (7) Finally, we discuss the importance of characterizing the true variance in the number of stars per mass bin in nature.