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In this second paper of a series on the accuracy and precision of thedetermination of age and metallicity of simple stellar populations (SSPs) bymeans of the full spectrum fitting technique, we study the influence of starcluster mass through stochastic fluctuations of the number of stars near thetop of the stellar mass function, which dominate the flux in certain wavelengthregimes depending on the age. We consider SSP models based on the Padovaisochrones, spanning the age range 7.0 $\leq$ log (age/yr) $\leq$ 10.1.Simulated spectra of star clusters in the mass range $10^4 \leq M/M_{\odot} <10^6$ are compared with SSP model spectra to determine best-fit ages andmetallicities using a full-spectrum fitting routine in four wavelength regimes:the blue optical (0.35-0.70 $\mu$m), the red optical (0.6-1.0 $\mu$m), thenear-IR (1.0-2.5 $\mu$m), and the mid-IR (2.5-5.0 $\mu$m). We compare the powerof each wavelength regime in terms of both the overall precision of age andmetallicity determination, and of its dependence on cluster mass. We also studythe relevance of spectral resolution in this context by utilizing two differentspectral libraries (BaSeL and BT-Settl). We highlight the power of the mid-IRregime in terms of identifying young massive clusters in dusty star formingregions in external galaxies. The spectra of the simulated star clusters andSSPs are made available online to enable follow-up studies by the community.

monthly notices of the royal astronomical society

On the precision of full-spectrum fitting of simple stellar populations.  II. The dependence on star cluster mass in the wavelength range 0.3-5.0  $\mu$m