SIMBAD references

We have measured K_S-band (2.0-2.3 µm) surface brightness fluctuations (SBFs) of 19 early-type galaxies in the Fornax Cluster. Fornax is ideally suited both for calibrating SBFs as distance indicators and for using SBFs to probe the unresolved stellar content of early-type galaxies. Combining our results with published data for other nearby clusters, we calibrate K_S-band SBFs using Hubble Space Telescope (HST) Cepheid cluster distances and I-band SBF distances to individual galaxies. With the latter, the resulting calibration is

M_KS=(-5.84±0.04)+(3.6±0.8)[(V-I_c)₀-1.15],

valid for 1.05<(V-I_c)₀<1.25 and not including any systematic errors in the HST Cepheid distance scale. The fit accounts for the covariance between V-I_c and M_KS when calibrated in this fashion. The intrinsic cosmic scatter of M_KS appears to be larger than that of I-band SBFs. S0 galaxies may follow a different relation, although the data are inconclusive. The discovery of correlation between K_S_-band fluctuation magnitudes and colors with V-I_c is a new clue into the star formation histories of early-type galaxies. This relation naturally accounts for galaxies previously claimed to have anomalously bright K-band SBFs, namely, M32 and NGC 4489. Models indicate that the stellar populations dominating the SBF signal have a significant range in age; some scatter in metallicity may also be present. The youngest ages imply some galaxies have very luminous giant branches, akin to those in intermediate-age (few Gyr) Magellanic Cloud clusters. The inferred metallicities are roughly solar, although this depends on the choice of theoretical models. A few Fornax galaxies have unusually bright K_S-band SBFs, perhaps originating from a high-metallicity burst of star formation in the last few Gyr. The increased spread and brightening of the K_S-band SBFs with bluer V-I_c suggest that the lower mass cluster galaxies (≲0.1L*) may have had more extended and more heterogeneous star formation histories than those of the more massive galaxies.