We present a multiwavelength catalog (15 mum, R-band, K-band, and 1.4 GHz flux) plus spectroscopic identifications for 406 15 mum sources detected in the European Large Area ISO Survey (ELAIS) region S1, over the flux density range 0.5 < S-15 mu m < 150 mJy. Three hundred thirty-two (similar to82%) sources are optically identified down to Rsimilar to23.0. Spectra or bona fide stellar identifications are obtained for 290 objects (similar to88% of the optically identified sources). The areal coverage, mid-infrared (MIR) and optical completeness of the sample are discussed in order to allow statistical and evolutionary analyses. Two main spectroscopic classes have been found to dominate the MIR extragalactic population: z < 0.5 star-forming galaxies [from absorbed to extreme starbursts: nu L-nu(15 mu m) approximate to 10(8)-10(11) L.], which account for similar to 75% of the sources, and active galactic nuclei (AGNs; both type 1 and 2), which account for similar to 25% of the sources. About 20% of the extragalactic sources are dust-enshrouded starburst galaxies [e(a) spectra], and all the starburst galaxies appear more dust-extincted in the optical than nearby normal galaxies. We also identified 91 stellar objects (similar to 22% of the MIR sources). The counts for starburst galaxies and AGNs down to 0.6 mJy have been derived. A general trend is found in the optical-MIR spectral energy distribution of the galaxies, where the MIR-luminous objects have larger MIR to optical luminosity ratios. Based on a variety of analyses, we suggest that the ELAIS sources fainter than R similar to 23 are luminous and ultraluminous MIR galaxies (LIG-ULIGs; nu L-nu(15 mu m) = 10(11)-10(12) L.) at intermediate redshifts (z = 0.5-1.5), and that consequently the present sample is virtually 100% spectroscopically complete up to z = 0.5.
La Franca F, Gruppioni C, Matute I, Pozzi F, Lari C, Mignoli M, et al. (2004). The nature of the mid-infrared population from optical identifications of the ELAIS-S1 sample. THE ASTRONOMICAL JOURNAL, 127(6), 3075-3088 [10.1086/420987].