To appear in MNRAS 2001. astro-ph/0104427

Abstract. We have observed 28 local galaxies in the wavelength range between 1 and 2.4 µm in order to define template spectra of the normal galaxies along the Hubble sequence. Five galaxies per morphological type were observed in most cases, and the resulting RMS spread of the normalized spectra of each class, including both intrinsic differences and observational uncertainties, is about 1% in K, 2% in H and 3% in J. Many absorption features can be accurately measured. The target galaxies and the spectroscopic aperture (7" × 53") were chosen to be similar to those used by Kinney et al. (1996) to define template UV and optical spectra. The two data sets are matched in order to build representative spectra between 0.1 and 2.4 µm. The continuum shape of the optical spectra and the relative normalization of the near-IR ones were set to fit the average effective colours of the galaxies of the various Hubble classes. The resulting spectra are used to compute the k-corrections of the normal galaxies in the near-IR bands and to check the predictions of various spectral synthesis models: while the shape of the continuum is generally well predicted, large discrepancies are found in the absorption lines. Among the other possible applications, here we also show how these spectra can be used to place constraints on the dominant stellar population in local galaxies. Spectra and k-corrections are publicly available and can be downloaded from the web site http://www.arcetri.astro.it/~filippo/spectra.

Key words: elliptical and lenticular, cD - galaxies: photometry - galaxies: spiral - galaxies: evolution - galaxies: stellar content - infrared: galaxies.

Table of Contents

INTRODUCTION

OBSERVATIONS AND DATA REDUCTION

CALIBRATION OF THE SPECTRA

MATCHING OPTICAL AND NEAR-IR SPECTRA

THE K-CORRECTIONS

COMPARING OBSERVATIONS AND MODELS

THE ABSORPTION LINES

THE DOMINANTS STELLAR POPULATION

SUMMARY

REFERENCES

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