1. INTRODUCTION

2. SAMPLE DESCRIPTION
2.1. Multi-wavelength coverage

3. SED-FITTING METHOD

4. ANALYSIS
4.1. Mid-infrared to bolometric luminosity ratio
4.2. Luminosities from observed rest-frame SED
4.3. Luminosities from SED-fitting
4.4. Disk luminosities: effect of the host-galaxy & reddening

5. MID-INFRARED TO BOLOMETRIC LUMINOSITY RATIO VERSUS L_bol

6. DISCUSSION
6.1. Dust reddened AGN population
6.2. Dependence of obscured AGN fraction with bolometric luminosity
6.3. Comparison to demographic based analysis
6.4. Dependence of obscured AGN fraction with hard X-ray luminosity
6.5. Evolution with redshift?
6.6. Torus models
6.7. Possible biases

7. SUMMARY AND CONCLUSIONS