Notes. Column definitions: Col. (1) central wavelength of the passband; Col. (2) full width half maximum (FWHM) of the point spread function (PSF) in the passband. In the shortest bands, the FWHM is limited by the under-sampling of the PSF; Col. (3) depth of the image at that wavelength, i.e., flux density of the faintest sources of the catalog. The depths listed in the table correspond to the 3σ limit. Due to local noise variations in the maps, some sources with slightly fainter flux densities may lie above this signal-to-noise threshold; Col. (4) total number of point sources above the 3-σ limit. For the Herschel PACS and SPIRE passbands, we list the number of sources identified using a PSF-fitting based on Spitzer-MIPS 24 μm prior positions, themselves resulting from Spitzer-IRAC 3.6 μm priors; Col. (5) number of sources identified with an optical counterpart having a spectroscopic redshift; Col. (6) fraction of sources with an optical counterpart having a spectroscopic redshift; Col. (7) fraction of sources with an optical counterpart having either a spectroscopic or a photometric redshift; Col. (8) number of sources used in the present study, i.e., sources which are both “clean” (not polluted by bright neighbors as discussed in Sect. 2.3) and for which a redshift either photometric or spectroscopic was measured; Col. (9) fraction of the sources listed in Col. (8) for which a spectroscopic redshift was determined. Columns (10) to (16) for GOODS–south are defined as Cols. (3) to (9) for GOODS–north. ^(a) The characteristics of the GOODS–Herschel PACS 100, 160 μm and SPIRE 250, 350 and 500 μm images and catalogs are given in the bottom part of the table. The SPIRE images extend over 30′  ×  30′ but we restricted the present analysis, hence also the number of sources given in the table, to the same field as the one covered with the PACS bands and to the sources with a 24 μm counterpart. The upper part of the table lists the characteristics of the Spitzer IRAC 3.6, 4.5, 5.8, 8 μm, IRS peakup array 16 μm and MIPS 24, 70 μm images and catalogs. ^(b) The depth of the SPIRE catalogs given here applies only to the sub-sample of “clean” galaxies, located in isolated areas as probed by the density maps obtained from the shorter wavelengths starting at 24 μm (see Sect. 2.3). This explains why they are much lower than the statistical confusion limits as listed by Nguyen et al. (2010) of 29, 31 and 34 mJy (5σ_conf confusion limits).