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Table 1

Depths of the GOODS-Herschel catalogsa in the GOODS-north and south fields.

GOODS-north GOODS-south
λ FWHM Depth All sources Clean  +  z Depth All sources Clean  +  z
(μm) (″) Nb % zspec % zall Nb % zsp Nb % zspec % zall Nb % zsp
(1) (2) (3) (4) (5) (6) (7) (8) (9) (10) (11) (12) (13) (14) (15) (16)

3.6 1.6a 17 μJy 24 476 3489 14 55 20 μJy 13 791 2933 21 99
4.5 1.6a 24 μJy 19 957 3445 17 63 35 μJy 10 203 2808 28 99
5.8 1.7a 129 μJy 8182 2648 32 76 137 μJy 4005 1943 49 100
8 2.0 150 μJy 6020 2324 39 84 134 μJy 3519 1760 50 100
16 4.0 32 μJy 1297 870 67 90 52 μJy 883 571 65 83
24 5.7 21 μJy 2575 1284 50 91 20 μJy 2063 1054 51 81
70 18.0 2.4 mJy 150 118 79 83 94 98 3.1 mJy 456 77 17 100 50 17
100 6.7 1.1 mJy 1095 693 63 93 959 72 0.8 mJy 531 375 71 91 485 77
160 11.0 2.7 mJy 781 517 66 94 355 77 2.4 mJy 296 216 73 90 170 84
250 18.1 5.7 mJyb 374 251 67 94 194 80
350 24.9 7.2 mJyb 173 114 66 94 91 78
500 36.6 9 mJyb 24 11 46 96 11 73
All 1263 776 61 89 990 72 555 385 69 91 498 41

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 (5σconf confusion limits).

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