Table 2
AGN-type selection comparison.
| CDFS | COSMOS | ||||||||||||
|
|
|||||||||||||
| Sample | Criterion | A 1 a | A 2 a | ℱ2 b | A H a | A L a | ℱH b | A 1 a | A 2 a | ℱ2 b | A H a | A L a | ℱH b |
|
|
|||||||||||||
| Ks+IRAC | [none] | 44 | 129 | 0.75 ( ) |
69 | 149 | 0.32 () |
543 | 515 | 0.49 ( ) |
961 | 457 | 0.68 ( )
|
| L07 | 35 | 78 | 0.69 ( , ) |
62 | 83 | 0.43 ( , ) |
470 | 376 | 0.44 (,) |
866 | 245 | 0.78 (,)
|
|
| S05 | 24 | 44 | 0.65 ( , ) |
39 | 41 | 0.49 ( , ) |
413 | 304 | 0.42 (, ) |
749 | 168 | 0.82 (, )
|
|
| D11 | 14 | 26 | 0.65 ( , ) |
24 | 23 | 0.51 ( , ) |
277 | 194 | 0.41 (, ) |
514 | 56 | 0.90 (, )
|
|
| KI | 28 | 55 | 0.66 (,) |
52 | 48 | 0.52 (, ) |
392 | 289 | 0.42 (,) |
759 | 118 | 0.87 (,)
|
|
|
|
|||||||||||||
| Ks+IRAC+ | [none] | 35 | 106 | 0.75 () |
61 | 110 | 0.36 () |
381 | 322 | 0.46 () |
600 | 238 | 0.72 ()
|
| MIPS24 μm | L07 | 31 | 61 | 0.66 (, ) |
54 | 62 | 0.47 (,) |
353 | 259 | 0.42 (,) |
567 | 156 | 0.78 ( ,)
|
| S05 | 22 | 37 | 0.63 ( , ) |
36 | 33 | 0.52 (, ) |
318 | 222 | 0.41 (, ) |
520 | 105 | 0.83 (,)
|
|
| D11 | 12 | 24 | 0.67 (, ) |
22 | 19 | 0.54 ( , ) |
234 | 161 | 0.41 ( ,) |
406 | 45 | 0.90 (,)
|
|
| KI | 24 | 43 | 0.64 (, ) |
45 | 35 | 0.56 ( ,) |
294 | 206 | 0.41 (,) |
509 | 75 | 0.87 (,)
|
|
| KIM | 19 | 37 | 0.66 (, ) |
36 | 32 | 0.53 (, ) |
237 | 170 | 0.42 (,) |
422 | 59 | 0.88 (,)
|
|
Notes. While in the upper group of rows reliable photometry is required – a magnitude error below 0.36 – in Ks+IRAC bands, in the lower group of rows we also require reliable 24 μm photometry. A1 stands for AGN type-1, whereas A2 for type-2 (X-ray or spectroscopic classifications). AL refers to the sources having intrinsic luminosities of log (LXR [erg s-1] ) < 43.5, while AH refers to those having log (LXR [erg s-1] ) ≥ 43.5.
AGN type fraction: ℱ2 = A2/(A1 + A2) and ℱH = AH/(AH + AL). Higher ℱ2 or ℱH values than those found for the whole sample (first row in each row group) imply a bias toward A2 or AH AGN, respectively. Numbers in parenthesis refer, respectively, to the statistical error and the photometric upper and lower error bars.
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