Table 7.
Characteristics and AGN identification statistics for a selection of medium area and wide field surveys across different wavebands, which we use for comparison with our Euclid yields.
| Survey | Band | Area (deg2) | Number of AGN | AGN Surface Density (deg−2) | Reference(s) |
|---|---|---|---|---|---|
| EWS (detected) | optical–NIR | 14 500 | 4.0 × 107 | 2800 | This work |
| EWS (selected) | optical–NIR | 14 500 | 8.1 × 106 | 556 | ” |
| EWS (selected, Euclid-only) | optical–NIR | 14 500 | 4.8 × 106 | 331 | ” |
| EDS (detected) | optical–NIR | 50 | 2.4 × 105 | 4700 | ” |
| EDS (selected) | optical–NIR | 50 | 3.5 × 104 | 692 | ” |
| EDS (selected, Euclid-only) | optical–NIR | 50 | 1.7 × 104 | 346 | ” |
| XMM-SERVS | 0.5–10 keV | 13.1 | 10 300 | 786 | Chen et al. (2018); |
| Ni et al. (2021) | |||||
| XXL-3XLSS | 0.5–10 keV | 50 | 26 056 | 521 | Chiappetti et al. (2018) |
| Spitzer cryogenic (a) | NIR–MIR | 55 | ∼20 000 | 364 | Lacy & Sajina (2020) |
| eFEDS | 0.2–2.3 keV | 142 | 22 079 | 155 | Liu et al. (2022); |
| Salvato et al. (2022) | |||||
| DES | optical–NIR | 4913 | 945 860 | 193 | Yang & Shen (2023) |
| SDSS | optical | 9376 | 750 414 | 80 (b) | Lyke et al. (2020) |
| eRASS1 (c) | 0.5–2 keV | ∼15 000 | 645 000 | 43 | Salvato et al. (in prep) |
| AllWISE (R90) | MIR | 30 093 | 4.54 × 106 | 151 | Assef et al. (2018) |
| AllWISE (C75) | MIR | 30 093 | 2.09 × 107 | 695 | Assef et al. (2018) |
Notes. The quoted area relates to the area considered in the survey AGN selection procedure as described in the corresponding reference(s). Euclid survey detected and selected yields as plotted in Fig. 14 are provided. Detected samples refer to the number of AGN with a 5σ detection in at least one Euclid filter. “Selected” samples correspond to the union of all selection criteria considered in Sect. 5.2 and “selected, Euclid-only” samples refer to AGN selected with selection criteria that incorporate Euclid bands exclusively.
Collation of AGN identified in Spitzer Space Telescope cryogenic surveys: The Spitzer Wide-Area Infrared Extragalactic Survey (SWIRE; Lonsdale et al. 2003), The AGN and Galaxy Evolution Survey (AGES; Kochanek et al. 2012), The Spitzer First Look survey (Lacy et al. 2005; Fadda et al. 2006), and the Spitzer COSMOS survey (S-COSMOS; Sanders et al. 2007).
Extragalactic counterparts are identified for eRASS1 soft band (0.5–2 keV) sources in the area that overlaps with the Legacy Survey DR10 (Dey et al. 2019; Zenteno et al., in prep.). A median AGN surface density is provided, given that the depth of eRASS1 increases getting closer to the South Ecliptic Pole (Liu et al., in prep.).
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