Table 1
Data used for SFR estimation.
| Wavelength | Instrument | Survey | Ω (deg2) | 3σ (μJy) | Ngals | References |
|---|---|---|---|---|---|---|
| COSMOS UV | GALEX (NUV) | DIS | 1.7 | 0.23 | 296 | (1) |
| COSMOS MIR | Spitzer-MIPS (24 μm) | S-COSMOS | 1.7 | 43 | 373 | (2,3) |
| COSMOS FIR | Herschel-PACS (100 μm) | PEP | 1.7 | 5000 | 87 | (4,5) |
| COSMOS Radio | VLA (S-band, 3 GHz) | VLA-COSMOS 3 GHz | 1.7 | 7 | 58 | (6,7) |
| SDSS UV | GALEX (FUV) | MIS | ~1000 | 1.8 | 1003 | (8) |
| SDSS MIR | WISE (W3, 12 μm) | AllWISE | ~8400 | 340 | 8333 | (9,10) |
| SDSS FIR | IRAS (60 μm) | FSC | ~8400 | 1.2 × 105 | 291 | (11) |
| SDSS Radio | VLA (L-band, 1.4 GHz) | FIRST, NVSS | ~8400 | 450 | 198 | (12,13,14) |
Notes. The area Ω quoted is the overlap between the particular wavelength and the SDSS or ACS surveys from which the morphological parameters are drawn. Ngals is the number of galaxies in our sample detected at each wavelength with robust mass, inclination, and SFR measurements (signal-to-noise ratio (S/N) >3). References. (1) Capak et al. (2007); (2) Sanders et al. (2007); (3) Le Floc’h et al. (2009); (4) Poglitsch et al. (2010); (5) Lutz et al. (2011); (6) Smolčić et al. (2017b); (7) Smolčić et al. (2017a); (8) Bianchi et al. (2011); (9) Wright et al. (2010); (10) Chang et al. (2015); (11) Moshir & et al. (1990); (12) Kimball & Ivezić (2014); (13) Becker et al. (1995); (14) Condon et al. (1998).
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