Table 1
Sample of IFRS observed with Herschel.
IFRS | RA | σRA | Dec | σDec | S1.4 GHz | S3.6 μm | S24 μm | S1.4 GHz/S3.6 μm | References |
ID | J2000.0 | [arcsec] | J2000.0 | [arcsec] | [mJy] | [μJy] | [μJy] | ||
|
|||||||||
S703 | 03:35:31.025 | 0.11 | –27:27:02.20 | 0.12 | 26.1 | <2.04 | <115 | >12 784 | (1), (4) |
S427 | 00:34:11.592 | 0.01 | –43:58:17.04 | 0.00 | 21.4 | 1.77 ± 0.54 | <150 | 12 000 | (2), (4) |
S509 | 00:31:38.633 | 0.01 | –43:52:20.80 | 0.01 | 22.2 | < 3 | <150 | >7400 | (2), (3) |
S749 | 00:29:05.229 | 0.04 | –43:34:03.94 | 0.04 | 7.0 | < 3 | <150 | >2337 | (2), (3) |
S798 | 00:39:07.934 | 0.04 | –43:32:05.83 | 0.03 | 7.8 | < 3 | <150 | >2597 | (2), (3) |
S973 | 00:38:43.489 | 0.04 | –43:19:26.94 | 0.04 | 9.1 | < 2.70 | <150 | >3385 | (2), (4) |
Notes. Infrared-faint radio source S703 is located in CDFS while the other five sources are located in the ELAIS-S1 field. All six IFRS are undetected at 3.6 μm in the SWIRE survey (3σ ~ 3 μJy) as presented by Zinn et al. (2011). Maini et al. (2015) analysed the deeper SERVS data for three IFRS observed with Herschel and find one week counterpart. All upper limits represent 3σ. S973 consists of two radio components. Here, we used the position of the strongest component as the position of the source, in contrast to Middelberg et al. who used the centre between both components. Positions, position uncertainties, radio and 24 μm flux densities were taken from the first reference listed in each row, S3.6 μm and S1.4 GHz/S3.6 μm from the second reference.
Reference. (1) Norris et al. (2006); (2) Middelberg et al. (2008a); (3) Zinn et al. (2011); (4) Maini et al. (2015).
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