Table 3
Characteristics and results of our sample of 34 IFRS in ELAIS-S1 and CDFS.
| IFRS | IAU designation | RA | Dec | S1.4 GHz/S3.6 μm | α | Classification |
| ID | J2000 | J2000 | ||||
|
|
||||||
| CS94 | ATCDFS J032740.72–285413.4 | 03:27:40.727 | –28:54:13.48 | 801 | −0.87 ± 0.13 | pl, poss. peak |
| CS97 | ATCDFS J032741.70–274236.6 | 03:27:41.700 | –27:42:36.61 | 614 | −0.86 ± 0.09 | pl |
| CS114 | ATCDFS J032759.89–275554.7 | 03:27:59.894 | –27:55:54.73 | > 2400 | −1.23 ± 0.13 | peak |
| CS164 | ATCDFS J032900.20–273745.7 | 03:29:00.200 | –27:37:45.70 | 640 | −0.61 ± 0.30 | peak, st |
| CS194 | ATCDFS J032928.59–283618.8 | 03:29:28.594 | –28:36:18.81 | > 2033 | −1.01 ± 0.04 | pl |
| CS215 | ATCDFS J032950.01–273152.6 | 03:29:50.010 | –27:31:52.60 | > 733 | −0.94 ± 0.16 | pl, poss. peak |
| CS241 | ATCDFS J033010.21–282653.0 | 03:30:10.210 | –28:26:53.00 | > 908 | −0.79 ± 0.17 | pl, poss. peak |
| CS265 | ATCDFS J033034.66–282706.5 | 03:30:34.661 | –28:27:06.51 | 634 | −0.84 ± 0.01 | pl |
| CS292 | ATCDFS J033056.94–285637.2 | 03:30:56.949 | –28:56:37.29 | 1842 | −0.99 ± 0.02 | pl |
| CS415 | ATCDFS J033213.07–274351.0 | 03:32:13.070 | –27:43:51.00 | > 1186 | −0.87 ± 0.05 | pl, poss. peak |
| CS520 | ATCDFS J033316.75–280016.0 | 03:33:16.754 | –28:00:16.02 | 500 | −0.85 ± 0.03 | pl |
| CS538 | ATCDFS J033330.20–283511.1 | 03:33:30.200 | –28:35:11.10 | > 648 | −1.39 ± 0.39 | peak |
| CS539 | ATCDFS J033330.54–285428.2 | 03:33:30.542 | –28:54:28.22 | 640 | −0.88 ± 0.03 | pl |
| CS574 | ATCDFS J033353.27–280507.3 | 03:33:53.279 | –28:05:07.31 | 1091 | −0.68 ± 0.04 | pl, poss. peak |
| CS603 | ATCDFS J033413.75–283547.4 | 03:34:13.759 | –28:35:47.47 | 709 | −0.62 ± 0.02 | upturn |
| CS618 | ATCDFS J033429.75–271744.9 | 03:34:29.754 | –27:17:44.95 | 1660 | −0.93 ± 0.02 | pl |
| CS649 | ATCDFS J033452.84–275813.0 | 03:34:52.846 | –27:58:13.05 | 1838 | −0.81 ± 0.27 | peak |
| CS703 | ATCDFS J033531.02–272702.2 | 03:35:31.025 | –27:27:02.20 | > 8700 | −0.93 ± 0.01 | pl |
| CS713 | ATCDFS J033537.52–275057.8 | 03:35:37.525 | –27:50:57.88 | 643 | −0.56 ± 0.04 | pl |
| ES5 | ATELAIS J003709.36–444348.1 | 00:37:09.365 | –44:43:48.11 | 1082 | −1.23 ± 0.02 | pl |
| ES66 | ATELAIS J003942.45–442713.7 | 00:39:42.452 | –44:27:13.77 | 1865 | −0.73 ± 0.02 | pl |
| ES201 | ATELAIS J003130.06–441510.6 | 00:31:30.068 | –44:15:10.69 | > 1683 | −1.14 ± 0.04 | pl |
| ES419 | ATELAIS J003322.76–435915.3 | 00:33:22.766 | –43:59:15.37 | 557 | −0.52 ± 0.34 | pl, poss. peak |
| ES427 | ATELAIS J003411.59–435817.0 | 00:34:11.592 | –43:58:17.04 | > 7120 | −0.96 ± 0.01 | st |
| ES509 | ATELAIS J003138.63–435220.8 | 00:31:38.633 | –43:52:20.80 | > 7400 | −0.97 ± 0.04 | peak, st |
| ES645 | ATELAIS J003934.76–434222.5 | 00:39:34.763 | –43:42:22.58 | 780 | −1.08 ± 0.21 | pl, poss. peak |
| ES749 | ATELAIS J002905.22–433403.9 | 00:29:05.229 | –43:34:03.94 | > 2337 | −0.92 ± 0.03 | st |
| ES798 | ATELAIS J003907.93–433205.8 | 00:39:07.934 | –43:32:05.83 | > 2597 | −0.96 ± 0.04 | st |
| ES973 | ATELAIS J003844.13–431920.4 | 00:38:44.139 | –43:19:20.43 | > 3046 | −1.08 ± 0.09 | st, poss. peak |
| ES1018 | ATELAIS J002946.52–431554.5 | 00:29:46.525 | –43:15:54.52 | 1012 | −0.71 ± 0.02 | pl |
| ES1021 | ATELAIS J003255.53–431627.1 | 00:32:55.534 | –43:16:27.15 | 575 | −0.85 ± 0.11 | pl, poss. peak |
| ES1156 | ATELAIS J003645.85–430547.3 | 00:36:45.856 | –43:05:47.39 | 2888 | −0.83 ± 0.21 | peak |
| ES1239 | ATELAIS J003547.96–425655.4 | 00:35:47.969 | –42:56:55.40 | 1220 | −0.78 ± 0.02 | pl |
| ES1259 | ATELAIS J003827.17–425133.7 | 00:38:27.170 | –42:51:33.70 | > 2063 | −1.36 ± 0.04 | pl |
Notes. The IAU designations and positions are taken from Norris et al. (2006) and Middelberg et al. (2008a), radio-to-IR flux density ratios from Zinn et al. (2011) and Maini et al. (2013). Spectral indices α and classification of the radio SEDs are results of our work as described in Sect. 3. If a source was found to show a turnover, it is classified by “peak” and the quoted spectral index was obtained from fitting the SSA model to the data. Sources with data that are well described by a single power law are labelled as “pl”. The additional classification “poss. peak” indicates sources for which a turnover cannot be ruled out down to 200 MHz, mainly because of their faintness. Sources steepening towards higher frequencies are labelled as “st”. Sources with increasing flux densities at the highest frequencies are indicated by “upturn”. Spectral indices were measured over different frequency ranges as discussed in Sect. 3.
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