Table 1.
Cepheids in the sample grouped according to field.
| ID | RA | Dec | Nn | Ncal | Std.dev. | σ(ZP) |
|---|---|---|---|---|---|---|
| 0320 | 00:39:33.82 | −73:44:54.3 | 25 | 12 | 0.015 | 0.006 |
| 1977 | 00:52:56.82 | −71:55:03.3 | 26 | 14 | 0.011 | 0.004 |
| 2533 | 00:56:20.90 | −73:23:13.9 | 21 | 10 | 0.018 | 0.008 |
| 2905 | 00:58:55.06 | −72:33:07.5 | 31 | 14 | 0.015 | 0.005 |
| 3311 | 01:01:49.49 | −72:05:45.4 | 25 | 14 | 0.010 | 0.004 |
| 4017 | 01:08:11.60 | −72:31:18.3 | 24 | 13 | 0.012 | 0.005 |
| 3927 | 01:07:17.54 | −73:13:26.1 | 24 | 12 | 0.020 | 0.008 |
| 4444 | 01:14:28.07 | −72:39:53.6 | 17 | 9 | 0.011 | 0.005 |
| 0958 | 00:47:10.43 | −72:57:37.9 | 24 | 14 | 0.014 | 0.005 |
| 0518 | 00:43:12.35 | −73:19:31.8 | 22 | 13 | 0.013 | 0.005 |
| 0524 | 00:43:18.77 | −73:20:19.8 | 22 | 13 | 0.013 | 0.005 |
| 1686 | 00:51:26.08 | −72:53:18.4 | 28 | 17 | 0.014 | 0.004 |
| 1693 | 00:51:27.36 | −72:51:35.1 | 28 | 17 | 0.014 | 0.004 |
| 1385 | 00:49:44.60 | −73:08:23.1 | 27 | 17 | 0.020 | 0.006 |
| 1410 | 00:49:55.28 | −73:09:16.2 | 27 | 17 | 0.020 | 0.006 |
| 1365 | 00:49:40.95 | −73:14:07.0 | 24 | 14 | 0.021 | 0.008 |
| 1403 | 00:49:52.88 | −73:14:41.0 | 24 | 14 | 0.021 | 0.008 |
| 1680 | 00:51:24.40 | −73:00:17.9 | 28 | 15 | 0.020 | 0.007 |
| 1723 | 00:51:39.32 | −73:01:30.6 | 28 | 15 | 0.020 | 0.007 |
| 1729 | 00:51:40.67 | −73:21:44.3 | 26 | 17 | 0.015 | 0.005 |
| 1750 | 00:51:49.15 | −73:21:55.5 | 26 | 17 | 0.015 | 0.005 |
| 1765 | 00:51:54.98 | −73:22:04.0 | 26 | 17 | 0.015 | 0.005 |
| 1712 | 00:51:36.22 | −73:06:15.1 | 33 | 19 | 0.010 | 0.003 |
| 1717 | 00:51:38.26 | −73:04:43.4 | 33 | 19 | 0.010 | 0.003 |
| 1761 | 00:51:53.58 | −73:06:01.6 | 33 | 19 | 0.010 | 0.003 |
| 1797 | 00:52:00.35 | −73:05:22.3 | 33 | 19 | 0.010 | 0.003 |
| mag | mag | |||||
Notes. The first group is all the fields containing a single Cepheid. The following groups show the remaining stars and fields. The table gives the OGLE-SMC-CEP identifier, the coordinates (J2000.0), the number of nights (Nn) the Cepheid has been observed, and the number of those nights (Ncal) that also had standard star observations. Finally the standard deviation of the photometric zero points from those nights and the resulting estimated zero point uncertainty are given.
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