6.8, 1.2         
  J181753    18:17:53.2   +06:31:49.5      34.98     10.41  18.5     0.34     59.6 0.08        7.4, 1.3      6.1, 1.1         
  J181816    18:18:16.0   +07:30:43.0      35.92     10.77  18.5     0.24     53.0 0.50        7.1, 1.3      5.9, 1.1         
  J182250    18:22:50.6   +07:54:36.8      36.79      9.93  19.1     0.31     64.5 0.13       10.8, 1.9      8.9, 1.5         
  J182347    18:23:47.7   +07:53:45.5      36.88      9.71  19.9     0.24     61.2 0.26       15.7, 2.6     13.0, 2.2         
  J195235    19:52:35.3   +18:43:54.8      56.56     -4.34  18.0     0.38     63.2 0.05       4.9, -0.4     4.1, -0.3         
  J200210    20:02:10.0   +18:43:07.3      57.72     -6.29  18.2     0.39     74.5 0.07       5.1, -0.6     4.2, -0.5         
  J220915    22:09:15.4   +55:34:38.5     101.37     -0.35  15.8     0.03     51.6 0.07        0.6, 0.0      0.5, 0.0         
  J230507    23:05:07.9   +34:17:23.4      99.14    -23.62  20.8     0.25     75.3 0.21      32.1,-12.8   26.5, -10.6                  Y
  J233907    23:39:07.3   +57:08:02.3     113.21     -4.36  18.4     0.18     67.6 0.15       4.1, -0.3     3.4, -0.3         
  J234635    23:46:35.6   +56:23:23.7     114.00     -5.35  15.8     0.38     68.6 0.18       1.8, -0.2     1.5, -0.1         
  --------- ------------ ------------- --------- --------- ------ ------- -------- ------- ------------ ------------- ------- ----------

For sources which fell within our search range we manually inspected each light curve to verify that the light curve was consistent with that of a stellar pulsator (cf Rodríguez et al 2007 for a recent example of a light curve for an SX Phe star) and to exclude light curves of low quality. We 