September 1997 WIYN followup priority list version 1.0. ====================================================================== FINAL REFERENCES NEEDED --> Only do this if the seeing is 1.1" or better! These images will be subtracted from every other image of the SNe, so they need to be good. The night does NOT need to be photometric for these images to be useful. Jog multiple exposures by a few tens of arcseconds relative to each other to avoid the chance of getting zapped in every image by a bad spot on the array coincident with the supernova host galaxy. Note that most of the high priority objects won't be available until within a couple hours of morning twilight. Generally, we try to do objects of airmass<2, but if the seeing is good at higher airmass, go for it. Use Harris R, Harris I filters. Prio: 1 is highest, 4 is lowest. FIELD RA(2000) Dec(2000) FILTER Texp Prio ----- -------- --------- ------ ---- ---- 9570 00:29:04.22 +07:51:20 R 3x1000 2 I 3x1000 2 95116 01:04:50.89 +04:33:53 I 2x1000 3 9568 02:24:55.50 +00:53:08 I 3x1000 3 95126 02:26:25.77 +00:48:44 R 3x1000 4 I 3x1000 4 95103 04:40:33.55 -05:30:04 R 3x1000 4 972 04:58:30.21 -03:16:04 R 4x1000 1 I 5x1000 1 974 04:55:14.25 -05:51:45 R 4x1000 1 I 5x1000 1 970/971 04:59:36.92 -03:09:19 R 3x1000 1 I 4x1000 1 ====================================================================== CALIBRATION INFORMATION --> Only do these if the night is photometric. They will be useful under any non-extreme seeing condition (i.e. any seeing <= 2" is probably OK). See the standard star fields below for a sample of appropriate Landolt fields. Note that for some fields, both calibration information and longer final reference information is needed. Do not do both the "final reference" exposure and the "calibration" exposure of a field on the same night. E.g., if a final reference of 974 is acquired on a photometric night along with standard stars, then there is no need to do a 300s exposure of that field; the 1000s exposures of the field will serve its purpose. Note that for most fields, the filter is listed as I, (R). This means that we really only _need_ I, but that if there is time, an R exposure would be useful as well for further confirmation of the calibration. Prio: 1 is highest, 4 is lowest. If prio is not 1, then _any_ priority of a final reference image is more important than this calibration image. FIELD RA(2000) Dec(2000) FILTER Texp Prio ----- -------- --------- ------ ---- ---- 9570 00:29:04.22 +07:51:20 I, (R) 2x300 3 9569 01:01:35.26 +04:26:15 I, (R) 2x300 3 95116 01:04:50.89 +04:33:53 I, (R) 2x300 3 9568 02:24:55.50 +00:53:08 I, (R) 2x300 3 95126 02:26:25.77 +00:48:44 I, (R) 2x300 3 95104 03:01:07.48 +00:21:19 I, (R) 2x300 3 95103 04:40:33.55 -05:30:04 I, (R) 2x300 3 972 04:58:30 -03:16:04 R 2x300 2 I 2x300 1 974 04:55:14 -05:51:45 R 2x300 2 I 2x300 1 970/971 04:59:37 -03:09:19 R 2x300 2 I 2x300 1 Standard fields: exposure times which do not saturate the Landolt stars (magnitude >11 typically) are appropriate, e.g. 5-10s. There are probably more fields listed than you will want to do, although, of course, with any calibration data, more is better! STANDARD FIELD RA(2000) Dec(2000) ----- -------- --------- SA113_167 21:42:41 +00:16:08 PG2213-006 22:16:24 -00:21:27 PG2331+055 23:33:49 +05:46:49 SA114_656 22:41:35 +01:11:13 SA92_249 00:54:41.5 +00:41:05 SA92_498 00:55:57 +01:10:40 F11 01:04:22 +04:13:37 F16 01:54:08 -06:42:54 PG0231+051 02:33:41 +05:18:40 SA94_394 02:56:22.5 +00:37:38 SA95_105 03:53:21 -00:00:20 SA96_21 04:51:29.5 -00:12:31.5 SA98_634 06:51:56 -00:20:57