September 1997 WIYN followup priority list version 1.0.

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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

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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