C100/ModSpec Exposure Times
Spectrophotometric Standard Stars
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Star RA (2000) DEC V Time
(sec)
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LTT 377 00:41:46.6 -33:39:10 11.229 60
LTT 1020 01:54:49.7 -27:28:29 11.522 60
EG 21 03:10:30.4 -68:36:05 11.379 60
LTT 1788 03:48:22.2 -39:08:35 13.155 300
LTT 2415 05:56:24.2 -27:51:26 12.214 200
Hilt 600 06:45:13.5 +02:08:15 10.441 30
LTT 3218 08:41:33.6 -32:56:55 11.858 90
LTT 3864 10:32:13.8 -35:37:42 12.171 100
LTT 4364 11:45:36.6 -64:50:24 11.504 60
Feige 56 12:06:39.7 +11:40:39 11.057 60
LTT 4816 12:38:50.7 -49:47:58 13.794 450
CD 32 14:11:46.3 -33:03:15 10.452 30
LTT 6248 15:38:59.8 -28:35:34 11.797 60
EG 274 16:23:33.7 -39:13:48 11.029 60
LTT 7379 18:36:26.2 -44:18:37 10.225 30
LTT 7987 20:10:57.1 -30:13:03 12.230 200
LTT 9239 22:52:40.9 -20:35:27 12.068 200
Feige 110 23:19:58.3 -05:09:56 11.826 150
LTT 9491 23:19:35.2 -17:05:28 14.112 600
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Supernovae for spectroscopy
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suggested
Name exposure time Priority RA DEC
(sec) (1 is highest) (2000.0)
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One spectrophotometric standard with 5" slit
SN 2003-448015 2x900 3 20 33 30.98 -24 37 15.0 (needs spectr. confirmation)
SN 2003ho 3x900 2 21 06 30.56 -48 07 29.9
SN 2003hy 2x900 1 21 54 22.72 +15 09 37.8 (needs spectr. confirmation)
SN 2003hg 3x900 2 23 51 24.13 +20 06 38.3
One spectrophotometric standard with 5" slit
SN 2003-202086 2x900 2 00 41 50.23 -09 18 19.0 (needs spectr. confirmation)
SN 2003gd 2x900 4 01 36 42.65 +15 44 20.9
SN 2003hd 3x900 2 01 49 46.31 -21 54 37.8
SN 2003hl 2x600 1 01 59 21.28 +19 00 14.5
SN 2003-895 2x600 1 02 21 35.70 -05 31 51.0 (needs spectr. confirmation)
SN 2003gs 2x900 3 02 27 38.36 -01 09 35.4
SN 2003hk 2x900 1 02 46 25.76 +03 36 32.2
SN 2003hv 2x300 3 03 04 09.32 -26 05 07.5
SN 2003hn 2x300 2 03 44 36.1 -44 37 49
SN 2003bg 2x900 3 04 10 59.42 -31 24 50.3
One spectrophotometric standard with 5" slit
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Note: In general, we should orient the slit along the paralactic angle. However,
if the SN is located close to the host it might be necessary to pick a different
and more convenient angle to avoid contamination of the host. If so, it would
be convenient to observe the SN at a low airmass.