MI/IMACS Exposure Times
Date of last modification: Mar. 15 2009, 06:25 pm Chilean time.
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 40
LTT 1020 01:54:49.7 -27:28:29 11.522 40
EG 21 03:10:30.4 -68:36:05 11.379 40
LTT 1788 03:48:22.2 -39:08:35 13.155 60
LTT 2415 05:56:24.2 -27:51:26 12.214 50
Hilt 600 06:45:13.5 +02:08:15 10.441 20
LTT 3218 08:41:33.6 -32:56:55 11.858 40
LTT 3864 10:32:13.8 -35:37:42 12.171 50
LTT 4364 11:45:45.4 -64:50:22 11.504 40
Feige 56 12:06:39.7 +11:40:39 11.057 30
LTT 4816 12:38:50.7 -49:47:58 13.794 70
CD 32 14:11:46.3 -33:03:15 10.452 20
LTT 6248 15:38:59.8 -28:35:34 11.797 40
EG 274 16:23:33.7 -39:13:48 11.029 30
LTT 7379 18:36:26.2 -44:18:37 10.225 15
LTT 7987 20:10:57.1 -30:13:03 12.230 50
LTT 9239 22:52:40.9 -20:35:27 12.068 50
Feige 110 23:19:58.3 -05:09:56 11.826 40
LTT 9491 23:19:35.2 -17:05:28 14.112 90
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A list of Spectrophotometric Standard Stars may be found here
Standards for telluric features correction
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Star RA (2000) DEC V Time
(sec)
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L745-46A 07:40:20.9 -17:24:42 13.0 100 DF,Bessell99
LTT 4364 11:45:45.4 -64:50:22 11.504 50
EG131 19:20:35.0 -07:40:00 12.28 60 Bessell99
NGC 7293 22:29:38.6 -20:50:14 13.5 180 PN central star
LTT 9491 23:19:35.4 -17:05:28 14.1 200 DC,Bessell99
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One telluric standard with narrow slit (followed by a comparison lamp).
Click on the star name to get a finding chart.
Supernovae
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Name spectr. Priority RA DEC Comments
(1 is highest) (2000.0)
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SN 2008bk 23:57:47.50 -32:33:24.00 faint
SN 2009mg 06:21:44.86 -59:44:26.00 Type-IIb 1 month past max.
SN 2006jd 08:02:07.43 +00:48:31.5 ?
SN 2005ip 09 32 06.42 +08 26 44.40 not too faint
SN 2009bb 10:31:33.87 -39:57:30.00 faint
SN 2009Y 14:42:24.55 -17:14:46.3 faint
2 - 3 Spectrophotometric standards with wide slit
One telluric standard with narrow (high s/n) slit.
Those times are rough estimates; the observer should check the signal-to-noise obtained and decide about
modifying exposure times and/or take 2 instead of 3 exposures per target.
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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.
The finding charts can be
found HERE and/or HERE.
