MI/IMACS Exposure Times
Date of last modification: Mar. 28 2011 07:45 pm Chilean time.
IMACS-f/4, grating 300/4.3


                                  Supernovae


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Name           spectr.  imaging   Priority        RA          DEC        V     Comments
                                (1 is highest)       (2000.0)
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SN2010kg                             2     04 40 08.7   +07 20 54.   18.5 
SN2006is-host                        1     05:17:34.37  -23:46:54.2         redshift
SN2010jr                             1     05 19 34.47  -32 39 14.6  19.0
SN2010ko                             3     05 32 49.4   -14 05 45    18.0   Joe
SN2010kw                             1     06 56 19.88  -54 03 47.1  19.0   classification
SN2010hg                             2     09:46:13.7  -30:27:13.3   18.5
SN2010ev                             2     10:25:28.99 -39:49:51.2   ?      BVg'r'i' imaging
PSNJ11352709-3800549                 3     11:35:27.09 -38:00:54.9   16.5   classification, Joe
cand_pgc37739                        3     11:58:55.30 -53:23:56.22  17.5   classification, Joe
SN2010cn                             2     11 04 06.57  +04 49 58.7  17.6   BVg'r'i' imaging
SN2011am                             1     12:16:26.00 -43:19:20.0   15.0
SN2011A                              1     13:01:01.19 -14:31:34.8   18.7   600l/mm?  u'g'B imaging
SN2011Z                              1     13:30:43.038 -20:57:13.97 16.0    u' imaging only  
PSNJ13490323-2803596                 1     13:49:03.23 -28:03:59.65  17.0   classification  Joe
SN2010as                             2     15 49 49.23  -29 23 09.7     ?   BVg'r'i' imaging 
SN2010gp                             3     16:52:57.39 +02:23:16.4      ?   BVg'r'i' imaging
PSNJ18593846-4145558                 1     18:59:38.46 -41:45:55.8   17.6   classification
 
2 - 3 Spectrophotometric standards with wide slit
One telluric standard with narrow (high s/n) slit.


The observer should check the signal-to-noise obtained and decide about 
exposure times and/or take 2 instead of 3 exposures per target.


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          Standard Stars

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Star         RA  (2000)  DEC     V        Time
                                         (sec)
----------------------------------------------------

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     150 
LTT 2415  05:56:24.2 -27:51:26 12.214     80 
Hilt 600  06:45:13.5 +02:08:15 10.441     40
LTT 3218   08:41:33.6 -32:56:55 11.858    60
LTT 3864  10:32:13.8 -35:37:42 12.171     80
LTT 4364  11:45:50.0 -64:50:30 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     150
CD 32     14:11:46.3 -33:03:15 10.452     40
LTT 6248  15:38:59.8 -28:35:34 11.797     70
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     80 
LTT 9239  22:52:40.9 -20:35:27 12.068     70
Feige 110 23:19:58.3 -05:09:56 11.826     70
LTT 9491  23:19:35.2 -17:05:28 14.112     150 
----------------------------------------------------

  • A list of Spectrophotometric Standard Stars may be found here Standards for telluric features correction -------------------------------------------------------------- Star RA (2000) DEC V Time (sec) -------------------------------------------------------------- L745-46A 07:40:20.9 -17:24:42 13.0 250 DF,Bessell99 LTT 4364 11:45:50.0 -64:50:30 11.504 150 EG131 19:20:35.0 -07:40:00 12.28 200 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 14.1 400 DC,Bessell99 -------------------------------------------------------------- One telluric standard with narrow slit (followed by a comparison lamp). Click on the star name to get a finding chart. 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.