Campaign 21 in normal ops will use the following standards. This plan is based on a campaign with a length of 18 days. target letter sp. F_12 (Jy) dec. HR 6606 A+ (decin) K0 1.73 +72 HR 6348 B+ (fred) K0 1.15 +61 ksi Dra C+ (decin) K2' 16.85 +56 HD 173511 D+ (harlo) K4 1.19 +61 eta1 Dor E+ (decin) A0 0.17 -66 HR 1014 F (decin*) A3 0.21 -66 HR 7341 G+ (decin) K3 1.40 +49 GSC 04212 H (faint) K2 0.04 +66 MRK 231 I (red) -- -- +56 MRK 231 J (red) -- -- +56 HD 163051 Z (dblstar) K3 0.48 -61 For a campaign lasting 18 days (plus any fraction), sources should be observed in the following order 18-day schedule............... day sequence day sequence 1 A+ 10 E+ 2 B+ 11 G+ 3 C+ 12 F 4 D+ 13 I 5 E+ 14 J 6 G+ 15 Z 7 H 16 F 8 A+ 17 D+ 9 C+ 18 H Note 1: The above schedule is tailored specifically to Campaign 21. Please note that objects F (HR 1014), I,J (Mrk 231) should be scheduled after May 29 (day 8 or later) and June 1 (day 11 or later) respectively because otherwise the slit orientations include a field star. Note 2: The targets with a "+" after their letters will require an offset sky observation to be conducted immediately before or after them. These sky AORs are included in the AOR file, and they have similar labels, with the name of the target replaced with "sky". For example, calsfx-21A-HR6606 and calsfx-21A-sky are a pair. Note 3: Target Z is the 3286-sec double-star experiment. It has been placed on the schedule for Day 15 (5 June 2005 UT), but this data can be changed if doing so would improve be more efficient. Any date on or after 2 June 2005 will be suitable. Due to the 1 degree/day rotation of the slit, observations prior to 2 June will invalidate the purpose of the observation. 5 June 2005 is the ideal date for the experiment. Note 4: If the campaign is shorter than 18 days, the schedule above can be compressed by combining two one-standard days into a single two-standard day. Note 5: If the campaign is longer than 18 days, the schedule above can be extended as long as one standard is observed each day. Note 6: In order to improve observatory efficiency, the scheduler should feel free to re-arrange the observing schedules above, as long as sources do not move by more than roughly +/- 24 hours, and as long as the spacing between successive observations of the same source remains roughly the same. Observational details DCEs for .................................... total AORNAME root SL2 SL1 LL2 LL1 SH LH PU DCEs T(s) calsfx-21A-HR6606 4x 6 4x 6 4x 14 12x 14 4x 30 16x 60 8 26 2474 calsfx-21A-sky 4x 30 16x 60 4 1657 calsfx-21B-HR6348 4x 6 4x 6 2x 30 6x 30 4x 30 8x 60 8 36 1850 calsfx-21B-sky 4x 30 8x 60 12 1055 calsfx-21C-ksiDra 4x 6 4x 6 6x 6 6x 60 8 28 1245 calsfx-21C-sky 6x 6 6x 60 12 831 calsfx-21D-HD173511 4x 6 4x 6 2x 30 6x 30 4x 30 8x 60 8 36 1849 calsfx-21D-sky 4x 30 8x 60 12 1055 calsfx-21E-eta1Dor 4x14 4x14 4x120 6x120 8 26 2225 calsfx-21F-HR1014 4x14 4x14 4x120 6x120 8 28 2212 calsfx-21G-HR7341 4x 6 4x 6 4x 30 8x 30 4x 30 8x 60 8 28 2030 calsfx-21G-sky 4x 30 8x 60 1267 calsfx-21H-GSC04212 4x14 4x14 4x120 6x120 8 26 2213 calsfx-21I-Mrk231 8x14 8x14 10x 6 10x 6 16x 30 12x 60 8 72 2843 calsfx-21J-Mrk231-Map 14x14 1043 calsfx-21H-GSC04212 4x14 4x14 4x120 6x120 8 26 2212 The number of DCEs is to the left of the "x", and the ramp time (in sec) is to the right. The number of DCEs is the total for each AOR, including both nod positions. (Version date: 10 Apr 05) (edited later)