README web version of /home/usg/OPS/MTS/readme_xml/readme_82045400
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
In order or priority, the goals of this program are:
1. Image Jupiter's atmosphere in 7 filters: PAH1, SIV_2, NeII_2, Q1, Q2, Q3, J7.9.
2. Spectroscopy at MR 7.5-9.3 microns north-south through both LRS and GRS.
3. Spectroscopy at HR 8.02 micron north-south through both LRS and GRS.
(Note that the finding chart labels the LRS as "Oval BA", its formal identification.)
Waiver Requests
Critical Observing Condition Constraints
Time-Critical Aspects
We have listed below a table of the dates in October 2008 when either
or both the Great Red Spot (GRS, expected longitude ~139 deg W) or the Little Red
Spot (LRS, expected longitude ~97 deg W) are available. We have eliminated times
when Jupiter is greater than than 1.7 airmasses and the local time is after 6:00
pm (2200 UT on the preceeding day).
For each date, we list below the times when each feature is expected to cross Jupiter's
central meridian (cm). We perfer the features to be obsered within 1.5 hours on
either side of this time in order to avoid suffering significant foreshortening.
This can be pushed 30 min further on either side without big problems. We have
also cut off the observing windows when Jupiter sets lower than 1.7 airmasses, but
this can also be pushed to 2.00 aimasses if necessary.
Optimal timing choice: Our highest priority imaging (SET 1) should be performed
when either or both southern-hemisphere features (GRS and LRS) are available on
the disk, as noted. Observations of the southern hemisphere on the opposite side
of the planet (a lower priority, SET 2) would then be made near the same time on
the subsequent night, or even later at multiples of 10 hours with a 5-hour phase
offset. On most nights the GRS and LRS can be imaged individually (as SET 1 and
SET 2), as noted.
Spectroscopy can be performed on any night either feature is (or both are) available.
It is a lower priority than the multi-spectral imaging.
Date: Comment:
October 2 LRS observable between 00:00 and 03:00 UT (Jupiter at AM>1.7 after
2:53 UT, otherwise good)
(October 4 LRS observable between 02:32 and 04:32 UT - backup date; Jupiter at
AM>1.7 after 2:42 UT)
October 7 LRS observable between 00:00 and 03:00 UT (Jupiter at AM>1.7 after
2:32 UT)
GRS observable between 01:23 and 03:23 UT (Jupiter at AM>1.7 after
2:32 UT)
October 9 LRS observable between 01:38 and 03:38 UT (Jupiter at AM>1.7 after
2:24 UT)
October 12 LRS observable between 23:06 and 01:06 UT (no high-airmass restrictions;
excellent)
GRS observable between 00:33 and 02:15 UT (Jupiter at AM>1.7 after
2:08 UT)
October 14 LRS observable between 00:43 and 02:43 UT (Jupiter at AM>1.7 after
1.58 UT)
October 17 GRS observable between 23:43 and 01:43 UT (no high-airmass restrictions;
excellent)
Please execute the OBs in the following order:
SET ONE:
1. MOV_img_jup_south_set1 (6 filters, 60s exposures, repeated twice with a 3 pixel
offset = 38.5 mins).
SET TWO:
2. MOV_img_jup_south_set2 (6 filters, 60s exposures, repeated twice with a 3 pixel
offset = 43.5 mins).
GRS SPECTROSCOPY (Can be on any night the GRS is available):
3. MOV_spect_jupiterGRS_HR8.02
4. CAL_spect_star_HR8.02
5. MOV_spect_jupiterGRS_MR7.5-9.3
6. CAL_spect_star_MR7.5-9.3
LRS SPECTROSCOPY (Can be on any night the LRS is available):
7. MOV_spect_jupiterLRS_HR8.02
8. CAL_spect_star_HR8.02-0
9. MOV_spect_jupiterLRS_MR7.5-9.3
10. CAL_spect_star_MR7.5-9.3-0
SET 3: NORTHERN HEMISPHERE IMAGING (Any night Jupiter is available):
11. MOV_img_jup_north_set1 (6 filters, 60s exposures, repeated twice with a 3 pixel
offset = 38.5 mins).
NB1: If observations take less time than predicted by P2PP, please execute MOV_img_jup_north_set1
a second time.
NB2: Blocks 1 and 2 must be executed together. Spectra and their calibrators must
be executed together.
NB3: In the observation blocks, RA and DEC have been given for October 10th 2008,
modifications can be found in the ephemeris datafile.
NB4: Observations can be done following 17 October, but the availability of Jupiter
will be extremely limited.
Special Execution Requirements
Within a single MOV_img block, the total integration time on each filter
is 60 seconds. Each filter must be repeated again at each epoch with an offset of
few pixels to correct for bad pixels. Do *NOT* run the acquisition again, just offset
the telescope by 3 pix in RA and 3 pix in DEC and repeat the observaton
IMAGING SEQUENCE: Our first priority is to survery the southern hemisphere, with
particular emphasis on the Little Red Spot (LRS) and the Great Red Spot (GRS), together
with imaging of a calibration star. This is a bit complicated, because the LRS
and GRS may actually be available on the same hemisphere on some nights (they are
60 deg apart in longitude and cross the planetary central meridian ~1-1/2 hours
apart: see the Timing Constraints section).
.
If only the GRS is observed, then the LRS should be observed next, and vice-versa.
If both are captured, then roughly the opposite hemisphere
should be observed. If time permits after spectroscopic OBs are executed, sample
the northern hemisphere at an artibtrary longitude. (This is priority 3, behind
the spectroscopic OBs.)
INTEGRATION TIME: With the Q-filters, integration times of 20s would be sufficient
to produce a good image. The key priority of this observing run is image quality.
10s of integration is sufficient for the calibration star imaging (shortening the
execution time dramatically). Reduced integration times should be used, if possible.
WEATHER FLAG: The weather flag must be set to P because Jupiter is bright and would
otherwise produce prominent horizontal striping.
POINTING: The second chop position will be discarded, so ensure chop throw is sufficient
to minimize overlap on the planet's southern hemisphere.
This can be set at 20 arcsec. For southern hemisphere imaging, Jupiter should be
centered right-left, with the southern limb some 3-4 pixels above the bottom of
the field of view. For northern hemisphere imaging, the northern limb should be
3-4 pixels below the top of the FOV.
POINTING FOR SPECTROSCOPY: Rotate slit so that it lies north-south across the target
(see finding charts).
Special Calibration Information
ToO Information
ToO Activators List
Is this a Pre-imaging run ?
Pre-imaging Requirements
Source(s) of Pre-imaging
Pre-imaging sources not listed above
Do all your OBs comply with the instrument-specific requirements listed
on the instrument-specific Phase 2 web page ?
If this is a pre-imaging run, did you select PRE-IMAGING for the Observing
Category for each Observing Template ?
Do all your finding charts comply with both the general and instrument-specific
Phase 2 Web Pages ?
If you submitted OBs for standard stars, did you specify the magnitude
and spectral type of all standard stars in the OBs ?
Have you included OBs for any calibrations that you need but which are
not part of the Calibration Plan ?
If you are observing Moving Targets, have you attached suitable ephemeris
files to your OBs?
If you have preferences which OBs should be executed first, did you make
use of the User Priority field in the OBs ?
If this is a run that requires coordinated observations with other facilities,
did you give proper instructions in the Time-Critical Aspects Section ?
If the provided finding chart is at a different wavelength than the observations,
did you clearly describe in the README file how to identify the target?
Did you specify a guide star brighter than V=12mag within a field of
r=5arcmin around the science target?
Last creation of page: Tue Oct 6 15:40:27 2009
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