README web version of /home/usg/OPS/MTS/readme_xml/readme_81049600
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
Below we prioritize the observing blocks for this run:
ONE: IMAGING NEPTUNES ATMOSPHERE:
Observations of Neptune's atmosphere in PAH1, 7.9, NEII-1 filters. We expect 1 hour
of execution time for each of three filters (total 3h). We also request that 2 calibration
OBs on HD216032 be performed just before and just after the previous 3 observations
(at SIMILAR airmass). This sequence should be repeated 6 hours later (if the airmass
<1.5 and the weather allow) when Uranus has rotated by 180 deg. in longitude
(see details below).
OBs for the first imaging set should be executed in the order:
1. HD216032_ima_N-1
2. MOV_Neptune_ima_PAH1-1
3. MOV_Neptune_ima_J7.9-1
4. MOV_Neptune_ima_NeII_1-1
5. HD216032_ima_N-2
NB1: As we stay on the same target between the 3 OBs, you can increase the integration(
exposure) time to fit OB execution time within 1h).
NB2: Our previous observation in Sept. 2006 showed that you may need to use the
tracking camera at the beginning of the OBs in order to locate Neptune.
OBs for the second imaging set should be executed in the order:
1. HD216032_ima_N-3
2. MOV_Neptune_ima_PAH1-2
3. MOV_Neptune_ima_J7.9-2
4. MOV_Neptune_ima_NeII_1-2
5. HD216032_ima_N-4
Timing: the goal for the second imaging set is to observe the opposite hemisphere
of Neptune, when the planet has rotated by 180 deg. in longitude. This corresponds
to ~6 h at our latitude of interest. This is best accomplished by observing the
intial imaging sequence in the early evening and repeating 6 hours later in the
morning. Neptune is higher than 1.5 airmasses at the VLT for 7 hours each night,
and the observations are possible during observing hours from late July through
early September.
If it is not possible to observe 6 h later, please, be sure for the second observation
to observe the opposite side of Neptune. This can be done on the successive night,
i.e. 24h later, PLUS or MINUS a 6-hour delay, e.g. an initial observation made at
0400 local time can be repeated on the next night at 2200; an initial observation
made at 2100 local
time can be repeated at 0300 the following night (i.e. 30 hours later) if weather
or other problems prevent a repeat with a short 6-hour delay. The time between
these should be made as short as possible, because we suspect that the phenomenon
is time dependent with a time scale for variability which are we trying to characterize.
TWO: MEDIUM RESOLUTION SPECTROSCOPY (10-13) MICRONS:
The slit should be aligned along Neptune's North-South rotational axis. These spectroscopic
observations should be performed BETWEEN the two imaging sets.
The OBs should be executed in the order:
1. MOV_Neptune_spectro_MR-1
2. MOV_Neptune_spectro_MR-2
3. HD216032_Spec_MR-1 (for calibration)
NB1: MOV_Neptune_spectro_MR-1 and MOV_Neptune_spectro_MR-2 are the same OBs. Thus
as you don't need to change the pointing, you can also increase the integration(
exposure) time to fit OB execution's time within 1h.
NB2: If the airmass is changing too rapidly, execute the Calibration OB (HD216032_Spec_MR-1)
between the first and the third one.
THREE: LOW RESOLUTION SPECTROSCOPY AT 8.1 AND 9.8 MICRONS:
The slit should be aligned along Neptune's North-South rotational axis.
The OBs should be executed in the order:
1. MOV_Neptune_spectro_LR_8.1-1
2. MOV_Neptune_spectro_LR_9.8-1
3. MOV_Neptune_spectro_LR_9.8-2
NB1: MOV_Neptune_spectro_LR_9.8-1 and MOV_Neptune_spectro_LR_9.8-2 are the same.
If exectuted in the same night, please increase the exposure time, as you do not
need any telescope pointing after the complete exectuion of the first one.
NB2: It would be very useful to obtain these observations on or near the same date
as the medium-resolution spectra, but it is not essential.
NB3: We do not need an calibration on a specific object.
FOUR: IMAGING IN Q3:
We expect to see a warm south pole.
The OBs should be executed in the order:
1. MOV_Neptune_ima_Q3-1
2. MOV_Neptune_ima_Q3-2
3. HD216032_ima_Q3-1 (for Calibration)
NB1: If the airmass is changing too rapidly, execute the Calibration OB (HD216032_ima_Q3-1)
between the first and the third one.
NB2: MOV_Neptune_ima_Q3-1 and MOV_Neptune_ima_Q3-2 are the same. Same advice as
before concerning exposure time.
Waiver Requests
Critical Observing Condition Constraints
Time-Critical Aspects
Special Execution Requirements
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 15:40:24 2009
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