README web version of /home/usg/OPS/MTS/readme_xml/readme_82503701
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
Aim: we need to record saturated images of beta Pictoris (herefater Bpic)
and saturated images of a PSF star (also called comparison star, as in the proposal)
(hr2435). We will also record unsaturated images of both stars (which will be used
as PSF and photometric references). The saturated images will be made at two different
rotator positions, separated by 30 degrees (runB, part 1) and -175 degrees (runB,
part 2).
Each OB consists of:
- an acquisition template
- a science template to get unsaturated images (using the NDL filter) at different
generic offsets
- 1 science template to get saturated images, at different generic offsets
- rotator change
- 1 science template to get saturated images, at different generic offsets
- 1 science template to get saturated images, at different generic offsets (see
below)
The run will execute successively :
- one OB on bpic with rot offset=30 degrees (bpic_Lp_runB_1)
- one OB on the PSF with rot offset=30 degrees (PSF_bpic_Lp_runB_1)
These two OBs constitute the first part (part 1) of our run. PSF_bpic_Lp_runB_1
shoudl be executed right after bpic_Lp_runB_1.
- one OB on bpic with rot offset=-175 degrees (bpic_Lp_runB_2)
- one OB on the PSF with rot offset =-175 degrees (PSF_bpic_Lp_runB_2)
These two OBs constitute the second part (part 2) of our run. PSF_bpic_Lp_runB_2
shoudl be executed right after bpic_Lp_runB_2.
Note that Part 1 and Part 2 are independant (ie are expected to be executed independantly).
Thye will be executed in 44 minutes each (see below0.
There are time-critical/execution constraints associated to these observations (valid
for part 1 and for part 2):
1- In order to avoid the spiders beeing too close to the Bpic disk PA (30 deg) during
the exposures, we need to start Bpic OB between 90 and 30 minutes prior to the meridian,
ie at LST in the range 04h17--05h17.
2- Bpic and the PSF should be observed at identical parallactic angles. To do so:
Bpic OB should be executed in 44 minutes precisely. In order to take into account
the uncertainty in the duration of the acquisition process, the OBs as prepared
last more than 44 minutes (this was done after acception of a WR). We ask the Astronomer
to STOP the OB 44 minutes after starting beta Pic OB and proceed immediately with
the PSF OB. The PSF OB should last 44 minutes as well.
Note that as a consequence, part 1 and part 2 will last 2*44 minutes each. Depending
on the actual durations of overheads, the last template of each OB may or may not
be started. We are aware that if started, it will be not completely executed.
3- Please avoid any delay between acquisition and science frames.
Important notes:
- finding charts: in both cases, the brightest objects in the FoV will be the targets
themselves.
- in all cases, the offset patterns assume that the targets are centered in the
FoV at the beginning of the template (ie prior to the first offset)
- the DITs of the unsaturated images (using the NDL filter) have been calculated
using the ETC; they are supposed to avoid the non linearity domain. If the level
of non linearity is reached at acquisition, please adjust the DIT so as to avoid
this non linearity domain (we are aware nevertheless of the 0.175s limit for the
mininum DIT).
- the DITs of the saturated images of bpic have been defined to saturate the core
of the PSF over a radius of 4 to 5 pixels. Please adjust the DIT according to the
actual observing conditions at the beginning of each template.
- same for the PSF.
- we have assumed (Naco UM, p 27) that twighlight flats would be done as part of
Naco Calibration plan.
- the OBs as written take into account the WRs answers.
- both targets will be used as a reference for AO
- both targets are the only bright objects in the Conica FoV
Waiver Requests
Waiver requests have been sent :
- to ask to be allowed to observe beta pic and hr2435 whch are brighter than 5 at
L'.
- to ask to execute the PSF OB immediately after the OB of the science target, bpic.
- to ask to prepare OBs with durations as estimated by p2pp longer than what is
allocated, but with ACTUAL
execution times (44 minutes) meeting the time allocation (see REDAME file); this
is to take into account the discrepancy mainly between the estimated acquisition
times and the actual acquisition times.
All these items were accepted.
Critical Observing Condition Constraints
Time-Critical Aspects
There are time-critical/execution constraints associated to these observations
(valid for part 1 and for part 2):
1- In order to avoid the spiders beeing too close to the Bpic disk PA (30 deg) during
the exposures, we need to start Bpic OB between 90 and 30 minutes prior to the meridian,
ie at LST in the range 04h17--05h17.
2- Bpic and the PSF should be observed at identical parallactic angles. To do so:
Bpic OB should be executed in 44 minutes precisely. In order to take into account
the uncertainty in the duration of the acquisition process, the OBs as prepared
last more than 44 minutes (this was done after acception of a WR). We ask the Astronomer
to STOP the OB 44 minutes after starting beta Pic OB and proceed immediately with
the PSF OB. The PSF OB should last 44 minutes as well.
Note that as a consequence, part 1 and part 2 will last 2*44 minutes each. Depending
on the actual durations of overheads, the last template of each OB may or may not
be started. We are aware that if started, it will be not completely executed.
3- Please avoid any delay between acquisition and science frames.
Special Execution Requirements
There are time-critical/execution constraints associated to these observations
(valid for part 1 and for part 2):
1- In order to avoid the spiders beeing too close to the Bpic disk PA (30 deg) during
the exposures, we need to start Bpic OB between 90 and 30 minutes prior to the meridian,
ie at LST in the range 04h17--05h17.
2- Bpic and the PSF should be observed at identical parallactic angles. To do so:
Bpic OB should be executed in 44 minutes precisely. In order to take into account
the uncertainty in the duration of the acquisition process, the OBs as prepared
last more than 44 minutes (this was done after acception of a WR). We ask the Astronomer
to STOP the OB 44 minutes after starting beta Pic OB and proceed immediately with
the PSF OB. The PSF OB should last 44 minutes as well.
Note that as a consequence, part 1 and part 2 will last 2*44 minutes each. Depending
on the actual durations of overheads, the last template of each OB may or may not
be started. We are aware that if started, it will be not completely executed.
3- Please avoid any delay between acquisition and science frames.
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 you have PSF reference star OBs, do the names of those OBs begin with
PSF_ ?
If there are Finding Charts attached to your OBs, is the field-of-view
of at least one of these charts 2' x 2' (with clearly labelled field orientation)
?
Have you clearly marked and labelled your wavefront reference objects
R1, R2, R3, ... (as specified in the NAOS Preparation Software) on your Finding
Charts ?
Have you specified the magnitude of the brightest object in the field-of-view
for each OB ?
Are there objects in any of your fields (including standard stars) which
are brighter than the limits specified in the User Manual and on NACO web Pages
?
If the previous answer is yes, have you given a list of OBs and a justification
for the brightness limit violation in the general description field ?
Last creation of page: Tue Oct 6 15:40:28 2009
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