README web version of /home/usg/OPS/MTS/readme_xml/readme_79056100
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
These second epoch observations will provide high-contrast, high-spatial
resolution imaging to confirm substellar companions candidates (Giant Planets or
Brown Dwarfs) orbiting nearby WDs (by common proper motion). The WDs were selected
from a sample of WDs up to 20 pc, where almost all have high proper motion. And
target with candidates were selected from first epoch observation carried out with
NACO. The observations consists of simple imaging in J-band with repeated jitters
in a WD position in very large exposure (& execution) times, to reach the required
detection limit of giant planets and/or low mass brown dwarfs. IMPORTANT: All the
targets OBs have two NACO_img_obs_Autojitter templates, each one with the ONLY differece
of their rotating angles. The reason is that we would like to know whether some
residuals from PSF substaction correspond to spurious residuals from the optic system
or real objects. Also we would like to improve our primary PSF substraction (Target)
by sustracting one image to other with different rotating angles but observed with
the SAME CONFIGURATION, EXPOSITION TIME, DIT and NDIT. These templates could have
DIT near to the saturation limit (but bellow) which is necessary to reach the required
depth to detect a giant planet with reasonable execution times (to lessen overheads).
So, in some cases it could be necesary to increase the DIT to reach the non-linear
range of ADU (~6000-7000 ADU) for the peak pixel of the target (to improve the depth).
Both templates are very important for the success of our project. We avoided that
any star in the FOV over-saturates the detector (i.e., with less than 1.5 times
of the number of counts of the saturation limit).
NB: Coordinates in the OBs are given in equinox J2000, for the epoch 2000.0 . Stars(Target)
have high proper motion, so proper motion have to be taken in account to calculate
coordinates for observation epoch.
J magnitude of
Target brighter object Separation Comments
in the FOV
WD2151-015 12.45 1''
WD2007-219 14.2 0''
WD1919+145 13.26 0'' Object with J=12.61 at 23.7'' from
target; out of FOV
WD1917-077 12.35 0'' Object with J=8.22 at 27.7'' from
target; out of FOV
WD1620-391 11.58 0''
WD1544-377 12.5 0'' Object with J=5.0 at 13.9'' from
target; out of FOV
WD1236-495 13.8 0''
WD0738-172 12.7 0''
WD0135-052 12.1 0''
Waiver Requests
Critical Observing Condition Constraints
It is necesary to make observations with very good seeing (0.6'') to reach
to detect very faint objects (24 mag in J-band). Also it is required to carry out
the observations in smaller airmass as this were possible, to lessen differential
color difraction and to obtain a better FWHM of the objects.
To get the airmass requirements for WD0738-172 it would be necesary to observe on
the period from 1 Apr to 15 Apr 2007 at the begining of the night!!
Time-Critical Aspects
Special Execution Requirements
In first epoch NACO observation for WD1620-391 was used a DIT=16 s to
reach the non-linear range for flux of peak pixel of target, ~6000-7000 ADU. Maybe
it could be necesary to increase the DIT(=5s) from the NACO_img_obs_Autojitter
templates.
In first epoch NACO observation for WD1917-077 was used a DIT=60 s to reach the
non-linear range for flux of peak pixel of target, ~6000-7000 ADU. Maybe it could
be necesary to increase the DIT(=15s) from the NACO_img_obs_Autojitter templates.
In first epoch NACO observation for WD1919+145 was used a DIT=30 s to reach the
non-linear range for flux of peak pixel of target, ~6000-7000 ADU. Maybe it could
be necesary to increase the DIT(=20s) from the NACO_img_obs_Autojitter templates.
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 15:40:19 2009
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