README web version of /home/usg/OPS/MTS/readme_xml/readme_77900300
Principal Investigator Email Address
Estimated Total Execution Time (hours, including overheads)
General Description
Programmes 77.A-9003(A) and 77.A-9003(B) form a joint programme to do
I-band
monitoring of the young open cluster NGC6611 in order to determine the
rotation periods for low-mass members in this cluster to study the angular
momentum evolution of these objects.
The method is based on the rotational brightness modulation by magnetic spots
on the surface of these objects, which will result in periodic flux variations
of 1-5 percent with periods ranging from 0.5 to 10 days. The flux variations
will be determined with relative photometry with respect to other non-variable
stars in the field.
The programme consists of a "core" time with densely sampled observation from
about the 13. to 19. July, in which we try to get good phase coverage for the
faster rotators,
and of "extended" time, which is spread out over the whole MPI time in order
to cover also the slower rotators. The extended time has usually few
integrations (except for the 6. July).
Moreover, we want to carry out a deep photometric observation in UBVRIHalpha.
These observations are planned for dark time, and should be done in the first
possible photometric night at or after the 18. July. We supply additional
calibration OBs with photometric standard fields for this observation.
Please note: we have received 46h of observing time for this programme.
Running the Execution time report of our OBs will, however, show 46h21min.
The reason for this "overtime" is that we supply OBs for three photometric
OBs (of 23min each), of which only *two* shall be executed (see below).
Thus this programme will stay within its alloted 46h.
Waiver Requests
Critical Observing Condition Constraints
There are no critical observing conditions from the weather and seeing
for
our OBs (except for the single UBVRIHalpha photometry ). This means that the
programme should be carried out even under poor conditions!
This will of course harm the depth, but the large number of images will
still allow us a proper analysis of the brighter stars, and thus give an
interesting and publishable result.
Time-Critical Aspects
To maximise the scientific output of our program it is important that
certain OBs are only carried out at certain nights.
Therefore:
*** we have named our OBs with the date. ***
*** Please execute the OBs on those days ***
*** e.g. n6611-6jul should be executed ***
*** in the night 6/7. July ***
Some nights have multiple OBs in order to cover a major part of that night.
These OBs should be executed consecutively one after the other.
Exception: For the nights of 12., 14., 15., and 19. July two OBs are provided.
For better time sampling it is *necessary not to execute them*
consecutively, but with a gap of two to four hours - say one in the first and
the other in the second part of the night.
Special Execution Requirements
For the calibration of our photometric observations we provide three
calibration OBs for three different Landolt SA fields, in addition to the
photometric calibration of the standard calibration plan.
However, only *two* of these three "Landolt calibration OBs" should be
executed:
Definitely executed should be Landolt SA-110, which is close to our science
field. In addion you should observe Landolt SA-107 or Landolt SA-113 depending
which one has the larger airmass. You should choose the one with the larger
airmass to have a better extinction correction.
One "Landolt calibration OB" should be done before and the other
after the UBVRIHalpha observations of NGC6611.
Special Calibration Information
We require calibrations from the standard calibration plan.
We are happy with large amounts of flats and biases.
For the calibration of our photometric observations we provide
three calibration OBs of Landolt SA fields, in addition to the
photometric calibration of the standard calibration plan.
Two of these additional OBs should be executed, one immediately
before and one after the photometric OB.
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 ?
Did you set 'New Preset' flag in all acquisition templates to 'True'?
Have all your submitted OBs the same filter for the acquisition template
and for the first science template?
Did you combine calibration templates with science templates for any
OB?
Did you combine imaging and spectroscopic templates for any OB?
Did you submit any Focus template?
Last creation of page: Tue Oct 6 15:40:14 2009
If you have comments, please contact usd-help@eso.org