Observing Constraints and Classification Rules
General Observing Constraints
Every requested observation has multiple observing constraints. Typical observing constraints are:
- the allowable brightest lunar phase
- the allowable smallest moon-to-object angular separation
- the allowable maximum airmass
- the allowable maximum image size (i.e. FWHM at observed wavelength, 'seeing')
- the allowable sky transparency
- for Adaptive Optics instruments (currently CRIRES, NACO and SINFONI), the Strehl ratio on the reference star.
- for instruments observing in mid-IR (CRIRES and VISIR), the allowable maximum Precipitable Water Vapour (PWV)
- the allowable absolute time window (i.e. for time critical events, multi-epoch monitoring)
- the allowable local sidereal time range (i.e. for ADI observation)
- for VLTI instruments, the availability of the desired baseline
The Observing Constraints are specified by the user at Phase 2 for each Observation Block. Since the execution conditions required by each programme are an important ingredient in the process of building up the Long Term Schedule of an observing semester, and thus determines which programmes can or cannot be scheduled, users are not allowed to specify at Phase 2 constraints that are more strict than those specified in the original proposal. Users can however relax the constraints during the submission of their Phase 2 material. The values in the OB constraint sets that are selected (and approved) during Phase 2 preparation (and review) cannot be changed later during the observing period.
General Classification Rules
Quality Control of OBs executed in Service Mode will be based on the user's specified constraints for airmass, atmospheric transparency, seeing (i.e. image quality), moon constraints, as well as Strehl ratio for Adaptive Optics mode observations.
Note: the seeing constraint as defined in the OB is judged against the full width at half maximum (FWHM) of a point source in the resulting image (or spectral image), i.e. at the observed wavelength, for most of the VLT instruments (i.e. it is the image quality).
Additional Observing Constraints for VIMOS
The lack of atmospheric dispersion correction places severe limits on the time window in which observations through a MOS mask can be successfully executed. In practice the requirements are that both pre-imaging and MOS of the same field must be obtained while the field is plus/minus 2 hours from the meridian. This holds for all targets that are taken with the default rotator offset angle of 90 deg. An exception are targets with declinations in the range -45<DEC<-5 deg that are taken with a rotator offset angle of 0 deg. Those can be observed up to plus/minus 3 hours from meridian. It is the user's responsibility to make sure that the airmass constraints specified in the OBs do not conflict with these operational requirements, i.e. the airmass constraints must be set such that they correspond to +/-2 hours (pink shaded area in the graph below) or +/-3 hours (green shaded area in the graph below) or less from the meridian:
Users may request to waive this rule, but are advised to carefully consider the potentially severe and negative effect this will have on their data quality.
Additional Classification Rules for VIMOS
As stated in the Call for Proposals, any set of MOS data obtained with VIMOS in Service Mode where at least 3 of the 4 arms functioned will be considered an observation completed within constraints.