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, 'image quality' )
- the allowable sky transparency
- for CRIRES, NACO and SINFONI, the Strehl ratio on the reference star (as applicable).
- for instruments observing in the mid-IR (CRIRES and VISIR), the allowable maximum Precipitable Water Vapour (PWV)
- the allowable twilight constraint that defines the earliest time in minutes with respect to the end of the astronomical twilight when the execution of the OB can be started
- the allowable absolute time window (i.e. for time critical events, multi-epoch monitoring)
- the allowable local sidereal time range (e.g. 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, image quality/seeing, moon constraints, as well as Strehl ratio for Adaptive Optics mode observations. If all constraints are fullfilled the OB will get assigned Quality Control grade "A", while the "B" quality control is assigned if some constraint is up to 10% violated. The observations with quality control grades A or B are completed, while those with quality control grade "C" (out of constraints) will be re-scheduled and may be repeated. In exceptional cases an OB may get status completed with quality grade "D", meaning that it is taken out of constraints but will not be repeated.
Note: for most instruments the image quality 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). For the instruments where the image quality cannot be directly measured (AO, VLTI, fibre instrument), it is either not used for classification or is obtained from the wavefront sensor of the active optics of the telescope.
Additional Observing Constraints and Classification Rules for VISIR
Quality Control of OBs executed in service mode will be mainly based on airmass and seeing constraints as well as PWV measurements and sensitivity estimates obtained from standard star observations during the observing night.
The image quality constraint, as defined in the OB, is compared to the full width at half maximum (FWHM) of the science data in imaging and spectroscopy modes. Note that this image quality constraint directly relates to the achieved spatial resolution of the science data in the infrared, and is not the optical seeing at zenith (which is specified in the Phase 1 proposal). However, the image quality constraint specified in the OB cannot be more stringent than the image quality corresponding to the optical seeing specified at Phase 1. The VISIR Exposure Time Calculator can be used to estimate the image quality corresponding to a given instrument setup and optical seeing.
In cases where the image quality cannot be measured directly (e.g. for faint or spatially extended sources), the image quality will be assessed from standard star data obtained close in time to the science observations. In case multiple filters are present within an OB, the image quality constraint will be assessed using the shortest-wavelength filter. A measured image quality of 0.3"(~10μm) and 0.6"(~20μm) will always satisfy the image quality constraint.
Atmospheric classification like PHO/CLR/THN/THK are not necessarily related to the photometric stability and sensitivity in the mid-infrared. The main guideline to classify a specific OB will be therefore based on photometric observations of mid-infrared standard stars, frequently monitored during the night. The sensitivities guaranteed by the observatory are listed in the corresponding section of the VISIR instrument page. The OB will be considered fully within constraints regarding sensitivity if an observation of a standard star at zenith in the same filter as the service OB results in an equal or better limiting flux as published ("grade A"). If the limiting flux obtained with standard stars exceeds the published sensitivities in the same filter by not more than 10%, the OB will be considered as "grade B", while the OB will be classified as "grade C" in all other cases. An analog classification scheme will be applied for spectroscopic observations.
Precipatable Water Vapour:
The opacity in the mid-infrared strongly depends on the precipitable water vapour (PWV) in the earth's atmosphere. On Paranal, the PWV contents of the atmosphere is continuously monitored by a dedicated radiometer. PWV can be set as an observing constraint in the constraint set in P2PP for VISIR observations conducted in service-mode. It can take values ranging from 0.5 to 20.0 mm. The median PWV value on Paranl is 2.1 mm, with string seasonal variations. The VISIR ETC can be used to simulate the influence of different precipitable water vapour (PWV) values. Typical values for the PWV constraint may be 3 mm for observations in the N-band and 1.5 mm for observations in Q.
Moon constraints are usually irrelevant in the mid-infrared and are not taken into account for the classification of the OB. Telescope guiding and active optics can, however, under certain circumstances be compromised for moon distances <30deg.