VLTI Configurations Overview
P105 and P106:
Since P104, AT configurations have to be requested by generic names ("small", "medium", "large" and "astrometric") rather than explicit configurations using AT positions. The following table shows which instrument / mode can request which configuration. By clicking on their name, the user can see the sky coverage corresponding to the standard AT positions for a given configuration.
|AT Configurations||PIONIER, MATISSE (from P103),GRAVITY single-feed
Note: the standard astrometric configuration, A0-G1-J2-K0, is a variation of the standard large configuration A0-G1-J2-J3. It has all its telescopes south of the delay line tunnel, which is mandatory for GRAVITY dual-feed observations.
This new scheme allows a more flexible execution of OBs, for example using intermediate configurations during AT relocations (transition nights between two standard configurations). This scheme will be primarily used for imaging programmes. The overlap in baseline length between standard and relocation configurations is detailed in this graphic. A criteria of at least 50% of baseline length overlap will be used to decide if OBs can be executed on an another onfiguration than the standard one. Based on this criteria, this table gives the correspondence between actual AT quadruplets and classification in terms of "small", "medium", "large" and ''astrometric" configurations.
Starting with P105, alternative baseline configuration can be specified at phase 1 in a keyword list, in order of priority. Each run will, however, be scheduled on only one configuration. Most likely, it will be the first (primary) choice. However, a run may exceptionally be scheduled on an alternative choice if the primary choice of the baseline configuration cannot be scheduled. Because a run will be scheduled on only one configuration, all observing set-ups of a run need to request exactly the same list of baseline configurations. If different configurations are needed, different runs need to be specified, each with one configuration.
As it is the case since P101, some single-feed observing blocks of service mode runs requesting the large configuration might still be executed on the astrometric configuration instead since it offers similar baseline lengths and sky coverage.
Instructions for Imaging programmes
- It is highly recommended to request imaging in service mode in order to benefit from an u,v coverage optimized by ESO and taking advantage of intermediate configurations. Imaging propsals requesting visitor mode are expected to present a strong science case justification.
- Taking into account the VLTI/AT field of view and the highest spatial frequency, the image that a user can aim at reconstructing at VLTI has approximatively 200x200 pixels. Each 4 AT observations bring 6 Visibilities and 3 (independent) CP, or 9 data points. 8 observations per configuration is a minimum to get enough data. A minimum of two configurations is mandatory to request an imaging programme. A u,v plane filling factor can be defined and computed for a set of AT configurations (including intermediate configurations that are only possible during relocation nights in service mode). In these graphs, this factor is plotted as a function of declination to take into account the observability constraints due to telescope shadowing and delay line limits. Based on these, we recommend requesting the following number of concatenations depending on the declination of the choosen targets:
- 6 concatenations per configuration for -75º<dec<-30º
- 4 concatenations per configuration for dec>-30º
Configurations offered using the Auxiliary Telescopes
The users are requested to provide their chosen AT quadruplet in their proposal at phase 1. The quadruplet cannot be changed after proposal submission.
Configurations offered using the Unit Telescopes
Configurations from previous periods
For reference, the configurations used in the previous periods can be found on this page.
For details on the offered modes please refer to the current Call for Proposals and the VLTI manual. In all cases, please verify your observations with ESO tool VisCalc, or alternatively, with the third party preparation software Aspro2, developped with inputs from ESO.