On this page, we list the main changes that affected the instrument and this web site.
Period 102: Some changes in the operations of the VLT and VLTI affect PIONIER, but are not specific to it:
First, the use of the p2pp software is phased out.In P102, VM and SM observations have to be prepared with p2 (http://www.eso.org/sci/observing/phase2/p2intro.html) for all VLT and VLTI instruments.
Second, in P102, a new operation scheme designed to stimulate the production of quality interferometric images will be tested at VLTI. The main goal of these operations is to fill the (u,v) spatial frequency plane in an optimized way to reconstruct interferometric images more easily and with more reliability. Users are referred to the VLTI User Manual and the Call for Proposals for more information.
Period 98:The optimum calibration strategy with respect to calibrator magnitude has been described in some more detail in the "Instrument Overview"
Period 95/ VLTI Lab refurbishment: PIONIER will be removed from its current location to make space for GRAVITY and mounted back above the FINITO fringe tracker table with periscope optics to inject the light into PIONIER. As part of this project, PIONIER will be integrated more tightly into the VLTI IT infrastructure, including daily calibration procedures that will result in public instrument health and quality control pages, as for other instruments.
December 2014: The PICNIC detector was replaced by the RAPID detector. This impoved both the sensitivity and read-out speed, making the instrument more robust against bad observing conditions. At the same time, the dispersive optics was replaced, so that now only two dispersion modes, GRISM (6 pixels) and FREE (1 pixel), are available.