MUSE p2 Tutorial
IMPORTANT: General guidelines for the preparation of Phase 2 material with p2 can be found here
This tutorial provides guidelines on how to prepare a set of Observation Blocks (OBs) with MUSE, the Multi Unit Spectroscopic Explorer on UT4 (Yepun) of the VLT. The specifics of this tutorial pertain to the preparation of OBs for Period 102 onwards.To follow this tutorial you should have familiarity with p2 : the web-based tool for the preparation of Phase 2 materials. Please refer to the main p2 webpage (and the items in the menu bar on the left of that page) for a general overview of p2 and generic instructions on the preparation of Observing Blocks (OB). Screenshots for this tutorial were made using the demo mode of p2, but should not differ in any way from one's experience in preparing your own OBs under your run.
Observations at the VLT are performed in terms of Observing Block (OB), which represents the basic observational unit. As such, astronomers specify their programmes in terms of OBs, which contain all the necessary information to obtain a single observation. Observations with MUSE are therefore performed through dedicated OBs that contain both general and MUSE specific information. In what follows we concentrate on the main MUSE specific information required to construct an OB, while for a quick summary of the general ESO Phase 2 material (i.e. details of the OB that are not instrument dependent) we refer the reader to this page.
- FoV= 59.9" x 60", pixel scale 0.25"Nominal filter: 480 - 930 nmExtended filter: 465 - 930 nm
- FoV=59.9" x 60", pixel scale 0.25"Nominal filter: 480 - 582 nm and 597 - 930 nmExtended filter: 465 - 576 nm and 601 - 930 nmFor the full AO mode (i.e. laser and TTS) the TTS must be located between 52" and 107" off axis and must be brighter than R=17.5 mag.A TTS-free mode is also offered
- FoV=7.42" x 7.43", pixel scale 25 masNominal filter: 480 - 578 nm and 605 - 930 nmNGS magnitude range: 5.5<J<19 (If requested Turbulence category is 10%, the airmass below 1.2 and the separation between target and NGS is smaller than 3"), brighter J-band limits apply otherwiseThe NGS must be located within 5.0" from the center of the FoV. No NGS-free mode is available
Observations with MUSE can be performed in the following modes:
The following table lists, for each observing mode, the available acquisition and observing templates
||Acquisition template||Observing template|
In your proposal you have already indicated the mode, and the time you need to fulfill your science goal. This was done by consulting the MUSE User Manual and the Exposure Time Calculator. Hence, at this point, when preparing your MUSE OB the most important decision you have to make regards the observing strategy:
- Number of on-source exposures
- how monitoring the sky background
- WFM-NOAO observations of sparse field (Strategy: on-target dithering and accurate target centering)
- WFM-NOAO observations of extended object (Strategy: off-target sky monitoring, simple preset and mosaicking a large area)
- WFM-AO observations of sparse field (Strategy: on-target dithering and accurate target centring)
- WFM-AO observations of extended object (Strategy: off-target sky monitoring)
- NFM on-axis observation of dense field (Strategy: on-target rotations+dithering, and off-target sky monitoring)
By logging into the p2 demo, under the programme ID 60.A-9253(R) you can access to the USD-Tutorials folder where we have stored a sample of OBs designed for different modes and observing strategy. The example OBs are not editable but can be exported if needed. Please refrain from creating new OBs in the USD-Tutorials folder.