Release of pipeline-processed MUSE 3D data cubes by the ESO Science Archive Facility

Published: 22 Jun 2016

All spectra obtained with the Integral Field Unit, Multi-Unit Spectroscopic Explorer, MUSE, in the wide field mode, from November 2014 till May 2015 are now published via the ESO archive as reduced data. The MUSE 3D science data cubes1 have their instrumental signature removed, and are astrometrically calibrated, sky- subtracted, wavelength and flux calibrated, using the MUSE pipeline, version muse-1.4 and higher. The data format is a three dimensional FITS image, with two spatial and one spectral axis in the first extension; see the ESO science data products standard (in particular the addendum dedicated to cubes) for a description of the data format and metadata information. Their wavelength scale is in the heliocentric reference system. All 3D data cubes come with error estimates (in the second extension) and a limiting magnitude estimated as 5σ limiting AB magnitude, in terms of the total flux of an unresolved source (i.e. point source). There are a number of files associated at download time to each 3D data cube, the broad – band image, also known as “ white – light ” image, plus graphical (preview) files and the complete pipeline log. The MUSE data collection will grow with time, with new reduced 3D data cubes being added as soon as they are processed. MUSE 3D cubes spectra acquired before November 2014 will also soon be added to the collection.

The MUSE 3D cubes tagged "MUSE" can be queried and downloaded using the Phase 3 generic query form that provides access to all Phase 3 data. Or the Phase 3 query forms dedicated to spectral data with query parameters suited to harvest 3D cube data.

More details about the data are available in the associated Phase 3 data release description for MUSE data. Instructions on how to read and display 3D data cube spectra in the 3 dimensional FITS image format can be found here

(1) The data cubes are normally stacked at the OB level, unless there is no overlap between the individual exposures. Shallow data cubes from the SKY observations are also processed.