A MUSE map of the central Orion Nebula (M 42) ^⋆,⋆⋆

¹ Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
e-mail: pweilbacher@aip.de
² GEPI, Observatoire de Paris, CNRS, Université Paris-Diderot, Place Jules Janssen, 92190 Meudon, France
³ Institut für Astrophysik, Universität Göttingen, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
⁴ ESO, European Southern Observatory, Karl-Schwarzschild Str. 2, 85748 Garching bei München, Germany
⁵ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
⁶ Institut für Physik und Astronomie, Universität Potsdam, 14476 Golm, Germany
⁷ CRAL, Observatoire de Lyon, CNRS, Université Lyon 1, 9 avenue Charles André, 69561 Saint-Genis Laval Cedex, France
⁸ ESO, European Southern Observatory, 3107 Alonso de Córdova, Santiago, Chile
⁹ Instituto de Astrofísica de Canarias (IAC), 38205, La Laguna, Tenerife, Spain
¹⁰ Departamento de Astrofísica, Universidad de La Laguna, 38206, La Laguna, Tenerife, Spain

Received: 13 May 2015
Accepted: 16 August 2015

Abstract

We present a new integral field spectroscopic dataset of the central part of the Orion Nebula (M 42), observed with the MUSE instrument at the ESO VLT. We reduced the data with the public MUSE pipeline. The output products are two FITS cubes with a spatial size of ~5.́9×4.́9 (corresponding to ~0.76 × 0.63 pc²) and a contiguous wavelength coverage of 4595...9366 Å, spatially sampled at 0.́2. We provide two versions with a sampling of 1.25 Å and 0.85 Å in dispersion direction. Together with variance cubes these files have a size of 75 and 110 GiB on disk. They are the largest integral field mosaics to date in terms of information content. We make them available for use in the community. To validate this dataset, we compare world coordinates, reconstructed magnitudes, velocities, and absolute and relative emission line fluxes to the literature values and find excellent agreement. We derive a 2D map of extinction and present de-reddened flux maps of several individual emission lines and of diagnostic line ratios. We estimate physical properties of the Orion Nebula, using the emission line ratios [N ii] and [S iii] (for the electron temperature T_e) and [S ii] and [Cl iii] (for the electron density N_e), and show 2D images of the velocity measured from several bright emission lines.