A MUSE map of the central Orion Nebula (M 42) Article - Octobre 2015

Peter M., Weilbacher, Ana, Monreal-Ibero, Wolfram, Kollatschny, Adam, Ginsburg, Anna F., Mcleod, Sebastian, Kamann, Christer, Sandin, Ralf, Palsa, Lutz, Wisotzki, Roland, Bacon, Fernando, Selman, Jarle, Brinchmann, Joseph, Caruana, Andreas, Kelz, Thomas, Martinsson, Arlette, Pécontal-Rousset, Johan, Richard, Martin, Wendt

Peter M., Weilbacher, Ana, Monreal-Ibero, Wolfram, Kollatschny, Adam, Ginsburg, Anna F., Mcleod, Sebastian, Kamann, Christer, Sandin, Ralf, Palsa, Lutz, Wisotzki, Roland, Bacon, Fernando, Selman, Jarle, Brinchmann, Joseph, Caruana, Andreas, Kelz, Thomas, Martinsson, Arlette, Pécontal-Rousset, Johan, Richard, Martin, Wendt, « A MUSE map of the central Orion Nebula (M 42)  », Chinese Astronomy and Astrophysics, octobre 2015, A114. ISSN 0275-1062

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’x4.9’ (corresponding to 0.76 pc x 0.63 pc) and a contiguous wavelength coverage of 4595...9366 Angstrom, spatially sampled at 0.2". We provide two versions with a sampling of 1.25 Angstrom and 0.85 Angstrom in dispersion direction. Together with variance cubes these files have a size of 75 and 110 GiB on disk. They represent one of 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 and find excellent agreement. We derive a two-dimensional 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 Te) and [S II] and [Cl III] (for the electron density Ne), and show two-dimensional images of the velocity measured from several bright emission lines.

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