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

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 pc 2 ) 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 [ (for the electron density N e ), and show 2D images of the velocity measured from several bright emission lines.

HERSCHEL/HIFI SPECTRAL MAPPING OF C+, CH+, AND CH IN ORION BN/KL: THE PREVAILING ROLE OF ULTRAVIOLET IRRADIATION IN CH+ FORMATION

“…The granular nature of the expanding and receding emission sources occurs at scale sizes similar to that measured from Figure 7, and possibly traces local enhancements in the electron density n e . Weilbacher et al (2015) have recently estimated electron temperatures and densities over a region of ∼6′×5′ that covers our observed area, using high-quality spectroscopic observations of Weilbacher et al 2015). Both are broadly consistent in their spatial distribution, but neither exhibits a clumped morphology that correlates very well with our C + observations.…”

Excitation of Molecular Hydrogen in the Orion Bar PhotodissociationRegion from a Deep Near-infrared IGRINS Spectrum

“…We therefore apply an extinction correction of A V = 8.25 or A K = 0.96 to our spectrum before extracting line fluxes. This value of the extinction is consistent with the foreground extinction of A V ∼ 1.3 mag or A K ∼ 0.15 mag towards the ionized gas (Weilbacher et al 2015), allowing for additional extinction between the ionized gas and the region of excited H 2 . Our value for extinction in the Bar is lower than the values of A K = 2.3 ± 0.8 mag and 2.6 ± 0.7 mag for two regions in the Bar ∼ 22 NE of the slit measured by Luhman et al (1998).…”

Serendipitous discovery of a brightening quasar at redshift z = 3.68

“…These zero point discrepancies are usually corrected by applying a zero point offset determined by photometric measurements on imaging data. Note that these discrepancies are not the result of an improper spectrophotometric calibration, which has consistently been shown to be good to within 5% (Weilbacher et al ), but rather they seem to arise from an artifact in the mechanism that the MUSE pipeline uses to extract synthetic photometry from the data cubes.…”

“…Note that these discrepancies are not the result of an improper spectrophotometric F I G U R E 1 MUSE finding chart with WD0308-565 near the center, and the fainter QSO at the lower right area of the image. The redder upper third of the slitlet stack where the standard is located is due to second-order contamination calibration, which has consistently been shown to be good to within 5% (Weilbacher et al 2015), but rather they seem to arise from an artifact in the mechanism that the MUSE pipeline uses to extract synthetic photometry from the data cubes.…”