A nebular analysis of the central Orion nebula with MUSE

Abstract

A nebular analysis of the central Orion nebula and its main structures is presented. We exploit observations from the integral field spectrograph Multi Unit Spectroscopic Explorer (MUSE) in the wavelength range 4595-9366 Å to produce the first O, S and N ionic and total abundance maps of a region spanning 6 arcmin × 5 arcmin with a spatial resolution of 0.2 arcsec. We use theas an indicator of the degree of ionization, to distinguish between the various small-scale structures. The only Orion bullet covered by MUSE is HH 201, which shows a double component in the [Fe II] λ8617 line throughout indicating an expansion, and we discuss a scenario in which this object is undergoing a disruptive event. We separate the proplyds located south of the Bright Bar into four categories depending on their S 23 values, propose the utility of the S 23 parameter as an indicator of the shock contribution to the excitation of line-emitting atoms, and show that the MUSE data are able to identify the proplyds associated with discs and microjets. We compute the second-order structure function for the Hα, [O III] λ5007, [S II] λ6731 and [O I] λ6300 emission lines to analyse the turbulent velocity field of the region covered with MUSE. We find that the spectral and spatial resolution of MUSE are not able to faithfully reproduce the structure functions of previous works.

Star Clusters Near and Far

“…Combining multiple optical gas emission lines (i.e., the Balmer lines or [SII] 6717,6731) lead to the detection of embedded objects in the gas, like Herbig-Haro (HH) jets and bipolar outflows. Recently this has become feasible also outside the Milky Way, namely in the Magellanic Clouds (McLeod et al 2016b(McLeod et al , 2018.…”

Synthetic observations of star formation and the interstellar medium

“…tween galaxies dominated by star formation or by AGN, but the advent of wide-field integral-field spectrographs such as MUSE 28 has lead to the use of this kind of diagnostic becoming more common in the study of Galactic H ii regions (see e.g. McLeod et al, 2015McLeod et al, , 2016.…”

An analysis of the turbulence in the central region of M 42 through structure functions

“…The previous contradicts the conclusion of Mc Leod et al (2016) which blamed the spectral and spatial resolution of M USE for the small exponents they obtained. They also pointed out that because of that, they were not able to reproduce the structure functions of previous works.…”