[Fe ii ] 1.257 μm and He i 1.083 μm Emission in the Central Region of the Orion Nebula: H ii Region, HH Flows, Jets, and Proplyds
Year: 2002
Type: article
Abstract: The [Fe II] 1.257 μm and He I 1.083 μm emission lines were observed in the central 6' × 8' region of the Orion Nebula, and their excitation in the photoionized H II region, HH flows, jets, and proplyds is investigated. Observations were carried out using the imaging Fabry-Perot spectrometer MUSE at the National Astronomical Observatory of Japan 1.5 m infrared telescope, which provides a 4' × 4' field of view and a spectral resolution λ/δλ of ~2000 at the observed wavelengths. The [Fe II] images exhibit (1) filamentary structures and diffuse emission, which presumably arise from ionization fronts of the photoionized H II region, and (2) a number of knots, some of which are newly identified. Centroidal velocities in most of the knots are negative relative to those in the ionization fronts by up to -60 km s -1 , and observed line profiles in the bright knots exhibit blueshifted wings, agreeing with bow shock models. The He I 1.083 μm emission in the observed region is dominated by the photoionized H II region, and its distribution reflects the complicated nature of the excitation. The He I images also contain blueshifted emission from several HH flows and jets and redshifted emission associated with proplyds. Our results for the shocks suggest that the [Fe II] 1.257 μm and He I 1.083 μm emission reflects the ionization of the preshock gas: the [Fe II] 1.257 μm emission is prominent in shocks propagating in molecular/atomic gas, while the He I 1.083 μm is prominent in shocks in the photoionized H II region. Different line excitation in these shocks can be explained by the following physical properties and processes: (1) difference of the excitation energies from the ground state (1 and 20 eV for the [Fe II] and He I lines, respectively), (2) resonance scattering and collisional excitation from the metastable state, enhancing the He I 1.083 μm line in shocks in the photoionized H II region, (3) a large photoionization cross section of Fe + , causing the absence of the [Fe II] emission in the same shocks, and possibly (4) charge exchange reactions of Fe, which could enhance the [Fe II] emission in neutral gas.
Source: The Astrophysical Journal
DOI: 10.1086/338245
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: bronze
OpenAlex ID: W2018744070