[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

Details [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 [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

Feb 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...566..910t&link_type=abstract

The Astrophysical Journal, Volume 566, Issue 2, pp. 910-924.

Astronomy and Astrophysics

Astronomy

13

Ism: H Ii Regions, Infrared: Ism, Ism: Individual (Orion Nebula), Stars: Formation

Scientific paper

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.

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