Abstract
This paper reviews the major advances achieved in the Orion Nebula through the use of integral field spectroscopy (IFS). Since the early work of Vasconcelos and collaborators in 2005, this technique has facilitated the investigation of global properties of the nebula and its morphology, providing new clues to better constrain its 3D structure. IFS has led to the discovery of shock-heated zones at the leading working surfaces of prominent Herbig-Haro objects as well as the first attempt to determine the chemical composition of Orion protoplanetary disks, also known asproplyds. The analysis of these morphologies using IFS has given us new insights into the abundance discrepancy problem, a long-standing and unresolved issue that casts doubt on the reliability of current methods used for the determination of metallicities in the universe from the analysis of H II regions. Results imply that high-density clumps and high-velocity flows may play an active role in the production of such discrepancies. Future investigations based on the large-scale IFS mosaic of Orion will be very valuable for exploring how the integrated effect of small-scale structures may have impact at larger scales in the framework of star-forming regions.
Highlights
H II regions are huge volumes of gas associated with recent star formation
The Huygens region is well known for containing hundreds of proplyds [25]. This term depicts a special class of protoplanetary disk, resulting from the evolution of a circumstellar disk in the presence of ionizing radiation from massive OB-type stars, and was coined by O’Dell and collaborators [26] to describe the silhouette and tear-drop shaped objects observed in the first imaging studies of the Orion Nebula using the Hubble Space Telescope (HST)
The aim of the present review is to summarize the recent advances that have been achieved in the Orion Nebula through the use of the integral field spectroscopy (IFS)
Summary
H II regions are huge volumes of gas associated with recent star formation. These gaseous clouds are mainly ionized and heated by the stellar ultraviolet (UV) radiation emitted by nearby OB-type stars. Reality turns out to be much more complicated, and such regions are found to be highly structured at all scales with complex internal motions Their morphology results from the structure of the parent molecular cloud, which is affected over time by the UV radiation, stellar winds, or high-velocity ejections associated with star-formation phenomena. The Huygens region is well known for containing hundreds of proplyds [25] This term depicts a special class of protoplanetary disk, resulting from the evolution of a circumstellar disk in the presence of ionizing radiation from massive OB-type stars, and was coined by O’Dell and collaborators [26] to describe the silhouette and tear-drop shaped objects observed in the first imaging studies of the Orion Nebula using the Hubble Space Telescope (HST). IFS studies in the Orion Nebula have found new and interesting clues in the context of this problem, which are reviewed here
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