Vasconcelos and collaborators [27] were the first using IFS in the Huygens region, focusing on the LV2 proplyd (see Figure 1) and, mainly, on its microjet.
In the work of Tsamis and Walsh, an accurate study of the surface brightness distributions of the red- and blue-shifted lobes in H[alpha], H[gamma], and [Fe III] 4658 [Angstrom] led the authors to conclude that the bipolar jet is being ejected in a projected axis almost perpendicular to the tail of the LV2 proplyd. From this result, it is clear that the use of IFS combined with high spectral resolution is a refined technique that can reveal unexpected properties that, on the other hand, would remain hidden--or would be more difficult to identify--under the view of the classical slit spectroscopy.
Morisset, "Gemini multi-object spectrograph integral field unit spectroscopy of the 167-317 (LV2) proplyd in orion," Astronomical Journal, vol.
Lopez, "Mass loss and jet outflow in the Orion Nebula proplyd LV 2," Astrophysical Journal Letters, vol.
Early evidence that proplyds exist in Orion includes some narrow-band images of the Trapezium from 1979 that show six unresolved stars with only emission lines.
The true nature of proplyds became clear after Hubble first observed this region in August 1991, and follow-up observations were made immediately after the telescope's refurbishment in December 1993.
The visible-light Hubble images reveal stars in a significant fraction of the proplyds. This has been confirmed by a recent near-infrared survey by Mark McCaughrean (Max Planck Institute) and Stauffer, in which low-mass, pre-main-sequence stars are seen in essentially all of the proplyds.