From Stardust to Planetesimals: Contributed Papers - NASA Lunar ...

Figure 1. M2.2 - M3.45 with ri,,: A grayscaled image of the M2.2 - M3.4s structure with ri,, contoursoverlaid. A 3 Q mask has been applied to the data in both Figure 1 and Figure 2. IRS 1, at (0,0), ismarked by "*". The maximum reddening value of 5 occurs at IRS 1. The south lobe is `blue' and has aT2Ce maximum value of 2.56. The majority of the ice absorption appears to be associated with IRS 1.a point on the nebula and IRS 1. Figure 2 shows scattering enhancements at theeast, south and west lobes. The scattering enhancements are due to either a clearerline of light to IRS 1 or a higher density of scatterers. The scattering enhancementsborder the molecular outflow which is known to have a wide opening angle, and thewest enhancement may be associated with the redshifted molecular outflow (Kastner1994.)4. CONCLUSIONS• The Tice structure suggests that the majority of the water ice is associated withIRS 1. However, a percentage of the T2Ce structure could be due to foregroundextinction.• The M 2.2- M3.45 color has a maximum value of 5.0 at IRS 1. The color and -ri,,structure suggest the presence of an icy-dusty disk around IRS 1.• The strong scattering enhancements in the east and south lobes in Figure 2define the boundary of the cavity produced by the molecular outflow. Thesmall scattering enhancement at the west lobe may be associated with the redshifted molecular outflow (Kastner 1994). The estimated opening angle of theblueshifted outflow from the 2.2 pm data is ti 45°.43