1. FGS/NIRISS Science Team Meeting October 20th & 21st 2015: Montréal Neil Rowlands COM DEV Dust & transition from AGB to proto-planetary nebulae with AMI 1

2. FGS/NIRISS Science Team Meeting October 20th & 21st 2015: Montréal The AGB – proto - PNe Linkage 2 IRAS Selected V & I images (most 3-4” on a side) Stellar ‘SOLE’ ‘DUPLEX’

3. FGS/NIRISS Science Team Meeting October 20th & 21st 2015: Montréal Spectral Energy Distributions 3 SEDs for ‘SOLE’ Objects SEDs for Stellar Objects

4. FGS/NIRISS Science Team Meeting October 20th & 21st 2015: Montréal AMI vs NIRCam LW Filters 4 3.3 µm PAH feature is of interest / Can AMI Mode use the 356W filter?

5. FGS/NIRISS Science Team Meeting October 20th & 21st 2015: Montréal Discussion Could be a good demonstration of AMI mode on extended objects Assuming that contrast of ~10 -2 at 65 mas is feasible (Ford etal 2014) Angular resolution in the MWIR comparable to Hubble visible images ‘Known’ objects – low risk and have complementary visible images / data for comparison & ‘calibration’. Objective: Determine the connection between nebular morphology & the chemical and physical properties of their central stars (no correlation found with visible/NIR data). Evolutionary history & origins of PNe asymmetry Better correlate dredge up history with nebular abundances Carbon / Oxygen / Silicon production Next Steps / Questions to address (just a start!) Object selection - thorough review of AGB/PNe candidate lists At least some objects should have Spitzer & ALMA image data Are observations with different field rotations needed? How should calibrators be selected? How often do they to be observed? Is there a SNR model available yet for AMI mode? 5