1. Young Star Disk Evolution in the Planet Formation Epoch Gregory Mace Mentor: Lisa Prato Northern Arizona University Physics and Astronomy

2. Introduction Circumstellar Disk Evolution Reference: JPL http://www.spitzer.caltech.edu/Media/041209telecon/visuals.shtml

3. Introduction IC 348 and NGC 2264  Young – 2.3 and 3.2 Myr  Nearby – 320 and 760 pc. (1pc = 3.2616 light-years)  Infrared Observations:  2MASS Survey Data  Spitzer Space Telescope Data  My Own Ground-Based Data

4. Introduction Why infrared? Reference: Web http://www.astro.helsinki.fi/~lehtinen/Work/DC303.html

5. Observations 1.8 meter Perkins Telescope Mimir – J (1.25 μm), H (1.635 μm),. K (2.20 μm) L,M bands planned 11.5 observing nights : 6 partially/fully photometric

6. Research Progression Literature Review Target Field Selection and Observing Run Preparation Learned how to run Mimir and do on-site Engineering Developing photometry software package –Series of Customized IDL Procedures Data Reduction Color Transformations to Standard 2MASS System

7. Results

8. Future Plans Complete Photometry of All Photometric Fields Compare to 2MASS –Variability Combine data with longer wavelength Spitzer data –Better identify the presence of disks Compute disk fractions (if able to get statistical sample)

9. Conclusions Near-Infrared Essential for Observing Planet-Forming Disks Young Clusters are Ideal for Observing the Planet Formation Epoch Quality of Observational Data Dependent on Numerous Conditions NGC 2264 has Larger Extinction which Supports Further Distance IC 348 has Larger Excesses which Supports its Younger Age