1. Color Maps of the Ohio State University Bright Spiral Galaxy Survey Melissa Butner, Austin Peay State University Susana Deustua, advisor

2. Goal Investigate the distribution and properties of the interstellar medium: dust and gas, and of the stellar population in each galaxy by undertaking a pixel by pixel analysis. Questions we are interested in: what is the star formation rate? how is the dust distributed and how does this affect extinction? how do these properties compare to other spiral galaxies?

3. The OSUBSGS The Ohio State University Bright Spiral Galaxy Survey ~200 spiral galaxies B <= 12 Selected from RC3 BVRJHK band images D < 6.5’ −80 ◦ < δ < +50 ◦ (due to observational limits)

4. Advantages of using Multi-wavelength Data Extinction measurement is independent of the dust temperature. Probe the temperatures and masses of the dust components to better constrain the heating mechanism for the dust. Helps in separating star and dust contributions to galaxy emission

5. Steps for pixel based analysis Align (register) images Match PSFs Determine flux and color for each pixel in each galaxy Use Pixel z or similar code to determine the spectral energy distribution of stars (from models of star formation) Use color maps to see the distribution of ISM components Compare SED and color maps

6. ic5235 Before Registration B imageJ image Image Size - 6.8’ x 6.8 ‘ Pixel Scale – 0.40 “/pixel Image Size – 4.4’ x 4.6’ Pixel Scale – 1.16 “/pixel

7. ic5325 After Registration B imageJ image

8. PSF Match ImageFWHM Before FWHM After B6.84 V6.586.07 R6.046.30 J4.5821.31 ? H4.665.73 K4.775.74

9. Color Maps BV B - V

10. Color Maps B – K B K

11. Future Work Finish registering Apply technique of Matching PSFs and generating color maps. Determine the spectral energy distribution Compare color maps with SED