1. SPECTRA OF GALACTIC COMPONENTS OBSERVED BY WMAP R.D.Davies, R.J.Davis Jodrell Bank Observatory C.Dickinson California Institute of Technology A.J.Banday, T.R.Jaffe MPI fur Astrophysik K.M.Gorski Caltech and JPL Five regions in each of the foregrounds (free-free, synchrotron and anomalous dust) were selected for study which were minimally contaminated by the others. The standard templates (H-alpha, 408 MHz and 100-micron dust) were used in both a T-T and a cross- correlation analysis. The emissivity of each component in the WMAP frequency range was determined. The implications for determining the correction for CMB foreground emission, both in total power and polarization, are discussed.

2. 12-15 September 2005Polarisation 20052

3. 12-15 September 2005Polarisation 20053 THE POSITIONS OF THE 15 REGIONS CHOSEN FOR STUDY Fields 1-5 are free-free; fields 6-10 are dust; fields 11-15 are synchrotron.

4. 12-15 September 2005Polarisation 20054 NOTES ON THE 15 FIELDS

5. 12-15 September 2005Polarisation 20055 FIELD 4 – FREE-FREE DOMINATED l = 250 to 260 b = -25 to -35

6. 12-15 September 2005Polarisation 20056 FIELD 6 – DUST DOMINATED l = 118 to 135 b = +20 to =37

7. 12-15 September 2005Polarisation 20057 FIELD 11 – SYNCHROTRON DOMINATED l = 33 to 45 b = +50 to +70

8. 12-15 September 2005Polarisation 20058 T-T PLOTS FOR FIELD 6 (DUST DOMINATED) The dust correlation for the K, Ka and Q bands

9. 12-15 September 2005Polarisation 20059 THE FREE-FREE EMISSION AT K AND Ka BANDS Comparison for Te = 8000K

10. 12-15 September 2005Polarisation 200510 DUST AND SYNCHROTRON EMISSION IN WMAP BANDS

11. 12-15 September 2005Polarisation 200511 CROSS-CORRLATION RESULTS FOR THE THREE FOREGROUNDS For each foreground the average value is given in each band. There is agreement with the T-T analysis.

12. 12-15 September 2005Polarisation 200512 DUST EMISSIVITIES IN 10 INDIVIDUAL CLOUDS

13. 12-15 September 2005Polarisation 200513 AVERAGE DUST EMISSIVITY (10 CLOUDS) SPARATED INTO VIBRATIONAL AND ANOMALOUS COMPONENTS Index of +1.67 is assumed for vibrational component.

14. 12-15 September 2005Polarisation 200514 CONCLUSIONS The spectra of the free-free and synchrotron components were essentially as expected. For free-free the electron temperature is in the range 7000 – 8000K, with a spectral index of -2.13. The synchrotron spectral index at WMAP frequencies is -3.0 to -3.1. However the anomalous dust emissivity varies by a factor of 2 from cloud to cloud. The construction of an anomalous dust template for Planck will need to account for this varying emissivity. The predicted polarized emission from dust may be similarly affected.