1. Jo-Anne Brown Observations of the Galactic Magnetic Field from the International Galactic Plane Survey

2. People SGPS CGPS Russ Taylor Tom Landecker Andrew Gray Rob Reid Roland Kothes Dave Delrizzo Bulent Uyaniker Marta Peracaula Marijke Haverkorn Bryan Gaensler Natalya Bizunok Naomi McClure-Griffiths John Dickey Anne Green

3. People SGPS CGPS Russ Taylor Tom Landecker Andrew Gray Rob Reid Roland Kothes Dave Delrizzo Bulent Uyaniker Marta Peracaula Marijke Haverkorn Bryan Gaensler Natalya Bizunok Naomi McClure-Griffiths John Dickey Anne Green

4. Outline  Introduction  Observations: CGPS  Observations: SGPS  Summary

5. The Galactic Magnetic Field field is concentrated in disk follows the spiral arms local field is cw Sagittarius field is ccw additional reversals unclear Determining the location of reversals may help understand the evolution of the field.

6. Faraday Rotation

7. Probes of the Field Pulsars EGS

8. Compact Polarised Sources Pulsars: 529

9. Compact Polarised Sources Pulsars: 529 EGS: 887 First Large Catalog of EGS (555 sources): Simard-Normandin, M, P. P. Kronberg, Button, S (1981) ApJS, 45, 91

10. Low-latitude Polarised Sources Pulsars: 375 EGS: 121

11. Low-latitude Polarised Sources EGS: 121 Pulsars: 375 SGPS CGPS

12. Observations

13. Canadian Galactic Plane Survey Pilot Project (PhD): Magdalen Normandeau

14. CGPS Region: Pulsars and EGS

16. Science with the CGPS Field Alignment with the spiral arms Reversals in the outer Galaxy Small-scale field correlation with the large-scale field. Latitude Dependence

17. Science with the CGPS Field Alignment with the spiral arms Reversals in the outer Galaxy Small-scale field correlation with the large-scale field. Latitude Dependence

18. Appropriate Longitude Range 105 o 135 o

19. Previous Studies Data ranges: Lyne & Smith (1989):105  < l < 135 , |b| < 30  Han et al. (1999): 104  < l < 119 , |b| < 30 

20. Path Length Comparison

21. CGPS for 105  < l < 135 

22. Combining Pulsars with CGPS EGS: No detectable magnetic field reversal in the outer Galaxy. Published: ApJ, 592:L29-L32, July 2003

23. Science with the CGPS Field Alignment with the spiral arms Reversals in the outer Galaxy Small-scale field correlation with the large-scale field. Latitude Dependence

24. CGPS Region: Pulsars and EGS

25. RM vs Latitude

27. Calculating the Scale Height

29. Southern Galactic Plane Survey PhD Thesis: Naomi Mclure-Griffiths

30. SGPS Region: Pulsars and EGS

32. Comparing CGPS and SGPS

33. RM vs Longitude: SGPS

34. RM Modulation by Spiral Arms

35. Binsize: 3 o Stepsize: 0.5 o Binned CGPS RMs over Stokes I

36. Summary  IGPS has yielded much needed EG RMs - 1078 (so far) in CGPS I,II,III - 149 in SGPS (depolarization)  No B-Field reversals in the Outer Galaxy  Rough calculations show magneto-ionic scale height of ~1.2 kpc at l=110 o  RM “oscillations” may correlate with H II or arms