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Jo-Anne Brown
Observations of the
Galactic Magnetic Fieldfrom the
International Galactic Plane Survey
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People
SGPSCGPS
• 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
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People
SGPSCGPS
• 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
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Outline
Introduction Observations: CGPS Observations: SGPS Summary
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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.
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Faraday Rotation
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Probes of the Field
Pulsars
EGS
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Compact Polarised Sources
Pulsars: 529
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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
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Low-latitude Polarised Sources
Pulsars: 375
EGS: 121
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Low-latitude Polarised Sources
EGS: 121
Pulsars: 375
SGPSCGPS
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Observations
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Canadian Galactic Plane Survey
Pilot Project (PhD): Magdalen Normandeau
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CGPS Region: Pulsars and EGS
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CGPS Region: Pulsars and EGS
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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
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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
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Appropriate Longitude Range
105o
135o
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Previous Studies
Data ranges: Lyne & Smith (1989):105 < l < 135, |b| < 30
Han et al. (1999): 104 < l < 119, |b| < 30
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Path Length Comparison
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CGPS for 105 < l < 135
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Combining Pulsars with CGPS EGS:
No detectablemagnetic field reversal in the outer Galaxy.
Published: ApJ, 592:L29-L32, July 2003
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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
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CGPS Region: Pulsars and EGS
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RM vs Latitude
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RM vs Latitude
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Calculating the Scale Height
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Calculating the Scale Height
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Southern Galactic Plane Survey
PhD Thesis: Naomi Mclure-Griffiths
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SGPS Region: Pulsars and EGS
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SGPS Region: Pulsars and EGS
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Comparing CGPS and SGPS
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RM vs Longitude: SGPS
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RM Modulation by Spiral Arms
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Binsize: 3o Stepsize: 0.5o
Binned CGPS RMs over Stokes I
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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=110o
RM “oscillations” may correlate with HII or arms
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