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Rotation Measures for Globular Cluster Pulsars ...
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Anna Ho
October 12, 2017
Science
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Rotation Measures for Globular Cluster Pulsars at a Unique Probe of the Galactic Magnetic Field
as presented at galaxy coffee at the MPIA on 9 October 2014
Anna Ho
October 12, 2017
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Transcript
Rota%on Measures for Globular Cluster Pulsars as a Unique
Probe of the Galac%c Magne%c Field Anna Ho Fulbright Scholar, MPIA Galaxy Coffee, 9 October 2014
Rota%on Measures for Globular Cluster Pulsars as a Unique
Probe of the Galac%c Magne%c Field 1. Measuring <B> using RotaHon Measures
Rota%on Measures for Globular Cluster Pulsars as a Unique
Probe of the Galac%c Magne%c Field 1. Measuring <B> using RotaHon Measures 2. Why pulsars in globular clusters?
Rota%on Measures for Globular Cluster Pulsars as a Unique
Probe of the Galac%c Magne%c Field 1. Measuring <B> using RotaHon Measures 2. Why pulsars in globular clusters? 3. CalculaHng pulsar rotaHon measures
Rota%on Measures for Globular Cluster Pulsars as a Unique
Probe of the Galac%c Magne%c Field 1. Measuring <B> using RotaHon Measures 2. Why pulsars in globular clusters? 3. CalculaHng pulsar rotaHon measures 4. Results: mapping <B>
Probing <B> with Rota%on Measures Faraday rota%on:
• λ-‐dependent rotaHon
Faraday rota%on: • λ-‐dependent rotaHon
Dispersion: • λ-‐dependent Hme delay Probing <B> with Rota%on Measures
Probing <B> with Rota%on Measures
Why Pulsars in Globular Clusters? Why Pulsars?
• Strong linear polarizaHon • No intrinsic Faraday rotaHon (Noutsos 2012) Why GC Pulsars? • Dense populaHons -‐> probe small-‐scale structure Terzan 5: 35 MSPs • D=5.9 kpc, l = 3.8º, b = 1.7º • 0.01-‐4 pc separaHon • Precise DMs (Ransom 2007)
Calcula%ng RM • 3 years of Green Bank
Telescope observaHons at L-‐band (1.5 GHz) and S-‐band (2 GHz) totaling > 5 days per pulsar • Least squares fit for RM: Ter5C, single phase bin RM0: 175, dRM: 1.51 +/-‐ 0.06 New RM: 176.51 +/-‐ 0.06 X2 = 1.48
Mapping <B>
None
Extra Slide: GC MSP PopulaHons
Extra Slide: GC ContribuHons
Extra Slide: Structure FuncHon