Radio Continuum Studies of Supernova Remnants and Pulsar Wind - - PowerPoint PPT Presentation

Science with the Effelsberg 100-m telescope (Feb 21 2018) – 1 / 22

Radio Continuum Studies of Supernova Remnants and Pulsar Wind Nebulae with the 100-m Effelsberg Telescope

• Dr. Roland Kothes

Dominion Radio Astrophysical Observatory Herzberg Programs in Astronomy and Astrophysics National Research Council Canada February 21, 2018

Why do we care?

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• Supernovae are the most significant source of:
• chemical enrichment
• energy
• cosmic ray acceleration

in the interstellar medium.

Why do we care?

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• Supernovae are the most significant source of:
• chemical enrichment
• energy
• cosmic ray acceleration

in the interstellar medium.

• They compress and amplify magnetic fields and play an

important role in the evolution of our Galaxy.

Why do we care?

Science with the Effelsberg 100-m telescope (Feb 21 2018) – 2 / 22

• Supernovae are the most significant source of:
• chemical enrichment
• energy
• cosmic ray acceleration

in the interstellar medium.

• They compress and amplify magnetic fields and play an

important role in the evolution of our Galaxy.

• Can put constraints on pulsar characteristics, such as age,

velocity, spin axis, progenitor star, and many more.

Evolution of SNRs and PWNe

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Radio Studies of SNRs and PWNe

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Ideal telescope combinations for the study of medium sized SNRs and PWNe:

• Northern Hemisphere:
• Low frequency: DRAO-ST or VLA + Effelsberg
• High Frequency: Effelsberg
• Southern Hemisphere:
• Low frequency: ATCA or VLA + Parkes
• High Frequency: Parkes?

SNR G106.3+2.7 in the NVSS

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Pulsar J2229+6114

SNR G106.3+2.7 in the CGPS

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Pulsar J2229+6114

Discovery of new SNRs: G182.4+4.3

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Effelsberg 11cm Survey: F¨ urst E., Reich W., Reich P ., Reif K., 1990, A&AS 85 691

Discovery of new SNRs: G182.4+4.3

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Effelsberg 6cm Observation Kothes R., F¨ urst E., Reich W., 1998, A&A 331, 661

Discovery of new SNRs: G181.1+9.5

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Kothes R., Reich P ., Foster T.J., Reich W., 2017, A&A 597, A116

• At

rms

• f

100

µK

• r

40 µJy/beam, the most sen- sitive 6cm map every ob- served with a single dish telescope.

• Only SNR known to interact

with high velocity clouds.

Magnetic Environment of SNRs

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Kothes, R. & Brown, J.-A., 2009, IAU Symposium 259, 75

B0 SNR SNR

G182.4+4.3

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G182.4+4.3 in the Milky Way Galaxy

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G182.4+4.3

DA 530 (G93.3+6.9)

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• 100
• 50

rad/m2

DA 530

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G67.7+1.8

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• 170
• 160
• 150
• 140
• 130
• 120
• 110
• 100
• 90
• 80
• 0.2
• 0.1

0.1 0.2 Rotation Measure [rad/m2] Offset [Radius] south north

⇒ Stellar Wind Bubble

Radio Emission from SNR G57.2+0.8

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Kothes R. Sun X., Gaensler B., Reich W., 2018, ApJ 852, 54:

The spectrum of the ”Boomerang”

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The Boomerang PWN

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Kothes R., Landecker T.L., Reich W., Safi-Harb S., Arzoumanian Z., 2008, ApJ 687, 516:

PWN DA 495

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Kothes R., Reich W., Uyanıker B., 2006, ApJ 638, 225:

PWN DA 495

Radio Continuum

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Radio Observations of PWN CTB87

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Kothes R., Reich W., Safi-Harb S., Matheson H., F¨ urst E., 2018:

Radio Observations of PWN CTB87

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Radio Observations of PWN CTB87

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Summary

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• Radio Continuum and Linear Polarization Measurements with the

Effelsberg telescope are essential for the study of Galactic SNRs and PWNe.

• We can study the acceleration of the Cosmic Ray population in

the Galaxy.

• We can use SNRs to probe magnetic environments and draw

conclusions for the large-scale magnetic field in the Galaxy.

• We can estimate important pulsar properties and sometimes

characteristics of the supernova’s progenitor.