Magnetic Field Lines in M51 |
 | Minimum credit line: Image courtesy of NRAO/AUI
(for details, see .
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The total radio continuum emission from the "whirlpool" galaxy M51
(distance estimates range between 13 and 30 million light years) is
strongest at the inner edges of the optical spiral arms, probably due
to the compression of magnetic fields by density waves. The vectors
give the orientations of the regular magnetic fields as derived from
the polarized emission. The field lines follow nicely the optical
spiral arms. Unexpectedly, strong polarized emission is observed also
between the optical arms which indicates the action of a dynamo.
This image was observed with the VLA in its most compact
configuration at 6cm radio wavelength (broadband continuum). As the VLA cannot detect the diffuse, large-scale radio emission, data from the Effelsberg 100-m telescope in Germany at the same wavelength was added. Investigator(s): Rainer Beck (MPIfR Bonn, Germany), Cathy Horellou (Onsala Space This image is available in the following downloadable versions:
- 392 x 229
- 613 x 358
- 1226 x 715
If you would like to obtain a higher resolution version of this image,
please contact .
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Telescope
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VLA
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Date of Observation
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1991-04-00
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Type of Observation
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Continuum Observations
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Band
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C
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Wavelength
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6 cm
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Frequency
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5.0 GHz
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Center of Image
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RA: 13:29:52.37, Dec: 47:11:40.80 (J2000)
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Field of View
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0.1667 x 0.2000 degrees
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Technical Caption
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VLA in D-array. VLA observations made 1991 March 23 and 1991 April 1; Effelsberg observations made summer 1996. VLA resolution 15\"; data from Effelsberg adds 2.5 minutes of arc.
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