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Quantifying the Magnetic Alignment of Hi and Dust in the Diffuse ISM

Part of: IAU Issue 315 - From Interstellar Clouds...

Published online by Cambridge University Press:  12 September 2016

S.E. Clark ,
J.E.G. Peek ,
J. Colin Hill  and
M.E. Putman
S.E. Clark
Affiliation:
Department of Astronomy, Columbia University, New York, NY 10027
J.E.G. Peek
Affiliation:
Space Telescope Science Institute, Baltimore, MD 21218
J. Colin Hill
Affiliation:
Department of Astronomy, Columbia University, New York, NY 10027
M.E. Putman
Affiliation:
Department of Astronomy, Columbia University, New York, NY 10027
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Abstract

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Sensitive, high resolution observations of Galactic neutral hydrogen (Hi) reveal an intricate network of slender linear features, much as sensitive surveys of dust in Galactic molecular clouds reveal ubiquitous filamentary structure. Across the high Galactic latitude sky, diffuse Histructures are aligned with the interstellar magnetic field, as revealed by background starlight polarization (Clark, Peek, & Putman 2014) and by Planck 353 GHz polarized dust emission (Clark et al. 2015). These discoveries were enabled by the Rolling Hough Transform, a recently developed, open source machine vision algorithm.

Keywords

magnetic fieldspolarizationISM: structure
Type
Poster Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S315: From Interstellar Clouds to Star-Forming Galaxies: Universal Processes? , August 2015 , E13
Copyright
Copyright © International Astronomical Union 2016 

References

André, Ph., Men'shchikov, A., Bontemps, S. et al. 2010, Astron. Astrophys., 518, L102 Google Scholar
Cabral, B. & Leedom, L. C., 1993, in Computer Graphics Proc., ACM SIGGRAPH, 263Google Scholar
Clark, S.E., Peek, J.E.G., & Putman, M.E. 2014, Astrophys. J., 789, 82 CrossRefGoogle Scholar
Clark, S.E., Hill, J. Colin, Peek, J.E.G., Putman, M.E. et al. 2015, Phys. Rev. Lett., 115, 241302 Google Scholar
Heiles, C. 2000, Astron. J., 119, 923 Google Scholar
Koch, E. W. & Rosolowsky, E.W. 2015, Mon. Not. R. Astron. Soc., 452, 3435 Google Scholar
McClure-Griffiths, N. M., Dickey, J. M., Gaensler, B. M., et al. 2006, Astrophys. J., 652, 1339 Google Scholar
Peek, J. E. G., Heiles, C., Douglas, K. A., et al. 2011, Astrophys. J. Suppl., 194, 20 Google Scholar
Planck Collaboration 2015, Astron. Astrophys. 576, A104 Google Scholar
Planck Collaboration, Astron. Astrophys. submitted arXiv:1409.6728Google Scholar
Soler, J. D., Hennebelle, P., Martin, P. G., et al. 2013, Astrophys. J., 774, 128 CrossRefGoogle Scholar
Sousbie, T. 2011, Mon. Not. R. Astron. Soc., 414, 350 Google Scholar