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Can we detect Galactic spiral arms? 3D dust distribution in the Milky Way

Published online by Cambridge University Press:  07 March 2018

Sara Rezaei Kh. Open the ORCID record for Sara Rezaei Kh. [Opens in a new window] ,
Coryn A. L. Bailer-Jones ,
Morgan Fouesneau  and
Richard Hanson
Sara Rezaei Kh.
Affiliation:
Max Planck Institute for Astronomy (MPIA), Königstuhl 17, 69117 Heidelberg, Germany email: sara@mpia.de
Coryn A. L. Bailer-Jones
Affiliation:
Max Planck Institute for Astronomy (MPIA), Königstuhl 17, 69117 Heidelberg, Germany email: sara@mpia.de
Morgan Fouesneau
Affiliation:
Max Planck Institute for Astronomy (MPIA), Königstuhl 17, 69117 Heidelberg, Germany email: sara@mpia.de
Richard Hanson
Affiliation:
Max Planck Institute for Astronomy (MPIA), Königstuhl 17, 69117 Heidelberg, Germany email: sara@mpia.de
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Abstract

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We present a model to map the 3D distribution of dust in the Milky Way. Although dust is just a tiny fraction of what comprises the Galaxy, it plays an important role in various processes. In recent years various maps of dust extinction have been produced, but we still lack a good knowledge of the dust distribution. Our presented approach leverages line-of-sight extinctions towards stars in the Galaxy at measured distances. Since extinction is proportional to the integral of the dust density towards a given star, it is possible to reconstruct the 3D distribution of dust by combining many lines-of-sight in a model accounting for the spatial correlation of the dust. Such a technique can be used to infer the most probable 3D distribution of dust in the Galaxy even in regions which have not been observed. This contribution provides one of the first maps which does not show the “fingers of God” effect. Furthermore, we show that expected high precision measurements of distances and extinctions offer the possibility of mapping the spiral arms in the Galaxy.

Keywords

Stars: ParallaxesStars: DistancesGalaxy: Dust MapGalaxy: Milky WayISM: DustISM: Extinction
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S330: Astrometry and Astrophysics in the Gaia sky , April 2017 , pp. 189 - 192
Copyright
Copyright © International Astronomical Union 2018 

References

Astraatmadja, T. L. & Bailer-Jones, C. A. L., 2016, ApJ, 833, 119 CrossRefGoogle Scholar
Bovy, J., Nidever, D. L., Rix, H.-W. et al., 2014, ApJ, 790, 127 CrossRefGoogle Scholar
Gaia Collaboration et al., 2016, A&A, 595, A2 Google Scholar
Green, G. M., Schlafly, E. F., Finkbeiner, D. P. et al. 2015, ApJ, 810, 25 CrossRefGoogle Scholar
Hanson, R. J. & Bailer-Jones, C. A. L., 2014, MNRAS, 438, 2938 CrossRefGoogle Scholar
Hanson, R. J., Bailer-Jones, C. A. L., Burgett, W. S. et al. 2016, MNRAS, 463, 3604 CrossRefGoogle Scholar
{Lallement, R., Vergely, J.-L., Valette, B., Puspitarini, L., Eyer, L., & Casagrande, L., 2014, A&A, 561, A91 Google Scholar
Majewski, S. R., Zasowski, G., & Nidever, D. L., 2011, ApJ, 739, 25 CrossRefGoogle Scholar
Marshall, D. J., Robin, A. C., Reyl, C., Schultheis, M., & Picaud, S., 2006, A&A, 453, 635 Google Scholar
Reid, M. J., Menten, K. M., Brunthaler, A. et al. 2014, ApJ, 783, 130 CrossRefGoogle Scholar
Rezaei Kh., S., Bailer-Jones, C. A. L., Hanson, R. J., & Fouesneau, M., 2017, A&A, 598, A125 Google Scholar
Sale, S. E., Drew, J. E., Barentsen, G. et al. 2014, MNRAS, 443, 2907 CrossRefGoogle Scholar
Schlafly, E. F., Green, G., Finkbeiner, D. P. et al. 2014, ApJ, 786, 29 CrossRefGoogle Scholar
Schlegel, D. J., Finkbeiner, D. P., & Davis, M., 1998, ApJ, 500, 525 CrossRefGoogle Scholar
Zasowski, G., Johnson, J. A., & Frinchaboy, P. M., 2013, AJ, 146, 81 CrossRefGoogle Scholar