Resolving nearby dust clouds. (arXiv:2004.06732v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Leike_R/0/1/0/all/0/1">R. H. Leike</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Glatzle_M/0/1/0/all/0/1">M. Glatzle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ensslin_T/0/1/0/all/0/1">T. A. Enßlin</a>
Aims: Mapping the interstellar medium in 3D provides a wealth of insights
into its inner working. The Milky Way is the only galaxy, for which a detailed
3D mapping can be achieved in principle. In this paper, we reconstruct the dust
density in and around the local super-bubble.
Methods: The combined data from surveys such as Gaia, 2MASS, PANSTARRS, and
ALLWISE provide the necessary information to make detailed maps of the
interstellar medium in our surrounding. To this end, we use variational
inference and Gaussian processes to model the dust extinction density,
exploiting its intrinsic correlations.
Results: We reconstruct a highly resolved dust map, showing the nearest dust
clouds at a distance of up to 400,pc with a resolution of 1,pc.
Conclusions: Our reconstruction provides insights into the structure of the
interstellar medium. We compute summary statistics of the spectral index and
the 1-point function of the logarithmic dust extinction density, which may
constrain simulations of the interstellar medium that achieve similar
resolution.
Aims: Mapping the interstellar medium in 3D provides a wealth of insights
into its inner working. The Milky Way is the only galaxy, for which a detailed
3D mapping can be achieved in principle. In this paper, we reconstruct the dust
density in and around the local super-bubble.
Methods: The combined data from surveys such as Gaia, 2MASS, PANSTARRS, and
ALLWISE provide the necessary information to make detailed maps of the
interstellar medium in our surrounding. To this end, we use variational
inference and Gaussian processes to model the dust extinction density,
exploiting its intrinsic correlations.
Results: We reconstruct a highly resolved dust map, showing the nearest dust
clouds at a distance of up to 400,pc with a resolution of 1,pc.
Conclusions: Our reconstruction provides insights into the structure of the
interstellar medium. We compute summary statistics of the spectral index and
the 1-point function of the logarithmic dust extinction density, which may
constrain simulations of the interstellar medium that achieve similar
resolution.
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