Hic sunt dracones: Cartography of the Milky Way spiral arms and bar resonances with Gaia Data Release 2. (arXiv:1910.06335v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Khoperskov_S/0/1/0/all/0/1">S. Khoperskov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerhard_O/0/1/0/all/0/1">O. Gerhard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matteo_P/0/1/0/all/0/1">P. Di Matteo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haywood_M/0/1/0/all/0/1">M. Haywood</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Katz_D/0/1/0/all/0/1">D. Katz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khrapov_S/0/1/0/all/0/1">S. Khrapov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khoperskov_A/0/1/0/all/0/1">A. Khoperskov</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arnaboldi_M/0/1/0/all/0/1">M. Arnaboldi</a>

In this paper we introduce a new method for analysing Milky Way phase-space
which allows us to reveal the imprint left by the Milky Way bar and spiral arms
in the stars with full phase-space data in Gaia Data Release 2. The
unprecedented quality and extended spatial coverage of these data enable us to
discover six prominent stellar density structures in the disc to a distance of
5 kpc from the Sun. Four of these structures correspond to the spiral arms
detected previously in the gas and young stars (Scutum-Centaurus, Sagittarius,
Local and Perseus), while the remaining two are associated with two main
resonances of the Milky Way bar. For the first time we provide evidence of the
imprint left by spiral arms and resonances in the stellar densities not relying
on a specific tracer, through a mean of enhancing the signatures left by these
asymmetries. Our method offers new avenues for studying how the stellar
populations in our Galaxy are shaped.

In this paper we introduce a new method for analysing Milky Way phase-space
which allows us to reveal the imprint left by the Milky Way bar and spiral arms
in the stars with full phase-space data in Gaia Data Release 2. The
unprecedented quality and extended spatial coverage of these data enable us to
discover six prominent stellar density structures in the disc to a distance of
5 kpc from the Sun. Four of these structures correspond to the spiral arms
detected previously in the gas and young stars (Scutum-Centaurus, Sagittarius,
Local and Perseus), while the remaining two are associated with two main
resonances of the Milky Way bar. For the first time we provide evidence of the
imprint left by spiral arms and resonances in the stellar densities not relying
on a specific tracer, through a mean of enhancing the signatures left by these
asymmetries. Our method offers new avenues for studying how the stellar
populations in our Galaxy are shaped.

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