Moving Groups Across Galactocentric Radius with Gaia DR3. (arXiv:2206.10633v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Lucchini_S/0/1/0/all/0/1">Scott Lucchini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pellett_E/0/1/0/all/0/1">Emil Pellett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DOnghia_E/0/1/0/all/0/1">Elena D&#x27;Onghia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguerri_J/0/1/0/all/0/1">J. Alfonso L. Aguerri</a>

The kinematic plane of stars near the Sun has proven an indispensable tool
for untangling the complexities of the structure of our Milky Way (MW). With
ever improving data, numerous kinematic “moving groups” of stars have been
better characterized and new ones continue to be discovered. Here we present an
improved method for detecting these groups using MGwave, a new open-source 2D
wavelet transformation code that we have developed. Our code implements similar
techniques to previous wavelet software; however, we include a more robust
significance methodology and also allow for the investigation of underdensities
which can eventually provide further information about the MW’s
non-axisymmetric features. Applying MGwave to the latest data release from Gaia
(DR3), we detect 45 groups of stars with coherent velocities. We reproduce the
majority of the previously detected moving groups in addition to identifying
four additional significant candidates: one near Antoja12-GCSIII-13, one near
GMG 5, and two with very low $V_r$ and similar $V_phi$ to Hercules. Finally,
we have followed these associations of stars beyond the solar neighborhood,
from Galactocentric radius of 6.5 to 10~kpc. Most detected groups are extended
throughout radius indicating that they are streams of stars possibly due to
non-axisymmetric features of the MW.

The kinematic plane of stars near the Sun has proven an indispensable tool
for untangling the complexities of the structure of our Milky Way (MW). With
ever improving data, numerous kinematic “moving groups” of stars have been
better characterized and new ones continue to be discovered. Here we present an
improved method for detecting these groups using MGwave, a new open-source 2D
wavelet transformation code that we have developed. Our code implements similar
techniques to previous wavelet software; however, we include a more robust
significance methodology and also allow for the investigation of underdensities
which can eventually provide further information about the MW’s
non-axisymmetric features. Applying MGwave to the latest data release from Gaia
(DR3), we detect 45 groups of stars with coherent velocities. We reproduce the
majority of the previously detected moving groups in addition to identifying
four additional significant candidates: one near Antoja12-GCSIII-13, one near
GMG 5, and two with very low $V_r$ and similar $V_phi$ to Hercules. Finally,
we have followed these associations of stars beyond the solar neighborhood,
from Galactocentric radius of 6.5 to 10~kpc. Most detected groups are extended
throughout radius indicating that they are streams of stars possibly due to
non-axisymmetric features of the MW.

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