Rotation of the Milky Way halo in the solar neighborhood based on GAIA DR3 catalog

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Resumo

The rotation of the Milky Way halo in the solar neighborhood is investigated using kinematic data from the GAIA DR3 catalog for RR Lyrae variable stars with parallax errors of less than 20%. Two criteria were used for selecting halo stars — kinematic and spatial. In both approaches, we confirm the existence of weak rotation of the halo in the direction opposite to the rotation of the Galactic disk with velocities of 4.08 ± 2.19 km/s for the kinematic criterion and 9.49 ± 2.59 km/s for the spatial criterion.

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Sobre autores

R. Tkachenko

Southern Federal University

Autor responsável pela correspondência
Email: rtkachenko@sfedu.ru

Institute of Physics

Rússia, Rostov-on-Don

A. Bryndina

Southern Federal University

Email: rtkachenko@sfedu.ru

Institute of Physics

Rússia, Rostov-on-Don

A. Zhmailova

Southern Federal University

Email: rtkachenko@sfedu.ru

Institute of Physics

Rússia, Rostov-on-Don

V. Korchagin

Southern Federal University

Email: rtkachenko@sfedu.ru

Institute of Physics

Rússia, Rostov-on-Don

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2. Fig. 1. Distribution of stars in the galactic coordinate system (l, b), where longitude l = 0 and latitude b = 0 correspond to the position of the galactic center. The scale on the right shows the heliocentric distances of objects d.

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3. Fig. 2. Top row: distribution of RR Lyrae stars in (x, y) and (x, z) spaces. Middle row: histograms of the (d, ∆N) and (Vφ, ∆N) distributions. Bottom: distributions of stars in (Vφ, Vz) and (Lz, E) spaces. The vertical dotted lines separate objects with prograde and retrograde rotation.

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4. Fig. 3. Histogram of the distribution of rotational velocity of halo stars and the distribution of halo stars in space (Lz, E), selected according to kinematic (upper row) and spatial (lower row) criteria.

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5. Fig. 4. Kinematic characteristics of stars selected by kinematic (left column) and spatial (right column) criteria. The distributions of pericenters rperi (upper row), apocenters rapo (middle row) and eccentricities e of stars (lower row) are shown.

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