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The Astrophysical Journal (ApJ)

Resumen/Descripción – provisto por la editorial en inglés

The Astrophysical Journal is an open access journal devoted to recent developments, discoveries, and theories in astronomy and astrophysics. Publications in ApJ constitute significant new research that is directly relevant to astrophysical applications, whether based on observational results or on theoretical insights or modeling.

Palabras clave – provistas por la editorial

astronomy; astrophysics

Disponibilidad

Institución detectada	Período	Navegá	Descargá	Solicitá
No detectada	desde jul. 1995 / hasta dic. 2023	IOPScience

Información

Tipo de recurso:

revistas

ISSN impreso

0004-637X

ISSN electrónico

1538-4357

Editor responsable

American Astronomical Society (AAS)

Idiomas de la publicación

inglés

País de edición

Reino Unido

Información sobre licencias CC

https://creativecommons.org/licenses/by/4.0/

Cobertura temática

Ciencias físicas

Tabla de contenidos

doi: 10.3847/1538-4357/ac04b5

Dynamical Model of the Milky Way Using APOGEE and Gaia Data

Maria Selina Nitschai; Anna-Christina Eilers; Nadine Neumayer; Michele Cappellari; Hans-Walter Rix

<jats:title>Abstract</jats:title> <jats:p>We construct a dynamical model of the Milky Way disk from a data set that combines Gaia EDR3 and APOGEE data throughout galactocentric radii in the range 5.0 kpc ≤ <jats:italic>R</jats:italic> ≤ 19.5 kpc. We make use of the spherically aligned Jeans anisotropic method to model the stellar velocities and their velocity dispersions. Building upon our previous work, our model is now fitted to kinematic maps that have been extended to larger galactocentric radii due to the expansion of our data set, probing the outer regions of the Galactic disk. Our best-fitting dynamical model suggests a logarithmic density slope of <jats:italic>α</jats:italic> <jats:sub>DM</jats:sub> = −1.602 ± 0.079<jats:sub>syst</jats:sub> for the dark matter halo and a dark matter density of <jats:italic>ρ</jats:italic> <jats:sub>DM</jats:sub>(<jats:italic>R</jats:italic> <jats:sub>⊙</jats:sub>) = (8.92 ± 0.56<jats:sub>syst</jats:sub>) × 10<jats:sup>−3</jats:sup> <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> pc<jats:sup>−3</jats:sup> (0.339 ± 0.022<jats:sub>syst</jats:sub> GeV cm<jats:sup>3</jats:sup>). We estimate a circular velocity at the solar radius of <jats:italic>v</jats:italic> <jats:sub>circ</jats:sub> = (234.7 ± 1.7<jats:sub>syst</jats:sub>) km s<jats:sup>−1</jats:sup> with a decline toward larger radii. The total mass density is <jats:italic>ρ</jats:italic> <jats:sub>tot</jats:sub>(<jats:italic>R</jats:italic> <jats:sub>⊙</jats:sub>) = (0.0672 ± 0.0015<jats:sub>syst</jats:sub>) <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> pc<jats:sup>−3</jats:sup> with a slope of <jats:italic>α</jats:italic> <jats:sub>tot</jats:sub> = −2.367 ± 0.047<jats:sub>syst</jats:sub> for 5 kpc ≤ <jats:italic>R</jats:italic> ≤ 19.5 kpc, and the total surface density is Σ(<jats:italic>R</jats:italic> <jats:sub>⊙</jats:sub>, ∣<jats:italic>z</jats:italic>∣ ≤ 1.1 kpc) = (55.5 ± 1.7<jats:sub>syst</jats:sub>) <jats:italic>M</jats:italic> <jats:sub>⊙</jats:sub> pc<jats:sup>−2</jats:sup>. While the statistical errors are small, the error budget of the derived quantities is dominated by the three to seven times larger systematic uncertainties. These values are consistent with our previous determination, but the systematic uncertainties are reduced due to the extended data set covering a larger spatial extent of the Milky Way disk. Furthermore, we test the influence of nonaxisymmetric features on our resulting model and analyze how a flaring disk model would change our findings.</jats:p>

Palabras clave: Space and Planetary Science; Astronomy and Astrophysics.

Pp. 112