Weighing the Galactic disk using phase-space spirals: I. Tests on one-dimensional simulations

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Weighing the Galactic disk using phase-space spirals : I. Tests on one-dimensional simulations. / Widmark, A.; Laporte, C.; de Salas, P. F.

In: Astronomy & Astrophysics, Vol. 650, A124, 21.06.2021.

Research output: Contribution to journalJournal articleResearchpeer-review

Harvard

Widmark, A, Laporte, C & de Salas, PF 2021, 'Weighing the Galactic disk using phase-space spirals: I. Tests on one-dimensional simulations', Astronomy & Astrophysics, vol. 650, A124. https://doi.org/10.1051/0004-6361/202140650

APA

Widmark, A., Laporte, C., & de Salas, P. F. (2021). Weighing the Galactic disk using phase-space spirals: I. Tests on one-dimensional simulations. Astronomy & Astrophysics, 650, [A124]. https://doi.org/10.1051/0004-6361/202140650

Vancouver

Widmark A, Laporte C, de Salas PF. Weighing the Galactic disk using phase-space spirals: I. Tests on one-dimensional simulations. Astronomy & Astrophysics. 2021 Jun 21;650. A124. https://doi.org/10.1051/0004-6361/202140650

Author

Widmark, A. ; Laporte, C. ; de Salas, P. F. / Weighing the Galactic disk using phase-space spirals : I. Tests on one-dimensional simulations. In: Astronomy & Astrophysics. 2021 ; Vol. 650.

Bibtex

@article{ea43c6d3fea54d9d8ab9c0245809cba3,
title = "Weighing the Galactic disk using phase-space spirals: I. Tests on one-dimensional simulations",
abstract = "We present a new method for inferring the gravitational potential of the Galactic disk, using the time-varying structure of a phase-space spiral in the (z, w)-plane (where z and w represent vertical position and vertical velocity). Our method of inference extracts information from the shape of the spiral and disregards the bulk density distribution that is usually used to perform dynamical mass measurements. In this manner, it is complementary to traditional methods that are based on the assumption of a steady state. Our method consists of fitting an analytical model for the phase-space spiral to data, where the spiral is seen as a perturbation of the stellar number density in the (z, w)-plane. We tested our method on one-dimensional simulations, which were initiated in a steady state and then perturbed by an external force similar to that of a passing satellite. We were able to retrieve the true gravitational potentials of the simulations with high accuracy. The gravitational potential at 400-500 parsec distances from the disk mid-plane was inferred with an error of only a few percent. This is the first paper of a series in which we plan to test and refine our method on more complex simulations, as well as apply our method to Gaia data.",
keywords = "Galaxy: kinematics and dynamics, Galaxy: disk, solar neighborhood, astrometry, MILKY-WAY, MASS MODELS, SAGITTARIUS, STARS, HALO, KINEMATICS, DENSITY, WAVES, PLANE, HUNT",
author = "A. Widmark and C. Laporte and {de Salas}, {P. F.}",
year = "2021",
month = jun,
day = "21",
doi = "10.1051/0004-6361/202140650",
language = "English",
volume = "650",
journal = "Astronomy and Astrophysics Supplement Series",
issn = "0004-6361",
publisher = "E D P Sciences",

}

RIS

TY - JOUR

T1 - Weighing the Galactic disk using phase-space spirals

T2 - I. Tests on one-dimensional simulations

AU - Widmark, A.

AU - Laporte, C.

AU - de Salas, P. F.

PY - 2021/6/21

Y1 - 2021/6/21

N2 - We present a new method for inferring the gravitational potential of the Galactic disk, using the time-varying structure of a phase-space spiral in the (z, w)-plane (where z and w represent vertical position and vertical velocity). Our method of inference extracts information from the shape of the spiral and disregards the bulk density distribution that is usually used to perform dynamical mass measurements. In this manner, it is complementary to traditional methods that are based on the assumption of a steady state. Our method consists of fitting an analytical model for the phase-space spiral to data, where the spiral is seen as a perturbation of the stellar number density in the (z, w)-plane. We tested our method on one-dimensional simulations, which were initiated in a steady state and then perturbed by an external force similar to that of a passing satellite. We were able to retrieve the true gravitational potentials of the simulations with high accuracy. The gravitational potential at 400-500 parsec distances from the disk mid-plane was inferred with an error of only a few percent. This is the first paper of a series in which we plan to test and refine our method on more complex simulations, as well as apply our method to Gaia data.

AB - We present a new method for inferring the gravitational potential of the Galactic disk, using the time-varying structure of a phase-space spiral in the (z, w)-plane (where z and w represent vertical position and vertical velocity). Our method of inference extracts information from the shape of the spiral and disregards the bulk density distribution that is usually used to perform dynamical mass measurements. In this manner, it is complementary to traditional methods that are based on the assumption of a steady state. Our method consists of fitting an analytical model for the phase-space spiral to data, where the spiral is seen as a perturbation of the stellar number density in the (z, w)-plane. We tested our method on one-dimensional simulations, which were initiated in a steady state and then perturbed by an external force similar to that of a passing satellite. We were able to retrieve the true gravitational potentials of the simulations with high accuracy. The gravitational potential at 400-500 parsec distances from the disk mid-plane was inferred with an error of only a few percent. This is the first paper of a series in which we plan to test and refine our method on more complex simulations, as well as apply our method to Gaia data.

KW - Galaxy: kinematics and dynamics

KW - Galaxy: disk

KW - solar neighborhood

KW - astrometry

KW - MILKY-WAY

KW - MASS MODELS

KW - SAGITTARIUS

KW - STARS

KW - HALO

KW - KINEMATICS

KW - DENSITY

KW - WAVES

KW - PLANE

KW - HUNT

U2 - 10.1051/0004-6361/202140650

DO - 10.1051/0004-6361/202140650

M3 - Journal article

VL - 650

JO - Astronomy and Astrophysics Supplement Series

JF - Astronomy and Astrophysics Supplement Series

SN - 0004-6361

M1 - A124

ER -

ID: 278482914