Estimating the local dark matter density in a non-axisymmetric wobbling disc
Abstract
The density of dark matter near the Sun, ρDM, ⊙, is important for experiments hunting for dark matter particles in the laboratory, and for constraining the local shape of the Milky Way’s dark matter halo. Estimates to date have typically assumed that the Milky Way’s stellar disc is axisymmetric and in a steady-state. Yet the Milky Way disc is neither, exhibiting prominent spiral arms and a bar, and vertical and radial oscillations. Here, we assess the impact of these assumptions on determinations of ρDM, ⊙ by applying a free-form, steady-state, Jeans method to two different N-body simulations of Milky Way-like galaxies. In one, the galaxy has experienced an ancient major merger, similar to the hypothesized Gaia–Sausage–Enceladus; in the other, the galaxy is perturbed more recently by the repeated passage and slow merger of a Sagittarius-like dwarf galaxy. We assess the impact of each of the terms in the Jeans–Poisson equations on our ability to correctly extract ρDM, ⊙ from the simulated data. We find that common approximations employed in the literature – axisymmetry and a locally flat rotation curve – can lead to significant systematic errors of up to a factor ~1.5 in the recovered surface mass density ~2 kpcmore »
- Authors:
-
[2];
[1];
[5];
- Stockholm Univ. (Sweden). Oskar Klein Centre for Cosmoparticle Physics
- Univ. of Surrey, Guildford (United Kingdom)
- University of Barcelona (Spain)
- Stockholm Univ. (Sweden). Oskar Klein Centre for Cosmoparticle Physics; Univ. of Copenhagen (Denmark)
- University of Barcelona (Spain); Univ. of Tokyo (Japan). Kavli Institute for the Physics and Mathematics of the Universe (WPI)
- Univ. of Zurich (Switzerland)
- Stockholm Univ. (Sweden). Oskar Klein Centre for Cosmoparticle Physics; Univ. of Texas, Austin, TX (United States); Nordic Institute for Theoretical Physics (NORDITA) (Sweden)
- Publication Date:
- Research Org.:
- Univ. of Texas, Austin, TX (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), High Energy Physics (HEP); Swedish Research Council (SRC); Carlsberg Foundation; European Research Council (ERC)
- Contributing Org.:
- University of Michigan
- OSTI Identifier:
- 1907436
- Grant/Contract Number:
- SC0022021; SC007859; 638-2013-8993; 621-2014-5772; CF15-0384; 852839
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Volume: 511; Journal Issue: 2; Journal ID: ISSN 0035-8711
- Publisher:
- Royal Astronomical Society
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS
Citation Formats
Sivertsson, S., Read, J. I., Silverwood, H., de Salas, P. F., Malhan, K., Widmark, A., Laporte, C. P., Garbari, S., and Freese, K. Estimating the local dark matter density in a non-axisymmetric wobbling disc. United States: N. p., 2022.
Web. doi:10.1093/mnras/stac094.
Sivertsson, S., Read, J. I., Silverwood, H., de Salas, P. F., Malhan, K., Widmark, A., Laporte, C. P., Garbari, S., & Freese, K. Estimating the local dark matter density in a non-axisymmetric wobbling disc. United States. https://doi.org/10.1093/mnras/stac094
Sivertsson, S., Read, J. I., Silverwood, H., de Salas, P. F., Malhan, K., Widmark, A., Laporte, C. P., Garbari, S., and Freese, K. Tue .
"Estimating the local dark matter density in a non-axisymmetric wobbling disc". United States. https://doi.org/10.1093/mnras/stac094. https://www.osti.gov/servlets/purl/1907436.
@article{osti_1907436,
title = {Estimating the local dark matter density in a non-axisymmetric wobbling disc},
author = {Sivertsson, S. and Read, J. I. and Silverwood, H. and de Salas, P. F. and Malhan, K. and Widmark, A. and Laporte, C. P. and Garbari, S. and Freese, K.},
abstractNote = {The density of dark matter near the Sun, ρDM, ⊙, is important for experiments hunting for dark matter particles in the laboratory, and for constraining the local shape of the Milky Way’s dark matter halo. Estimates to date have typically assumed that the Milky Way’s stellar disc is axisymmetric and in a steady-state. Yet the Milky Way disc is neither, exhibiting prominent spiral arms and a bar, and vertical and radial oscillations. Here, we assess the impact of these assumptions on determinations of ρDM, ⊙ by applying a free-form, steady-state, Jeans method to two different N-body simulations of Milky Way-like galaxies. In one, the galaxy has experienced an ancient major merger, similar to the hypothesized Gaia–Sausage–Enceladus; in the other, the galaxy is perturbed more recently by the repeated passage and slow merger of a Sagittarius-like dwarf galaxy. We assess the impact of each of the terms in the Jeans–Poisson equations on our ability to correctly extract ρDM, ⊙ from the simulated data. We find that common approximations employed in the literature – axisymmetry and a locally flat rotation curve – can lead to significant systematic errors of up to a factor ~1.5 in the recovered surface mass density ~2 kpc above the disc plane, implying a fractional error on ρDM, ⊙ of the order of unity. However, once we add in the tilt term and the rotation curve term in our models, we obtain an unbiased estimate of ρDM, ⊙, consistent with the true value within our 95 percent confidence intervals for realistic 20 percent uncertainties on the baryonic surface density of the disc. Other terms – the axial tilt, 2nd Poisson and time-dependent terms – contribute less than 10 percent to ρDM, ⊙ (given current data) and can be safely neglected for now. In the future, as more data become available, these terms will need to be included in the analysis.},
doi = {10.1093/mnras/stac094},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 2,
volume = 511,
place = {United States},
year = {Tue Feb 08 00:00:00 EST 2022},
month = {Tue Feb 08 00:00:00 EST 2022}
}
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