Determination of Dark Matter Halo Mass from Dynamics of Satellite Galaxies
Abstract
We propose that the mass of a dark matter halo can be inferred from the dynamical status of its satellite galaxies. Using nine dark matter simulations of halos like the Milky Way (MW), we find that the present-day substructures in each halo follow a characteristic distribution in the phase space of orbital binding energy and angular momentum, and that this distribution is similar from halo to halo, but has an intrinsic dependence on the halo formation history. We build this distribution directly from the simulations for a specific halo and extend the result to halos of similar formation history but different masses by scaling. The mass of an observed halo can then be estimated by maximizing the likelihood in comparing the measured kinematic parameters of its satellite galaxies with these distributions. We test the validity and accuracy of this method with mock samples taken from the simulations. Using the positions, radial velocities, and proper motions of nine tracers and assuming observational uncertainties comparable to those of MW satellite galaxies, we find that the halo mass can be recovered to within $$\sim 40 \% $$. The accuracy can be improved to within ~25% if 30 tracers are used. Yet, the dependence of the phase-space distribution on the halo formation history sets a minimum uncertainty of $$\sim 20 \% $$ that cannot be reduced by using more tracers. We believe that this minimum uncertainty also applies to any mass determination for a halo when the phase-space information of other kinematic tracers is used.
- Authors:
-
- Key Lab. for Research in Galaxies and Cosmology, Shanghai (China); Chinese Academy of Sciences (CAS), Beijing (China)
- Shanghai Jiao Tong Univ., Shanghai (China)
- Univ. of Minnesota, Minneapolis, MN (United States); Tsung-Dao Lee Inst., Shanghai (China)
- Key Lab. for Research in Galaxies and Cosmology, Shanghai (China)
- Publication Date:
- Research Org.:
- Univ. of Minnesota, Minneapolis, MN (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC), Nuclear Physics (NP)
- OSTI Identifier:
- 1511018
- Grant/Contract Number:
- FG02-87ER40328
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 850; Journal Issue: 2; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; dark matter; galaxies; dwarf Galaxy; halo Galaxy; kinematics and dynamics; numerical methods; statistical methods
Citation Formats
Li, Zhao-Zhou, Jing, Y. P., Qian, Yong-Zhong, Yuan, Zhen, and Zhao, Dong-Hai. Determination of Dark Matter Halo Mass from Dynamics of Satellite Galaxies. United States: N. p., 2017.
Web. doi:10.3847/1538-4357/aa94c0.
Li, Zhao-Zhou, Jing, Y. P., Qian, Yong-Zhong, Yuan, Zhen, & Zhao, Dong-Hai. Determination of Dark Matter Halo Mass from Dynamics of Satellite Galaxies. United States. https://doi.org/10.3847/1538-4357/aa94c0
Li, Zhao-Zhou, Jing, Y. P., Qian, Yong-Zhong, Yuan, Zhen, and Zhao, Dong-Hai. Wed .
"Determination of Dark Matter Halo Mass from Dynamics of Satellite Galaxies". United States. https://doi.org/10.3847/1538-4357/aa94c0. https://www.osti.gov/servlets/purl/1511018.
@article{osti_1511018,
title = {Determination of Dark Matter Halo Mass from Dynamics of Satellite Galaxies},
author = {Li, Zhao-Zhou and Jing, Y. P. and Qian, Yong-Zhong and Yuan, Zhen and Zhao, Dong-Hai},
abstractNote = {We propose that the mass of a dark matter halo can be inferred from the dynamical status of its satellite galaxies. Using nine dark matter simulations of halos like the Milky Way (MW), we find that the present-day substructures in each halo follow a characteristic distribution in the phase space of orbital binding energy and angular momentum, and that this distribution is similar from halo to halo, but has an intrinsic dependence on the halo formation history. We build this distribution directly from the simulations for a specific halo and extend the result to halos of similar formation history but different masses by scaling. The mass of an observed halo can then be estimated by maximizing the likelihood in comparing the measured kinematic parameters of its satellite galaxies with these distributions. We test the validity and accuracy of this method with mock samples taken from the simulations. Using the positions, radial velocities, and proper motions of nine tracers and assuming observational uncertainties comparable to those of MW satellite galaxies, we find that the halo mass can be recovered to within $\sim 40 \% $. The accuracy can be improved to within ~25% if 30 tracers are used. Yet, the dependence of the phase-space distribution on the halo formation history sets a minimum uncertainty of $\sim 20 \% $ that cannot be reduced by using more tracers. We believe that this minimum uncertainty also applies to any mass determination for a halo when the phase-space information of other kinematic tracers is used.},
doi = {10.3847/1538-4357/aa94c0},
journal = {The Astrophysical Journal (Online)},
number = 2,
volume = 850,
place = {United States},
year = {Wed Nov 22 00:00:00 EST 2017},
month = {Wed Nov 22 00:00:00 EST 2017}
}
Web of Science
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