Milky Way mass with K giants and BHB stars using LAMOST, SDSS/SEGUE, and Gaia : 3D spherical Jeans equation and tracer mass estimator
Abstract
We measure the enclosed Milky Way mass profile to Galactocentric distances of ~70 and ~50 kpc using the smooth, diffuse stellar halo samples of Bird et al. The samples are Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) and Sloan Digital Sky Survey/Sloan Extension for Galactic Understanding and Exploration (SDSS/SEGUE) K giants (KG) and SDSS/SEGUE blue horizontal branch (BHB) stars with accurate metallicities. The 3D kinematics are available through LAMOST and SDSS/SEGUE distances and radial velocities and Gaia DR2 proper motions. Two methods are used to estimate the enclosed mass: 3D spherical Jeans equation and Evans et al. tracer mass estimator (TME). We remove substructure via the Xue et al. method based on integrals of motion. We evaluate the uncertainties on our estimates due to random sampling noise, systematic distance errors, the adopted density profile, and non-virialization and non-spherical effects of the halo. The tracer density profile remains a limiting systematic in our mass estimates, although within these limits we find reasonable agreement across the different samples and the methods applied. Out to ~70 and ~50 kpc, the Jeans method yields total enclosed masses of 4.3 ± 0.95 (random) ±0.6 (systematic) × 1011 M⊙ and 4.1 ± 1.2 (random) ±0.6 (systematic) × 1011 M⊙ for the KG and BHB stars, respectively. For the KG and BHB samples, we find a dark matter virial mass of M200=0.55$$^{+0.15}_{-0.11}$$ (random) ±0.083 (systematic) × 1012 M⊙ and M200=1.00$$^{+0.67}_{-0.33}$$ (random) ±0.15 (systematic) × 1012 M⊙, respectively.
- Publication Date:
- Research Org.:
- US Department of Energy (USDOE), Washington, DC (United States). Office of Science, Sloan Digital Sky Survey (SDSS)
- Sponsoring Org.:
- USDOE Office of Science (SC); National Natural Science Foundation of China (NSFC); National Key Research and Development Program of China; China Manned Space Project; Alfred P. Sloan Foundation; National Science Foundation (NSF)
- OSTI Identifier:
- 1884374
- Alternate Identifier(s):
- OSTI ID: 1982640
- Grant/Contract Number:
- 11988101; 2019YFA0405500; 1189069; 11873057; 187305; 12025302; 11873034; 11773052; 11761131016; 2018YFA0404501; CMS-CSST-2021-B03; CMS-CSST-2021-A09; CMS-CSST-2021-A08
- Resource Type:
- Published Article
- Journal Name:
- Monthly Notices of the Royal Astronomical Society
- Additional Journal Information:
- Journal Name: Monthly Notices of the Royal Astronomical Society Journal Volume: 516 Journal Issue: 1; Journal ID: ISSN 0035-8711
- Publisher:
- Oxford University Press
- Country of Publication:
- United Kingdom
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; stars; individual; BHB; K giants; galaxies; Milky Way; kinematics and dynamics, galaxy; halo; stellar content
Citation Formats
Bird, Sarah A., Xue, Xiang-Xiang, Liu, Chao, Flynn, Chris, Shen, Juntai, Wang, Jie, Yang, Chengqun, Zhai, Meng, Zhu, Ling, Zhao, Gang, and Tian, Hai-Jun. Milky Way mass with K giants and BHB stars using LAMOST, SDSS/SEGUE, and Gaia : 3D spherical Jeans equation and tracer mass estimator. United Kingdom: N. p., 2022.
Web. doi:10.1093/mnras/stac2036.
Bird, Sarah A., Xue, Xiang-Xiang, Liu, Chao, Flynn, Chris, Shen, Juntai, Wang, Jie, Yang, Chengqun, Zhai, Meng, Zhu, Ling, Zhao, Gang, & Tian, Hai-Jun. Milky Way mass with K giants and BHB stars using LAMOST, SDSS/SEGUE, and Gaia : 3D spherical Jeans equation and tracer mass estimator. United Kingdom. https://doi.org/10.1093/mnras/stac2036
Bird, Sarah A., Xue, Xiang-Xiang, Liu, Chao, Flynn, Chris, Shen, Juntai, Wang, Jie, Yang, Chengqun, Zhai, Meng, Zhu, Ling, Zhao, Gang, and Tian, Hai-Jun. Sat .
"Milky Way mass with K giants and BHB stars using LAMOST, SDSS/SEGUE, and Gaia : 3D spherical Jeans equation and tracer mass estimator". United Kingdom. https://doi.org/10.1093/mnras/stac2036.
@article{osti_1884374,
title = {Milky Way mass with K giants and BHB stars using LAMOST, SDSS/SEGUE, and Gaia : 3D spherical Jeans equation and tracer mass estimator},
author = {Bird, Sarah A. and Xue, Xiang-Xiang and Liu, Chao and Flynn, Chris and Shen, Juntai and Wang, Jie and Yang, Chengqun and Zhai, Meng and Zhu, Ling and Zhao, Gang and Tian, Hai-Jun},
abstractNote = {We measure the enclosed Milky Way mass profile to Galactocentric distances of ~70 and ~50 kpc using the smooth, diffuse stellar halo samples of Bird et al. The samples are Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) and Sloan Digital Sky Survey/Sloan Extension for Galactic Understanding and Exploration (SDSS/SEGUE) K giants (KG) and SDSS/SEGUE blue horizontal branch (BHB) stars with accurate metallicities. The 3D kinematics are available through LAMOST and SDSS/SEGUE distances and radial velocities and Gaia DR2 proper motions. Two methods are used to estimate the enclosed mass: 3D spherical Jeans equation and Evans et al. tracer mass estimator (TME). We remove substructure via the Xue et al. method based on integrals of motion. We evaluate the uncertainties on our estimates due to random sampling noise, systematic distance errors, the adopted density profile, and non-virialization and non-spherical effects of the halo. The tracer density profile remains a limiting systematic in our mass estimates, although within these limits we find reasonable agreement across the different samples and the methods applied. Out to ~70 and ~50 kpc, the Jeans method yields total enclosed masses of 4.3 ± 0.95 (random) ±0.6 (systematic) × 1011 M⊙ and 4.1 ± 1.2 (random) ±0.6 (systematic) × 1011 M⊙ for the KG and BHB stars, respectively. For the KG and BHB samples, we find a dark matter virial mass of M200=0.55$^{+0.15}_{-0.11}$ (random) ±0.083 (systematic) × 1012 M⊙ and M200=1.00$^{+0.67}_{-0.33}$ (random) ±0.15 (systematic) × 1012 M⊙, respectively.},
doi = {10.1093/mnras/stac2036},
journal = {Monthly Notices of the Royal Astronomical Society},
number = 1,
volume = 516,
place = {United Kingdom},
year = {Sat Jul 23 00:00:00 EDT 2022},
month = {Sat Jul 23 00:00:00 EDT 2022}
}
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