TRIGONOMETRIC PARALLAXES OF HIGH MASS STAR FORMING REGIONS: THE STRUCTURE AND KINEMATICS OF THE MILKY WAY

Reid, M. J.; Menten, K. M.; Brunthaler, A.; Zheng, X. W.; Dame, T. M.; Xu, Y.; Wu, Y.; Zhang, B.; Sanna, A.; Sato, M.; Hachisuka, K.; Choi, Y. K.; Immer, K.; Moscadelli, L.; Rygl, K. L. J.; Bartkiewicz, A.

doi:10.1088/0004-637x/783/2/130

Cited by 1,379Stellar, planetary, and galactic studiesAstrophysics and Star Formation StudiesGalaxies: Formation, Evolution, Phenomena

TRIGONOMETRIC PARALLAXES OF HIGH MASS STAR FORMING REGIONS: THE STRUCTURE AND KINEMATICS OF THE MILKY WAY

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Reid, M. J., Menten, K. M., Brunthaler, A., Zheng, X. W., Dame, T. M., Xu, Y., Wu, Y., Zhang, B. +8 more·2014·The Astrophysical Journal

DOI 10.1088/0004-637x/783/2/130

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Abstract

Over 100 trigonometric parallaxes and proper motions for masers associated with young, high-mass stars have been measured with the Bar and Spiral Structure Legacy Survey, a Very Long Baseline Array key science project, the European VLBI Network, and the Japanese VLBI Exploration of Radio Astrometry project. These measurements provide strong evidence for the existence of spiral arms in the Milky Way, accurately locating many arm segments and yielding spiral pitch angles ranging from about 7° to 20°. The widths of spiral arms increase with distance from the Galactic center. Fitting axially symmetric models of the Milky Way with the three-dimensional position and velocity information and conservative priors for the solar and average source peculiar motions, we estimate the distance to the Galactic center, R 0 , to be 8.34 ± 0.16 kpc, a circular rotation speed at the Sun, Θ 0 , to be 240 ± 8 km s −1 , and a rotation curve that is nearly flat (i.e., a slope of −0.2 ± 0.4 km s −1 kpc −1 ) between Galactocentric radii of ≈5 and 16 kpc. Assuming a "universal" spiral galaxy form for the rotation curve, we estimate the thin disk scale length to be 2.44 ± 0.16 kpc. With this large data set, the parameters R 0 and Θ 0 are no longer highly correlated and are relatively insensitive to different forms of the rotation curve. If one adopts a theoretically motivated prior that high-mass star forming regions are in nearly circular Galactic orbits, we estimate a global solar motion component in the direction of Galactic rotation, V ☉ = 14.6 ± 5.0 km s −1 . While Θ 0 and V ☉ are significantly correlated, the sum of these parameters is well constrained, Θ 0 + V ☉ = 255.2 ± 5.1 km s −1 , as is the angular speed of the Sun in its orbit about the Galactic center, (Θ 0 + V ☉ )/ R 0 = 30.57 ± 0.43 km s −1 kpc −1 . These parameters improve the accuracy of estimates of the accelerations of the Sun and the Hulse–Taylor binary pulsar in their Galactic orbits, significantly reducing the uncertainty in tests of gravitational radiation predicted by general relativity.

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The BeSSeL (Reid et al., 2014) and VERA (Honma et al., 2012) surveys have used ∼100 masers to constrain R⊙ = 8.34 ± 0.16 kpc and vc(R0) = 240 ± 8 km s^-1.
“The BeSSeL (Reid et al., 2014) and VERA (Honma et al., 2012) surveys have used ∼ 100 masers to constrain R ⊙ = 8 . 34 ± 0 . 16 kpc and vc ( R 0 ) = 240 ± 8 km s -1 .”
From The rotation curve of the Milky Way: State of the art, the Keplerian decline debate, and implications for dark matter (2026) · cites this paper as Reid et al., 2014

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Flagged first, then by citations

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Authors: Reid, M. J., Menten, K. M., Brunthaler, A., Zheng, X. W., Dame, T. M., Xu, Y., Wu, Y., Zhang, B., Sanna, A., Sato, M., Hachisuka, K., Choi, Y. K., Immer, K., Moscadelli, L., Rygl, K. L. J., & Bartkiewicz, A.
Affiliations: Center for Astrophysics Harvard & Smithsonian (US)
Max Planck Institute for Radio Astronomy (DE)
Nanjing University (CN)
Chinese Academy of Sciences (CN)
Shanghai Astronomical Observatory (CN)
Arcetri Astrophysical Observatory (IT)
European Space Agency (FR)
Nicolaus Copernicus University (PL)
ORCID: Rygl, K. L. J.
Venue: The Astrophysical Journal
Publisher: American Astronomical Society
Published: 2014-02-24
Volume: 783
Issue: 2
Pages: 130
ISSN: 0004-637X (ISSN-L)
1538-4357
DOI: 10.1088/0004-637x/783/2/130
OpenAlex: W1974878478
Cited by: 1,379
References: 81
Citations by year: 2026: 49 · 2025: 94 · 2024: 77 · 2023: 90 · 2022: 92 · 2021: 111 · 2020: 135 · 2019: 151 · 2018: 148 · 2017: 153 · 2016: 121 · 2015: 109 · 2014: 48 · 2013: 1
FWCI: 77.39
Type: journal article
Language: en
Open access: bronze
doi.org
Licence: iopscience.iop.org/info/page/text-and-data-mining (tdm)
iopscience.iop.org/page/copyright (vor)
Locations: The Astrophysical Journal (publishedVersion)
arXiv (Cornell University) (submittedVersion)
arXiv (Cornell University)
Topics: Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
Keywords: stellar parallax, masers, massive star-forming regions, Milky Way spiral structure, spiral arms, galactocentric distance, galaxy rotation curves, solar motion, proper motions, Hulse-Taylor binary pulsar, galactic kinematics, axisymmetric model, radio astrometry

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TRIGONOMETRIC PARALLAXES OF HIGH MASS STAR FORMING REGIONS: THE STRUCTURE AND KINEMATICS OF THE MILKY WAY

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