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The Two Young Star Disks in the Central Parsec of the Galaxy: Properties, Dynamics, and Formation
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We report the definite spectroscopic identification of ≃40 OB supergiants, giants, and main-sequence stars in the central parsec of the Galaxy. Detection of their absorption lines has become possible with the high spatial and spectral resolution and sensitivity of the adaptive optics integral field spectrometer SPIFFI/SINFONI on the ESO VLT. Several of these OB stars appear to be helium- and nitrogen-rich. Almost all of the ≃80 massive stars now known in the central parsec (central arcsecond excluded) reside in one of two somewhat thick (⟨ / R ⟩ ≃ 0.14) rotating disks. These stellar disks have fairly sharp inner edges ( R ≃ 1′′) and surface density profiles that scale as R -2 . We do not detect any OB stars outside the central 0.5 pc. The majority of the stars in the clockwise system appear to be on almost circular orbits, whereas most of those in the "counterclockwise" disk appear to be on eccentric orbits. Based on its stellar surface density distribution and dynamics, we propose that IRS 13E is an extremely dense cluster (ρ core ≳ 3 × 10 8 M ☉ pc -3 ) that has formed in the counterclockwise disk. The stellar contents of both systems are remarkably similar, indicating a common age of ≃6 ± 2 Myr. The K -band luminosity function of the massive stars suggests a top-heavy mass function and limits the total stellar mass contained in both disks to ≃1.5 × 10 4 M ☉ . Our data strongly favor in situ star formation from dense gas accretion disks for the two stellar disks. This conclusion is very clear for the clockwise disk and highly plausible for the counterclockwise system.
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“Additionally, the rotation vectors of individual stars within the clockwise system slightly vary from each other but, overall, remain at an inclination of 122 ◦ ± 7 ◦ (about ∼ 30 ◦ away from the Galactic rotation axis) (Paumard et al. 2006; Bartko et al. 2009; Lu et al. 2008; Genzel et al. 2010).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Paumard et al. 2006
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“A younger generation of stars (age ≈ 6 ± 2 Myr) is also observed within the central 0 . 5 pc (Paumard et al. 2006; Bartko et al. 2009).”
From The Fermi/eROSITA bubbles: a look into the nuclear outflow from the Milky Way (2024) · cites this paper as Paumard et al. 2006
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Cited by
Sorted by citations
MONITORING STELLAR ORBITS AROUND THE MASSIVE BLACK HOLE IN THE GALACTIC CENTER
Gillessen, S., Eisenhauer, F., Trippe, S., Alexander, T., Genzel, R., Martins, F., & Ott, T. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/692/2/1075 · Cited by 1,779
Self-citationThe Galaxy in Context: Structural, Kinematic, and Integrated Properties
Bland-Hawthorn, J., & Gerhard, O. (2016) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081915-023441 · Cited by 1,656
Toward Understanding Massive Star Formation
Zinnecker, H., & Yorke, H. (2007) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev.astro.44.051905.092549 · Cited by 1,016
The Galactic Center massive black hole and nuclear star cluster
Genzel, R., Eisenhauer, F., & Gillessen, S. (2010) · Reviews of Modern Physics · doi:10.1103/revmodphys.82.3121 · Cited by 1,236
Self-citationGIANT GAMMA-RAY BUBBLES FROM FERMI-LAT: ACTIVE GALACTIC NUCLEUS ACTIVITY OR BIPOLAR GALACTIC WIND?
Su, M., Slatyer, T., & Finkbeiner, D. (2010) · The Astrophysical Journal · doi:10.1088/0004-637x/724/2/1044 · Cited by 756
Metadata
- Authors
- Paumard, T., Genzel, R., Martins, F., Nayakshin, S., Beloborodov, A. M., Levin, Y., Trippe, S., Eisenhauer, F., Ott, T., Gillessen, S., Abuter, R., Cuadra, J., Alexander, T., & Sternberg, A.
- Affiliations
- Max Planck Institute for Extraterrestrial Physics (DE)
- University of Leicester (GB)
- P.N. Lebedev Physical Institute of the Russian Academy of Sciences (RU)
- Leiden University (NL)
- Max Planck Institute for Astrophysics (DE)
- Weizmann Institute of Science (IL)
- Tel Aviv University (IL)
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2006-06
- Volume
- 643
- Issue
- 2
- Pages
- 1011-1035
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2114914177
- Cited by
- 690
- References
- 96
- Citations by year
- 2026: 20 · 2025: 30 · 2024: 34 · 2023: 26 · 2022: 27 · 2021: 23 · 2020: 25 · 2019: 30 · 2018: 20 · 2017: 32 · 2016: 40 · 2015: 32 · 2014: 39 · 2013: 45 · 2012: 44
- FWCI
- 31.80
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- Max Planck Institute for Plasma Physics (submittedVersion)
- Leicester Research Archive (University of Leicester) (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 › Astrophysical Phenomena and Observations
- Keywords
- OB stars, in situ star formation, stellar orbits, eccentric orbits, K-band luminosity function, helium-rich stars, nitrogen-rich stars, young stellar clusters
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
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