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Cited by 690Stellar, planetary, and galactic studiesAstrophysics and Star Formation StudiesAstrophysical Phenomena and Observations

The Two Young Star Disks in the Central Parsec of the Galaxy: Properties, Dynamics, and Formation

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Paumard, T., Genzel, R., Martins, F., Nayakshin, S., Beloborodov, A. M., Levin, Y., Trippe, S., Eisenhauer, F. +6 more·2006·The Astrophysical Journal
DOI 10.1086/503273
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Abstract

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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  • The rotation vectors of individual stars within the clockwise system slightly vary but overall remain at an inclination of 122°±7° (about ~30° away from the Galactic rotation axis).

    “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

    Section 3.2.2 reports a finite but moderate thickness for the clockwise disk, consistent with some variation among stellar orbital orientations. Table 4 gives the disk an inclination of 127°±2° relative to the sky, rather than 122°±7°. Its listed normal vector and the Galaxy’s imply an angle of about 72° between their rotation axes, not about 30°; Section 4.1 likewise says the disk is at a large angle to the Galactic plane. (LLM, conf=0.87)

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  • A younger generation of stars (age≈6±2 Myr) is observed within the central 0.5 pc.

    “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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Research works printed but not linked: 9

  1. Aller, L. H., et al. 1982, Landolt-Bo ¨rnstein Numerical Data and Relationships in Science and Technology, Vol. 2 ( Berlin: Springer)
  2. Beloborodov, A. M., Levin, Y., Eisenhauer, F., Genzel, R., Paumard, T., Gillessen, S., & Ott, T. 2006, ApJ, in press
  3. Bonnet, H., et al. 2003, Proc. SPIE, 4839, 329
  4. ---. 2003b, Proc. SPIE, 4841, 1548
  5. Forrest, W. J., Shure, M. A., Pipher, J. L., & Woodward, C. A. 1987, in AIP Conf. Proc. 155, The Galactic Center, ed. D. Backer ( New York: AIP), 153
  6. Lenzen, R., et al. 2003, Proc. SPIE, 4841, 944
  7. Nayakshin, S. 2005, MNRAS, submitted (astro-ph/0512255) · arXiv
  8. Rousset, G., et al. 2003, Proc. SPIE, 4839, 140
  9. Schmidt-Kaler, T. 1982, in Landoldt-Bo ¨rnstein, Vol. VI/2b, ed. K. Schaifers & H. H. Voigt ( Berlin: Springer), 1

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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)
ORCID
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
DOI
10.1086/503273
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
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

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