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Cited by 188Galaxies: Formation, Evolution, PhenomenaStellar, planetary, and galactic studiesAstrophysical Phenomena and Observations

A Comprehensive Model for the Monoceros Tidal Stream

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Penarrubia, J., Martinez‐Delgado, D., Rix, H. W., Gomez‐Flechoso, M. A, Munn, J., Newberg, H., Bell, E. F., Yanny, B. +2 more·2005·The Astrophysical Journal
DOI 10.1086/429903
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Abstract

We have compiled an extensive data set on potential parts of the Monoceros tidal stream and performed an exhaustive survey of dwarf galaxy semianalytic orbits in order to constrain its orbital properties. The best-fit orbits are subsequently realized as self-consistent N -body simulations in order to reproduce the spatial and velocity distribution of satellite debris. We find that all kinematic and geometric constraints can be fit by a single stream allowing for multiple wraps. The orbital eccentricity and inclination of the progenitor are strongly constrained to be e = 0.10 ± 0.05 and i = 25 ° ± 5 ° . Ten new estimates of proper motions from the Sloan Digital Sky Survey clearly exclude all retrograde orbits. Particles lost by the satellite populate two nearly concentric rings, naturally explaining the detection of stream stars at both 6-8 kpc (Ibata et al.; Newberg et al.) and 12-18 kpc (the Tri/And stream; Rocha-Pinto et al.) from the Sun. We have attempted to predict the present location of the Monoceros stream progenitor using different information: (1) the kinematical and spatial distribution of detections, and (2) the different mean metallicity in the inner and the outer rings. Because of the lack of observational data in the whole range of Galactic latitudes, the geometrical/kinematical constraints lead to a wide range of possible locations. By associating older parts of the model stream with lower metallicity parts of the observed data, we argue in favor of a current location of l ~ 245 ° , b ~ -18 ° , with a distance to the Sun r s ≃ 15 kpc. The mass of the progenitor has been poorly constrained because of the slow orbital decay. Similar fits have been obtained for masses (3-9) × 10 8 M ☉ . We have analyzed the possible common origin of the Canis Major dwarf and the Monoceros stream. The Canis Major dwarf moves on a prograde, nearly circular orbit ( e ≃ 0.16) in the Milky Way disk ( i ≃ 4 deg). This orbital inclination is too low to account for the large vertical dispersion of stream stars. However, the bimodal distribution of radial velocities in the central region found by Martin et al. probably indicates that their selection criteria for identifying dwarf stars lead to a contamination of background stars. In that case, the kinematical data outlined above might result in an underestimate of the orbital inclination. Finally, the distance estimation to Canis Major dwarf is around a factor of 2 smaller than that obtained from our model. Unfortunately, the possible identification of the Monoceros stream progenitor in Canis Major remains unclear.

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Research works printed but not linked: 3

  1. Binney, J., & Tremaine, S. 1987, Galactic Dynamics ( Princeton: Princeton Univ. Press)
  2. Navarro, J. 2004, preprint (astro-ph /0405497)
  3. Pen ˜arrubia J. 2003, Ph.D. thesis, Univ. Heidelberg

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Authors
Penarrubia, J., Martinez‐Delgado, D., Rix, H. W., Gomez‐Flechoso, M. A., Munn, J., Newberg, H., Bell, E. F., Yanny, B., Zucker, D., & Grebel, E. K.
Affiliations
  • Max Planck Institute for Astronomy (DE)
  • Universidad Europea de Madrid (ES)
  • United States Naval Observatory (US)
  • Rensselaer Polytechnic Institute (US)
  • Fermi National Accelerator Laboratory (US)
  • University of Basel (CH)
Venue
The Astrophysical Journal
Publisher
American Astronomical Society
Published
2005-06-10
Volume
626
Issue
1
Pages
128-144
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
DOI
10.1086/429903
OpenAlex
W2141002982
Cited by
188
References
41
Citations by year
2024: 2 · 2023: 3 · 2022: 4 · 2021: 5 · 2020: 8 · 2019: 3 · 2018: 6 · 2017: 11 · 2016: 7 · 2015: 8 · 2014: 6 · 2013: 5 · 2012: 13
FWCI
13.19
Type
journal article
Language
en
Open access
Locations
  • The Astrophysical Journal (publishedVersion)
  • arXiv (Cornell University) (submittedVersion)
  • ABACUS. Repositorio de Producción Científica (Universidad Europea) (submittedVersion, other-oa)
  • arXiv (Cornell University)
Funders
  • National Science Foundation
  • U.S. Department of Energy
  • National Aeronautics and Space Administration
  • Alfred P. Sloan Foundation
  • Princeton University
  • University of Chicago
  • University of Washington
  • Johns Hopkins University
  • University of Pittsburgh
  • New Mexico State University
  • Max-Planck-Gesellschaft
  • Max-Planck-Institut für Astronomie
  • U.S. Naval Observatory
  • Fermilab
  • Los Alamos National Laboratory
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Galaxies: Formation, Evolution, Phenomena
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
Keywords
satellite debris, metallicity, proper motions, N-body simulations, Galactic halo, stream kinematics, radial velocity dispersion, orbital decay, progenitor mass

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