期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 443, 期 3, 页码 2757-2765出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu1292
关键词
methods: numerical; Galaxy: disc; Galaxy: kinematics and dynamics
资金
- STFC
- Large Facilities Capital Fund of BIS
- PRACE
- Alfred P. Sloan Foundation
- National Science Foundation
- US Department of Energy Office of Science
- University of Arizona
- Brazilian Participation Group
- Brookhaven National Laboratory
- Carnegie Mellon University
- University of Florida
- French Participation Group
- German Participation Group
- Harvard University
- Instituto de Astrofisica de Canarias
- Michigan State/Notre Dame/JINA Participation Group
- Johns Hopkins University
- Lawrence Berkeley National Laboratory
- Max Planck Institute for Astrophysics
- Max Planck Institute for Extraterrestrial Physics
- New Mexico State University
- New York University
- Ohio State University
- Pennsylvania State University
- University of Portsmouth
- Princeton University
- Spanish Participation Group
- University of Tokyo
- University of Utah
- Vanderbilt University
- University of Virginia
- University of Washington
- Yale University
- EPSRC [EP/K000144/1, EP/K000136/1] Funding Source: UKRI
- STFC [ST/H008586/1, ST/K000373/1, ST/K000977/1, ST/J005673/1, ST/K00333X/1, ST/J500914/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/J500914/1, 1064627, ST/H008586/1, ST/K00333X/1, ST/K000373/1, ST/J005673/1, ST/K000977/1] Funding Source: researchfish
We have observed a snapshot of our N-body/smoothed particle hydrodynamics simulation of a Milky Way-sized barred spiral galaxy in a similar way to how we can observe the Milky Way. The simulated galaxy shows a corotating spiral arm, i.e. the spiral arm rotates with the same speed as the circular speed. We observed the rotation and radial velocities of the gas and stars as a function of the distance from our assumed location of the observer at the three lines of sight on the disc plane, (l, b) = (90, 0), (120, 0) and (150, 0) deg. We find that the stars tend to rotate slower (faster) behind (at the front of) the spiral arm and move outwards (inwards), because of the radial migration. However, because of their epicycle motion, we see a variation of rotation and radial velocities around the spiral arm. On the other hand, the cold gas component shows a clearer trend of rotating slower (faster) and moving outwards (inwards) behind (at the front of) the spiral arm, because of the radial migration. We have compared the results with the velocity of the maser sources from Reid et al., and find that the observational data show a similar trend in the rotation velocity around the expected position of the spiral arm at l = 120 deg. We also compared the distribution of the radial velocity from the local standard of the rest, V-LSR, with the Apache Point Observatory Galactic Evolution Experiment (APOGEE) data at l = 90 deg as an example.
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