How maser observations unravel the gas motions in the Galactic Center

Immer, K.; Reid, M.; Brunthaler, A.; Menten, K.; Zhang, Q.; Lu, X.; Mills, E. A. C.; Ginsburg, A.; Henshaw, J.; Longmore, S.; Kruijssen, D.; Pillai, T.

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How maser observations unravel the gas motions in the Galactic Center

MPS-Authors

Immer, K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Reid, M.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Brunthaler, A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Menten, K.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zhang, Q.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Lu, X.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Mills, E. A. C.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Ginsburg, A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Henshaw, J.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Longmore, S.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Kruijssen, D.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Pillai, T.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

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https://ui.adsabs.harvard.edu/abs/2018IAUS..336..176I
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Citation

Immer, K., Reid, M., Brunthaler, A., Menten, K., Zhang, Q., Lu, X., et al. (2018). How maser observations unravel the gas motions in the Galactic Center.

Cite as: https://hdl.handle.net/21.11116/0000-0005-CD1C-6

Abstract

The Central Molecular Zone (CMZ), the inner 450 pc of our Galaxy, is an exceptional region where the volume and column densities, gas temperatures, velocity dispersions, etc. are much higher than in the Galactic plane. It has been suggested that the formation of stars and clusters in this area is related to the orbital dynamics of the gas. The complex kinematic structure of the molecular gas was revealed by spectral line observations. However, these results are limited to the line-of-sight-velocities. To fully understand the motions of the gas within the CMZ, we have to know its location in 6D space (3D location + 3D motion). Recent orbital models have tried to explain the inflow of gas towards and its kinematics within this region. With parallax and proper motion measurements of masers in the CMZ we can discriminate among these models and constrain how our Galactic Center is fed with gas.