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Molecular gas kinematics of the CMZ: Great oaks from little acorns grow

Published online by Cambridge University Press:  09 February 2017

Jonathan D. Henshaw
Jonathan D. Henshaw*
Affiliation:
Astrophysics Research Institute, Liverpool John Moores University, Liverpool, L3 5RF, UK email: j.d.henshaw@ljmu.ac.uk
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Abstract

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The central molecular zone (CMZ) hosts some of the most massive and dense molecular clouds and star clusters in the Galaxy, offering an important window into star formation under extreme conditions. Star formation in this extreme environment may be closely linked to the 3-D distribution and orbital dynamics of the gas. Here I discuss how our new, accurate description of the {l,b,v} structure of the CMZ is helping to constrain its 3-D geometry. I also present the discovery of a highly-regular, corrugated velocity field located just upstream from the dust ridge molecular clouds (which include G0.253+0.016 and Sgr B2). The extremes in this velocity field correlate with a series of massive (~ 104 M⊙) cloud condensations. The corrugation wavelength (~23 pc) and cloud separation (~8 pc) closely agree with the predicted Toomre (~17 pc) and Jeans (~6 pc) lengths, respectively. I conclude that gravitational instabilities are driving the formation of molecular clouds within the Galactic Centre gas stream. Furthermore, I suggest that these seeds are the historical analogues of the dust ridge molecular clouds – possible progenitors of some of the most massive and dense molecular clouds in the Galaxy. If our current best understanding for the 3-D geometry of this system is confirmed, these clouds may pinpoint the beginning of an evolutionary sequence that can be followed, in time, from cloud condensation to star formation.

Keywords

stars: formationISM: kinematics and dynamicsGalaxy: center
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S322: The Multi-Messenger Astrophysics of the Galactic Centre , July 2016 , pp. 85 - 89
Copyright
Copyright © International Astronomical Union 2017 

References

Bally, J., et al., 1988, Apj, 324, 223 CrossRefGoogle Scholar
Caswell, J. L., et al., 2010, MNRAS, 404, 1029 CrossRefGoogle Scholar
Crocker, R. M., 2012, MNRAS, 423, 3512 CrossRefGoogle Scholar
Henshaw, J. D., et al., 2016a, MNRAS, 457, 2675 CrossRefGoogle Scholar
Henshaw, J. D., Longmore, S. N., & Kruijssen, J. M. D., 2016b, MNRAS, in press, arXiv:1609.01721Google Scholar
Jones, P. A., et al., 2012, MNRAS, 419, 2961 CrossRefGoogle Scholar
Kruijssen, J. M. D., et al., 2014, MNRAS, 440, 3370 CrossRefGoogle Scholar
Kruijssen, J. M. D., Dale, J. E., & Longmore, S. N., 2015, MNRAS, 447, 1059 CrossRefGoogle Scholar
Launhardt, R., Zylka, R., & Mezger, P. G., 2002, A&A, 384, 112 Google Scholar
Longmore, S. N., et al., 2012, Apj, 746, 117 CrossRefGoogle Scholar
Longmore, S. N., et al., 2013a, MNRAS, 429, 987 CrossRefGoogle Scholar
Longmore, S. N., et al., 2013b, MNRAS, 433, L15 CrossRefGoogle Scholar
Longmore, S. N., et al., 2014, preprint, (arXiv: 1401.4175)Google Scholar
Lu, X., et al., 2015, Apj, 814, L18 CrossRefGoogle Scholar
Mills, E. A. C., et al., 2015, Apj, 805, 72 CrossRefGoogle Scholar
Molinari, S., et al., 2011, Apj, 735, L33 CrossRefGoogle Scholar
Rathborne, J. M., et al., 2014, Apj, 786, 140 CrossRefGoogle Scholar
Rathborne, J. M., et al., 2015, Apj, 802, 125 CrossRefGoogle Scholar
Sawada, T., et al., 2004, MNRAS, 349, 1167 CrossRefGoogle Scholar
Sofue, Y., 1995, PASJ, 47, 527 Google Scholar
Toomre, A., 1964, Apj, 139, 1217 CrossRefGoogle Scholar
Walsh, A. J., et al., 2014, MNRAS, 442, 2240 CrossRefGoogle Scholar