Hostname: page-component-77c89778f8-cnmwb Total loading time: 0 Render date: 2024-07-23T00:09:16.482Z Has data issue: false hasContentIssue false
  • English
  • Français

Study of the Milky Way's hot coronal gas with its dwarf galaxies

Published online by Cambridge University Press:  09 May 2016

Stefano Pasetto ,
Mark Cropper ,
Yutaka Fujita ,
Cesare Chiosi  and
Eva K. Grebel
Stefano Pasetto
Affiliation:
Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, United Kingdom email: s.pasetto@ucl.ac.uk
Mark Cropper
Affiliation:
Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, United Kingdom email: s.pasetto@ucl.ac.uk
Yutaka Fujita
Affiliation:
Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama-cho, Toyonaka-shi, Osaka 560-0043, Japan
Cesare Chiosi
Affiliation:
Dept. of Physics & Astronomy“Galileo Galilei”, University of Padua, Vicolo dell'Osservatorio, 5, 35141 Padova PD, Italy
Eva K. Grebel
Affiliation:
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg, Mönchhofstr 12-14, 69120, Heidelberg, Germany
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

A large amount (5 × 1010 M⊙) of hot gas is thought to exist in an extended (≈ 200 kpc) hot diffuse halo around the Milky Way. We investigate the competitive role of the different dissipative phenomena acting on the onset of star formation of this gravitationally bound systems in this external environment. Ram pressure, Kelvin-Helmholtz and Rayleigh- Taylor instabilities, and tidal forces are accounted for separately in an analytical framework and compared in their role in influencing the star forming regions. We present an analytical criterion to elucidate the dependence of star formation in a spherical stellar system on its surrounding environment, useful in observational applications as well as theoretical interpretations of numerical results. We consider the different signatures of these phenomena in synthetically realized colour-magnitude diagrams (CMDs) of the orbiting system, thus investigating the detectability limits and relevance of these different effects for future observational projects. The theoretical framework developed has direct applications to the cases of our MW system as well as dwarf galaxies in galaxy clusters or any primordial gas-rich star cluster of stars orbiting within its host galaxy.

Keywords

Galaxy: haloGalaxy: fundamental parametersgalaxies: dwarf
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Issue S317: The General Assembly of Galaxy Halos: Structure, Origin and Evolution , August 2015 , pp. 340 - 341
Copyright
Copyright © International Astronomical Union 2016 

References

Bertelli, G., Nasi, E., Girardi, L., & Marigo, P., 2009, A&A, 508, 355Google Scholar
Fujita, Y., 1998, ApJ, 509, 587Google Scholar
Fukugita, M. & Peebles, P. J. E., 2006, ApJ, 639, 590Google Scholar
Grebel, E. K., Gallagher, J. S. III, & Harbeck, D., 2003, AJ, 125, 1926CrossRefGoogle Scholar
Pasetto, S., Bertelli, G., Grebel, E. K., Chiosi, C., & Fujita, Y., 2012, A&A, 542, A17Google Scholar
Pasetto, S., et al., 2012, A&A, 547, A70Google Scholar
Pasetto, S., Grebel, E. K., Berczik, P., Chiosi, C., & Spurzem, R., 2011, A&A, 525, A99Google Scholar