Skip to main content Accessibility help
×
Home

Modeling high-redshift galaxies: what can we learn from high and ultra-high resolution hydrodynamical simulations?

  • J. Devriendt (a1), A. Slyz (a1), L. Powell (a1), C. Pichon (a1) (a2) and R. Teyssier (a3) (a4)...

Abstract

We present results from a high resolution cosmological galaxy formation simulation called Mare Nostrum and a ultra-high resimulation of the first 500 million years of a single, Milky Way (MW) sized galaxy. Using the cosmological run, we measure UV luminosity functions and assess their sensitivity to both cosmological parameters and dust extinction. We find remarkably good agreement with the existing data over the redshift range 4 < z < 7 provided we adopt the favoured cosmology (WMAP 5 year parameters) and a self-consistent treatment of the dust. Cranking up the resolution, we then study in detail a z = 9 protogalaxy sitting at the intersection of cold gas filaments. This high-z MW progenitor grows a dense, rapidly spinning, thin disk which undergoes gravitational fragmention. Star formation in the resulting gas clumps rapidly turns them into globular clusters. A far reaching galactic wind develops, co-powered by the protogalaxy and its cohort of smaller companions populating the filaments. Despite such an impressive blow out, the smooth filamentary material is hardly affected at these redshifts.

    • Send article to Kindle

      To send this article to your Kindle, first ensure no-reply@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about sending to your Kindle. Find out more about sending to your Kindle.

      Note you can select to send to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be sent to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

      Find out more about the Kindle Personal Document Service.

      Modeling high-redshift galaxies: what can we learn from high and ultra-high resolution hydrodynamical simulations?
      Available formats
      ×

      Send article to Dropbox

      To send this article to your Dropbox account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Dropbox.

      Modeling high-redshift galaxies: what can we learn from high and ultra-high resolution hydrodynamical simulations?
      Available formats
      ×

      Send article to Google Drive

      To send this article to your Google Drive account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Google Drive.

      Modeling high-redshift galaxies: what can we learn from high and ultra-high resolution hydrodynamical simulations?
      Available formats
      ×

Copyright

References

Hide All
Birnboim, Y., & Dekel, A. 2003, MNRAS, 345, 349
Bouwens, R., et al. 2007, ApJ, 670, 928
Bouwens, R., et al. 2008, ApJ, 686, 230
Brooks, A. M., Governato, F., Quinn, T., Brook, C. B., & Wadsley, J. 2009, ApJ, 694, 396
Calzetti, D, Kinney, A., & Storchi-Bergmann, T 1994, ApJ, 429, 582
Dekel, A. & Birnboim, Y. 2006, MNRAS, 368, 2
Devriendt, J. E. G., Guiderdoni, B., & Sadat, R. 1999, A&A, 350, 381
Dubois, Y. & Teyssier, R. 2008, A&A, 477, 79
Dunkley, J., et al. 2009, ApJS, 180, 306
Guiderdoni, B. & Rocca-Volmerange, B. 1987, A&A, 186, 1
Haardt, F. & Madau, P. 1996, ApJ, 461, 20
Heckman, T. et al. 2005, ApJ, 619, L35
Keres, D., Katz, N., Weinberg, D. H., & Davé, R. 2005, MNRAS, 363, 2
Ocvirk, P., Pichon, C., & Teyssier, R. 2008, MNRAS, 390, 1326
Spergel, D., et al. 2003, ApJS, 148, 175
Springel, V. & Hernquist, L. 2003, MNRAS, 339, 289
Steidel, C., et al. 1999, ApJ, 519, 1
Teyssier, R. 2002, A&A, 385, 337
White, S. & Rees, M. 1978, MNRAS, 183, 341
MathJax
MathJax is a JavaScript display engine for mathematics. For more information see http://www.mathjax.org.

Keywords

Metrics

Full text views

Total number of HTML views: 0
Total number of PDF views: 0 *
Loading metrics...

Abstract views

Total abstract views: 0 *
Loading metrics...

* Views captured on Cambridge Core between <date>. This data will be updated every 24 hours.

Usage data cannot currently be displayed