Hostname: page-component-77c89778f8-sh8wx Total loading time: 0 Render date: 2024-07-18T12:22:11.575Z Has data issue: false hasContentIssue false
  • English
  • Français

Star formation properties in barred galaxies

Published online by Cambridge University Press:  17 August 2012

Zhi-Min Zhou ,
Chen Cao  and
Hong Wu
Zhi-Min Zhou
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: zmzhou@bao.ac.cn
Chen Cao
Affiliation:
School of Space Science and Physics, Shandong University at Weihai, Weihai, Shandong 264209, China
Hong Wu
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China email: zmzhou@bao.ac.cn
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.

Stellar bars are important structures for the internal secular evolution of galaxies. They can drive gas into the central region of galaxies, and result in an enhancement of star formation activity there. Previous studies are limited in the comparisons between barred and unbarred galaxies. Here we try to investigate the connection between star formation activities and different bars, based on multi-wavelength data in a sample of barred spirals. We find that there is no clearly trend of the surface star formation rates in different structures along the bar strength. In addition, there is larger scatter for the properties of star formation activity in the galaxies with middle-strength bars, which may indicate that a variety of star formation stages are more likely associated with these bars.

Keywords

galaxies: evolution — galaxies: photometry — galaxies: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S284: The Spectral Energy Distribution of Galaxies , September 2011 , pp. 349 - 351
Copyright
Copyright © International Astronomical Union 2012

References

Athanassoula, E. 2003, MNRAS, 341, 1179Google Scholar
Athanassoula, E. 1992, MNRAS, 259, 345CrossRefGoogle Scholar
Coelho, P. & Gadotti, D. A. 2011, arXiv1111.1736Google Scholar
Dale, D. A., et al. 2009, ApJ, 703, 517CrossRefGoogle Scholar
Ho, L. C., Filippenko, A. V., & Sargent, W. L. W. 1997, ApJ, 487, 591CrossRefGoogle Scholar
Kennicutt, R. C. et al. 2003, PASP, 115, 928CrossRefGoogle Scholar
Kormendy, J. & Kennicutt, R. C. 2004, ARAA, 42, 603CrossRefGoogle Scholar
Martin, D. C., et al. 2005, ApJ, 619, 1CrossRefGoogle Scholar
Pahre, M. A., Ashby, M. L. N., Fazio, G. G., & Willner, S. P. 2004, ApJS, 154, 235CrossRefGoogle Scholar
Sakamoto, K., Okumura, S. K., Ishizuki, S., & Scoville, N. Z. 1999, ApJ, 525, 691Google Scholar
Sellwood, J. A. & Wilkinson, A. 1993, Rep. Prog. Phys., 56, 173Google Scholar
Sheth, K., Vogel, S. N., Regan, M. W., Thornley, M. D., & Teuben, P. J. 2005, ApJ, 632, 217CrossRefGoogle Scholar
Werner, M. W., et al. 2004, ApJS, 154, 1CrossRefGoogle Scholar