Hostname: page-component-cd9895bd7-gbm5v Total loading time: 0 Render date: 2024-12-28T20:24:56.035Z Has data issue: false hasContentIssue false
  • English
  • Français

Low Metallicity Galaxies at z ~ 0.7: Keys to the Origins of Metallicity Scaling Laws

Published online by Cambridge University Press:  01 June 2008

David J. Rosario ,
Carlos Hoyos ,
David Koo  and
Andrew Phillips
David J. Rosario
Affiliation:
Dept. of Astronomy and Astrophysics, University of California – Santa Cruz, Santa Cruz, California, USA, 95064 email: rosario@ucolick.org, koo@ucolick.org, phillips@ucolick.org
Carlos Hoyos
Affiliation:
Departmento de Fisica Teórica, Universidad Autónoma de Madrid, Carretera de Colmenar Viejo kn 15.600 28049, Madrid, Spain email: charly.hoyos@uam.es
David Koo
Affiliation:
Dept. of Astronomy and Astrophysics, University of California – Santa Cruz, Santa Cruz, California, USA, 95064 email: rosario@ucolick.org, koo@ucolick.org, phillips@ucolick.org
Andrew Phillips
Affiliation:
Dept. of Astronomy and Astrophysics, University of California – Santa Cruz, Santa Cruz, California, USA, 95064 email: rosario@ucolick.org, koo@ucolick.org, phillips@ucolick.org
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.

We present a study of remarkably luminous and unique dwarf galaxies at redshifts of 0.5 < z < 0.7, selected from the DEEP2 Galaxy Redshift survey by the presence of the temperature sensitive [OIII]λ4363 emission line. Measurements of this important auroral line, as well as other strong oxygen lines, allow us to estimate the integrated oxygen abundances of these galaxies accurately without being subject to the degeneracy inherent in the standard R23 system used by most studies. [O/H] estimates range between 1/5–1/10 of the solar value. Not surprisingly, these systems are exceedingly rare and hence represent a population that is not typically present in local surveys such as SDSS, or smaller volume deep surveys such as GOODS.

Our low-metallicity galaxies exhibit many unprecedented characteristics. With B-band luminosities close to L*, thse dwarfs lie significantly away from the luminosity-metallicity relationships of both local and intermediate redshift star-forming galaxies. Using stellar masses determined from optical and NIR photometry, we show that they also deviate strongly from corresponding mass-metallicity relationships. Their specific star formation rates are high, implying a significant burst of recent star formation. A campaign of high resolution spectroscopic follow-up shows that our galaxies have dynamical properties similar to local HII and compact emission line galaxies, but mass-to-light ratios that are much higher than average star-forming dwarfs.

The low metallicities, high specific star formation rates, and small halo masses of our galaxies mark them as lower redshift analogs of Lyman-Break galaxies, which, at z ~ 2 are evolving onto the metallicity sequence that we observe in the galaxy population of today. In this sense, these systems offer fundamental insights into the physical processes and regulatory mechanisms that drive galaxy evolution in that epoch of major star formation and stellar mass assembly.

Keywords

surveysgalaxies: abundancesgalaxies: kinematicsgalaxies: starburst
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Issue S255: Low-Metallicity Star Formation: From the First Stars to Dwarf Galaxies , June 2008 , pp. 397 - 401
Copyright
Copyright © International Astronomical Union 2008

References

Bruzual, G. & Charlot, S. 2003, MNRAS, 344, 1000CrossRefGoogle Scholar
Coil, A., Newman, J., Kaiser, N., Davis, M., Ma, C., Kocevski, D., & Koo, D. 2004, ApJ, 617, 765CrossRefGoogle Scholar
Davis, M. et al. 2003, Proc SPIE, 4834, 161CrossRefGoogle Scholar
Davis, M. et al. 2005, ASPC Vol. 339, 128Google Scholar
Davis, M. et al. 2007, ApJ (Letters), 660, L1CrossRefGoogle Scholar
Erb, D., Shapley, A., Pettini, M., Steidel, C., Reddy, N., & Adelberger, K. 2006, ApJ, 644, 813CrossRefGoogle Scholar
Guzmán, R., Östlin, G., Kunth, D., Bershady, M., Koo, D., & Pahre, M. 2003, ApJL, 586, L45CrossRefGoogle Scholar
Hoyos, C., Koo, D., Phillips, A., Willmer, C., & Guhathakurta, P. 2005, ApJL, 635, L21CrossRefGoogle Scholar
Hoyos, C., Rosario, D., Koo, D., & Phillips, A. 2008, in prepGoogle Scholar
Kennicutt, R., Tamblyn, P., & Congdon, C. 1994, ApJ, 435, 22CrossRefGoogle Scholar
Koo, D., Guzman, R., Faber, S., Illingworth, G., Bershady, M., Kron, R., & Takamiya, M. 1995, ApJL, 440, L49CrossRefGoogle Scholar
Lee, H., Skillman, E., Cannon, J., Jackson, D., Gehrz, R., Polomski, E., & Woodward, C. 2006, ApJ, 647, 970CrossRefGoogle Scholar
Lin, L., et al. 2007, ApJL, 660, L51CrossRefGoogle Scholar
Maier, C., Lilly, S., Carollo, C., Stockton, A., & Brodwin, M. 2005, ApJ, 634, 849CrossRefGoogle Scholar
Pagel, B., Simonson, E., Terlevich, R., & Edmunds, M. 1992, MNRAS, 255, 325CrossRefGoogle Scholar
Pérez-Montero, E., & Dáz, A. I. 2003, MNRAS, 346, 105CrossRefGoogle Scholar
Savaglio, S., et al. 2005, ApJ, 635, 260CrossRefGoogle Scholar
Shapley, A., Erb, D., Pettini, M., Steidel, C., & Adelberger, K. 2004, ApJ, 612, 108CrossRefGoogle Scholar
Tremonti, C. A. et al. 2004, ApJ, 613, 898CrossRefGoogle Scholar
Willmer, C. N. A., et al. 2006, ApJ, 647, 853CrossRefGoogle Scholar