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Spectroscopic signatures of galaxy evolution in Cl0024+16 at $z\sim 0.4$

Published online by Cambridge University Press:  06 October 2004

Sean M. Moran ,
Richard S. Ellis  and
Tommaso Treu
Sean M. Moran
Affiliation:
California Institute of Technology, Department of Astronomy, Mail Code 105-24, Pasadena, CA 91125, USA email: [email protected], [email protected]
Richard S. Ellis
Affiliation:
California Institute of Technology, Department of Astronomy, Mail Code 105-24, Pasadena, CA 91125, USA email: [email protected], [email protected]
Tommaso Treu
Affiliation:
University of California at Los Angeles, Department of Physics & Astronomy, Los Angeles, CA 90095, USA email: [email protected]
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Abstract

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We report the first results from a panoramic spectroscopic survey of galaxies in the rich cluster Cl0024+1654 ($z\simeq 0.4$). Using HST imaging we examine the properties of early-types as a function of cluster radius. At all cluster radii, our sample lies on a self-consistent Fundamental Plane whose zero point implies evolution since $z=0$ corresponding to $\Delta[\log (M/L_V)] = 0.14 \pm 0.06$, an overall trend consistent with previous work. Using diagnostic [O II] emission and Balmer absorption lines, we locate a population of intrinsically faint galaxies at 1–2.4 Mpc radius undergoing a period of star formation. The luminosity-dependent radial trends are suggestive of the gradual quenching of star formation for infalling galaxies. We discuss physical mechanisms that may be responsible for this environmental evolution.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUC195 , March 2004 , pp. 384 - 389
Copyright
© 2004 International Astronomical Union