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Please use this identifier to cite or link to this item: http://hdl.handle.net/1959.3/93975
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- An imaging K-band survey - II. the redshift survey and galaxy evolution in the infrared
- Glazebrook, Karl; Peacock, J. A.; Collins, C. A.; Miller, L.
- We present further results from an imaging K-band survey of 552 arcmin2, complete to a 5σ limit of K ≃ 17.3. This paper describes a redshift survey of 124 galaxies, and addresses the colours of faint galaxies and the evolution of the K-band luminosity function. The optical-to-infrared colours are consistent with the range expected from synthetic galaxy spectra, although there are some cases of very red nuclei. These may possibly be attributed to either extinction or metallicity gradients. Our data show no evidence for evolution of the K-band luminosity function at z < 0.5, and the results are well described by a Schechter function with M K = -22.75 ± 0.13 + 5 log10 h and Φ = 0.026±0.003 h3 Mpc−3. This is a somewhat higher normalization than has been found by previous workers, and it removes much of the excess in faint K and bJ counts with respect to a no-evolution model. However, we do find evidence for evolution at z > 0.5: M K is approximately 0.75 mag. brighter at z = 1. This luminosity evolution is balanced by a reduced normalization at high redshift: the total luminosity density is required to be approximately constant in order not to exceed the faint counts. The overall evolution is thus opposite to that expected in simple merger-dominated models; we briefly consider possible interpretations of this result.
- Publication type
- Journal article
- Monthly Notices of the Royal Astronomical Society, Vol. 275 (1995), pp. 169-184
- Publication year
- Galaxy evolution; Infrared; Low-mass stars; Luminosity function; Mass function; Redshift galaxies; Surveys
- Wiley-Blackwell Publishing
- Publisher URL
- Copyright © 1995 RAS. The accepted manuscript of the paper is reproduced here in accordance with the copyright policy of the publisher. The definitive publication is available at www.interscience.wiley.com.
- Full text
- Peer reviewed