Pozzi, F.; Gruppioni, C.; Oliver, S.; Matute, I.; La Franca, F.; Lari, C.; Zamorani, G.; Serjeant, S.; Franceschini, A. and Rowan-Robinson, M.
|DOI (Digital Object Identifier) Link:||http://doi.org/10.1086/420963|
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We present the first determination of the 15 mum luminosity function of galaxies from the European Large Area ISO Survey (ELAIS) southern fields. We have adopted a new criterion to separate the quiescent, nonevolving and the starburst, evolving populations based on the ratio of mid-infrared to optical luminosity. Strong evolution is suggested by our data for the starburst galaxy population, while normal spiral galaxies are consistent with no evolution. The starburst population must evolve both in luminosity and in density with rates of the order L(z)~(1+z)3.5 and rho(z)~(1+z)3.8, respectively, up to z~1. The evolutionary parameters of our model have been tested by comparing the model predictions with other observables, like source counts at all flux density levels (from 0.1 to 300 mJy) and redshift distributions and luminosity functions at high z (0.7<z<1.0 from Hubble Deep Field North [HDF-N] data). The agreement between our model predictions and the observed data is remarkably good. We use our data to estimate the star formation density of the universe up to z=0.4, and we use the luminosity function model to predict the trend of the star formation history up to z=1.
|Item Type:||Journal Article|
|Extra Information:||Some of the symbols may not have transferred correctly into this bibliographic record and/or abstract.|
|Keywords:||evolution; galaxies; luminosity function; mass function; spiral; starburst; infrared|
|Academic Unit/Department:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Users 13 not found.|
|Date Deposited:||25 Oct 2006|
|Last Modified:||04 Oct 2016 09:55|
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