2001/09/13 by S. Phleps, Phleps, S., K. Meisenheimer +1
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #FOS: Physical sciences #Galaxies: Formation, Evolution, Phenomena #Scientific Research and Discoveries #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0109202
5 pages, to appear in ''Where's the Matter? Mapping Dark and Bright Matter with the New Generation of Large Scale Surveys'', Proceedings of a Conference held in Marseille, June 25.-29. 2001
arxiv created 2001/09/13 · openalex publication_date 2001/09/13 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present results of an investigation of clustering evolution of field galaxies between a redshift of z~1 and the present epoch. The current analysis relies on a sample of ~3600 galaxies from the Calar Alto Deep Imaging Survey (CADIS). The multicolor classification and redshift determination is reliable up to I=23. The redshift distribution extends to z~1.1, the resolution is Delta cz=12000 km s-1. Thus the amplitude of the three-dimensional correlation function has to be estimated by means of the projected correlation function w(rp). The validity of the deprojection was tested on the Las Campanas Redshift Survey (LCRS). The LCRS also serves as ''local'' measurement. We invented a new method to overcome the influence of redshift errors on w(rp). For evolution of the clustering strength the ansatz xi(rcom,z)proportional to (1+z)q is used. For the galaxies as a whole the evolution parameter turns out to be q~-1.9, according to the prediction of linear theory. A formal dependency on the cosmology is presumably due to the small number of fields observed. However, the measured clustering growth clearly depends on Hubble type. At z~1 early type galaxies are already much stronger clustered, an increase with q~-1 is sufficient to explain the present day amplitude of the correlation function.