The Faintest and Closest Clusters in CFHTLS W4

Abstract

Introduction

Material and Methods

Results

Discussion

Keywords

• Photometric redshift,large scale structure,galaxies

References

1. Arnouts, S. et al., 1999, Measuring and modelling the redshift evolution of clustering: the Hubble Deep Field North, Monthly Notices of the Royal Astronomical Society, 310, 540.
2. Coleman, G. D. et al., 1980, Colors and magnitudes predicted for high redshift galaxies, The Astrophysics of Journal Suplement, 43, 393C.
3. Coupon, J. et al., 2009, Photometric redshifts for the CFHTLS T0004 deep and wide fields, Astronomy & Astrophysics, 500, 981C.
4. Feuerbacher, B. and Stoewer, H., 2006, Utilization of Space: Today and Tomorrow, Springer, ISBN: 354029970X.
5. Garilli, B., et al., 2014, The VIMOS Public Extragalactic Survey (VIPERS). First Data Release of 57 204 spectroscopic measurements, Astronomy & Astrophysics, 562A, 23G.
6. Hudelot, P. et al., 2012, T0007: The Final CFHTLS Release, CFHTLS, http://www.cfht.hawaii.edu/Science/CFHLS/T0007/, [visiting date: 1st June 2013].
7. Ilbert, O. et al., 2006, Accurate Photometric Redshifts for the CFHT Legacy Survey Calibrated Using the VIMOS VLT Deep Survey, Astronomy & Astrophysics, 457, 841.
8. İğdi-Şen, M. 2018, The Reliability of Redshift Values in Determination of Structures in the Universe, JoCREST, 4, 69-80.

9. Kinney, A. L. et al., 1996, Template Ultraviolet to Near-Infrared Spectra of Star-forming Galaxies and Their Application to K-Corrections, The Astrophysics of Journal, 467, 38.
10. Le Fèvre, O. et al., 2005, The VIMOS VLT deep survey. First epoch VVDS-deep survey: 11 564 spectra with 17.5 ≤ IAB ≤ 24, and the redshift distribution over 0 ≤ z ≤ 5, Astronomy & Astrophysics,439, 845L.
11. Terapix1, 2012, CFHTLS-Deep &Wide targets, Terapix, http://terapix.iap.fr/ cplt/T0007/table_syn_T0007.html, [visiting date: 1st January 2015].
12. Wen, Z. L.and Han, J. L., 2011, Galaxy Clusters at High Redshift and Evolution of Brightest Cluster Galaxies, The Astrophysics of Journal, 734, 68W.