Euclid Collaboration R. Vannier 2 , S. Maurogordato 2 , A. Biviano 4 , C. Adami 5 , B. Ascaso 6 , F. Bellagamba 7 ,8 , C. Benoist 2 , A. Cappi 2 ,8 , A. Durret 10 , S. Farrens 11 , A. Gonzalez 12 , A. Iovino 13 , R. Licitra 6 ,14 , M. Maturi 15 , S. Mei 6 ,14 ,16 , A. Merson 16 ,17 , E. Munari 4 ,18 ,19 , R. Ricci 2 , P. Rocci 2 , M. Roncarelli 7 ,8 , F. Sarron 10 , Y. Amoura 10 , S. Andreon 13 , N. Apostolakos 21 , M. Arnaud 11 ,22 , S. Bardelli 8 , J. Bartlett 23 , C.
Baugh 24 , S. Borgani 4 ,18 ,25 , M. Brodwin 26 , F. Castander 27 ,28 , G. Castignani 6 ,29 ,2 ,44 , O. Cucciati 8 , G. De Lucia 4 , P. Dubath 21 , P. Fosalba 27 ,28 , C. Giocoli 7 ,8 ,30 , H. Hoekstra 31 , G. Mamon 10 , J. Melin 11 , L. Moscardini 7 ,8 ,30 , S. Paltani 21 , M. Radovich 32 , B. Sartoris 18 , M. Schultheis 2 , M. Sereno 8 ,7 , J. Weller 33 ,34 ,35 , C. Burigana 36 ,37 ,38 , C. Carvalho 39 , L. Corcione 40 , H. Kurki-Suonio 41 , P. Lilje 42 , G. Sirri 30 , R.
Toledo-Moreo 43 and G. Zamorani 8. Adam oca. Received: 18 January Accepted: 27 May Galaxy cluster counts in bins of mass and redshift have been shown to be a competitive probe to test cosmological models. This method requires an efficient blind detection of clusters from surveys with a well-known selection function and robust mass estimates, which is particularly challenging at high redshift.
The Euclid wide survey will cover 15 deg 2 of the sky, avoiding contamination by light from our Galaxy and our solar system in the optical and near-infrared bands, down to magnitude 24 in the H -band. The objective of these challenges was to select the cluster detection algorithms that best meet the requirements of the Euclid mission. The final CFC included six independent detection algorithms, based on different techniques, such as photometric redshift tomography, optimal filtering, hierarchical approach, wavelet and friend-of-friends algorithms.
These algorithms were blindly applied to a mock galaxy catalog with representative Euclid -like properties. Galaxy clusters are good tracers of the matter density peaks in the cosmic web. They additionally provide efficient tests for cosmological models as they form via gravitational collapse in the expanding Universe for a review, see Allen et al.
