Bibcode
Ascaso, B.; Quintana, J. M.; Prada, F.; Husillos, C.; Infante, L.; Hurtado-Gil, L.; Delgado, R. M. González; Cristóbal-Hornillos, D.; Cerviño, M.; Cabrera-Caño, J.; Castander, F. J.; Cepa, J.; Broadhurst, T.; Aparicio-Villegas, T.; Alfaro, E.; Perea, J.; Moles, M.; Olmo, A. Del; Viironen, K.; Aguerri, J. A. L.; Varela, J.; Pović, M.; Masegosa, J.; Nieves-Seoane, L.; Márquez, I.; Dupke, R.; Cenarro, A. J.; Martínez, V. J.; Díaz-García, L. A.; Merson, A. I.; Huertas-Company, M.; Jiménez-Teja, Y.; Schoenell, W.; Molino, A.; López-Sanjuan, C.; Arnalte-Mur, P.; Fernández-Soto, A.; Benítez, N.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society, Volume 452, Issue 1, p.549-565
Advertised on:
9
2015
Citations
17
Refereed citations
17
Description
We present a catalogue of 348 galaxy clusters and groups with 0.2 < z
< 1.2 selected in the 2.78 deg2 Advanced Large,
Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey.
The high precision of our photometric redshifts, close to 1 per cent,
and the wide spread of the seven ALHAMBRA pointings ensure that this
catalogue has better mass sensitivity and is less affected by cosmic
variance than comparable samples. The detection has been carried out
with the Bayesian Cluster Finder, whose performance has been checked in
ALHAMBRA-like light-cone mock catalogues. Great care has been taken to
ensure that the observable properties of the mocks photometry accurately
correspond to those of real catalogues. From our simulations, we expect
to detect galaxy clusters and groups with both 70 per cent completeness
and purity down to dark matter halo masses of Mh ˜ 3
× 1013 M⊙ for z < 0.85. Cluster
redshifts are expected to be recovered with ˜0.6 per cent
precision for z < 1. We also expect to measure cluster masses with
σ _{M_h|M^*_{CL}}˜ 0.25-0.35 dex precision down to ˜ 3
× 1013 M⊙, masses which are 50 per cent
smaller than those reached by similar work. We have compared these
detections with previous optical, spectroscopic and X-rays work, finding
an excellent agreement with the rates reported from the simulations. We
have also explored the overall properties of these detections such as
the presence of a colour-magnitude relation, the evolution of the
photometric blue fraction and the clustering of these sources in the
different ALHAMBRA fields. Despite the small numbers, we observe
tentative evidence that, for a fixed stellar mass, the environment is
playing a crucial role at lower redshifts (z < 0.5).
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