Euclid: A blue galaxy population and a brightest cluster galaxy in the making in a z∼ 1.74 MaDCoWS2 galaxy cluster candidate

We present an example cluster follow-up study with . Our target, a z∼ 1.74 candidate cluster nicknamed the `Puddle', was initially discovered by the Massive and Distant Clusters of WISE Survey 2 as a z_ ∼ 1.65 candidate cluster. It was also detected independently as a z_ ∼ 1.5 candidate with the two cluster-finding algorithms in Euclid Quick Release 1 (Q1). A Keck MOSFIRE spectrum shows the brightest nucleus is at z=1.74 and is dominated by an active galactic nucleus. Our analysis focused on the galaxy population and the brightest cluster galaxy (BCG), and is based on and ancillary photometry. Compared to similar fields, we measured an overdensity of 110± 14 galaxies with ̋Ełeq 22.25 in a imaging revealed that six or seven galaxies appear to be assembling to form the future BCG. Spectral energy distribution fitting suggests that the merging BCG has a stellar mass of 5.7± 0.3 ,M_⊙ and that it experienced a short burst of star formation ∼ 300,Myr ago. Its morphology and star-formation history suggest that the proto-BCG is a more evolved version of the merging core of SPT2349-56. These systems indicate that multiobject mergers might be a common BCG formation process. Assuming a similar density of mergers in the Euclid Wide Survey, we expect that will discover approximately 400 assembling BCGs by the end of its mission. Euclid phot phot Euclid radius around the BCG. About 18± 4% of the completeness-corrected galaxy population is red, which is consistent with some clusters at z>1.5 but lower than others. Euclid 10^ 11 Euclid

Authors

Publication Details

Journal
Springer Link (Chiba Institute of Technology)
Published
2026-03-16
DOI
https://doi.org/10.1051/0004-6361/202557760/pdf
Primary Topic
Galaxies: Formation, Evolution, Phenomena
Type
article
Field-Weighted Citation Impact
0.00
Controls
|||
ALL TIME
JAN
FEB
MAR
APR
MAY
JUN
JUL
AUG
SEP
OCT
article

Euclid: A blue galaxy population and a brightest cluster galaxy in the making in a z∼ 1.74 MaDCoWS2 galaxy cluster candidate

E. (E) Maiorano, E. (E) Branchini, M. (M) Frailis, S. (S) Cavuoti et al.
Springer Link (Chiba Institute of Technology)
Galaxies: Formation, Evolution, Phenomena
article

Euclid: A blue galaxy population and a brightest cluster galaxy in the making in a z∼ 1.74 MaDCoWS2 galaxy cluster candidate

E. (E) Maiorano, E. (E) Branchini, M. (M) Frailis, S. (S) Cavuoti, S. (S) Mei, F. (F) Dubath, S. (S) Bardelli, O. (O) Marggraf, T. (T) Vassallo, L. (L) Valenziano, C. (C.A.J) Duncan, A. (A.M.C) Le Brun, Z. (Z) Sakr, F. (F) Courbin, A. (A) Cimatti, M. (M) Fumana, W. (W.J) Percival, H. (H) Degaudenzi, N. (N) Martinet, S. (S) Serrano, E. (E) Medinaceli, B. (B) Gillis, S. (S) Camera, S-M. (S.-M) Niemi, S. (S) Ferriol, S. Moreno Pires, J. (J) Weller, G. (G) Congedo, K. (K) George, H. (H) Dole, G. (G) Seidel, J. (J) García-Bellido, K. (K) Jahnke, A. (A) Balestra, A. (A) Mora, F. (F.M) Zerbi, C. (C) Giocoli, S. (S) Andreon, J. (J) Gracia-Carpio, R. (R) Toledo-Moreo, L. (L) Pozzetti, E. (E) Zucca, Y. (Y) Wang, C. (C.J) Conselice, G. (G) Castignani, F. (F) Finelli, E. (E) Romelli, G. (G) Meylan, M. (M) Meneghetti, B. Sartoris, A. (A) Renzi, J. (J) Valiviita, P. (P.R.M) Eisenhardt, L. (L) Moscardini, K. Thongkham, M. (M) Castellano, M. (M) Farina, R. (R) Massey, S. (S.V.H) Haugan, H. (H.I) Teplitz, F. (F) Torradeflot, B. (B) Altieri, F. (F) Pasian, J. (J) Rhodes, X. (X) Dupac, I. (I) Tutusaus, M. (M) Cropper, M. Maturi, R. (R) Saglia, F. (F) Raison, B. (B) Kubik, M. (M) Kunz, I. (I) Lloro, C. (C) Baccigalupi, A. (A) Hornstrup, E. (E) Keihänen, V. (V) Scottez, A. (A) Secroun, K. (K) Pedersen, V. (V) Pettorino, A. Trudeau, S. (S) Escoffier, C. (C) Carbone, G. (G) Polenta, S. (S) Dusini, J. (J) Steinwagner, F. (F) Marulli, F. (F) Faustini, C. (C) Neissner, D. (D) Sapone, B. (B) Joachimi, G. (G) Sirri, S. (S) Galeotta, S. Shamyati, S. (S) Taamoli, E. (E) Merlin, H. (H.M) Courtois, S. (S.A) Stanford, D. (D) Maino, Y. (Y) Copin, M. (M) Fabricius, K. (K.C) Chambers, A. (A) da Silva, S. (S) Ligori, C. (C) Colodro-Conde, H. (H) Kurki-Suonio, S. (S) Paltani, A. (A.H) Gonzalez, S. (S) Toft, P. (P.B) Lilje, P. (P) Schneider, G. (G) Canas-Herrera, L. (L.A) Popa, G. (G) de Lucia, O. (O) Mansutti, V. (V) Capobianco, G. (G) Riccio, M. (M) Poncet, D. (D) Le Mignant, N. (N) Tessore, S. (S) Kermiche, M. (M) Jhabvala, L. (L) Conversi, J. (J) Carretero, F. (F) Grupp, M. (M) Kilbinger, B. (B) Mobasher, E. (E) Franceschi, V. (V) Lindholm, M. (M) Sereno, A. (A) Biviano, C. (C) Padilla, M. (M) Martinelli, R. (R) Nakajima, M. (M) Baldi, M. (M) Kümmel, Y. Mellier, M. (M) Roncarelli, A. (A) Grazian, D. (D) Stern, T. (T) Schrabback, F. (F) Hormuth, M. (M) Brescia, C. (C) Sirignano, G. (G) Zamorani, A. Starke Taylor, G. (G) Mainetti, S. (S) Casas, I. (I) Tereno, W. (W) Holmes, M. (M) Douspis, E. (E) Munari, S. (S) Maurogordato, P. Tallada-Crespí, L. (L) Stanco
article en

Abstract

We present an example cluster follow-up study with . Our target, a z∼ 1.74 candidate cluster nicknamed the `Puddle', was initially discovered by the Massive and Distant Clusters of WISE Survey 2 as a z_ ∼ 1.65 candidate cluster. It was also detected independently as a z_ ∼ 1.5 candidate with the two cluster-finding algorithms in Euclid Quick Release 1 (Q1). A Keck MOSFIRE spectrum shows the brightest nucleus is at z=1.74 and is dominated by an active galactic nucleus. Our analysis focused on the galaxy population and the brightest cluster galaxy (BCG), and is based on and ancillary photometry. Compared to similar fields, we measured an overdensity of 110± 14 galaxies with ̋Ełeq 22.25 in a imaging revealed that six or seven galaxies appear to be assembling to form the future BCG. Spectral energy distribution fitting suggests that the merging BCG has a stellar mass of 5.7± 0.3 ,M_⊙ and that it experienced a short burst of star formation ∼ 300,Myr ago. Its morphology and star-formation history suggest that the proto-BCG is a more evolved version of the merging core of SPT2349-56. These systems indicate that multiobject mergers might be a common BCG formation process. Assuming a similar density of mergers in the Euclid Wide Survey, we expect that will discover approximately 400 assembling BCGs by the end of its mission. Euclid phot phot Euclid radius around the BCG. About 18± 4% of the completeness-corrected galaxy population is red, which is consistent with some clusters at z>1.5 but lower than others. Euclid 10^ 11 Euclid

Springer Link (Chiba Institute of Technology)
Openalex Percentile: Top 16%
Galaxies: Formation, Evolution, Phenomena
DOISourceOpenAlex
AI Navigator

Ask Laika to Summarize, Analyze, and Connect papers live on the map.

Summarize Papers & Methodologies

Extract key findings, datasets, and comparative methods across publications.

Benchmark Rankings & Visual Analytics

Rank top research institutions, authors, funders, topics, and journals by Field-Weighted Citation Impact (FWCI) and paper volume with instant charts.

Connect Distant Disciplines

Bridge topological clusters on the map to find hidden collaborative intersections.