Euclid Quick Data Release (Q1)

作者：L. Bisigello, G. Rodighiero, S. Fotopoulou, F. Ricci, K. Jahnkę, A. Feltre, V. Allevato, F. Shankar, P. Cassata, E. Dalla Bontà, G. Gandolfi, G. Girardi, M. Giulietti, A. Grazian, C. R. Lovell, R. Maiolino, T. Matamoro Zatarain, M. Mezcua, I. Prandoni, D. Roberts, W. Roster, M. Salvato, M. Siudek, F. Tarsitano, Yoshiki Toba, A. Vietri, Lingyu Wang, G. Zamorani, M. Baes, S. Belladitta, Angelos Nersesian, L. Spinoglio, X. López López, N. Aghanim, B. Altieri, A. Amara, S. Andreon, N. Auricchio, H. Aussel, C. Baccigalupi, M. Baldi, A. Balestra, S. Bardelli, Alberto Basset, P Battaglia, R. Bender, A. Biviano, A Bonchi, E. Branchini, M. Brescia, J. Brinchmann, S. Camera, G Cañas-Herrera, V. Capobianco, C. Carbone, J. Carretero, Santiago Casas, M. Castellano, G. Castignani, S Cavuoti, K. C. Chambers, A Cimatti, C. Colodro-Conde, G. Congedo, Christopher J. Conselice, L. Conversi, Y. Copin, F Courbin, H. M. Courtois, M. Cropper, A. Da Silva, H. Degaudenzi, G. De Lucia, A. M. Di Giorgio, C. Dolding, H. Dole, F Dubath, C. A. J. Duncan, X. Dupac, S. Dusini, A. Ealet, S. Escoffier, M. Farina, R Farinelli, F Faustini, S Ferriol, F. Finelli⋆, M. Frailis, E. Franceschi, S. Galeotta, Koshy George, W. Gillard, B Gillis, C. Giocoli, P. Gómez-Álvarez, J. Gracia-Carpio, B. R. Granett, F. Grupp, Stephen Gwyn, S. V. H. Haugan, Henk Hoekstra, W. A. Holmes, I. Hook, F. Hormuth, A. Hornstrup, P. Hudelot, M. Jhabvala, E. Keihänen, S. Kermiche, A. Kiessling, B. Kubik, M. Kümmel, M. Kunz, H Kurki-Suonio, Q. Le Boulc'h, A.M.C Le Brun, D. Le Mignant, P. Liebing, S. Ligori, P. B. Lilje, V. Lindholm, I. Lloro, G Mainetti, D Maino, E Maiorano, O. Mansutti, S. Marcin, O Marggraf, M. Martinelli, N. Martinet, F. Marulli, R Massey, S. Maurogordato, E. Medinaceli, S. Mei, M. Melchior, Y. Mellier, M. Meneghetti, E Merlin, G. Meylan, A. Mora, M. Moresco, L. Moscardini, R. Nakajima, C. Neissner, S.-M Niemi, J.W Nightingale, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, Will J. Percival, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L.A. Popa, L. Pozzetti, F. Raison, R. Rébolo, A. Renzi, Jason Rhodes, G. Riccio, E. Romelli, M. Roncarelli, E. Rossetti, H. J. A. Röttgering, B. Rusholme, R Saglia, Z. Sakr, D Sapone, B. Sartoris, J.A Schewtschenko, M. Schirmer, Peter Schneider, T. Schrabback, M. Scodeggio, A. Secroun, G Seidel, S Serrano, P. Šimon, C. Sirignano, G. Sirri, L. Stanco, J. Steinwagner, P. Tallada-Crespí, A.N. Taylor, H.I Teplitz, I. Tereno, Sune Toft, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, L. Valenziano, J. Väliviita, T. Vassallo, G. Verdoes Kleijn, A. Veropalumbo, Yun Wang, J. Weller, A Zacchei, F. M. Zerbi, I. A. Zinchenko, E. Zucca, M. Ballardini, M. Bolzonella, E. Bozzo, C. Burigana, R. Cabanac, A. Cappi, D. Di Ferdinando, J.A. Escartin Vigo, L. Gabarra, J Martín-Fleitas, S Matthew, M. Maturi, N. Mauri, A Pezzotta, M. Pöntinen, C. Porciani, I Risso, V Scottez, M. Sereno, M. Tenti, Matteo Viel, M. Wiesmann, Y. Akrami, I.T Andika, S Anselmi, M. Archidiacono, F. Atrio‐Barandela, Christophe Benoıst, K Benson, Daniele Bertacca, M. Béthermin, A. Blanchard, L Blot, M.L Brown, S Bruton, A Calabrò, F Caro, C. S. Carvalho, T. Castro, Yann Philippe Charles, F Cogato, T. Contini, A.R. Cooray, O. Cucciati, S. Davini, F. De Paolis, G. Desprez, A. Díaz‐Sánchez, J.J Diaz, S. Di Domizio, J. M. Diego, A Enia, Yuhong Fang, A.G Ferrari, P.G Ferreira, A. Finoguenov, A. Fontana, Fabio Fontanot, A. Franco, K. Ganga, J. García-Bellido, T Gasparetto, V Gautard, E. Gaztañaga, F. Giacomini, F. Gianotti, G. Gozaliasl, M Guidi, C. M. Gutiérrez, Alex Hall, W.G Hartley, Shoubaneh Hemmati, C. Hernández-Monteagudo, H. Hildebrandt, J. Hjorth, J. J. E. Kajava, Y. W. Kang, V. Kansal, D. Karagiannis, K. Kiiveri, C. C. Kirkpatrick, Sandor Kruk, J Le Graet, L Legrand, Maria Lembo, F Lepori, G Leroy, G.F Lesci, J. Lesgourgues, L. Leuzzi, T.I Liaudat, A. Loureiro, J. F. Macías–Pérez, G. Maggio, M. Magliocchetti, E. A. Magnier, C. Mancini, F. Mannucci, R. Maoli, C.J.A.P. Martins, L. Maurin, M Miluzio, P. Monaco, Claudio Moretti, G Morgante, S. Nadathur, Krishna Naidoo, A. Navarro-Alsina, S Nesseris, F Passalacqua, K. Paterson, L. Patrizii, A. Pisani, D. Potter, S Quai, M. Radovich, P.-F Rocci, S Sacquegna, M Sahlén, D. B. Sanders, E Sarpa, Claudia Scarlata, J. Schaye, Aurel Schneider, D Sciotti, E. Sellentin, A. Shulevski, L. C. Smith, K Tanidis, C. Tao, G. Testera, R Teyssier, S. Tosi, A. Troja, M. Tucci, C Valieri, A. Venhola, D. Vergani, G Verza, P Vielzeuf, A. Viitanen, N. A. Walton, John R. Weaver, É. Soubrié, D. Scott · 发表于：Astronomy and Astrophysics · 年份：2025 · DOI：10.1051/0004-6361/202554537 · 被引用次数：9 · 研究领域：Impact of Light on Environment and Health、Astronomical Observations and Instrumentation

Recent observations with the James Webb Space Telescope (JWST) have revealed an interesting population of sources with a compact morphology and a characteristic v-shaped continuum, namely blue at a rest frame λ < 4000 Å and red at longer wavelengths. The nature of these sources, which are called little red dots (LRDs), is still highly debated because it is unclear whether they host active galactic nuclei (AGNs) and their number seems to drop drastically at z < 4. We took advantage of the 63 deg 2 covered by the Euclid Quick Data Release (Q1) to extend the search for LRDs to brighter magnitudes and lower redshifts than what was possible with JWST. This is fundamental for a broader view of the evolution of this peculiar galaxy population. The selection was performed by fitting the available photometric data ( Euclid , the Spitzer Infrared Array Camera (IRAC), and ground-based griz data) with two power laws to retrieve the rest-frame optical and UV slopes consistently over a wide redshift range (i.e. z < 7.6). We then excluded extended objects and possible line emitters and inspected the data visually to remove any imaging artefacts. The final selection included 3341 LRD candidates from z = 0.33 to z = 3.6, 29 of which were also detected in IRAC. The resulting rest-frame UV luminosity function, in contrast with previous JWST studies, shows that the number density of LRD candidates increases from high redshift to z = 1.5–2.5 and decreases at even lower redshifts. The sub...