Euclid Quick Data Release (Q1). Euclid spectroscopy of quasars. 1. Identification and redshift determination of 3500 bright quasars

The slitless spectroscopy mode of the on board the Euclid telescope has enabled efficient spectroscopy of objects within a large field of view. Nevertheless, the relatively low spectral resolution, overlapping spectra, and contamination pose challenges to source classification and redshift determination using the spectra alone. In this work, we present a large and homogeneous sample of bright quasars identified from the Euclid Quick Data Release (Q1), constructed by combining high-purity candidate selections from to wavelengths without telluric lines, which will be pivotal to quasar spectral analysis. We obtained an empirical spectroscopic depth of JE łesssim 21.5 and ̋E łesssim 21.3 at the sensitivity of the Wide Field Survey, beyond which the number of securely identified quasars declines sharply. Accordingly, the sample presented in this paper comprises spectroscopically confirmed quasars brighter than these limits. We analysed morphological parameters from the Visible Camera (VIS) using Sérsic and model-independent (CAS) metrics, and a deep-learning point spread function fraction to track nuclear dominance. The VIS morphologies show a clear redshift dependence: at low redshift (z<0.5), obvious host structures are common and a single Sérsic model fits about half of the sources; at intermediate redshift (0.5<z<2), the nuclear component dominates, with 90% of the Sérsic fits saturating at the upper index limit. In this intermediate redshift regime, f_ nisp nisp and WISE with the new spectroscopic capabilities of Euclid. Through visual inspection of the Euclid spectra of these quasar candidates, we identify approximately 3500 quasars and determine reliable redshifts in the range of 0< z łesssim4.8. Of these, 2686 are new spectroscopic identifications relative to existing public compilations. We generated the first Euclid composite spectrum of quasars covering rest-frame nuv nir nir PSF is available, and we use it as a more reliable compactness measure than the single-Sérsic and CAS parameters to quantify nuclear versus host emission. We also explore the novel Euclid colour space and discuss the role of these quasars in refining active galactic nucleus selection techniques for future Euclid data releases. nir

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Springer Link (Chiba Institute of Technology)
Published
2026-03-13
DOI
https://doi.org/10.1051/0004-6361/202558490/pdf
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Galaxies: Formation, Evolution, Phenomena
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Euclid Quick Data Release (Q1). Euclid spectroscopy of quasars. 1. Identification and redshift determination of 3500 bright quasars

E. (E) Maiorano, T. Matamoro Zatarain, E. (E) Branchini, D. (D) Paoletti et al.
Springer Link (Chiba Institute of Technology)
Galaxies: Formation, Evolution, Phenomena
article

Euclid Quick Data Release (Q1). Euclid spectroscopy of quasars. 1. Identification and redshift determination of 3500 bright quasars

E. (E) Maiorano, T. Matamoro Zatarain, E. (E) Branchini, D. (D) Paoletti, D. (D) Di Ferdinando, S. (S) Anselmi, M. (M) Frailis, L. (L) Maurin, A. (A) Díaz-Sánchez, J. (J) Lesgourgues, C. (C) Porciani, F. Tarsitano, L. (L) Gabarra, S. (S) Cavuoti, S. (S) Mei, D. G. I. Scott, H. (H) Hildebrandt, F. (F) Dubath, S. (S) Bardelli, A. (A) Calabro, G. (G) Verza, O. (O) Marggraf, P. (P) Simon, L. (L.C) Smith, T. (T) Vassallo, L. (L) Valenziano, C. (C.A.J) Duncan, M. (M) Tenti, A. (A.M.C) Le Brun, A. (A) Blanchard, J-L. (J.-L) Starck, D. (D) Potter, N. (N) Fourmanoit, Y. (Y) Fang, Z. (Z) Sakr, F. (F) Courbin, L. (L) Legrand, A. (A) Cimatti, A. (A) Veropalumbo, R. (R) Farinelli, M. (M) Fumana, W. (W.J) Percival, H. (H) Degaudenzi, B. (B) Margalef-Bentabol, J. (J) Martín-Fleitas, T. (T.I) Liaudat, W. (W) Roster, V. (V) Allevato, N. (N) Martinet, I. (I) Risso, P. (P.A.C) Cunha, S. (S) Serrano, E. (E) Medinaceli, B. (B) Gillis, S. (S) Camera, S-M. (S.-M) Niemi, K. (K) Kuijken, S. (S) Ferriol, S. Moreno Pires, S. Alvi, J. (J) Weller, G. (G) Congedo, K. (K) Tanidis, M. (M) Scodeggio, S. (S) Quai, S. (S) Bruton, K. (K) George, H. (H) Dole, F. (F) Shankar, A. (A) Feltre, G. (G) Morgante, G. (G) Seidel, A. (A) Viitanen, J. (J) García-Bellido, R. (R.C) Nichol, K. (K) Jahnke, D. (D) Vergani, A. (A) Enia, A. (A) Balestra, S. (S) Nadathur, A. (A) Pisani, A. (A) Mora, G. (G) Gozaliasl, W. (W) Gillard, M. (M) Sahlén, C. (C.M) Gutierrez, J. (J.G) Sorce, M. (M) Miluzio, C. (C) Giocoli, M. Banerji, A. (A.R) Cooray, S. (S) Andreon, J. (J) Gracia-Carpio, P. (P) Natoli, R. (R) Toledo-Moreo, L. (L) Pozzetti, C. (C) Scarlata, E. (E) Zucca, Y. (Y) Wang, J. (J.) Kim, C. (C.J) Conselice, G. (G) Castignani, E. (E) Lusso, F. (F) Finelli, R. (R.B) Metcalf, E. (E) Romelli, F. (F) Cogato, A. (A) Humphrey, C. A. B. DE CARVALHO, G. (G) Meylan, M. (M) Meneghetti, B. Sartoris, A. (A) Troja, A. (A) Renzi, J. (J) Valiviita, K. (K) Markovic, Y. (Y) Toba, C. (C.J.A.P) Martins, C. (C) Tao, M. (M.J) Page, C. (C) Dolding, S. (S) Marcin, L. (L) Moscardini, M. (M) Castellano, M. J. I. Brown, D. M. Alexander, J. (J.M) Diego, M. (M) Farina, R. (R) Massey, S. (S.V.H) Haugan, P. (P) Fosalba, S. (S) Matthew, H. (H.I) Teplitz, V. (V) Le Brun, F. (F) Torradeflot, F. (F) Pasian, D. (D.B) Sanders, E. (E) Sellentin, F. (F) Giacomini, J. (J) Rhodes, C. (C) Surace, M. (M) Wiesmann, P-F. (P.-F) Rocci, X. (X) Dupac, I. (I) Tutusaus, M. (M) Cropper, C. (C.C) Kirkpatrick, D. (D) Sciotti, A. (A) Pezzotta, R. (R) Saglia, F. (F) Raison, E. (E) Sefusatti, B. (B) Kubik, M. (M) Kunz, I. (I) Lloro, K. (K) Naidoo, F. (F) Lepori, C. (C) Baccigalupi, A. (A) Hornstrup, C. (C) Mancini, M. (M) Melchior, E. (E) Bañados, F. (F) Fontanot, E. (E) Keihänen, V. (V) Scottez, A. (A) Secroun, K. (K) Pedersen, B. Camacho Quevedo, V. (V) Pettorino, M. (M) Bethermin, M. (M) Huertas-Company, S. (S) Escoffier, G. Vietri, M. (M) Magliocchetti, C. (C) Carbone, G. (G) Polenta, K. (K) Paterson, S. (S) Dusini, D. (D) Tavagnacco, A. (A) Loureiro, L. (L) Spinoglio, J. (J) Steinwagner, E. (E) Aubourg, A. (A) Cappi, J. (J) Le Graet, F. (F) Marulli, F. (F) Ricci, C. (C) Neissner, J. (J) Hjorth, Y. (Y) Kang, M. (M) Calabrese, S. (S) Kruk, D. (D) Sapone, B. (B) Joachimi, M. (M) Schirmer, G. (G) Sirri, Q. L. Liu, S. (S) Galeotta, A. (A) Zacchei, R. (R) Cabanac, D. (D) Bertacca, A. (A) Costille, M. (M) Salvato, L. (L) Blot, A. (A) Hall, F. (F) Mannucci, E. (E) Merlin, J. (J.R) Weaver, E. (E) Rossetti, K. (K) Kiiveri, H. (H.M) Courtois, M. (M) Lembo, B. Laloux, F. (F) Caro, D. (D) Maino, M. (M) Radovich, Y. (Y) Copin, R. (R) Teyssier, P. (P) Dimauro, M. (M) Tucci, V. (V) Gautard, A. (A) Finoguenov, M. (M) Fabricius, K. (K.C) Chambers, C. (C) Burigana, O. (O) Cucciati, G. (G) Rodighiero, P. (P) Vielzeuf, A. (A) da Silva, S. (S) Ligori, A. (A.A) Nucita, C. (C) Colodro-Conde, H. (H) Kurki-Suonio, S. (S) Paltani, Y. (Y) Fu, V. (V) Kansal, S. (S) Toft, J. Wolf, G. (G) Daste, S. Belladitta, D. (D) Karagiannis, F. (F) Passalacqua, R. (R) Laureijs, S. (S) Borgani, P. (P.B) Lilje, P. (P) Schneider, E. (E) Gaztanaga, J. (J) Macias-Perez, M. (M) Viel, P-A. (P.-A) Duc, M. Scialpi, L. (L) Patrizii, T. (T) Gasparetto, G. (G) Canas-Herrera, F. (F) Gianotti, L. (L.A) Popa, A. (A) Franco, C. (C) Moretti, Y.-H. Zhang, F. (F) de Paolis, P. (P) Monaco, E. (E) Sarpa, G. (G) de Lucia, G. (G) Desprez, G. (G.F) Lesci, O. (O) Mansutti, M. (M) Guidi, G. Leroy, J. Calhau, J. Casanueva Diaz, V. (V) Capobianco, M. Siudek, G. (G) Riccio, M. (M) Poncet, N. (N) Tessore, P. (P) Franzetti, D. (D) Vibert, P. (P) Battaglia, M. (M) Pöntinen, S. (S) Kermiche, E. (E) Soubrie, A. (A) Venhola, R. Bouwens, M. (M) Ballardini, M. (M) Jhabvala, M. (M) Archidiacono, L. (L) Conversi, J. (J) Carretero, F. (F) Grupp, M. (M) Bonici, A. (A.G) Ferrari, J. A. Escartin Vigo, K. (K.I) Caputi, E. (E) Franceschi, V. (V) Lindholm, E. (E) Bozzo, M. (M) Sereno, A. (A) Schneider, A. (A) Biviano, C. (C) Padilla, A. (A) Kiessling, M. I. Gray, S. (S) Nesseris, M. (M) Martinelli, M. (M) Bolzonella, R. (R) Nakajima, M. (M) Baldi, M. (M) Kümmel, Y. Mellier, M. (M) Roncarelli, M. (M) Moresco, A. (A) Grazian, K. (K) Ganga, D. (D) Stern, T. (T) Schrabback, N. (N.A) Walton, F. (F) Hormuth, R. (R) Maoli, W. (W.G) Hartley, M. (M) Brescia, G. (G) Testera, S. (S) Di Domizio, S. (S) Tosi, H. (H) Landt, S. (S) Conseil, I. (I) Hook, N. (N) Auricchio, S. (S) Sacquegna, N. (N) Mauri, R. (R) Rebolo, M. (M.Y) Elkhashab, C. (C) Sirignano, I. (I.T) Andika, A. (A) Navarro-Alsina, S. Bisogni, G. (G) Zamorani, A. Starke Taylor, H. (H) Hoekstra, G. (G) Mainetti, S. (S) Casas, I. (I) Tereno, L. (L) Wang, W. (W) Holmes, Y. (Y) Akrami, D. Yang, L. (L) Guzzo, C. (C) Valieri, H. (H.J.A) Rottgering, J. (J.J.E) Kajava, F. (F) Atrio-Barandela, L. (L) Bisigello, P. Tallada-Crespí, L. (L) Stanco, C. (C) Hernández-Monteagudo, T. (T) Castro, J. (J) Brinchmann
article en

Abstract

The slitless spectroscopy mode of the on board the Euclid telescope has enabled efficient spectroscopy of objects within a large field of view. Nevertheless, the relatively low spectral resolution, overlapping spectra, and contamination pose challenges to source classification and redshift determination using the spectra alone. In this work, we present a large and homogeneous sample of bright quasars identified from the Euclid Quick Data Release (Q1), constructed by combining high-purity candidate selections from to wavelengths without telluric lines, which will be pivotal to quasar spectral analysis. We obtained an empirical spectroscopic depth of JE łesssim 21.5 and ̋E łesssim 21.3 at the sensitivity of the Wide Field Survey, beyond which the number of securely identified quasars declines sharply. Accordingly, the sample presented in this paper comprises spectroscopically confirmed quasars brighter than these limits. We analysed morphological parameters from the Visible Camera (VIS) using Sérsic and model-independent (CAS) metrics, and a deep-learning point spread function fraction to track nuclear dominance. The VIS morphologies show a clear redshift dependence: at low redshift (z<0.5), obvious host structures are common and a single Sérsic model fits about half of the sources; at intermediate redshift (0.5<z<2), the nuclear component dominates, with 90% of the Sérsic fits saturating at the upper index limit. In this intermediate redshift regime, f_ nisp nisp and WISE with the new spectroscopic capabilities of Euclid. Through visual inspection of the Euclid spectra of these quasar candidates, we identify approximately 3500 quasars and determine reliable redshifts in the range of 0< z łesssim4.8. Of these, 2686 are new spectroscopic identifications relative to existing public compilations. We generated the first Euclid composite spectrum of quasars covering rest-frame nuv nir nir PSF is available, and we use it as a more reliable compactness measure than the single-Sérsic and CAS parameters to quantify nuclear versus host emission. We also explore the novel Euclid colour space and discuss the role of these quasars in refining active galactic nucleus selection techniques for future Euclid data releases. nir

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