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Euclid Quick Data Release (Q1). The first Euclid view of Planck galaxy protocluster candidates at cosmic noon

Euclid Collaboration, T. Dusserre, H. Dole, F. Sarron, G. Castignani, N. Ramos-Chernenko, N. Aghanim, A. Garic, I. -E. Mellouki, N. Dagoneau, O. Chapuis, B. L. Frye, M. Polletta, H. Dannerbauer, M. Langer, L. Maurin, E. Soubrie, A. Biviano, S. Mei, N. Mai, B. Altieri, A. Amara, S. Andreon, N. Auricchio, C. Baccigalupi, M. Baldi, A. Balestra, S. Bardelli, P. Battaglia, A. Bonchi, D. Bonino, E. Branchini, M. Brescia, J. Brinchmann, S. Camera, G. Cañas-Herrera, V. Capobianco, C. Carbone, J. Carretero, S. Casas, M. Castellano, S. Cavuoti, K. C. Chambers, A. Cimatti, C. Colodro-Conde, G. Congedo, C. J. Conselice, L. Conversi, Y. Copin, A. Costille, F. Courbin, H. M. Courtois, M. Cropper, A. Da Silva, H. Degaudenzi, G. De Lucia, A. M. Di Giorgio, C. Dolding, F. Dubath, C. A. J. Duncan, X. Dupac, S. Dusini, A. Ealet, S. Escoffier, M. Farina, R. Farinelli, F. Faustini, S. Ferriol, F. Finelli, P. Fosalba, S. Fotopoulou, M. Frailis, E. Franceschi, M. Fumana, S. Galeotta, K. George, B. Gillis, C. Giocoli, P. Gómez-Alvarez, J. Gracia-Carpio, B. R. Granett, A. Grazian, F. Grupp, L. Guzzo, S. Gwyn, S. V. H. Haugan, J. Hoar, W. Holmes, F. Hormuth, A. Hornstrup, P. Hudelot, K. Jahnke, M. Jhabvala, B. Joachimi, E. Keihänen, S. Kermiche, A. Kiessling, B. Kubik, K. Kuijken, M. Kümmel, M. Kunz, H. Kurki-Suonio, Q. Le Boulc'h, A. M. C. Le Brun, D. Le Mignant, 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, M. Melchior, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, A. Mora, M. Moresco, L. Moscardini, R. Nakajima, C. Neissner, R. C. Nichol, S. -M. Niemi, J. W. Nightingale, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, W. J. Percival, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L. A. Popa, L. Pozzetti, F. Raison, R. Rebolo, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, R. Saglia, Z. Sakr, A. G. Sánchez, D. Sapone, B. Sartoris, J. A. Schewtschenko, M. Schirmer, P. Schneider, T. Schrabback, A. Secroun, G. Seidel, S. Serrano, P. Simon, C. Sirignano, G. Sirri, L. Stanco, J. Steinwagner, P. Tallada-Crespí, A. N. Taylor, H. I. Teplitz, I. Tereno, S. Toft, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, L. Valenziano, J. Valiviita, T. Vassallo, G. Verdoes Kleijn, A. Veropalumbo, Y. Wang, J. Weller, A. Zacchei, G. Zamorani, F. M. Zerbi, I. A. Zinchenko, E. Zucca, V. Allevato, M. Ballardini, M. Bolzonella, E. Bozzo, C. Burigana, R. Cabanac, A. Cappi, D. Di Ferdinando, J. A. Escartin Vigo, G. Fabbian, L. Gabarra, M. Huertas-Company, J. Martín-Fleitas, S. Matthew, M. Maturi, N. Mauri, R. B. Metcalf, A. Pezzotta, M. Pöntinen, C. Porciani, I. Risso, V. Scottez, M. Sereno, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, S. Alvi, I. T. Andika, S. Anselmi, M. Archidiacono, F. Atrio-Barandela, K. Benson, P. Bergamini, D. Bertacca, M. Bethermin, A. Blanchard, L. Blot, H. Böhringer, S. Borgani, M. L. Brown, S. Bruton, A. Calabro, B. Camacho Quevedo, F. Caro, C. S. Carvalho, T. Castro, F. Cogato, T. Contini, A. R. Cooray, M. Costanzi, O. Cucciati, S. Davini, F. De Paolis, G. Desprez, A. Díaz-Sánchez, J. J. Diaz, S. Di Domizio, J. M. Diego, P. Dimauro, P. -A. Duc, A. Enia, Y. Fang, A. G. Ferrari, P. G. Ferreira, A. Finoguenov, A. Franco, K. Ganga, J. García-Bellido, T. Gasparetto, V. Gautard, E. Gaztanaga, F. Giacomini, F. Gianotti, A. H. Gonzalez, G. Gozaliasl, A. Gruppuso, M. Guidi, C. M. Gutierrez, A. Hall, W. G. Hartley, S. Hemmati, C. Hernández-Monteagudo, H. Hildebrandt, J. Hjorth, J. J. E. Kajava, Y. Kang, V. Kansal, D. Karagiannis, K. Kiiveri, C. C. Kirkpatrick, S. Kruk, J. Le Graet, L. Legrand, M. Lembo, F. Lepori, G. Leroy, G. F. Lesci, J. Lesgourgues, L. Leuzzi, T. I. Liaudat, S. J. Liu, A. Loureiro, J. Macias-Perez, G. Maggio, M. Magliocchetti, E. A. Magnier, F. Mannucci, R. Maoli, C. J. A. P. Martins, M. Migliaccio, M. Miluzio, P. Monaco, C. Moretti, G. Morgante, S. Nadathur, K. Naidoo, A. Navarro-Alsina, S. Nesseris, F. Passalacqua, K. Paterson, L. Patrizii, A. Philippon, A. Pisani, D. Potter, S. Quai, M. Radovich, G. Rodighiero, S. Sacquegna, M. Sahlén, D. B. Sanders, E. Sarpa, A. Schneider, D. Sciotti, E. Sellentin, F. Shankar, L. C. Smith, S. A. Stanford, K. Tanidis, G. Testera, R. Teyssier, S. Tosi, A. Troja, M. Tucci, C. Valieri, A. Venhola, D. Vergani, G. Verza, P. Vielzeuf, N. A. Walton, J. R. Weaver, J. G. Sorce, D. Scott

Abstract

[ABRIGED ABSTRACT] A large catalogue of candidate galaxy protoclusters with high star-formation rates was produced by the Planck collaboration. We search, in the first data release (Q1) of the Euclid survey, for the visible and infrared counterparts of the Planck galaxy protocluster candidates expected to be above $z > 1.5$. Eight of them are in Euclid Q1. Our goal is to investigate the optical nature of these overdensities previously detected in the submillimetre wavelength range. We search for overdensities using the DETECTIFz algorithm, an overdensity finder based on Delaunay tessellation that uses photometric redshift probability distributions through Monte Carlo simulations. Focusing our search on the eight high-star forming Planck protocluster candidates, we find that two of them have one Euclid counterpart, and six have between two and four Euclid counterparts, which amounts to a total of 20 Euclid counterparts. These Euclid counterparts lie at photometric redshifts $1.4<z_{\rm ph} < 2.7$ and 12 of them also have partial Herschel coverage. All detections have also been confirmed by at least one other independent protocluster detection algorithm. We study the colours, derived stellar masses and star-formation rates (SFRs) of the detected member galaxies of those protocluster candidate counterparts. We also estimate the total stellar masses, SFRs, and the halo mass lower limits for all Euclid protocluster candidates. We find that in the dark matter halo mass ($M_{\rm h}$) / redshift plane, these Planck and Euclid overdense regions lie in the region $12.6 <\log_{10} (M_{\rm h}/M_\odot)< 13.4$, $1.4<z< 2.7$. This means that the halos of our objects are expected to have experienced a transition between cold flows in hot media to accretion of hot material.

Euclid Quick Data Release (Q1). The first Euclid view of Planck galaxy protocluster candidates at cosmic noon

Abstract

[ABRIGED ABSTRACT] A large catalogue of candidate galaxy protoclusters with high star-formation rates was produced by the Planck collaboration. We search, in the first data release (Q1) of the Euclid survey, for the visible and infrared counterparts of the Planck galaxy protocluster candidates expected to be above . Eight of them are in Euclid Q1. Our goal is to investigate the optical nature of these overdensities previously detected in the submillimetre wavelength range. We search for overdensities using the DETECTIFz algorithm, an overdensity finder based on Delaunay tessellation that uses photometric redshift probability distributions through Monte Carlo simulations. Focusing our search on the eight high-star forming Planck protocluster candidates, we find that two of them have one Euclid counterpart, and six have between two and four Euclid counterparts, which amounts to a total of 20 Euclid counterparts. These Euclid counterparts lie at photometric redshifts and 12 of them also have partial Herschel coverage. All detections have also been confirmed by at least one other independent protocluster detection algorithm. We study the colours, derived stellar masses and star-formation rates (SFRs) of the detected member galaxies of those protocluster candidate counterparts. We also estimate the total stellar masses, SFRs, and the halo mass lower limits for all Euclid protocluster candidates. We find that in the dark matter halo mass () / redshift plane, these Planck and Euclid overdense regions lie in the region , . This means that the halos of our objects are expected to have experienced a transition between cold flows in hot media to accretion of hot material.

Paper Structure

This paper contains 29 sections, 3 equations, 9 figures, 5 tables.

Table of Contents

  1. Introduction
  2. observations, data processing, and selected sky areas in the Q1 footprint
  3. observations and data processing
  4. data
  5. Selected sky areas: the field of interest for eight Planck protocluster candidates
  6. Protocluster detection algorithms and selection
  7. Selection for input
  8. DETECTIFz protocluster-finding algorithm
  9. Post detection after DETECTIFz: the -Planck protocluster sample
  10. Results
  11. Properties of the protocluster candidates
  12. Position and photometric redshift distribution of the 20 counterparts
  13. Stellar masses and SFRs
  14. Halo masses
  15. Properties of the member galaxies
  16. ...and 14 more sections

Figures (9)

  • Figure 1: Histograms of and magnitudes for all galaxy members. Our cut at $\HE \leq 23.5$ is clearly visible.
  • Figure 2: NNPZ-estimated redshift ($z_{\rm\tt NNPZ }$) versus PHZ-estimated photometric redshift ($z_{\rm\tt PHZ }$) plane for $z_{\rm \texttt{NNPZ}}>1.3$. The background shows the distribution of 100 000 sources in the EDF-S and EDF-F fields. Darker tones represent higher densities of sources. The blue line is the iso-density contour inside which 68% of sources lie.
  • Figure 3: Histograms of the four main physical quantities (derived with NNPZ) of the 20 counterparts of the eight Planck protocluster candidates: photometric redshift; total stellar mass; total star-formation rate; and number of member galaxies.
  • Figure 4: Protocluster halo mass ($M_{\rm h}$) versus redshift $z$, colour-coded by star-formation rate (SFR, colour bar). Triangles represent protocluster, with the halo mass estimated using Method B (shuntov2022 S22, see Sect. \ref{['sect:halo_mass']} for details. Circles and squares are protoclusters from the literature: casey2016, hill2020, polletta2021, laporte2022, morishita2023, morishita2024, sillassen2024, and shimakawa2024. The red and blue lines illustrate the different predicted gas-cooling regimes: the red dotted line comes from dekel06 and the blue dotted line from daddi2022 and separate loci of cold gas in a hot medium (right) and hot gas (left); halo masses below the horizontal red dashed line $M_{\rm shock}$, coming from dekel06, are predicted to contain only cold flows with no shock heating within halos at $z<5$. The grey lines indicate the average halo mass growth history for halos of present day masses $10^{13}$, $10^{14}$, and $10^{15} \: M_\odot$ as determined from behroozi2013.
  • Figure 5: SFR$-M_\star$ of member galaxies of each overdensity. Blue dots show the position of each member galaxy of the 20 protocluster candidates. Shaded region is the main sequence from schreiber2015 plotted with errors at 1 $\sigma$ (orange) and 3 $\sigma$ (green) computed from uncertainties on the model's parameters. Dashed lines indicate a factor of 3 around the main sequence. Protoclusters are ordered by increasing redshift, from left to right and from top to bottom. Most galaxies remain within a factor of 3 around the main sequence.
  • ...and 4 more figures