| Title: |
Euclid preparation LXXIII. Spatially resolved stellar populations of local galaxies with Euclid: A proof of concept using synthetic images with the TNG50 simulation |
| Authors: |
Abdurro’uf; Tortora, C.; Baes, M.; Nersesian, A.; Kovačić, I.; Bolzonella, M.; Lançon, A.; Bisigello, L.; Annibali, F.; Bremer, M.N.; Carollo, D.; Conselice, C.J.; Enia, A.; Ferguson, A.M.N.; Ferré-Mateu, A.; Hunt, L.K.; Iodice, E.; Knapen, J.H.; Iovino, A.; Marleau, F.R.; Peletier, R.F.; Ragusa, R.; Rejkuba, M.; Robotham, A.S.G.; Román, J.; Saifollahi, T.; Salucci, P.; Scodeggio, M.; Siudek, M.; van der Wel, A.; Voggel, K.; Altieri, B.; Andreon, S.; Baccigalupi, C.; Baldi, M.; Bardelli, S.; Biviano, A.; Bonchi, A.; Bonino, D.; Branchini, E.; Brescia, M.; Brinchmann, J.; Caillat, A.; Camera, S.; Cañas-Herrera, G.; Capobianco, V.; Carbone, C.; Carretero, J.; Casas, S.; Castellano, M.; Castignani, G.; Cavuoti, S.; Chambers, K.C.; Cimatti, A.; Colodro-Conde, C.; Congedo, G.; Conversi, L.; Copin, Y.; Courbin, F.; Courtois, H.M.; Cropper, M.; Da Silva, A.; Degaudenzi, H.; De Lucia, G.; Di Giorgio, A.M.; Dinis, J.; Dole, H.; Dubath, F.; Dupac, X.; Dusini, S.; Escoffier, S.; Farina, M.; Farinelli, R.; Farrens, S.; Faustini, F.; Ferriol, S.; Finelli, F.; Fotopoulou, S.; Frailis, M.; Franceschi, E.; Fumana, M.; Galeotta, S.; Gillis, B.; Giocoli, C.; Goméz-Alvarez, P.; Gracía-Carpio, J.; Grazian, A.; Grupp, F.; Holmes, W.; Hormuth, F.; Hornstrup, A.; Hudelot, P.; Jahnke, K.; Jhabvala, M.; Keihänen, E.; Kermiche, S.; Kiessling, A.; Kilbinger, M.; Kubik, B.; Kümmel, M.; Kunz, M.; Kurki-Suonio, H.; Le Brun, A.M.C.; Ligori, S.; Lilje, P.B.; Lindholm, V.; Lloro, I.; Mainetti, G.; Maino, D.; Maiorano, E.; Mansutti, O.; Marggraf, O.; Markovič, K.; Martinelli, M.; Martinet, N.; Marulli, F.; Massey, R.; Medinaceli, E.; Mei, S.; Melchior, M.; Mellier, Y.; Meneghetti, M.; Merlin, E.; Meylan, G.; Mora, A.; Moresco, M.; Moscardini, L.; Niemi, S.-M.; Nightingale, J.W.; Padilla, C.; Paltani, S.; Pasian, F.; Pedersen, K.; Pettorino, V.; Polenta, G.; Poncet, M.; Popa, L.A.; Pozzetti, L.; Raison, F.; Renzi, A.; Rhodes, J.; Riccio, G.; Romelli, E.; Roncarelli, M.; Rossetti, E.; Saglia, R.; Sakr, Z.; Sapone, D.; Sartoris, B.; Schirmer, M.; Schneider, P.; Schrabback, T.; Secroun, A.; Sefusatti, E.; Seidel, G.; Serrano, S.; Simon, P.; Sirignano, C.; Sirri, G.; Stanco, L.; Steinwagner, J.; Tallada-Crespí, P.; Andrew Taylor, A.N.; Tereno, I.; Toft, S.; Toledo-Moreo, R.; Torradeflot, F.; Tutusaus, I.; Valenziano, L.; Väliviita, J.; Vassallo, T.; Verdoes Kleijn, G.; Veropalumbo, A.; Wang, Y.; Weller, J.; Zamorani, G.; Zucca, E.; Bozzo, E.; Burigana, C.; Calabrese, M.; Di Ferdinando, D.; Escartin Vigo, J.A.; Matthew, S.; Mauri, N.; Pöntinen, M.; Porciani, C.; Scottez, V.; Tenti, M.; Viel, M.; Wiesmann, M.; Akrami, Y.; Allevato, V.; Anselmi, S.; Archidiacono, M.; Atrio-Barandela, F.; Ballardini, M.; Bertacca, D.; Blanchard, A.; Blot, L.; Borgani, S.; Brown, M.L.; Bruton, S.; Cabanac, R.; Calabro, A.; Cappi, A.; Caro, F.; Carvalho, C.S.; Castro, T.; Cogato, F.; Contini, T.; Cooray, A.R.; Cucciati, O.; Desprez, G.; Díaz-sánchez, A.; Di Domizio, S.; Ferrari, A.G.; Ferrero, I.; Finoguenov, A.; Fontana, A.; Fornari, F.; Ganga, K.; García-Bellido, J.; Gasparetto, T.; Gaztañaga, E.; Giacomini, F.; Gianotti, F.; Gozaliasl, G.; Gregorio, A.; Guidi, M.; Gutiérrez, C.M.; Hall, A.; Hemmati, S.; Hildebrandt, H.; Hjorth, J.; Huertas-Company, M.; Jimenez Muñoz, A.; Kajava, J.J.E.; Kang, Y.; Kansal, V.; Karagiannis, D.; Kirkpatrick, C.C.; Kruk, S.; Lattanzi, M.; Lee, S.; Le Graët, J.; Legrand, L.; Lembo, M.; Lesgourgues, J.; Liaudat, T.I.; Loureiro, A.; MacÍas-Pérez, J.; Magliocchetti, M.; Mannucci, F.; Maoli, R.; Martín-Fleitas, J.; Martins, C.J.A.P.; Maurin, L.; Metcalf, R.B.; Miluzio, M.; Monaco, P.; Moretti, C.; Morgante, G.; Naidoo, K.; Walton, N.A.; Paterson, K.; Patrizii, L.; Pisani, A.; Popa, V.; Potter, D.; Risso, I.; Rocci, P.-F.; Sahlén, M.; Sarpa, E.; Schneider, A.; Sciotti, D.; Sellentin, E.; Sereno, M.; Tanidis, K.; Tao, C.; Testera, G.; Teyssier, R.; Tosi, S.; Troja, A.; Tucci, M.; Valieri, C.; Vergani, D.; Verza, G.; Vielzeuf, P.; Euclid Collaboration |
| Contributors: |
Tuorlan observatorio, Tuorla Observatory; 1.2.246.10.2458963.20.90670098848 |
| Publisher Information: |
EDP Sciences; France; Ranska; FR |
| Publication Year: |
2026 |
| Collection: |
University of Turku: UTUPub / Turun yliopisto |
| Description: |
The European Space Agency’s Euclid mission will observe approximately 14000 deg 2 of the extragalactic sky and deliver high-quality imaging of a large number of galaxies. The depth and high spatial resolution of the data will enable a detailed analysis of the stellar population properties of local galaxies through spatially resolved spectral energy distribution (SED) fitting. In this study, we test our pipeline for spatially resolved SED fitting using synthetic images of Euclid , LSST, and GALEX generated from the TNG50 simulation using the SKIRT 3D radiative transfer code. Our pipeline uses functionalities in piXedfit for processing the simulated data cubes and carrying out SED fitting. We apply our pipeline to 25 simulated galaxies at z ∼ 0 to recover their resolved stellar population properties. For each galaxy, we produce three types of data cubes: GALEX + LSST + Euclid , LSST + Euclid , and Euclid -only. We performed the SED fitting tests with two stellar population synthesis (SPS) models in a Bayesian framework. Because the age, metallicity ( Z ), and dust attenuation estimates are biased when applying only classical formulations of flat priors (even with the combined GALEX + LSST + Euclid data), we examined the effects of additional physically motivated priors in the forms of mass-age and mass-metallicity relations, constructed using a combination of empirical and simulated data. Stellar-mass surface densities can be recovered well using any of the three data cubes, regardless of the SPS model and prior variations. The new priors then significantly improve the measurements of mass-weighted age and Z compared to results obtained without priors, but they may play an excessive role compared to the data in determining the outcome when no ultraviolet (UV) data is available. Compared to varying the spectral extent of the data cube or including and discarding the additional priors, replacing one SPS model family with the other has little effect on the results. The spatially resolved SED fitting method is ... |
| Document Type: |
other/unknown material |
| Language: |
English |
| Relation: |
702; A72; Astronomy and Astrophysics; https://www.utupub.fi/handle/10024/195926 |
| DOI: |
10.1051/0004-6361/202554516 |
| Availability: |
https://www.utupub.fi/handle/10024/195926; https://doi.org/10.1051/0004-6361/202554516 |
| Accession Number: |
edsbas.67096F54 |
| Database: |
BASE |