A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Euclid preparation : LIII. LensMC, weak lensing cosmic shear measurement with forward modelling and Markov Chain Monte Carlo sampling
Alaotsikko: LIII. LensMC, weak lensing cosmic shear measurement with forward modelling and Markov Chain Monte Carlo sampling
Tekijät: Congedo G.; Miller L.; Taylor A. N.; Cross N.; Duncan C. A. J.; Kitching T.; Martinet N.; Matthew S.; Schrabback T.; Tewes M.; Welikala N.; Aghanim N.; Amara A.; Andreon S.; Auricchio N.; Baldi M.; Bardelli S.; Bender R.; Bodendorf C.; Bonino D.; Branchini E.; Brescia M.; Brinchmann J.; Camera S.; Capobianco V.; Carbone C.; Cardone V. F.; Carretero J.; Casas S.; Castander F. J.; Castellano M.; Cavuoti S.; Cimatti A.; Conselice C. J.; Conversi L.; Copin Y.; Courbin F.; Courtois H. M.; Cropper M.; Da Silva A.; Degaudenzi H.; Di Giorgio A. M.; Dinis J.; Dubath F.; Dupac X.; Farina M.; Farrens S.; Ferriol S.; Fosalba P.; Frailis M.; Franceschi E.; Galeotta S.; Garilli B.; Gillis B.; Giocoli C.; Grazian A.; Grupp F.; Haugan S. V. H.; Holliman M. S.; Holmes W.; Hormuth F.; Hornstrup A.; Hudelot P.; Jahnke K.; Keihänen E.; Kermiche S.; Kiessling A.; Kilbinger M.; Kubik B.; Kuijken K.; Kümmel M.; Kunz M.; Kurki-Suonio H.; Ligori S.; Lilje P. B.; Lindholm V.; Lloro I.; Maino D.; Maiorano E.; Mansutti O.; Marggraf O.; Markovic K.; Marulli F.; Massey R.; Maurogordato S.; McCracken H. J.; Medinaceli E.; Mei S.; Melchior M.; Meneghetti M.; Merlin E.; Meylan G.; Moresco M.; Morin B.; Moscardini L.; Munari E.; Niemi S.-M.; Nightingale J. W.; Padilla C.; Paltani S.; Pasian F.; Pedersen K.; Percival W. J.; Pettorino V.; Pires S.; Polenta G.; Poncet M.; Popa L. A.; Pozzetti L.; Raison F.; Rebolo R.; Renzi A.; Rhodes J.; Riccio G.; Romelli E.; Roncarelli M.; Rossetti E.; Saglia R.; Sapone D.; Sartoris B.; Schneider P.; Secroun A.; Seidel G.; Serrano S.; Sirignano C.; Sirri G.; Stanco L.; Tallada-Crespí P.; Tavagnacco D.; Tereno I.; Toledo-Moreo R.; Torradeflot F.; Tutusaus I.; Valentijn E. A.; Valenziano L.; Vassallo T.; Veropalumbo A.; Wang Y.; Weller J.; Zamorani G.; Zoubian J.; Zucca E.; Biviano A.; Bolzonella M.; Boucaud A.; Bozzo E.; Burigana C.; Colodro-Conde C.; Di Ferdinando D.; Graciá-Carpio J.; Mauri N.; Neissner C.; Nucita A. A.; Sakr Z.; Scottez V.; Tenti M.; Viel M.; Wiesmann M.; Akrami Y.; Allevato V.; Anselmi S.; Baccigalupi C.; Ballardini M.; Borgani S.; Borlaff A. S.; Bruton S.; Cabanac R.; Cappi A.; Carvalho C. S.; Castignani G.; Castro T.; Cañas-Herrera G.; Chambers K. C.; Cooray A. R.; Coupon J.; Davini S.; De Lucia G.; Desprez G.; Di Domizio S.; Dole H.; Díaz-Sánchez A.; Escartin Vigo J. A.; Escoffier S.; Ferrero I.; Finelli F.; Gabarra L.; García-Bellido J.; Gaztanaga E.; Giacomini F.; Gozaliasl G.; Guinet D.; Hall A.; Hildebrandt H.; Ilić S.; Jimenez Muñoz A.; Joudaki S.; Kajava J. J. E.; Kansal V.; Karagiannis D.; Kirkpatrick C. C.; Legrand L.; Macias-Perez J.; Maggio G.; Magliocchetti M.; Maoli R.; Martinelli M.; Martins C. J. A. P.; Maturi M.; Maurin L.; Metcalf R. B.; Migliaccio M.; Monaco P.; Morgante G.; Nadathur S.; Patrizii L.; Peel A.; Pezzotta A.; Popa V.; Porciani C.; Potter D.; Pöntinen M.; Reimberg P.; Rocci P.-F.; Sánchez A. G.; Schewtschenko J. A.; Schneider A.; Sefusatti E.; Sereno M.; Simon P.; Spurio Mancini A.; Stadel J.; Steinwagner J.; Testera G.; Teyssier R.; Toft S.; Tosi S.; Troja A.; Tucci M.; Valieri C.; Valiviita J.; Vergani D.
Kustantaja: EDP Sciences
Julkaisuvuosi: 2024
Journal: Astronomy and Astrophysics
Tietokannassa oleva lehden nimi: Astronomy & Astrophysics
Vuosikerta: 691
ISSN: 0004-6361
eISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/202450617
Verkko-osoite: https://doi.org/10.1051/0004-6361/202450617
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/477946750
LENSMC is a weak lensing shear measurement method developed for Euclid and Stage-IV surveys. It is based on forward modelling in order to deal with convolution by a point spread function (PSF) with comparable size to many galaxies, sampling the posterior distribution of galaxy parameters via Markov chain Monte Carlo, and marginalisation over nuisance parameters for each of the 1.5 billion galaxies observed by Euclid. We quantified the scientific performance through high-fidelity images based on the Euclid Flagship simulations and emulation of the Euclid VIS images, realistic clustering with a mean surface number density of 250 arcmin−2 (IE < 29.5) for galaxies, and 6 arcmin−2 (IE < 26) for stars, and a diffraction-limited chromatic PSF with a full width at half maximum of 0′.′2 and spatial variation across the field of view. LENSMC measured objects with a density of 90 arcmin−2 (IE < 26.5) in 4500 deg2. The total shear bias was broken down into measurement (our main focus here) and selection effects (which will be addressed in future work). We found measurement multiplicative and additive biases of m1 = (−3.6 ± 0.2) × 10−3, m2 = (−4.3 ± 0.2) × 10−3, c1 = (−1.78 ± 0.03) × 10−4, and c2 = (0.09 ± 0.03) × 10−4; a large detection bias with a multiplicative component of 1.2 × 10−2 and an additive component of −3 × 10−4; and a measurement PSF leakage of α1 = (−9 ± 3) × 10−4 and α2 = (2 ± 3) × 10−4. When model bias is suppressed, the obtained measurement biases are close to Euclid requirement and largely dominated by undetected faint galaxies (−5 × 10−3). Although significant, model bias will be straightforward to calibrate given its weak sensitivity on galaxy morphology parameters. LENSMC is publicly available at gitlab.com/gcongedo/LensMC.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
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Acknowledgements. GC acknowledges support provided by the United Kingdom Space Agency with grant numbers ST/X00189X/1, ST/W002655/1, ST/V001701/1, and ST/N001761/1. GC thanks the University of Oxford for support, where this work was started. GC thanks D. Bauer, S. Fayer (Imperial College London), P. Clarke, R. Currie (University of Edinburgh), and the GridPP Collaboration for support on getting access to and use of GridPP where the final simulations were run. GC acknowledges the use of the Euclid clusters in Edinburgh, and thanks J. Patterson for support on the Astrophysics cluster in Oxford where the initial simulations were run. TS acknowledges support provided by the Austrian Research Promotion Agency (FFG) and the Federal Ministry of the Republic of Austria for Climate Action, Environment, Energy, Mobility, Innovation and Technology (BMK) via the Austrian Space Applications Programme with grant numbers 899537 and 900565. MT acknowledges support from the German Federal Ministry for Economic Affairs and Climate Action (BMWK) provided by DLR under projects 50QE1103, 50QE2002, and 50QE2302. The Euclid Consortium acknowledges the European Space Agency and a number of agencies and institutes that have supported the development of Euclid, in particular the Agenzia Spaziale Italiana, the Austrian Forschungsförderungsgesellschaft funded through BMK, the Belgian Science Policy, the Canadian Euclid Consortium,
the Deutsches Zentrum für Luft- und Raumfahrt, the DTU Space and the Niels Bohr Institute in Denmark, the French Centre National d’Etudes Spatiales, the Fundação para a Ciência e a Tecnologia, the Hungarian Academy of Sciences, the Ministerio de Ciencia, Innovación y Universidades, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Research Council of Finland, the Romanian Space Agency, the State Secretariat for Education, Research, and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency
