uncertainties. Especially in the case of small shear fields, it also makes sense to consider using the response method. Although harder to implement, improving more than two orders of magnitude in runtime can be worth it.

When moving to simulations including clustering, we want to highlight the need to quantify the dominant contribution to the runtime for a particular shape measurement method and simulation pipeline in order to decide if it is worth to implement pixel noise cancellation also on top of shape noise cancellation. This is because our simulations with positions drawn from the Flagship catalogue (including clustering) have shown that the area improvements for these simulations are very comparable with and without the additional pixel noise cancellation for our setups with local shape noise cancellation at least. However since *Euclid* has a complex PSF that has to be simulated with a higher degree of detail as conducted in our work, it might well be that the PSF generation and convolution becomes a more dominant contribution to the overall runtime, in which case the addition of pixel noise cancellation would provide larger runtime improvements.

In the interest of repeatability and transparency, we make the code publicly available<fnref n="6" />. These scripts are not a product of the Euclid Consortium Science Ground Segment. They are created exclusively for the present analysis and made public for reproducibility of the results presented in this paper. We also provide the scripts and data to generate each plot in this paper under the same address.

*Acknowledgements.* We thank Andy Taylor, Shun-Sheng Li, and the anonymous referee for their useful comments and discussions about this work. H.J. and T.S. acknowledge 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, as well as the German Research Foundation (DFG) under grant 415537506. M.T. acknowledges support from the German Federal Ministry for Economic Affairs and Climate Action (BMWK) provided by DLR under projects nos. 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 Academy of Finland, the Agenzia Spaziale Italiana, the Belgian Science Policy, the Canadian Euclid Consortium, the French Centre National d'Etudes Spatiales, the Deutsches Zentrum für Luft- und Raumfahrt, the Danish Space Research Institute, the Fundação para a Ciência e a Tecnologia, the Ministerio de Ciencia e Innovación, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, 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. A complete and detailed list is available on the *Euclid* web site (http://www.euclid-ec.org).

## References

Aihara, H., Arimoto, N., Armstrong, R., et al. 2018, PASJ, 70, S4

Albrecht, A., Bernstein, G., Cahn, R., et al. 2006, arXiv e-prints [arXiv:astro-ph/0609591]

Bertin, E., & Arnouts, S. 1996, A&AS, 117, 393

Carretero, J., Tallada, P., Casals, J., et al. 2017, in Proc. Eur. Phys. Soc. Conf. on High Energy Physics, 488

Castro, P. G., Heavens, A. F., & Kitching, T. D. 2005, Phys. Rev. D, 72, 023516

Cropp, M., Pottinger, S., Niemi, S., et al. 2016, Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave, 9904, 99040Q

Dark Energy Survey Collaboration (Abbott, T., et al.) 2016, MNRAS, 460, 1270

de Jong, J. T. A., Kuijken, K., Applegate, D., et al. 2013, The Messenger, 154, 44

Erben, T., Van Waaerbeke, L., Bertin, E., Mellier, Y., & Schneider, P. 2001, A&A, 366, 717

Euclid Collaboration (Martinet, N., et al.) 2019, A&A, 627, A59

Fenech Conti, I., Herbonnet, R., Hoekstra, H., et al. 2017, MNRAS, 467, 1627

Guzik, J., & Bernstein, G. 2005, Phys. Rev. D, 72, 043503

Hernández-Martín, B., Schrabback, T., Hoekstra, H., et al. 2020, A&A, 640, A117

Heymans, C., Van Waaerbeke, L., Bacon, D., et al. 2006, MNRAS, 368, 1323

Hirata, C., & Seljak, U. 2003, MNRAS, 343, 459

Hoekstra, H. 2021, A&A, 656, A135

Hoekstra, H., Franx, M., Kuijken, K., & Squires, G. 1998, ApJ, 504, 636

Hoekstra, H., Herbonnet, R., Muzzin, A., et al. 2015, MNRAS, 449, 685

Hoekstra, H., Viola, M., & Herbonnet, R. 2017, MNRAS, 468, 3295

Hoekstra, H., Kannawadi, A., & Kitching, T. D. 2021, A&A, 646, A124

Hoffmann, K., Secco, L. F., Blazek, J., et al. 2022, Phys. Rev. D, 106, 123510

Huterer, D., Takada, M., Bernstein, G., & Jain, B. 2006, MNRAS, 366, 101

Kaiser, N., Squires, G., & Broadhurst, T. 1995, ApJ, 449, 460

Kannawadi, A., Hoekstra, H., Miller, L., et al. 2019, A&A, 624, A92

Kitching, T. D. & Deshpande, A. C. 2022, Open J. Astrophys., 5, 6

Kitching, T. D., Tessore, N., & Taylor, P. L. 2023, Open J. Astrophys., submitted [arXiv:2302.14656]

Kurucz, R. L. 2011, Modelled spectra for Vega, http://kurucz.harvard.edu/stars/vega/

Laureijs, R., Amiaux, J., Arduini, S., et al. 2011, arXiv e-prints [arXiv:1110.3193]

Li, S.-S., Kuijken, K., Hoekstra, H., et al. 2023, A&A, 670, A100

Liu, D. Z., Meng, X. M., Er, X. Z., et al. 2023, A&A, 669, A128

Luppino, G. A., & Kaiser, N. 1997, ApJ, 475, 20

MacCrann, N., Becker, M. R., McCullough, J., et al. 2022, MNRAS, 509, 3371

Mandelbaum, R., Hirata, C. M., Seljak, U., et al. 2005, MNRAS, 361, 1287

Mandelbaum, R., Rowe, B., Bosch, J., et al. 2014, ApJS, 212, 5

Mandelbaum, R., Lanusse, F., Leauthaud, A., et al. 2018, ApJS, 152, 163

Marquardt, D. W. 1963, J. Soc. Ind. Appl. Math., 11, 431

Massey, R., Heymans, C., Bergé, J., et al. 2007, MNRAS, 376, 13

Melchior, P., & Viola, M. 2012, MNRAS, 424, 2757

Moritz, P., Nishihara, R., Wang, S., et al. 2017, arXiv e-prints [arXiv:1712.05889]

Nakajima, R., & Bernstein, G. 2007, AJ, 133, 1763

Potter, D., Stadel, J., & Teyssier, R. 2017, Comput. Astrophys. Cosmol., 4, 2

Pujol, A., Kilbinger, M., Sureau, F., & Bobin, J. 2019, A&A, 621, A2

Rix, H.-W., Barden, M., Beckwith, S. V. W., et al. 2004, ApJS, 152, 163

Rowe, B. T. P., Jarvis, M., Mandelbaum, R., et al. 2015, Astron. Comput., 10, 121

Schneider, P. 2006, in Saas-Fee Advanced Courses (Springer Berlin Heidelberg), 269

Sheldon, E. S., & Huff, E. M. 2017, ApJ, 841, 24

Spergel, D., Gehrels, N., Baltay, C., et al. 2015, arXiv e-prints [arXiv:1503.03757]

Tallada, P., Carretero, J., Casals, J., et al. 2020, Astron. Comput., 32, 100391

Tewes, M., Kuntzer, T., Nakajima, R., et al. 2019, A&A, 621, A36

<footnote n="1">¹ Universität Bonn, Argelander-Institut für Astronomie, Auf dem Hügel 71, 53121 Bonn, Germany</footnote>

<footnote n="2">² Universität Innsbruck, Institut für Astro- und Teilchenphysik, Technikerstr. 25/8, 6020 Innsbruck, Austria
e-mail: Henning.Jansen@uibk.ac.at</footnote>

<footnote n="3">³ Université Paris-Saclay, CNRS, Institut d'astrophysique spatiale, 91405 Orsay, France</footnote>

<footnote n="4">⁴ Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK</footnote>

<footnote n="5">⁵ INAF-Osservatorio Astronomico di Brera, Via Brera 28, 20122 Milano, Italy</footnote>

<footnote n="6">⁶ INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Piero Gobetti 93/3, 40129 Bologna, Italy</footnote>

<footnote n="7">⁷ Dipartimento di Fisica e Astronomia, Università di Bologna, Via Gobetti 93/2, 40129 Bologna, Italy</footnote>

<footnote n="8">⁸ INFN-Sezione di Bologna, Viale Berti Pichat 6/2, 40127 Bologna, Italy</footnote>

<footnote n="9">⁹ Dipartimento di Fisica, Università di Genova, Via Dodecaneso 33, 16146, Genova, Italy</footnote>

<footnote n="10">¹⁰ INFN-Sezione di Genova, Via Dodecaneso 33, 16146, Genova, Italy</footnote>

<footnote n="11">¹¹ Department of Physics “E. Pancini”, University Federico II, Via Cinthia 6, 80126, Napoli, Italy</footnote>

<footnote n="12">¹² INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy</footnote>

<footnote n="13">¹³ Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal</footnote>

<footnote n="14">¹⁴ Dipartimento di Fisica, Università degli Studi di Torino, Via P. Giuria 1, 10125 Torino, Italy</footnote>

<footnote n="15">¹⁵ INFN-Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy</footnote>

<footnote n="16">¹⁶ INAF-Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025 Pino Torinese (TO), Italy</footnote>

<footnote n="6">⁶ https://github.com/HenningJ99/noise_mitigation_code
A240, page 18 of 23</footnote>
uncertainties. Especially in the case of small shear fields, it also makes sense to consider using the response method. Although harder to implement, improving more than two orders of magnitude in runtime can be worth it.

When moving to simulations including clustering, we want to highlight the need to quantify the dominant contribution to the runtime for a particular shape measurement method and simulation pipeline in order to decide if it is worth to implement pixel noise cancellation also on top of shape noise cancellation. This is because our simulations with positions drawn from the Flagship catalogue (including clustering) have shown that the area improvements for these simulations are very comparable with and without the additional pixel noise cancellation for our setups with local shape noise cancellation at least. However since *Euclid* has a complex PSF that has to be simulated with a higher degree of detail as conducted in our work, it might well be that the PSF generation and convolution becomes a more dominant contribution to the overall runtime, in which case the addition of pixel noise cancellation would provide larger runtime improvements.

In the interest of repeatability and transparency, we make the code publicly available<fnref n="6" />. These scripts are not a product of the Euclid Consortium Science Ground Segment. They are created exclusively for the present analysis and made public for reproducibility of the results presented in this paper. We also provide the scripts and data to generate each plot in this paper under the same address.

*Acknowledgements.* We thank Andy Taylor, Shun-Sheng Li, and the anonymous referee for their useful comments and discussions about this work. H.J. and T.S. acknowledge 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, as well as the German Research Foundation (DFG) under grant 415537506. M.T. acknowledges support from the German Federal Ministry for Economic Affairs and Climate Action (BMWK) provided by DLR under projects nos. 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 Academy of Finland, the Agenzia Spaziale Italiana, the Belgian Science Policy, the Canadian Euclid Consortium, the French Centre National d'Etudes Spatiales, the Deutsches Zentrum für Luft- und Raumfahrt, the Danish Space Research Institute, the Fundação para a Ciência e a Tecnologia, the Ministerio de Ciencia e Innovación, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, 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. A complete and detailed list is available on the *Euclid* web site (http://www.euclid-ec.org).

## References

Aihara, H., Arimoto, N., Armstrong, R., et al. 2018, PASJ, 70, S4

Albrecht, A., Bernstein, G., Cahn, R., et al. 2006, arXiv e-prints [arXiv:astro-ph/0609591]

Bertin, E., & Arnouts, S. 1996, A&AS, 117, 393

Carretero, J., Tallada, P., Casals, J., et al. 2017, in Proc. Eur. Phys. Soc. Conf. on High Energy Physics, 488

Castro, P. G., Heavens, A. F., & Kitching, T. D. 2005, Phys. Rev. D, 72, 023516

Cropp, M., Pottinger, S., Niemi, S., et al. 2016, Space Telescopes and Instrumentation 2016: Optical, Infrared, and Millimeter Wave, 9904, 99040Q

Dark Energy Survey Collaboration (Abbott, T., et al.) 2016, MNRAS, 460, 1270

de Jong, J. T. A., Kuijken, K., Applegate, D., et al. 2013, The Messenger, 154, 44

Erben, T., Van Waaerbeke, L., Bertin, E., Mellier, Y., & Schneider, P. 2001, A&A, 366, 717

Euclid Collaboration (Martinet, N., et al.) 2019, A&A, 627, A59

Fenech Conti, I., Herbonnet, R., Hoekstra, H., et al. 2017, MNRAS, 467, 1627

Guzik, J., & Bernstein, G. 2005, Phys. Rev. D, 72, 043503

Hernández-Martín, B., Schrabback, T., Hoekstra, H., et al. 2020, A&A, 640, A117

Heymans, C., Van Waaerbeke, L., Bacon, D., et al. 2006, MNRAS, 368, 1323

Hirata, C., & Seljak, U. 2003, MNRAS, 343, 459

Hoekstra, H. 2021, A&A, 656, A135

Hoekstra, H., Franx, M., Kuijken, K., & Squires, G. 1998, ApJ, 504, 636

Hoekstra, H., Herbonnet, R., Muzzin, A., et al. 2015, MNRAS, 449, 685

Hoekstra, H., Viola, M., & Herbonnet, R. 2017, MNRAS, 468, 3295

Hoekstra, H., Kannawadi, A., & Kitching, T. D. 2021, A&A, 646, A124

Hoffmann, K., Secco, L. F., Blazek, J., et al. 2022, Phys. Rev. D, 106, 123510

Huterer, D., Takada, M., Bernstein, G., & Jain, B. 2006, MNRAS, 366, 101

Kaiser, N., Squires, G., & Broadhurst, T. 1995, ApJ, 449, 460

Kannawadi, A., Hoekstra, H., Miller, L., et al. 2019, A&A, 624, A92

Kitching, T. D. & Deshpande, A. C. 2022, Open J. Astrophys., 5, 6

Kitching, T. D., Tessore, N., & Taylor, P. L. 2023, Open J. Astrophys., submitted [arXiv:2302.14656]

Kurucz, R. L. 2011, Modelled spectra for Vega, http://kurucz.harvard.edu/stars/vega/

Laureijs, R., Amiaux, J., Arduini, S., et al. 2011, arXiv e-prints [arXiv:1110.3193]

Li, S.-S., Kuijken, K., Hoekstra, H., et al. 2023, A&A, 670, A100

Liu, D. Z., Meng, X. M., Er, X. Z., et al. 2023, A&A, 669, A128

Luppino, G. A., & Kaiser, N. 1997, ApJ, 475, 20

MacCrann, N., Becker, M. R., McCullough, J., et al. 2022, MNRAS, 509, 3371

Mandelbaum, R., Hirata, C. M., Seljak, U., et al. 2005, MNRAS, 361, 1287

Mandelbaum, R., Rowe, B., Bosch, J., et al. 2014, ApJS, 212, 5

Mandelbaum, R., Lanusse, F., Leauthaud, A., et al. 2018, ApJS, 152, 163

Marquardt, D. W. 1963, J. Soc. Ind. Appl. Math., 11, 431

Massey, R., Heymans, C., Bergé, J., et al. 2007, MNRAS, 376, 13

Melchior, P., & Viola, M. 2012, MNRAS, 424, 2757

Moritz, P., Nishihara, R., Wang, S., et al. 2017, arXiv e-prints [arXiv:1712.05889]

Nakajima, R., & Bernstein, G. 2007, AJ, 133, 1763

Potter, D., Stadel, J., & Teyssier, R. 2017, Comput. Astrophys. Cosmol., 4, 2

Pujol, A., Kilbinger, M., Sureau, F., & Bobin, J. 2019, A&A, 621, A2

Rix, H.-W., Barden, M., Beckwith, S. V. W., et al. 2004, ApJS, 152, 163

Rowe, B. T. P., Jarvis, M., Mandelbaum, R., et al. 2015, Astron. Comput., 10, 121

Schneider, P. 2006, in Saas-Fee Advanced Courses (Springer Berlin Heidelberg), 269

Sheldon, E. S., & Huff, E. M. 2017, ApJ, 841, 24

Spergel, D., Gehrels, N., Baltay, C., et al. 2015, arXiv e-prints [arXiv:1503.03757]

Tallada, P., Carretero, J., Casals, J., et al. 2020, Astron. Comput., 32, 100391

Tewes, M., Kuntzer, T., Nakajima, R., et al. 2019, A&A, 621, A36

<footnote n="1">¹ Universität Bonn, Argelander-Institut für Astronomie, Auf dem Hügel 71, 53121 Bonn, Germany</footnote>

<footnote n="2">² Universität Innsbruck, Institut für Astro- und Teilchenphysik, Technikerstr. 25/8, 6020 Innsbruck, Austria
e-mail: Henning.Jansen@uibk.ac.at</footnote>

<footnote n="3">³ Université Paris-Saclay, CNRS, Institut d'astrophysique spatiale, 91405 Orsay, France</footnote>

<footnote n="4">⁴ Institute of Cosmology and Gravitation, University of Portsmouth, Portsmouth PO1 3FX, UK</footnote>

<footnote n="5">⁵ INAF-Osservatorio Astronomico di Brera, Via Brera 28, 20122 Milano, Italy</footnote>

<footnote n="6">⁶ INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna, Via Piero Gobetti 93/3, 40129 Bologna, Italy</footnote>

<footnote n="7">⁷ Dipartimento di Fisica e Astronomia, Università di Bologna, Via Gobetti 93/2, 40129 Bologna, Italy</footnote>

<footnote n="8">⁸ INFN-Sezione di Bologna, Viale Berti Pichat 6/2, 40127 Bologna, Italy</footnote>

<footnote n="9">⁹ Dipartimento di Fisica, Università di Genova, Via Dodecaneso 33, 16146, Genova, Italy</footnote>

<footnote n="10">¹⁰ INFN-Sezione di Genova, Via Dodecaneso 33, 16146, Genova, Italy</footnote>

<footnote n="11">¹¹ Department of Physics “E. Pancini”, University Federico II, Via Cinthia 6, 80126, Napoli, Italy</footnote>

<footnote n="12">¹² INAF-Osservatorio Astronomico di Capodimonte, Via Moiariello 16, 80131 Napoli, Italy</footnote>

<footnote n="13">¹³ Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal</footnote>

<footnote n="14">¹⁴ Dipartimento di Fisica, Università degli Studi di Torino, Via P. Giuria 1, 10125 Torino, Italy</footnote>

<footnote n="15">¹⁵ INFN-Sezione di Torino, Via P. Giuria 1, 10125 Torino, Italy</footnote>

<footnote n="16">¹⁶ INAF-Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025 Pino Torinese (TO), Italy</footnote>

<footnote n="6">⁶ https://github.com/HenningJ99/noise_mitigation_code
A240, page 18 of 23</footnote>
17 INAF-IASF Milano, Via Alfonso Corti 12, 20133 Milano, Italy

18 INAF-Osservatorio Astronomico di Roma, Via Frascati 33, 00078 Monteporzio Catone, Italy

19 INFN-Sezione di Roma, Piazzale Aldo Moro 2, c/o Dipartimento di Fisica, Edificio G. Marconi, 00185 Roma, Italy

20 Institut de Física d'Altes Energies (IFAE), The Barcelona Institu-
tute of Science and Technology, Campus UAB, 08193 Bellaterra
(Barcelona), Spain

21 Port d'Informació Científica, Campus UAB, C. Albareda s/n, 08193 Bellaterra (Barcelona), Spain

22 Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University, 52056 Aachen, Germany

23 INFN section of Naples, Via Cinthia 6, 80126 Napoli, Italy

24 Dipartimento di Fisica e Astronomia "Augusto Righi" - Alma Mater Studiorum Università di Bologna, Viale Berti Pichat 6/2, 40127 Bologna, Italy

25 Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK

26 European Space Agency/ESRIN, Largo Galileo Galilei 1, 00044 Frascati, Roma, Italy

27 ESAC/ESA, Camino Bajo del Castillo, s/n., Urb. Villafranca del Castillo, 28692 Villanueva de la Cañada, Madrid, Spain

28 University of Lyon, Univ Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, 69622 Villeurbanne, France

29 Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland

30 UCB Lyon 1, CNRS/IN2P3, IUF, IP2I Lyon, 4 rue Enrico Fermi, 69622 Villeurbanne, France

31 Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Edifício C8, Campo Grande, 1749-016 Lisboa, Portugal

32 Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências, Universidade de Lisboa, Campo Grande, 1749-016 Lisboa, Portugal

33 Department of Astronomy, University of Geneva, ch. d'Ecogia 16, 1290 Versoix, Switzerland

34 INAF-Istituto di Astrofisica e Planetologia Spaziali, via del Fosso del Cavaliere, 100, 00100 Roma, Italy

35 Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191 Gif-sur-Yvette, France

36 INAF-Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34143 Trieste, Italy

37 INAF-Osservatorio Astronomico di Padova, Via dell'Osservatorio 5, 35122 Padova, Italy

38 Max Planck Institute for Extraterrestrial Physics, Giessenbachstr. 1, 85748 Garching, Germany

39 University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, 81679 Munich, Germany

40 Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway

41 Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands

42 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA, 91109, USA

43 von Hoerner & Sulger GmbH, Schloßplatz 8, 68723 Schwetzingen, Germany

44 Technical University of Denmark, Elektrovej 327, 2800 Kgs. Lyngby, Denmark

45 Cosmic Dawn Center (DAWN), Copenhagen, Denmark

46 Institut d'Astrophysique de Paris, UMR 7095, CNRS, and Sorbonne Université, 98 bis boulevard Arago, 75014 Paris, France

47 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany

48 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK

49 Aix-Marseille Université, CNRS/IN2P3, CPPM, Marseille, France

50 Université Paris-Saclay, Université Paris Cité, CEA, CNRS, Astro-
physique, Instrumentation et Modélisation Paris-Saclay, 91191
Gif-sur-Yvette, France

51 Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UK

52 Department of Physics, PO Box 64, 00014 University of Helsinki, Finland

53 Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland

54 NOVA optical infrared instrumentation group at ASTRON, Oude Hoogeveensedijk 4, 7991PD, Dwingeloo, The Netherlands

55 Aix-Marseille Université, CNRS, CNES, LAM, Marseille, France

56 Dipartimento di Fisica e Astronomia "Augusto Righi" - Alma Mater Studiorum Università di Bologna, via Piero Gobetti 93/2, 40129 Bologna, Italy

57 Department of Physics, Institute for Computational Cosmology, Durham University, South Road, DH1 3LE, UK

58 Université Paris Cité, CNRS, Astroparticule et Cosmologie, 75013 Paris, France

59 University of Applied Sciences and Arts of Northwestern Switzerland, School of Engineering, 5210 Windisch, Switzerland

60 Institut d'Astrophysique de Paris, 98bis Boulevard Arago, 75014 Paris, France

61 CEA Saclay, DFR/IRFU, Service d'Astrophysique, Bat. 709, 91191 Gif-sur-Yvette, France

62 Department of Physics, Oxford University, Keble Road, Oxford OX1 3RH, UK

63 European Space Agency/ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands

64 Department of Physics and Astronomy, University of Aarhus, Ny Munkegade 120, 8000 Aarhus C, Denmark

65 Space Science Data Center, Italian Space Agency, via del Politecnico snc, 00133 Roma, Italy

66 Centre National d'Etudes Spatiales - Centre spatial de Toulouse, 18 avenue Edouard Belin, 31401 Toulouse Cedex 9, France

67 Dipartimento di Fisica e Astronomia "G. Galilei", Università di Padova, Via Marzolo 8, 35131 Padova, Italy

68 INFN-Padova, Via Marzolo 8, 35131 Padova, Italy

69 Universitäts-Sternwarte München, Fakultät für Physik, Ludwig-Maximilians-Universität München, Scheinerstrasse 1, 81679 München, Germany

70 Departamento de Física, FCFM, Universidad de Chile, Blanco Encalada 2008, Santiago, Chile

71 Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capitá 2-4, 08034 Barcelona, Spain

72 Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain

73 Satlantis, University Science Park, Sede Bld 48940, Leioa-Bilbao, Spain

74 Centre for Electronic Imaging, Open University, Walton Hall, Milton Keynes, MK7 6AA, UK

75 Centro de Investigaciones Energéticas, Medioambientales y TEC-
nológicas (CIEMAT), Avenida Complutense 40, 28040 Madrid,
Spain

76 Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciên-
cias, Universidade de Lisboa, Tapada da Ajuda, 1349-018 Lisboa,
Portugal

77 Universidad Politécnica de Cartagena, Departamento de Elec-
trónica y Tecnología de Computadoras, Plaza del Hospital 1, 30202
Cartagena, Spain

78 Institut de Recherche en Astrophysique et Planétologie (IRAP), Uni-
versité de Toulouse, CNRS, UPS, CNES, 14 Av. Edouard Belin,
31400 Toulouse, France

79 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands

80 INFN-Bologna, Via Irnerio 46, 40126 Bologna, Italy

81 Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA

82 Instituto de Astrofísica de Canarias, Calle Vía Láctea s/n, 38204, San Cristóbal de La Laguna, Tenerife, Spain

83 Junia, EPA department, 41 Bd Vauban, 59800 Lille, France
17 INAF-IASF Milano, Via Alfonso Corti 12, 20133 Milano, Italy

18 INAF-Osservatorio Astronomico di Roma, Via Frascati 33, 00078 Monteporzio Catone, Italy

19 INFN-Sezione di Roma, Piazzale Aldo Moro 2, c/o Dipartimento di Fisica, Edificio G. Marconi, 00185 Roma, Italy

20 Institut de Física d'Altes Energies (IFAE), The Barcelona Institute of Science and Technology, Campus UAB, 08193 Bellaterra (Barcelona), Spain

21 Port d'Informació Científica, Campus UAB, C. Albareda s/n, 08193 Bellaterra (Barcelona), Spain

22 Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University, 52056 Aachen, Germany

23 INFN section of Naples, Via Cinthia 6, 80126 Napoli, Italy

24 Dipartimento di Fisica e Astronomia "Augusto Righi" - Alma Mater Studiorum Università di Bologna, Viale Berti Pichat 6/2, 40127 Bologna, Italy

25 Institute for Astronomy, University of Edinburgh, Royal Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK

26 European Space Agency/ESRIN, Largo Galileo Galilei 1, 00044 Frascati, Roma, Italy

27 ESAC/ESA, Camino Bajo del Castillo, s/n., Urb. Villafranca del Castillo, 28692 Villanueva de la Cañada, Madrid, Spain

28 University of Lyon, Univ Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, 69622 Villeurbanne, France

29 Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL), Observatoire de Sauverny, 1290 Versoix, Switzerland

30 UCB Lyon 1, CNRS/IN2P3, IUF, IP2I Lyon, 4 rue Enrico Fermi, 69622 Villeurbanne, France

31 Departamento de Física, Faculdade de Ciências, Universidade de Lisboa, Edifício C8, Campo Grande, 1749-016 Lisboa, Portugal

32 Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências, Universidade de Lisboa, Campo Grande, 1749-016 Lisboa, Portugal

33 Department of Astronomy, University of Geneva, ch. d'Ecogia 16, 1290 Versoix, Switzerland

34 INAF-Istituto di Astrofisica e Planetologia Spaziali, via del Fosso del Cavaliere, 100, 00100 Roma, Italy

35 Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM, 91191 Gif-sur-Yvette, France

36 INAF-Osservatorio Astronomico di Trieste, Via G. B. Tiepolo 11, 34143 Trieste, Italy

37 INAF-Osservatorio Astronomico di Padova, Via dell'Osservatorio 5, 35122 Padova, Italy

38 Max Planck Institute for Extraterrestrial Physics, Giessenbachstr. 1, 85748 Garching, Germany

39 University Observatory, Faculty of Physics, Ludwig-Maximilians-Universität, Scheinerstr. 1, 81679 Munich, Germany

40 Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway

41 Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands

42 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA, 91109, USA

43 von Hoerner & Sulger GmbH, Schloßplatz 8, 68723 Schwetzingen, Germany

44 Technical University of Denmark, Elektrovej 327, 2800 Kgs. Lyngby, Denmark

45 Cosmic Dawn Center (DAWN), Copenhagen, Denmark

46 Institut d'Astrophysique de Paris, UMR 7095, CNRS, and Sorbonne Université, 98 bis boulevard Arago, 75014 Paris, France

47 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany

48 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK

49 Aix-Marseille Université, CNRS/IN2P3, CPPM, Marseille, France

50 Université Paris-Saclay, Université Paris Cité, CEA, CNRS, Astrophysique, Instrumentation et Modélisation Paris-Saclay, 91191 Gif-sur-Yvette, France

51 Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT, UK

52 Department of Physics, PO Box 64, 00014 University of Helsinki, Finland

53 Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University of Helsinki, Helsinki, Finland

54 NOVA optical infrared instrumentation group at ASTRON, Oude Hoogeveensedijk 4, 7991PD, Dwingeloo, The Netherlands

55 Aix-Marseille Université, CNRS, CNES, LAM, Marseille, France

56 Dipartimento di Fisica e Astronomia "Augusto Righi" - Alma Mater Studiorum Università di Bologna, via Piero Gobetti 93/2, 40129 Bologna, Italy

57 Department of Physics, Institute for Computational Cosmology, Durham University, South Road, DH1 3LE, UK

58 Université Paris Cité, CNRS, Astroparticule et Cosmologie, 75013 Paris, France

59 University of Applied Sciences and Arts of Northwestern Switzerland, School of Engineering, 5210 Windisch, Switzerland

60 Institut d'Astrophysique de Paris, 98bis Boulevard Arago, 75014 Paris, France

61 CEA Saclay, DFR/IRFU, Service d'Astrophysique, Bat. 709, 91191 Gif-sur-Yvette, France

62 Department of Physics, Oxford University, Keble Road, Oxford OX1 3RH, UK

63 European Space Agency/ESTEC, Keplerlaan 1, 2201 AZ Noordwijk, The Netherlands

64 Department of Physics and Astronomy, University of Aarhus, Ny Munkegade 120, 8000 Aarhus C, Denmark

65 Space Science Data Center, Italian Space Agency, via del Politecnico snc, 00133 Roma, Italy

66 Centre National d'Etudes Spatiales - Centre spatial de Toulouse, 18 avenue Edouard Belin, 31401 Toulouse Cedex 9, France

67 Dipartimento di Fisica e Astronomia "G. Galilei", Università di Padova, Via Marzolo 8, 35131 Padova, Italy

68 INFN-Padova, Via Marzolo 8, 35131 Padova, Italy

69 Universitäts-Sternwarte München, Fakultät für Physik, Ludwig-Maximilians-Universität München, Scheinerstrasse 1, 81679 München, Germany

70 Departamento de Física, FCFM, Universidad de Chile, Blanco Encalada 2008, Santiago, Chile

71 Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capitá 2-4, 08034 Barcelona, Spain

72 Institute of Space Sciences (ICE, CSIC), Campus UAB, Carrer de Can Magrans, s/n, 08193 Barcelona, Spain

73 Satlantis, University Science Park, Sede Bld 48940, Leioa-Bilbao, Spain

74 Centre for Electronic Imaging, Open University, Walton Hall, Milton Keynes, MK7 6AA, UK

75 Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), Avenida Complutense 40, 28040 Madrid, Spain

76 Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências, Universidade de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal

77 Universidad Politécnica de Cartagena, Departamento de Electrónica y Tecnología de Computadoras, Plaza del Hospital 1, 30202 Cartagena, Spain

78 Institut de Recherche en Astrophysique et Planétologie (IRAP), Université de Toulouse, CNRS, UPS, CNES, 14 Av. Edouard Belin, 31400 Toulouse, France

79 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands

80 INFN-Bologna, Via Irnerio 46, 40126 Bologna, Italy

81 Infrared Processing and Analysis Center, California Institute of Technology, Pasadena, CA 91125, USA

82 Instituto de Astrofísica de Canarias, Calle Vía Láctea s/n, 38204, San Cristóbal de La Laguna, Tenerife, Spain

83 Junia, EPA department, 41 Bd Vauban, 59800 Lille, France
# Appendix A: Binned improvements additive bias

The binned improvements can also be studied for the additive bias. In Fig. A.1, these are shown for the grid simulations and in Figs. A.2 and A.3 for random positions.

<figure><img src="image_16.png" /><figcaption>**Fig. A.1.** Magnitude-binned runtime improvement of the additive bias for the grid-based simulations. The position of the points marks the center of each bin. The runtime improvement is always compared to the fit method without any cancellation. Error bars are smaller than the symbols and therefore omitted for better visibility.</figcaption></figure>

<figure><img src="image_17.png" /><figcaption>**Fig. A.2.** Magnitude-binned runtime improvement of the additive bias for the random position simulations in the large shear interval. In the left panel, the data is binned in $m_{AUTO}$ from SExtractor, while the input magnitude is used for the binning in the right panel to point out the differences. The position of the points marks the center of each bin. The runtime improvement is always compared to the fit method without any cancellation. For this figure, no signal-to-noise cut is applied. Error bars are smaller than the symbols and therefore omitted for better visibility.</figcaption></figure>
# Appendix A: Binned improvements additive bias

The binned improvements can also be studied for the additive bias. In Fig. A.1, these are shown for the grid simulations and in Figs. A.2 and A.3 for random positions.

<figure><img src="image_19.png" /><figcaption>**Fig. A.1.** Magnitude-binned runtime improvement of the additive bias for the grid-based simulations. The position of the points marks the center of each bin. The runtime improvement is always compared to the fit method without any cancellation. Error bars are smaller than the symbols and therefore omitted for better visibility.</figcaption></figure>

<figure><img src="image_20.png" /><figcaption>**Fig. A.2.** Magnitude-binned runtime improvement of the additive bias for the random position simulations in the large shear interval. In the left panel, the data is binned in $m_{AUTO}$ from SExtractor, while the input magnitude is used for the binning in the right panel to point out the differences. The position of the points marks the center of each bin. The runtime improvement is always compared to the fit method without any cancellation. For this figure, no signal-to-noise cut is applied. Error bars are smaller than the symbols and therefore omitted for better visibility.</figcaption></figure>
<figure><img src="image_18.png" /><figcaption>**Fig. A.3.** Magnitude-binned runtime improvement of the additive bias for the random position simulations in the small shear interval. In the left panel, the data is binned in $m_{AUTO}$ from SExtractor, while the input magnitude is used for the binning in the right panel to point out the differences. The position of the points marks the center of each bin. The runtime improvement is always compared to the fit method without any cancellation. For this figure, no signal-to-noise cut is applied. Error bars are smaller than the symbols and therefore omitted for better visibility.</figcaption></figure>

## Appendix B: Binned absolute biases

In order to test if the different methods yield accurate bias estimates, we compare the outcome of the absolute bias measurements for each method in each bin. For the multiplicative bias these comparisons can be seen in Fig. B.1 and Fig. B.2 for the large and the small input shear interval, respectively. For the additive bias they are shown in Fig. B.3 and Fig. B.4. We observe that the methods are compatible in every magnitude bin, ensuring that every method can be used to determine the biases. The decision of which method to choose only depends on the efficiency of the method.

<figure><img src="image_19.png" /><figcaption>**Fig. B.1.** Absolute multiplicative bias comparison in the large shear interval. The general trend of the multiplicative bias at different magnitudes is presented in the main plot. An additional zoomed version of each magnitude bin is shown to better compare the bias estimates since the error bars are too small to be visible in the main plot. For the left panel, no signal-to-noise cut is applied.</figcaption></figure>
<figure><img src="image_21.png" /><figcaption>**Fig. A.3.** Magnitude-binned runtime improvement of the additive bias for the random position simulations in the small shear interval. In the left panel, the data is binned in $m_{AUTO}$ from SExtractor, while the input magnitude is used for the binning in the right panel to point out the differences. The position of the points marks the center of each bin. The runtime improvement is always compared to the fit method without any cancellation. For this figure, no signal-to-noise cut is applied. Error bars are smaller than the symbols and therefore omitted for better visibility.</figcaption></figure>

## Appendix B: Binned absolute biases

In order to test if the different methods yield accurate bias estimates, we compare the outcome of the absolute bias measurements for each method in each bin. For the multiplicative bias these comparisons can be seen in Fig. B.1 and Fig. B.2 for the large and the small input shear interval, respectively. For the additive bias they are shown in Fig. B.3 and Fig. B.4. We observe that the methods are compatible in every magnitude bin, ensuring that every method can be used to determine the biases. The decision of which method to choose only depends on the efficiency of the method.

<figure><img src="image_22.png" /><figcaption>**Fig. B.1.** Absolute multiplicative bias comparison in the large shear interval. The general trend of the multiplicative bias at different magnitudes is presented in the main plot. An additional zoomed version of each magnitude bin is shown to better compare the bias estimates since the error bars are too small to be visible in the main plot. For the left panel, no signal-to-noise cut is applied.</figcaption></figure>
<figure><img src="image_20.png" /><figcaption>**Fig. B.2.** Absolute multiplicative bias comparison in the small shear interval. The general trend of the multiplicative bias at different magnitudes is presented in the main plot. An additional zoomed version of each magnitude bin is shown to better compare the bias estimates since the error bars are too small to be visible in the main plot. For the left panel, no signal-to-noise cut is applied.</figcaption></figure>

<figure><img src="image_21.png" /><figcaption>**Fig. B.3.** Absolute additive bias comparison in the large shear interval. For the left panel, no signal-to-noise cut is applied.</figcaption></figure>
<figure><img src="image_23.png" /><figcaption>**Fig. B.2.** Absolute multiplicative bias comparison in the small shear interval. The general trend of the multiplicative bias at different magnitudes is presented in the main plot. An additional zoomed version of each magnitude bin is shown to better compare the bias estimates since the error bars are too small to be visible in the main plot. For the left panel, no signal-to-noise cut is applied.</figcaption></figure>

<figure><img src="image_24.png" /><figcaption>**Fig. B.3.** Absolute additive bias comparison in the large shear interval. For the left panel, no signal-to-noise cut is applied.</figcaption></figure>
<figure><img src="image_22.png" /><figcaption>**Fig. B.4.** Absolute additive bias comparison in the small shear interval. For the left panel, no signal-to-noise cut is applied.</figcaption></figure>
<figure><img src="image_25.png" /><figcaption>Fig. B.4. Absolute additive bias comparison in the small shear interval. For the left panel, no signal-to-noise cut is applied.</figcaption></figure>