Cosmological simulations for combined-probe analyses: Covariance and neighbour-exclusion bias

J. Harnois-Déraps; A. Amon; A. Choi; V. Demchenko; C. Heymans; A. Kannawadi; R. Nakajima; E. Sirks; L. van Waerbeke; Yan Chuan Cai; B. Giblin; H. Hildebrandt; H. Hoekstra; L. Miller; T. Tröster

doi:10.1093/MNRAS/STY2319

Cosmological simulations for combined-probe analyses: Covariance and neighbour-exclusion bias

J. Harnois-Déraps, A. Amon, A. Choi, V. Demchenko, C. Heymans, A. Kannawadi, R. Nakajima, E. Sirks, L. van Waerbeke, Yan Chuan Cai, B. Giblin, H. Hildebrandt, H. Hoekstra, L. Miller, T. Tröster

Research output: Contribution to journal › Article › peer-review

44 Scopus citations

Abstract

We present a public suite of weak-lensing mock data, extending the Scinet Light Cone Simulations (SLICS) to simulate cross-correlation analyses with different cosmological probes. These mocks include Kilo Degree Survey (KiDS)-450-and LSST-like lensing data, cosmic microwave background lensing maps and simulated spectroscopic surveys that emulate the Galaxy And Mass Assembly, BOSS, and 2-degree Field Lensing galaxy surveys. With 844 independent realizations, our mocks are optimized for combined-probe covariance estimation, which we illustrate for the case of a joint measurement involving cosmic shear, galaxy-galaxy lensing, and galaxy clustering from KiDS-450 and BOSS data. With their high spatial resolution, the SLICS are also optimal for predicting the signal for novel lensing estimators, for the validation of analysis pipelines, and for testing a range of systematic effects such as the impact of neighbour-exclusion bias on the measured tomographic cosmic shear signal. For surveys like KiDS and Dark Energy Survey, where the rejection of neighbouring galaxies occurs within ~2 arcsec, we show that the measured cosmic shear signal will be biased low, but by less than a per cent on the angular scales that are typically used in cosmic shear analyses. The amplitude of the neighbour-exclusion bias doubles in deeper, LSST-like data. The simulation products described in this paper are made available at http://slics.roe.ac.uk/.

Original language	English (US)
Pages (from-to)	1337-1367
Number of pages	31
Journal	Monthly Notices of the Royal Astronomical Society
Volume	481
Issue number	1
DOIs	https://doi.org/10.1093/MNRAS/STY2319
State	Published - Nov 1 2018
Externally published	Yes

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Dark matter
Gravitational lensing: weak
Large-scale structure of Universe
Methods: numerical

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10.1093/MNRAS/STY2319

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Harnois-Déraps, J., Amon, A., Choi, A., Demchenko, V., Heymans, C., Kannawadi, A., Nakajima, R., Sirks, E., van Waerbeke, L., Cai, Y. C., Giblin, B., Hildebrandt, H., Hoekstra, H., Miller, L., & Tröster, T. (2018). Cosmological simulations for combined-probe analyses: Covariance and neighbour-exclusion bias. Monthly Notices of the Royal Astronomical Society, 481(1), 1337-1367. https://doi.org/10.1093/MNRAS/STY2319

@article{0b8e01d61f2540c080df257cbacc3a85,

title = "Cosmological simulations for combined-probe analyses: Covariance and neighbour-exclusion bias",

abstract = "We present a public suite of weak-lensing mock data, extending the Scinet Light Cone Simulations (SLICS) to simulate cross-correlation analyses with different cosmological probes. These mocks include Kilo Degree Survey (KiDS)-450-and LSST-like lensing data, cosmic microwave background lensing maps and simulated spectroscopic surveys that emulate the Galaxy And Mass Assembly, BOSS, and 2-degree Field Lensing galaxy surveys. With 844 independent realizations, our mocks are optimized for combined-probe covariance estimation, which we illustrate for the case of a joint measurement involving cosmic shear, galaxy-galaxy lensing, and galaxy clustering from KiDS-450 and BOSS data. With their high spatial resolution, the SLICS are also optimal for predicting the signal for novel lensing estimators, for the validation of analysis pipelines, and for testing a range of systematic effects such as the impact of neighbour-exclusion bias on the measured tomographic cosmic shear signal. For surveys like KiDS and Dark Energy Survey, where the rejection of neighbouring galaxies occurs within ~2 arcsec, we show that the measured cosmic shear signal will be biased low, but by less than a per cent on the angular scales that are typically used in cosmic shear analyses. The amplitude of the neighbour-exclusion bias doubles in deeper, LSST-like data. The simulation products described in this paper are made available at http://slics.roe.ac.uk/.",

keywords = "Dark matter, Gravitational lensing: weak, Large-scale structure of Universe, Methods: numerical",

author = "J. Harnois-D{\'e}raps and A. Amon and A. Choi and V. Demchenko and C. Heymans and A. Kannawadi and R. Nakajima and E. Sirks and {van Waerbeke}, L. and Cai, {Yan Chuan} and B. Giblin and H. Hildebrandt and H. Hoekstra and L. Miller and T. Tr{\"o}ster",

note = "Funding Information: The HOD calculations used in the paper inherits from the code written by Marcello Cacciato, who also provided many advices on general HOD strategies. Shadab Alam and Chris Blake also contributed to these discussions, which helped us in deciding what strategy best suited our needs. We would like to thank Ian Fenech Conti, and Ricardo Herbonnet for their help with the image simulations, Alexander Smith for sharing the details of his GAMA HOD prescription, Joe Zuntz for providing the LSST n(z) and for his insights on the DES shape measurement strategy, and the anonymous referee for their useful comments. This work also benefitted from discussions about blending with Javier Sanchez and Joe Zuntz. We would like to acknowledge the input of many users that have tested the different simulation products and provided invaluable feedback that helped us finding bugs and making the mock products easier to use, notably Chris Blake, Massimo Viola, Edo van Uitert, Marika Asgari, India Rose Friswell, Harry Johnston, Nicolas Martinet and Axel Buddendiek, Elena Sellentin, and Chien-Hao Lin. We thank Martin Kilbinger for help with the ATHENA correlation function measurement software and the NICAEA theoretical modelling software, Mike Jarvis for maintaining TREECORR, and Joe Zuntz for help with COSMOSIS. JHD is supported by the European Commission under a Marie-Sklodowska-Curie European Fellowship (EU project 656869). CH and AA acknowledge support from the European Research Council under grant number 647112; AA is further supported by a LSSTC Data Science Fellowship.VDacknowledges the Higgs Centre Nimmo Scholarship and the Edinburgh Global Research Scholarship. AKand HHo acknowledge support from the Netherlands Organisation for Scientific Research (NWO) Vici grant 639.043.512. RN acknowledges support from the German Federal Ministry for Economic Affairs and Energy (BMWi) provided via DLR under project no. 50QE1103. LvW is supported by the NSERC of Canada. HHi is supported by an Emmy Noether grant (No. Hi 1495/2-1) of the Deutsche Forschungsgemeinschaft. LM acknowledges support from STFC grant ST/N000919/1. Computations for the N-body simulations were performed in part on the Orcinus supercomputer at the WestGrid HPC consortium (www.westgrid.ca), in part on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by: the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund - Research Excellence; and the University of Toronto. The post-processing calculations were mainly carried out on the Cuillin cluster at the Royal Observatory of Edinburgh, which is run by Eric Tittley. The mock data presented in this paper are calibrated against observations from KiDS, GAMA, and BOSS. This KiDS data are based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017, and 177.A-3018. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT, and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/. Also based on observations made with ESO Telescopes under programme ID 177.A-3016. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. We would finally like to thank McGill University for its hospitality, where an important part of the HOD code development was made. All authors contributed to the development and writing of this paper. The authorship list is given in three groups: the lead author (JHD), followed by two alphabetical groups. Members of the first alphabetical group carried out key infrastructure work specifically for this paper. Members of the second alphabetical group provided proprietary data central to this work, or contributed to the analysis. Funding Information: Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Funding Information: Computations for the N-body simulations were performed in part on the Orcinus supercomputer at the WestGrid HPC consortium (www.westgrid.ca), in part on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by: the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund – Research Excellence; and the University of Toronto. The post-processing calculations were mainly carried out on the Cuillin cluster at the Royal Observatory of Edinburgh, which is run by Eric Tittley. Funding Information: GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT, and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/. Also based on observations made with ESO Telescopes under programme ID 177.A-3016. Funding Information: JHD is supported by the European Commission under a Marie-Sk{\l}odowska-Curie European Fellowship (EU project 656869). CH and AA acknowledge support from the European Research Council under grant number 647112; AA is further supported by a LSSTC Data Science Fellowship. VD acknowledges the Higgs Centre Nimmo Scholarship and the Edinburgh Global Research Scholarship. AK and HHo acknowledge support from the Netherlands Organisation for Scientific Research (NWO) Vici grant 639.043.512. RN acknowledges support from the German Federal Ministry for Economic Affairs and Energy (BMWi) provided via DLR under project no. 50QE1103. LvW is supported by the NSERC of Canada. HHi is supported by an Emmy Noether grant (No. Hi 1495/2-1) of the Deutsche Forschungsgemeinschaft. LM acknowledges support from STFC grant ST/N000919/1. Publisher Copyright: {\textcopyright} 2018 The Author(s).",

year = "2018",

month = nov,

day = "1",

doi = "10.1093/MNRAS/STY2319",

language = "English (US)",

volume = "481",

pages = "1337--1367",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "1",

}

Harnois-Déraps, J, Amon, A, Choi, A, Demchenko, V, Heymans, C, Kannawadi, A, Nakajima, R, Sirks, E, van Waerbeke, L, Cai, YC, Giblin, B, Hildebrandt, H, Hoekstra, H, Miller, L & Tröster, T 2018, 'Cosmological simulations for combined-probe analyses: Covariance and neighbour-exclusion bias', Monthly Notices of the Royal Astronomical Society, vol. 481, no. 1, pp. 1337-1367. https://doi.org/10.1093/MNRAS/STY2319

TY - JOUR

T1 - Cosmological simulations for combined-probe analyses

T2 - Covariance and neighbour-exclusion bias

AU - Harnois-Déraps, J.

AU - Amon, A.

AU - Choi, A.

AU - Demchenko, V.

AU - Heymans, C.

AU - Kannawadi, A.

AU - Nakajima, R.

AU - Sirks, E.

AU - van Waerbeke, L.

AU - Cai, Yan Chuan

AU - Giblin, B.

AU - Hildebrandt, H.

AU - Hoekstra, H.

AU - Miller, L.

AU - Tröster, T.

N1 - Funding Information: The HOD calculations used in the paper inherits from the code written by Marcello Cacciato, who also provided many advices on general HOD strategies. Shadab Alam and Chris Blake also contributed to these discussions, which helped us in deciding what strategy best suited our needs. We would like to thank Ian Fenech Conti, and Ricardo Herbonnet for their help with the image simulations, Alexander Smith for sharing the details of his GAMA HOD prescription, Joe Zuntz for providing the LSST n(z) and for his insights on the DES shape measurement strategy, and the anonymous referee for their useful comments. This work also benefitted from discussions about blending with Javier Sanchez and Joe Zuntz. We would like to acknowledge the input of many users that have tested the different simulation products and provided invaluable feedback that helped us finding bugs and making the mock products easier to use, notably Chris Blake, Massimo Viola, Edo van Uitert, Marika Asgari, India Rose Friswell, Harry Johnston, Nicolas Martinet and Axel Buddendiek, Elena Sellentin, and Chien-Hao Lin. We thank Martin Kilbinger for help with the ATHENA correlation function measurement software and the NICAEA theoretical modelling software, Mike Jarvis for maintaining TREECORR, and Joe Zuntz for help with COSMOSIS. JHD is supported by the European Commission under a Marie-Sklodowska-Curie European Fellowship (EU project 656869). CH and AA acknowledge support from the European Research Council under grant number 647112; AA is further supported by a LSSTC Data Science Fellowship.VDacknowledges the Higgs Centre Nimmo Scholarship and the Edinburgh Global Research Scholarship. AKand HHo acknowledge support from the Netherlands Organisation for Scientific Research (NWO) Vici grant 639.043.512. RN acknowledges support from the German Federal Ministry for Economic Affairs and Energy (BMWi) provided via DLR under project no. 50QE1103. LvW is supported by the NSERC of Canada. HHi is supported by an Emmy Noether grant (No. Hi 1495/2-1) of the Deutsche Forschungsgemeinschaft. LM acknowledges support from STFC grant ST/N000919/1. Computations for the N-body simulations were performed in part on the Orcinus supercomputer at the WestGrid HPC consortium (www.westgrid.ca), in part on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by: the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund - Research Excellence; and the University of Toronto. The post-processing calculations were mainly carried out on the Cuillin cluster at the Royal Observatory of Edinburgh, which is run by Eric Tittley. The mock data presented in this paper are calibrated against observations from KiDS, GAMA, and BOSS. This KiDS data are based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 177.A-3016, 177.A-3017, and 177.A-3018. GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT, and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/. Also based on observations made with ESO Telescopes under programme ID 177.A-3016. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. We would finally like to thank McGill University for its hospitality, where an important part of the HOD code development was made. All authors contributed to the development and writing of this paper. The authorship list is given in three groups: the lead author (JHD), followed by two alphabetical groups. Members of the first alphabetical group carried out key infrastructure work specifically for this paper. Members of the second alphabetical group provided proprietary data central to this work, or contributed to the analysis. Funding Information: Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/. SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. Funding Information: Computations for the N-body simulations were performed in part on the Orcinus supercomputer at the WestGrid HPC consortium (www.westgrid.ca), in part on the GPC supercomputer at the SciNet HPC Consortium. SciNet is funded by: the Canada Foundation for Innovation under the auspices of Compute Canada; the Government of Ontario; Ontario Research Fund – Research Excellence; and the University of Toronto. The post-processing calculations were mainly carried out on the Cuillin cluster at the Royal Observatory of Edinburgh, which is run by Eric Tittley. Funding Information: GAMA is a joint European-Australasian project based around a spectroscopic campaign using the Anglo-Australian Telescope. The GAMA input catalogue is based on data taken from the Sloan Digital Sky Survey and the UKIRT Infrared Deep Sky Survey. Complementary imaging of the GAMA regions is being obtained by a number of independent survey programmes including GALEX MIS, VST KiDS, VISTA VIKING, WISE, Herschel-ATLAS, GMRT, and ASKAP providing UV to radio coverage. GAMA is funded by the STFC (UK), the ARC (Australia), the AAO, and the participating institutions. The GAMA website is http://www.gama-survey.org/. Also based on observations made with ESO Telescopes under programme ID 177.A-3016. Funding Information: JHD is supported by the European Commission under a Marie-Skłodowska-Curie European Fellowship (EU project 656869). CH and AA acknowledge support from the European Research Council under grant number 647112; AA is further supported by a LSSTC Data Science Fellowship. VD acknowledges the Higgs Centre Nimmo Scholarship and the Edinburgh Global Research Scholarship. AK and HHo acknowledge support from the Netherlands Organisation for Scientific Research (NWO) Vici grant 639.043.512. RN acknowledges support from the German Federal Ministry for Economic Affairs and Energy (BMWi) provided via DLR under project no. 50QE1103. LvW is supported by the NSERC of Canada. HHi is supported by an Emmy Noether grant (No. Hi 1495/2-1) of the Deutsche Forschungsgemeinschaft. LM acknowledges support from STFC grant ST/N000919/1. Publisher Copyright: © 2018 The Author(s).

PY - 2018/11/1

Y1 - 2018/11/1

N2 - We present a public suite of weak-lensing mock data, extending the Scinet Light Cone Simulations (SLICS) to simulate cross-correlation analyses with different cosmological probes. These mocks include Kilo Degree Survey (KiDS)-450-and LSST-like lensing data, cosmic microwave background lensing maps and simulated spectroscopic surveys that emulate the Galaxy And Mass Assembly, BOSS, and 2-degree Field Lensing galaxy surveys. With 844 independent realizations, our mocks are optimized for combined-probe covariance estimation, which we illustrate for the case of a joint measurement involving cosmic shear, galaxy-galaxy lensing, and galaxy clustering from KiDS-450 and BOSS data. With their high spatial resolution, the SLICS are also optimal for predicting the signal for novel lensing estimators, for the validation of analysis pipelines, and for testing a range of systematic effects such as the impact of neighbour-exclusion bias on the measured tomographic cosmic shear signal. For surveys like KiDS and Dark Energy Survey, where the rejection of neighbouring galaxies occurs within ~2 arcsec, we show that the measured cosmic shear signal will be biased low, but by less than a per cent on the angular scales that are typically used in cosmic shear analyses. The amplitude of the neighbour-exclusion bias doubles in deeper, LSST-like data. The simulation products described in this paper are made available at http://slics.roe.ac.uk/.

AB - We present a public suite of weak-lensing mock data, extending the Scinet Light Cone Simulations (SLICS) to simulate cross-correlation analyses with different cosmological probes. These mocks include Kilo Degree Survey (KiDS)-450-and LSST-like lensing data, cosmic microwave background lensing maps and simulated spectroscopic surveys that emulate the Galaxy And Mass Assembly, BOSS, and 2-degree Field Lensing galaxy surveys. With 844 independent realizations, our mocks are optimized for combined-probe covariance estimation, which we illustrate for the case of a joint measurement involving cosmic shear, galaxy-galaxy lensing, and galaxy clustering from KiDS-450 and BOSS data. With their high spatial resolution, the SLICS are also optimal for predicting the signal for novel lensing estimators, for the validation of analysis pipelines, and for testing a range of systematic effects such as the impact of neighbour-exclusion bias on the measured tomographic cosmic shear signal. For surveys like KiDS and Dark Energy Survey, where the rejection of neighbouring galaxies occurs within ~2 arcsec, we show that the measured cosmic shear signal will be biased low, but by less than a per cent on the angular scales that are typically used in cosmic shear analyses. The amplitude of the neighbour-exclusion bias doubles in deeper, LSST-like data. The simulation products described in this paper are made available at http://slics.roe.ac.uk/.

KW - Dark matter

KW - Gravitational lensing: weak

KW - Large-scale structure of Universe

KW - Methods: numerical

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U2 - 10.1093/MNRAS/STY2319

DO - 10.1093/MNRAS/STY2319

M3 - Article

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SN - 0035-8711

VL - 481

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EP - 1367

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

Cosmological simulations for combined-probe analyses: Covariance and neighbour-exclusion bias

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