text:
@article{2023MNRAS.518..477A,
 abbr = {MNRAS},
 abstract = {{We evaluate the consistency between lensing and clustering based on
measurements from Baryon Oscillation Spectroscopic Survey
combined with galaxy-galaxy lensing from Dark Energy Survey
(DES) Year 3, Hyper Suprime-Cam Subaru Strategic Program (HSC)
Year 1, and Kilo-Degree Survey (KiDS)-1000. We find good
agreement between these lensing data sets. We model the
observations using the DARK EMULATOR and fit the data at two
fixed cosmologies: Planck (S$_{8}$ = 0.83), and a Lensing
cosmology (S$_{8}$ = 0.76). For a joint analysis limited to
large scales, we find that both cosmologies provide an
acceptable fit to the data. Full utilization of the higher
signal-to-noise small-scale measurements is hindered by
uncertainty in the impact of baryon feedback and assembly bias,
which we account for with a reasoned theoretical error budget.
We incorporate a systematic inconsistency parameter for each
redshift bin, A, that decouples the lensing and clustering. With
a wide range of scales, we find different results for the
consistency between the two cosmologies. Limiting the analysis
to the bins for which the impact of the lens sample selection is
expected to be minimal, for the Lensing cosmology, the
measurements are consistent with A = 1; A = 0.91
{\ensuremath{\pm}} 0.04 (A = 0.97 {\ensuremath{\pm}} 0.06) using
DES+KiDS (HSC). For the Planck case, we find a discrepancy: A =
0.79 {\ensuremath{\pm}} 0.03 (A = 0.84 {\ensuremath{\pm}} 0.05)
using DES+KiDS (HSC). We demonstrate that a kinematic Sunyaev-
Zeldovich-based estimate for baryonic effects alleviates some of
the discrepancy in the Planck cosmology. This analysis
demonstrates the statistical power of small-scale measurements;
however, caution is still warranted given modelling
uncertainties and foreground sample selection effects.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2023MNRAS.518..477A},
 altmetric = {123134747},
 archiveprefix = {arXiv},
 arxiv = {2202.07440},
 author = {{Amon}, A. and {Robertson}, N.~C. and {Miyatake}, H. and {Heymans}, C. and {White}, M. and {DeRose}, J. and {Yuan}, S. and {Wechsler}, R.~H. and {Varga}, T.~N. and {Bocquet}, S. and {Dvornik}, A. and {More}, S. and {Ross}, A.~J. and {Hoekstra}, H. and {Alarcon}, A. and {Asgari}, M. and {Blazek}, J. and {Campos}, A. and {Chen}, R. and {Choi}, A. and {Crocce}, M. and {Diehl}, H.~T. and {Doux}, C. and {Eckert}, K. and {Elvin-Poole}, J. and {Everett}, S. and {Fert{\'e}}, A. and {Gatti}, M. and {Giannini}, G. and {Gruen}, D. and {Gruendl}, R.~A. and {Hartley}, W.~G. and {Herner}, K. and {Hildebrandt}, H. and {Huang}, S. and {Huff}, E.~M. and {Joachimi}, B. and {Lee}, S. and {MacCrann}, N. and {Myles}, J. and {Navarro-Alsina}, A. and {Nishimichi}, T. and {Prat}, J. and {Secco}, L.~F. and {Sevilla-Noarbe}, I. and {Sheldon}, E. and {Shin}, T. and {Tr{\"o}ster}, T. and {Troxel}, M.~A. and {Tutusaus}, I. and {Wright}, A.~H. and {Yin}, B. and {Aguena}, M. and {Allam}, S. and {Annis}, J. and {Bacon}, D. and {Bilicki}, M. and {Brooks}, D. and {Burke}, D.~L. and {Carnero Rosell}, A. and {Carretero}, J. and {Castander}, F.~J. and {Cawthon}, R. and {Costanzi}, M. and {da Costa}, L.~N. and {Pereira}, M.~E.~S. and {de Jong}, J. and {De Vicente}, J. and {Desai}, S. and {Dietrich}, J.~P. and {Doel}, P. and {Ferrero}, I. and {Frieman}, J. and {Garc{\'\i}a-Bellido}, J. and {Gerdes}, D.~W. and {Gschwend}, J. and {Gutierrez}, G. and {Hinton}, S.~R. and {Hollowood}, D.~L. and {Honscheid}, K. and {Huterer}, D. and {Kannawadi}, A. and {Kuehn}, K. and {Kuropatkin}, N. and {Lahav}, O. and {Lima}, M. and {Maia}, M.~A.~G. and {Marshall}, J.~L. and {Menanteau}, F. and {Miquel}, R. and {Mohr}, J.~J. and {Morgan}, R. and {Muir}, J. and {Paz-Chinch{\'o}n}, F. and {Pieres}, A. and {Plazas Malag{\'o}n}, A.~A. and {Porredon}, A. and {Rodriguez-Monroy}, M. and {Roodman}, A. and {Sanchez}, E. and {Serrano}, S. and {Shan}, H. and {Suchyta}, E. and {Swanson}, M.~E.~C. and {Tarle}, G. and {Thomas}, D. and {To}, C. and {Zhang}, Y.},
 bibtex_show = {true},
 doi = {10.1093/mnras/stac2938},
 eprint = {2202.07440},
 journal = {Monthly Notices of the Royal Astronomical Society},
 keywords = {gravitational lensing: weak, large-scale structure of Universe, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {January},
 number = {1},
 pages = {477-503},
 primaryclass = {astro-ph.CO},
 title = {{Consistent lensing and clustering in a low-S$_{8}$ Universe with BOSS, DES Year 3, HSC Year 1, and KiDS-1000}},
 volume = {518},
 year = {2023}
}

@article{2022arXiv221203257Z,
 abstract = {{Cosmological weak lensing measurements rely on a precise measurement of
the shear two-point correlation function (2PCF) along with a
deep understanding of systematics that affect it. In this work,
we demonstrate a general framework for describing the impact of
PSF systematics on the cosmic shear 2PCF, and mitigating its
impact on cosmological analysis. Our framework can describe
leakage and modeling error from all spin-2 quantities
contributed by the PSF second and higher moments, rather than
just the second moments. We interpret null tests using the HSC
Year 3 (Y3) catalogs with this formalism, and find that leakage
from the spin-2 combination of PSF fourth moments is the leading
contributor to additive shear systematics, with total
contamination that is an order of magnitude higher than that
contributed by PSF second moments alone. We conducted a mock
cosmic shear analysis for HSC Y3, and find that, if uncorrected,
PSF systematics can bias the cosmological parameters $\Omega_m$
and $S_8$ by $\sim$0.3$\sigma$. The traditional second moment-
based model can only correct for a 0.1$\sigma$ bias, leaving the
contamination largely uncorrected. We conclude it is necessary
to model both PSF second and fourth moment contamination for HSC
Y3 cosmic shear analysis. We also reanalyze the HSC Y1 cosmic
shear analysis with our updated systematics model, and identify
a 0.07$\sigma$ bias on $\Omega_m$ when using the more restricted
second moment model from the original analysis. We demonstrate
how to self-consistently use the method in both real space and
Fourier space, assess shear systematics in tomographic bins, and
test for PSF model overfitting.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2022arXiv221203257Z},
 archiveprefix = {arXiv},
 arxiv = {2212.03257},
 author = {{Zhang}, Tianqing and {Li}, Xiangchong and {Dalal}, Roohi and {Mandelbaum}, Rachel and {Strauss}, Michael A. and {Kannawadi}, Arun and {Miyatake}, Hironao and {Nicola}, Andrina and {Plazas Malag{\'o}n}, Andr{\'e}s A. and {Shirasaki}, Masato and {Sugiyama}, Sunao and {Takada}, Masahiro},
 bibtex_show = {true},
 doi = {10.48550/arXiv.2212.03257},
 eid = {arXiv:2212.03257},
 eprint = {2212.03257},
 journal = {arXiv e-prints},
 keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {December},
 pages = {arXiv:2212.03257},
 primaryclass = {astro-ph.CO},
 title = {{A General Framework for Removing Point Spread Function Additive Systematics in Cosmological Weak Lensing Analysis}},
 year = {2022}
}

@article{2022MNRAS.tmp.3141Z,
 abbr = {MNRAS},
 abstract = {{Weak lensing is one of the most powerful probes for dark matter and dark
energy science, although it faces increasing challenges in
controlling systematic uncertainties as the statistical errors
become smaller. The Point Spread Function (PSF) needs to be
precisely modeled to avoid systematic error on the weak lensing
measurements. The weak lensing biases induced by errors in the
PSF model second moments, i.e. its size and shape, are well-
studied. However, Zhang et al. (2021) showed that errors in the
higher moments of the PSF may also be a significant source of
systematics for upcoming weak lensing surveys. Therefore, this
work comprehensively investigate the modeling quality of PSF
moments from the 3$^{rd}$ to 6$^{th}$ order, and propagate the
PSFEX higher moments modeling error in the HSC survey dataset to
the weak lensing shear-shear correlation functions and their
cosmological analyses. The overall multiplicative shear bias
associated with errors in PSF higher moments can cause a
\raisebox{-0.5ex}\textasciitilde0.1{\ensuremath{\sigma}} shift
on the cosmological parameters for LSST Y10, while the
associated additive biases can induce 1{\ensuremath{\sigma}}
uncertainties in cosmology parameter inference for LSST Y10, if
not accounted. We compare the PSFEX model with PSF in Full FOV
(PIFF), and find similar performance in modeling the PSF higher
moments. We conclude that PSF higher moment errors of the future
PSF models should be reduced from those in current methods,
otherwise needed to be explicitly modeled in the weak lensing
analysis.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.tmp.3141Z},
 altmetric = {128439621},
 archiveprefix = {arXiv},
 arxiv = {2205.07892},
 author = {{Zhang}, Tianqing and {Almoubayyed}, Husni and {Mandelbaum}, Rachel and {Meyers}, Joshua E. and {Jarvis}, Mike and {Kannawadi}, Arun and {Schmitz}, Morgan A. and {Guinot}, Axel and {LSST Dark Energy Science Collaboration}},
 bibtex_show = {true},
 custom_keywords = {major},
 doi = {10.1093/mnras/stac3350},
 eprint = {2205.07892},
 journal = {Monthly Notices of the Royal Astronomical Society},
 keywords = {methods: data analysis, gravitational lensing: weak, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics},
 month = {November},
 primaryclass = {astro-ph.CO},
 title = {{Impact of point spread function higher moments error on weak gravitational lensing II: A comprehensive study}},
 year = {2022}
}

@article{2022arXiv220909253M,
 abstract = {{We provide a detailed exploration of the connection between choice of
coaddition schemes and the point-spread function (PSF) of the
resulting coadded images. In particular, we investigate what
properties of the coaddition algorithm lead to the final coadded
image having a well-defined PSF. The key elements of this
discussion are as follows: 1. We provide an illustration of how
linear coaddition schemes can produce a coadd that lacks a well-
defined PSF even for relatively simple scenarios and choices of
weight functions. 2. We provide a more formal demonstration of
the fact that a linear coadd only has a well-defined PSF in the
case that either (a) each input image has the same PSF or (b)
the coadd is produced with weights that are independent of the
signal. 3. We discuss some reasons that two plausible nonlinear
coaddition algorithms (median and clipped-mean) fail to produce
a consistent PSF profile for stars. 4. We demonstrate that all
nonlinear coaddition procedures fail to produce a well-defined
PSF for extended objects. In the end, we conclude that, for any
purpose where a well-defined PSF is desired, one should use a
linear coaddition scheme with weights that do not correlate with
the signal and are approximately uniform across typical objects
of interest.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2022arXiv220909253M},
 archiveprefix = {arXiv},
 arxiv = {2209.09253},
 author = {{Mandelbaum}, Rachel and {Jarvis}, Mike and {Lupton}, Robert H. and {Bosch}, James and {Kannawadi}, Arun and {Murphy}, Michael D. and {Zhang}, Tianqing and {the LSST Dark Energy Science Collaboration}},
 bibtex_show = {true},
 custom_keywords = {major},
 doi = {10.48550/arXiv.2209.09253},
 eid = {arXiv:2209.09253},
 eprint = {2209.09253},
 journal = {arXiv e-prints},
 keywords = {Astrophysics - Instrumentation and Methods for Astrophysics},
 month = {September},
 pages = {arXiv:2209.09253},
 primaryclass = {astro-ph.IM},
 title = {{PSFs of coadded images}},
 year = {2022}
}

@article{2022arXiv220802781B,
 abstract = {{The Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST)
dataset will dramatically alter our understanding of the
Universe, from the origins of the Solar System to the nature of
dark matter and dark energy. Much of this research will depend
on the existence of robust, tested, and scalable algorithms,
software, and services. Identifying and developing such tools
ahead of time has the potential to significantly accelerate the
delivery of early science from LSST. Developing these
collaboratively, and making them broadly available, can enable
more inclusive and equitable collaboration on LSST science. To
facilitate such opportunities, a community workshop entitled
``From Data to Software to Science with the Rubin Observatory
LSST'' was organized by the LSST Interdisciplinary Network for
Collaboration and Computing (LINCC) and partners, and held at
the Flatiron Institute in New York, March 28-30th 2022. The
workshop included over 50 in-person attendees invited from over
300 applications. It identified seven key software areas of
need: (i) scalable cross-matching and distributed joining of
catalogs, (ii) robust photometric redshift determination, (iii)
software for determination of selection functions, (iv)
frameworks for scalable time-series analyses, (v) services for
image access and reprocessing at scale, (vi) object image access
(cutouts) and analysis at scale, and (vii) scalable job
execution systems. This white paper summarizes the discussions
of this workshop. It considers the motivating science use cases,
identified cross-cutting algorithms, software, and services,
their high-level technical specifications, and the principles of
inclusive collaborations needed to develop them. We provide it
as a useful roadmap of needs, as well as to spur action and
collaboration between groups and individuals looking to develop
reusable software for early LSST science.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2022arXiv220802781B},
 archiveprefix = {arXiv},
 arxiv = {2208.02781},
 author = {{Breivik}, Katelyn and {Connolly}, Andrew J. and {Ford}, K.~E. Saavik and {Juri{\'c}}, Mario and {Mandelbaum}, Rachel and {Miller}, Adam A. and {Norman}, Dara and {Olsen}, Knut and {O'Mullane}, William and {Price-Whelan}, Adrian and {Sacco}, Timothy and {Sokoloski}, J.~L. and {Villar}, Ashley and {Acquaviva}, Viviana and {Ahumada}, Tomas and {AlSayyad}, Yusra and {Alves}, Catarina S. and {Andreoni}, Igor and {Anguita}, Timo and {Best}, Henry J. and {Bianco}, Federica B. and {Bonito}, Rosaria and {Bradshaw}, Andrew and {Burke}, Colin J. and {Rodrigues de Campos}, Andresa and {Cantiello}, Matteo and {Caplar}, Neven and {Chandler}, Colin Orion and {Chan}, James and {Nicolaci da Costa}, Luiz and {Danieli}, Shany and {Davenport}, James R.~A. and {Fabbian}, Giulio and {Fagin}, Joshua and {Gagliano}, Alexander and {Gall}, Christa and {Garavito Camargo}, Nicol{\'a}s and {Gawiser}, Eric and {Gezari}, Suvi and {Gomboc}, Andreja and {Gonzalez-Morales}, Alma X. and {Graham}, Matthew J. and {Gschwend}, Julia and {Guy}, Leanne P. and {Holman}, Matthew J. and {Hsieh}, Henry H. and {Hundertmark}, Markus and {Ili{\'c}}, Dragana and {Ishida}, Emille E.~O. and {Jurki{\'c}}, Tomislav and {Kannawadi}, Arun and {Kosakowski}, Alekzander and {Kova{\v{c}}evi{\'c}}, Andjelka B. and {Kubica}, Jeremy and {Lanusse}, Fran{\c{c}}ois and {Lazar}, Ilin and {Levine}, W. Garrett and {Li}, Xiaolong and {Lu}, Jing and {Luna}, Gerardo Juan Manuel and {Mahabal}, Ashish A. and {Malz}, Alex I. and {Mao}, Yao-Yuan and {Medan}, Ilija and {Moeyens}, Joachim and {Nikoli{\'c}}, Mladen and {Nikutta}, Robert and {O'Dowd}, Matt and {Olsen}, Charlotte and {Pearson}, Sarah and {Villicana Pedraza}, Ilhuiyolitzin and {Popinchalk}, Mark and {Popovi{\'c}}, Luka C. and {Pritchard}, Tyler A. and {Quint}, Bruno C. and {Radovi{\'c}}, Viktor and {Ragosta}, Fabio and {Riccio}, Gabriele and {Riley}, Alexander H. and {Ro{\.z}ek}, Agata and {S{\'a}nchez-S{\'a}ez}, Paula and {Sarro}, Luis M. and {Saunders}, Clare and {Savi{\'c}}, {\DJ}or{\dj}e V. and {Schmidt}, Samuel and {Scott}, Adam and {Shirley}, Raphael and {Smotherman}, Hayden R. and {Stetzler}, Steven and {Storey-Fisher}, Kate and {Street}, Rachel A. and {Trilling}, David E. and {Tsapras}, Yiannis and {Ustamujic}, Sabina and {van Velzen}, Sjoert and {V{\'a}zquez-Mata}, Jos{\'e} Antonio and {Venuti}, Laura and {Wyatt}, Samuel and {Yu}, Weixiang and {Zabludoff}, Ann},
 bibtex_show = {true},
 custom_keywords = {white},
 doi = {10.48550/arXiv.2208.02781},
 eid = {arXiv:2208.02781},
 eprint = {2208.02781},
 journal = {arXiv e-prints},
 keywords = {Astrophysics - Instrumentation and Methods for Astrophysics},
 month = {August},
 pages = {arXiv:2208.02781},
 primaryclass = {astro-ph.IM},
 title = {{From Data to Software to Science with the Rubin Observatory LSST}},
 year = {2022}
}

@inproceedings{2022SPIE12189E..0MG,
 abstract = {{The Vera C. Rubin Observatory will advance many areas of astronomy over
the next decade with its unique widefast- deep multi-color
imaging survey, the Legacy Survey of Space and Time (LSST).1 The
LSST will produce approximately 20TB of raw data per night,
which will be automatically processed by the LSST Science
Pipelines to generate science-ready data products - processed
images, catalogs and alerts. To ensure that these data products
enable transformative science with LSST, stringent requirements
have been placed on their quality and scientific fidelity, for
example on image quality and depth, astrometric and photometric
performance, and object recovery completeness. In this paper we
introduce faro, a framework for automatically and efficiently
computing scientific performance metrics on the LSST data
products for units of data of varying granularity, ranging from
single-detector to full-survey summary statistics. By measuring
and monitoring metrics, we are able to evaluate trends in
algorithmic performance and conduct regression testing during
development, compare the performance of one algorithm against
another, and verify that the LSST data products will meet
performance requirements by comparing to specifications. We
present initial results using faro to characterize the
performance of the data products produced on simulated and
precursor data sets, and discuss plans to use faro to verify the
performance of the LSST commissioning data products.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2022SPIE12189E..0MG},
 archiveprefix = {arXiv},
 arxiv = {2206.15447},
 author = {{Guy}, Leanne P. and {Bechtol}, Keith and {Carlin}, Jeffrey L. and {Dennihy}, Erik and {Ferguson}, Peter S. and {Krughoff}, K. Simon and {Lupton}, Robert H. and {Slater}, Colin T. and {Findeisen}, Krzysztof and {Kannawadi}, Arun and {Kelvin}, Lee S. and {Lust}, Nate B. and {MacArthur}, Lauren A. and {Martinez}, Michael N. and {Reed}, Sophie L. and {Taranu}, Dan S. and {Wood-Vasey}, W. Michael},
 bibtex_show = {true},
 booktitle = {Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series},
 custom_keywords = {major},
 doi = {10.1117/12.2628887},
 eid = {121890M},
 eprint = {2206.15447},
 keywords = {Astrophysics - Instrumentation and Methods for Astrophysics},
 month = {August},
 pages = {121890M},
 primaryclass = {astro-ph.IM},
 series = {Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series},
 title = {{Faro: a framework for measuring the scientific performance of petascale Rubin Observatory data products}},
 volume = {12189},
 year = {2022}
}

@article{2022A&A...664A.170V,
 abbr = {A&A},
 abstract = {{We present a cosmic shear analysis with an improved redshift calibration
for the fourth data release of the Kilo-Degree Survey
(KiDS-1000) using self-organising maps (SOMs). Compared to the
previous analysis of the KiDS-1000 data, we expand the redshift
calibration sample to more than twice its size, now consisting
of data of 17 spectroscopic redshift campaigns, and
significantly extending the fraction of KiDS galaxies we are
able to calibrate with our SOM redshift methodology. We then
enhanced the calibration sample with precision photometric
redshifts from COSMOS2015 and the Physics of the Accelerated
Universe Survey (PAUS), allowing us to fill gaps in the
spectroscopic coverage of the KiDS data. Finally we performed a
Complete Orthogonal Sets of E/B-Integrals (COSEBIs) cosmic shear
analysis of the newly calibrated KiDS sample. We found S$_{8}$ =
0.748$_{{\ensuremath{-}}0.025}$$^{+0.021}$, which is in good
agreement with previous KiDS studies and increases the tension
with measurements of the cosmic microwave background to
3.4{\ensuremath{\sigma}}. We repeated the redshift calibration
with different subsets of the full calibration sample and
obtained, in all cases, agreement within at most
0.5{\ensuremath{\sigma}} in S$_{8}$ compared to our fiducial
analysis. Including additional photometric redshifts allowed us
to calibrate an additional 6\% of the source galaxy sample. Even
though further systematic testing with simulated data is
necessary to quantify the impact of redshift outliers, precision
photometric redshifts can be beneficial at high redshifts and to
mitigate selection effects commonly found in spectroscopically
selected calibration samples.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2022A&A...664A.170V},
 altmetric = {125994512},
 archiveprefix = {arXiv},
 arxiv = {2204.02396},
 author = {{van den Busch}, J.~L. and {Wright}, A.~H. and {Hildebrandt}, H. and {Bilicki}, M. and {Asgari}, M. and {Joudaki}, S. and {Blake}, C. and {Heymans}, C. and {Kannawadi}, A. and {Shan}, H.~Y. and {Tr{\"o}ster}, T.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202142083},
 eid = {A170},
 eprint = {2204.02396},
 journal = {Astronomy and Astrophysics},
 keywords = {cosmology: observations, gravitational lensing: weak, galaxies: distances and redshifts, surveys, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {August},
 pages = {A170},
 primaryclass = {astro-ph.CO},
 title = {{KiDS-1000: Cosmic shear with enhanced redshift calibration}},
 volume = {664},
 year = {2022}
}

@article{2022PASJ...74..421L,
 abbr = {PASJ},
 abstract = {{We present the galaxy shear catalog that will be used for the three-year
cosmological weak gravitational lensing analyses using data from
the Wide layer of the Hyper Suprime-Cam (HSC) Subaru Strategic
Program (SSP) Survey. The galaxy shapes are measured from the
i-band imaging data acquired from 2014 to 2019 and calibrated
with image simulations that resemble the observing conditions of
the survey based on training galaxy images from the Hubble Space
Telescope in the COSMOS region. The catalog covers an area of
433.48 deg$^{2}$ of the northern sky, split into six fields. The
mean i-band seeing is ${0{^{\prime \prime}_{.}}59}$. With
conservative galaxy selection criteria (e.g., i-band magnitude
brighter than 24.5), the observed raw galaxy number density is
22.9 arcmin$^{-2}$, and the effective galaxy number density is
19.9 arcmin$^{-2}$. The calibration removes the galaxy property-
dependent shear estimation bias to the level
|{\ensuremath{\delta}}m| < 9 {\texttimes} 10$^{-3}$. The bias
residual {\ensuremath{\delta}}m shows no dependence on redshift
in the range 0 < z {\ensuremath{\leq}} 3. We define the
requirements for cosmological weak-lensing science for this
shear catalog, and quantify potential systematics in the catalog
using a series of internal null tests for systematics related to
point-spread function modelling and shear estimation. A variety
of the null tests are statistically consistent with zero or
within requirements, but (i) there is evidence for PSF model
shape residual correlations; and (ii) star-galaxy shape
correlations reveal additive systematics. Both effects become
significant on >1{\textdegree} scales and will require
mitigation during the inference of cosmological parameters using
cosmic shear measurements.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2022PASJ...74..421L},
 altmetric = {108532937},
 archiveprefix = {arXiv},
 arxiv = {2107.00136},
 author = {{Li}, Xiangchong and {Miyatake}, Hironao and {Luo}, Wentao and {More}, Surhud and {Oguri}, Masamune and {Hamana}, Takashi and {Mandelbaum}, Rachel and {Shirasaki}, Masato and {Takada}, Masahiro and {Armstrong}, Robert and {Kannawadi}, Arun and {Takita}, Satoshi and {Miyazaki}, Satoshi and {Nishizawa}, Atsushi J. and {Plazas Malagon}, Andres A. and {Strauss}, Michael A. and {Tanaka}, Masayuki and {Yoshida}, Naoki},
 bibtex_show = {true},
 doi = {10.1093/pasj/psac006},
 eprint = {2107.00136},
 journal = {Publications of the ASJ},
 keywords = {catalogs, cosmology: miscellaneous, gravitational lensing: weak, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {April},
 number = {2},
 pages = {421-459},
 primaryclass = {astro-ph.CO},
 title = {{The three-year shear catalog of the Subaru Hyper Suprime-Cam SSP Survey}},
 volume = {74},
 year = {2022}
}

@article{2022A&A...660A..27T,
 abbr = {A&A},
 abstract = {{We conduct a pseudo-C$_{{\ensuremath{\ell}}}$ analysis of the
tomographic cross-correlation between 1000 deg$^{2}$ of weak-
lensing data from the Kilo-Degree Survey (KiDS-1000) and the
thermal Sunyaev-Zeldovich (tSZ) effect measured by Planck and
the Atacama Cosmology Telescope (ACT). Using HMX, a halo-model-
based approach that consistently models the gas, star, and dark
matter components, we are able to derive constraints on both
cosmology and baryon feedback for the first time from these
data, marginalising over redshift uncertainties, intrinsic
alignment of galaxies, and contamination by the cosmic infrared
background (CIB). We find our results to be insensitive to the
CIB, while intrinsic alignment provides a small but significant
contribution to the lensing-tSZ cross-correlation. The
cosmological constraints are consistent with those of other low-
redshift probes and prefer strong baryon feedback. The inferred
amplitude of the lensing-tSZ cross-correlation signal, which
scales as {\ensuremath{\sigma}}$_{8}$({\ensuremath{\Omega}}$_{m}
$/0.3)$^{0.2}$, is low by {\ensuremath{\sim}}2
{\ensuremath{\sigma}} compared to the primary cosmic microwave
background constraints by Planck. The lensing-tSZ measurements
are then combined with pseudo-C$_{{\ensuremath{\ell}}}$
measurements of KiDS-1000 cosmic shear into a novel joint
analysis, accounting for the full cross-covariance between the
probes, providing tight cosmological constraints by breaking
parameter degeneracies inherent to both probes. The joint
analysis gives an improvement of 40\% on the constraint of
S$_{8}$ =
{\ensuremath{\sigma}}$_{8}${\ensuremath{\Omega}}$_{m}$/0.3 over
cosmic shear alone, while providing constraints on baryon
feedback consistent with hydrodynamical simulations,
demonstrating the potential of such joint analyses with baryonic
tracers such as the tSZ effect. We discuss remaining modelling
challenges that need to be addressed if these baryonic probes
are to be included in future precision-cosmology analyses.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2022A&A...660A..27T},
 altmetric = {113196745},
 archiveprefix = {arXiv},
 arxiv = {2109.04458},
 author = {{Tr{\"o}ster}, Tilman and {Mead}, Alexander J. and {Heymans}, Catherine and {Yan}, Ziang and {Alonso}, David and {Asgari}, Marika and {Bilicki}, Maciej and {Dvornik}, Andrej and {Hildebrandt}, Hendrik and {Joachimi}, Benjamin and {Kannawadi}, Arun and {Kuijken}, Konrad and {Schneider}, Peter and {Shan}, Huan Yuan and {van Waerbeke}, Ludovic and {Wright}, Angus H.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202142197},
 eid = {A27},
 eprint = {2109.04458},
 journal = {Astronomy and Astrophysics},
 keywords = {cosmology: observations, cosmological parameters, large-scale structure of Universe, gravitational lensing: weak, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {April},
 pages = {A27},
 primaryclass = {astro-ph.CO},
 title = {{Joint constraints on cosmology and the impact of baryon feedback: Combining KiDS-1000 lensing with the thermal Sunyaev-Zeldovich effect from Planck and ACT}},
 volume = {660},
 year = {2022}
}

@article{2022MNRAS.510.6150L,
 abbr = {MNRAS},
 abstract = {{Lensing without borders is a cross-survey collaboration created to
assess the consistency of galaxy-galaxy lensing signals
({\ensuremath{\Delta}}{\ensuremath{\Sigma}}) across different
data sets and to carry out end-to-end tests of systematic
errors. We perform a blind comparison of the amplitude of
{\ensuremath{\Delta}}{\ensuremath{\Sigma}} using lens samples
from BOSS and six independent lensing surveys. We find good
agreement between empirically estimated and reported systematic
errors which agree to better than 2.3{\ensuremath{\sigma}} in
four lens bins and three radial ranges. For lenses with z$_{L}$
> 0.43 and considering statistical errors, we detect a
3-4{\ensuremath{\sigma}} correlation between lensing amplitude
and survey depth. This correlation could arise from the
increasing impact at higher redshift of unrecognized galaxy
blends on shear calibration and imperfections in photometric
redshift calibration. At z$_{L}$ > 0.54, amplitudes may
additionally correlate with foreground stellar density. The
amplitude of these trends is within survey-defined systematic
error budgets that are designed to include known shear and
redshift calibration uncertainty. Using a fully empirical and
conservative method, we do not find evidence for large unknown
systematics. Systematic errors greater than 15 per cent (25 per
cent) ruled out in three lens bins at 68 per cent (95 per cent)
confidence at z < 0.54. Differences with respect to predictions
based on clustering are observed to be at the 20-30 per cent
level. Our results therefore suggest that lensing systematics
alone are unlikely to fully explain the 'lensing is low' effect
at z < 0.54. This analysis demonstrates the power of cross-
survey comparisons and provides a promising path for identifying
and reducing systematics in future lensing analyses.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2022MNRAS.510.6150L},
 altmetric = {117834433},
 archiveprefix = {arXiv},
 arxiv = {2111.13805},
 author = {{Leauthaud}, A. and {Amon}, A. and {Singh}, S. and {Gruen}, D. and {Lange}, J.~U. and {Huang}, S. and {Robertson}, N.~C. and {Varga}, T.~N. and {Luo}, Y. and {Heymans}, C. and {Hildebrandt}, H. and {Blake}, C. and {Aguena}, M. and {Allam}, S. and {Andrade-Oliveira}, F. and {Annis}, J. and {Bertin}, E. and {Bhargava}, S. and {Blazek}, J. and {Bridle}, S.~L. and {Brooks}, D. and {Burke}, D.~L. and {Rosell}, A. Carnero and {Carrasco Kind}, M. and {Carretero}, J. and {Castander}, F.~J. and {Cawthon}, R. and {Choi}, A. and {Costanzi}, M. and {da Costa}, L.~N. and {Pereira}, M.~E.~S. and {Davis}, C. and {De Vicente}, J. and {DeRose}, J. and {Diehl}, H.~T. and {Dietrich}, J.~P. and {Doel}, P. and {Eckert}, K. and {Everett}, S. and {Evrard}, A.~E. and {Ferrero}, I. and {Flaugher}, B. and {Fosalba}, P. and {Garc{\'\i}a-Bellido}, J. and {Gatti}, M. and {Gaztanaga}, E. and {Gruendl}, R.~A. and {Gschwend}, J. and {Hartley}, W.~G. and {Hollowood}, D.~L. and {Honscheid}, K. and {Jain}, B. and {James}, D.~J. and {Jarvis}, M. and {Joachimi}, B. and {Kannawadi}, A. and {Kim}, A.~G. and {Krause}, E. and {Kuehn}, K. and {Kuijken}, K. and {Kuropatkin}, N. and {Lima}, M. and {MacCrann}, N. and {Maia}, M.~A.~G. and {Makler}, M. and {March}, M. and {Marshall}, J.~L. and {Melchior}, P. and {Menanteau}, F. and {Miquel}, R. and {Miyatake}, H. and {Mohr}, J.~J. and {Moraes}, B. and {More}, S. and {Surhud}, M. and {Morgan}, R. and {Myles}, J. and {Ogando}, R.~L.~C. and {Palmese}, A. and {Paz-Chinch{\'o}n}, F. and {Malag{\'o}n}, A.~A. Plazas and {Prat}, J. and {Rau}, M.~M. and {Rhodes}, J. and {Rodriguez-Monroy}, M. and {Roodman}, A. and {Ross}, A.~J. and {Samuroff}, S. and {S{\'a}nchez}, C. and {Sanchez}, E. and {Scarpine}, V. and {Schlegel}, D.~J. and {Schubnell}, M. and {Serrano}, S. and {Sevilla-Noarbe}, I. and {Sif{\'o}n}, C. and {Smith}, M. and {Speagle}, J.~S. and {Suchyta}, E. and {Tarle}, G. and {Thomas}, D. and {Tinker}, J. and {To}, C. and {Troxel}, M.~A. and {Van Waerbeke}, L. and {Vielzeuf}, P. and {Wright}, A.~H.},
 bibtex_show = {true},
 doi = {10.1093/mnras/stab3586},
 eprint = {2111.13805},
 journal = {Monthly Notices of the Royal Astronomical Society},
 keywords = {cosmology: observations, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {March},
 number = {4},
 pages = {6150-6189},
 primaryclass = {astro-ph.CO},
 title = {{Lensing without borders - I. A blind comparison of the amplitude of galaxy-galaxy lensing between independent imaging surveys}},
 volume = {510},
 year = {2022}
}

@article{2021A&A...655A..11R,
 abbr = {A&A},
 abstract = {{We carry out a multi-probe self-consistency test of the flat Lambda Cold
Dark Matter ({\ensuremath{\Lambda}}CDM) model with the aim of
exploring potential causes of the reported tensions between
high- and low-redshift cosmological observations. We divide the
model into two theory regimes determined by the smooth
background (geometry) and the evolution of matter density
fluctuations (growth), each governed by an independent set of
{\ensuremath{\Lambda}}CDM cosmological parameters. This extended
model is constrained by a combination of weak gravitational
lensing measurements from the Kilo-Degree Survey, galaxy
clustering signatures extracted from Sloan Digital Sky Survey
campaigns and the Six-Degree Field Galaxy Survey, and the
angular baryon acoustic scale and the primordial scalar
fluctuation power spectrum measured in Planck cosmic microwave
background (CMB) data. For both the weak lensing data set
individually and the combined probes, we find strong consistency
between the geometry and growth parameters, as well as with the
posterior of standard {\ensuremath{\Lambda}}CDM analysis. In the
non-split analysis, for which one single set of parameters was
used, tension in the amplitude of matter density fluctuations as
measured by the parameter S$_{8}$ persists at around
3{\ensuremath{\sigma}}, with a 1.5\% constraint of S$_{8}$ =
0.776$_{{\ensuremath{-}}0.008}$$^{+0.016}$ for the combined
probes. We also observe a less significant preference (at least
2{\ensuremath{\sigma}}) for higher values of the Hubble
constant, H$_{0}$ = 70.5$_{{\ensuremath{-}}1.5}$$^{+0.7}$ km
s$^{{\ensuremath{-}}1}$ Mpc$^{{\ensuremath{-}}1}$, as well as
for lower values of the total matter density parameter
{\ensuremath{\Omega}}$_{m}$ =
0.289$_{{\ensuremath{-}}0.005}$$^{+0.007}$ compared to the full
Planck analysis. Including the subset of the CMB information in
the probe combination enhances these differences rather than
alleviate them, which we link to the discrepancy between low and
high multipoles in Planck data. Our geometry versus growth
analysis does not yet yield clear signs regarding whether the
origin of the discrepancies lies in {\ensuremath{\Lambda}}CDM
structure growth or expansion history but holds promise as an
insightful test for forthcoming, more powerful data.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...655A..11R},
 altmetric = {106190548},
 archiveprefix = {arXiv},
 arxiv = {2105.09545},
 author = {{Ruiz-Zapatero}, Jaime and {St{\"o}lzner}, Benjamin and {Joachimi}, Benjamin and {Asgari}, Marika and {Bilicki}, Maciej and {Dvornik}, Andrej and {Giblin}, Benjamin and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Kannawadi}, Arun and {Kuijken}, Konrad and {Tr{\"o}ster}, Tilman and {van den Busch}, Jan Luca and {Wright}, Angus H.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202141350},
 eid = {A11},
 eprint = {2105.09545},
 journal = {Astronomy and Astrophysics},
 keywords = {cosmological parameters, methods: data analysis, cosmology: theory, large-scale structure of Universe, gravitational lensing: weak, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {November},
 pages = {A11},
 primaryclass = {astro-ph.CO},
 title = {{Geometry versus growth. Internal consistency of the flat {\ensuremath{\Lambda}}CDM model with KiDS-1000}},
 volume = {655},
 year = {2021}
}

@article{2021A&A...654A..76F,
 abbr = {A&A},
 abstract = {{We constrain the luminosity and redshift dependence of the intrinsic
alignment (IA) of a nearly volume-limited sample of luminous red
galaxies selected from the fourth public data release of the
Kilo-Degree Survey (KiDS-1000). To measure the shapes of the
galaxies, we used two complementary algorithms, finding
consistent IA measurements for the overlapping galaxy sample.
The global significance of IA detection across our two
independent luminous red galaxy samples, with our favoured
method of shape estimation, is
{\ensuremath{\sim}}10.7{\ensuremath{\sigma}}. We find no
significant dependence with redshift of the IA signal in the
range 0.2 < z < 0.8, nor a dependence with luminosity below
L$_{r}$ {\ensuremath{\lesssim}} 2.9 {\texttimes} {}10$^{10}$
h$^{{\ensuremath{-}}2}$L$_{r, {\ensuremath{\odot}}}$. Above this
luminosity, however, we find that the IA signal increases as a
power law, although our results are also compatible with linear
growth within the current uncertainties. This behaviour
motivates the use of a broken power law model when accounting
for the luminosity dependence of IA contamination in cosmic
shear studies.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...654A..76F},
 altmetric = {113004148},
 archiveprefix = {arXiv},
 arxiv = {2109.02556},
 author = {{Fortuna}, Maria Cristina and {Hoekstra}, Henk and {Johnston}, Harry and {Vakili}, Mohammadjavad and {Kannawadi}, Arun and {Georgiou}, Christos and {Joachimi}, Benjamin and {Wright}, Angus H. and {Asgari}, Marika and {Bilicki}, Maciej and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Kuijken}, Konrad and {Von Wietersheim-Kramsta}, Maximilian},
 bibtex_show = {true},
 custom_keywords = {major},
 doi = {10.1051/0004-6361/202140706},
 eid = {A76},
 eprint = {2109.02556},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, cosmology: observations, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies},
 month = {October},
 pages = {A76},
 primaryclass = {astro-ph.CO},
 title = {{KiDS-1000: Constraints on the intrinsic alignment of luminous red galaxies}},
 volume = {654},
 year = {2021}
}

@article{2021A&A...653A..82B,
 abbr = {A&A},
 abstract = {{We present a bright galaxy sample with accurate and precise photometric
redshifts (photo-zs), selected using ugriZYJHK$_{s}$ photometry
from the Kilo-Degree Survey (KiDS) Data Release 4. The highly
pure and complete dataset is flux-limited at r < 20 mag, covers
{\ensuremath{\sim}}1000 deg$^{2}$, and contains about 1 million
galaxies after artifact masking. We exploit the overlap with
Galaxy And Mass Assembly spectroscopy as calibration to
determine photo-zs with the supervised machine learning neural
network algorithm implemented in the ANNz2 software. The photo-
zs have a mean error of
|⟨{\ensuremath{\delta}}z⟩|{\ensuremath{\sim}}5 {\texttimes}
10$^{{\ensuremath{-}}4}$ and low scatter (scaled mean absolute
deviation of {\ensuremath{\sim}}0.018(1 + z)); they are both
practically independent of the r-band magnitude and photo-z at
0.05 < z$_{phot}$ < 0.5. Combined with the 9-band photometry,
these allow us to estimate robust absolute magnitudes and
stellar masses for the full sample. As a demonstration of the
usefulness of these data, we split the dataset into red and blue
galaxies, used them as lenses, and measured the weak
gravitational lensing signal around them for five stellar mass
bins. We fit a halo model to these high-precision measurements
to constrain the stellar-mass-halo-mass relations for blue and
red galaxies. We find that for high stellar mass
(M$_{{\ensuremath{\star}}}$ > 5 {\texttimes} {}10$^{11}$
M$_{{\ensuremath{\odot}}}$), the red galaxies occupy dark matter
halos that are much more massive than those occupied by blue
galaxies with the same stellar mass.
\textbackslash\textbackslashData available from <A href=``http:/
/kids.strw.leidenuniv.nl/DR4/brightsample.php''>http://kids.strw
.leidenuniv.nl/DR4/brightsample.php</A>}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...653A..82B},
 altmetric = {97884590},
 archiveprefix = {arXiv},
 arxiv = {2101.06010},
 author = {{Bilicki}, M. and {Dvornik}, A. and {Hoekstra}, H. and {Wright}, A.~H. and {Chisari}, N.~E. and {Vakili}, M. and {Asgari}, M. and {Giblin}, B. and {Heymans}, C. and {Hildebrandt}, H. and {Holwerda}, B.~W. and {Hopkins}, A. and {Johnston}, H. and {Kannawadi}, A. and {Kuijken}, K. and {Nakoneczny}, S.~J. and {Shan}, H.~Y. and {Sonnenfeld}, A. and {Valentijn}, E.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202140352},
 eid = {A82},
 eprint = {2101.06010},
 journal = {Astronomy and Astrophysics},
 keywords = {galaxies: distances and redshifts, catalogs, large-scale structure of Universe, gravitational lensing: weak, methods: data analysis, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics},
 month = {September},
 pages = {A82},
 primaryclass = {astro-ph.GA},
 title = {{Bright galaxy sample in the Kilo-Degree Survey Data Release 4. Selection, photometric redshifts, and physical properties}},
 volume = {653},
 year = {2021}
}

@article{2021A&A...651A..76Y,
 abbr = {A&A},
 abstract = {{We constrain the redshift dependence of gas pressure bias
⟨b$_{y}$P$_{e}$⟩ (bias-weighted average electron pressure),
which characterises the thermodynamics of intergalactic gas,
through a combination of cross-correlations between galaxy
positions and the thermal Sunyaev-Zeldovich (tSZ) effect, as
well as galaxy positions and the gravitational lensing of the
cosmic microwave background (CMB). The galaxy sample is from the
fourth data release of the Kilo-Degree Survey (KiDS). The tSZ y
map and the CMB lensing map are from the Planck 2015 and 2018
data releases, respectively. The measurements are performed in
five redshift bins with z {\ensuremath{\lesssim}} 1. With these
measurements, combining galaxy-tSZ and galaxy-CMB lensing cross-
correlations allows us to break the degeneracy between galaxy
bias and gas pressure bias, and hence constrain them
simultaneously. In all redshift bins, the best-fit values of
⟨b$_{y}$P$_{e}$⟩ are at a level of {\ensuremath{\sim}}0.3 meV
cm$^{{\ensuremath{-}}3}$ and increase slightly with redshift.
The galaxy bias is consistent with unity in all the redshift
bins. Our results are not sensitive to the non-linear details of
the cross-correlation, which are smoothed out by the Planck
beam. Our measurements are in agreement with previous
measurements as well as with theoretical predictions. We also
show that our conclusions are not changed when CMB lensing is
replaced by galaxy lensing, which shows the consistency of the
two lensing signals despite their radically different redshift
ranges. This study demonstrates the feasibility of using CMB
lensing to calibrate the galaxy distribution such that the
galaxy distribution can be used as a mass proxy without relying
on the precise knowledge of the matter distribution.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...651A..76Y},
 altmetric = {100224097},
 archiveprefix = {arXiv},
 arxiv = {2102.07701},
 author = {{Yan}, Ziang and {van Waerbeke}, Ludovic and {Tr{\"o}ster}, Tilman and {Wright}, Angus H. and {Alonso}, David and {Asgari}, Marika and {Bilicki}, Maciej and {Erben}, Thomas and {Gu}, Shiming and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Hinshaw}, Gary and {Koukoufilippas}, Nick and {Kannawadi}, Arun and {Kuijken}, Konrad and {Mead}, Alexander and {Shan}, HuanYuan},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202140568},
 eid = {A76},
 eprint = {2102.07701},
 journal = {Astronomy and Astrophysics},
 keywords = {large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {July},
 pages = {A76},
 primaryclass = {astro-ph.CO},
 title = {{Probing galaxy bias and intergalactic gas pressure with KiDS Galaxies-tSZ-CMB lensing cross-correlations}},
 volume = {651},
 year = {2021}
}

@article{2021A&A...650A.113B,
 abbr = {A&A},
 abstract = {{We present measurements of the radial gravitational acceleration around
isolated galaxies, comparing the expected gravitational
acceleration given the baryonic matter (g$_{bar}$) with the
observed gravitational acceleration (g$_{obs}$), using weak
lensing measurements from the fourth data release of the Kilo-
Degree Survey (KiDS-1000). These measurements extend the radial
acceleration relation (RAR), traditionally measured using galaxy
rotation curves, by 2 decades in g$_{obs}$ into the low-
acceleration regime beyond the outskirts of the observable
galaxy. We compare our RAR measurements to the predictions of
two modified gravity (MG) theories: modified Newtonian dynamics
and Verlinde's emergent gravity (EG). We find that the measured
relation between g$_{obs}$ and g$_{bar}$ agrees well with the MG
predictions. In addition, we find a difference of at least
6{\ensuremath{\sigma}} between the RARs of early- and late-type
galaxies (split by S{\'e}rsic index and u {\ensuremath{-}} r
colour) with the same stellar mass. Current MG theories involve
a gravity modification that is independent of other galaxy
properties, which would be unable to explain this behaviour,
although the EG theory is still limited to spherically symmetric
static mass models. The difference might be explained if only
the early-type galaxies have significant (M$_{gas}$
{\ensuremath{\approx}} M$_{{\ensuremath{\star}}}$)
circumgalactic gaseous haloes. The observed behaviour is also
expected in {\ensuremath{\Lambda}}-cold dark matter
({\ensuremath{\Lambda}}CDM) models where the galaxy-to-halo mass
relation depends on the galaxy formation history. We find that
MICE, a {\ensuremath{\Lambda}}CDM simulation with hybrid halo
occupation distribution modelling and abundance matching,
reproduces the observed RAR but significantly differs from
BAHAMAS, a hydrodynamical cosmological galaxy formation
simulation. Our results are sensitive to the amount of
circumgalactic gas; current observational constraints indicate
that the resulting corrections are likely moderate. Measurements
of the lensing RAR with future cosmological surveys (such as
Euclid) will be able to further distinguish between MG and
{\ensuremath{\Lambda}}CDM models if systematic uncertainties in
the baryonic mass distribution around galaxies are reduced.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...650A.113B},
 altmetric = {108008835},
 archiveprefix = {arXiv},
 arxiv = {2106.11677},
 author = {{Brouwer}, Margot M. and {Oman}, Kyle A. and {Valentijn}, Edwin A. and {Bilicki}, Maciej and {Heymans}, Catherine and {Hoekstra}, Henk and {Napolitano}, Nicola R. and {Roy}, Nivya and {Tortora}, Crescenzo and {Wright}, Angus H. and {Asgari}, Marika and {van den Busch}, Jan Luca and {Dvornik}, Andrej and {Erben}, Thomas and {Giblin}, Benjamin and {Graham}, Alister W. and {Hildebrandt}, Hendrik and {Hopkins}, Andrew M. and {Kannawadi}, Arun and {Kuijken}, Konrad and {Liske}, Jochen and {Shan}, HuanYuan and {Tr{\"o}ster}, Tilman and {Verlinde}, Erik and {Visser}, Manus},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202040108},
 eid = {A113},
 eprint = {2106.11677},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, methods: statistical, surveys, galaxies: halos, dark matter, cosmology: theory, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology, High Energy Physics - Theory},
 month = {June},
 pages = {A113},
 primaryclass = {astro-ph.GA},
 title = {{The weak lensing radial acceleration relation: Constraining modified gravity and cold dark matter theories with KiDS-1000}},
 volume = {650},
 year = {2021}
}

@article{2021A&A...649A.146R,
 abbr = {A&A},
 abstract = {{We measured the cross-correlation between galaxy weak lensing data from
the Kilo Degree Survey (KiDS-1000, DR4) and cosmic microwave
background (CMB) lensing data from the Atacama Cosmology
Telescope (ACT, DR4) and the Planck Legacy survey. We used two
samples of source galaxies, selected with photometric redshifts,
(0.1 < z$_{B}$ < 1.2) and (1.2 < z$_{B}$ < 2), which produce a
combined detection significance of the CMB lensing and weak
galaxy lensing cross-spectrum of 7.7{\ensuremath{\sigma}}. With
the lower redshift galaxy sample, for which the cross-
correlation was detected at a significance of
5.3{\ensuremath{\sigma}}, we present joint cosmological
constraints on the matter density parameter,
{\ensuremath{\Omega}}$_{m}$, and the matter fluctuation
amplitude parameter, {\ensuremath{\sigma}}$_{8}$, marginalising
over three nuisance parameters that model our uncertainty in the
redshift and shear calibration as well as the intrinsic
alignment of galaxies. We find our measurement to be consistent
with the best-fitting flat {\ensuremath{\Lambda}}CDM
cosmological models from both Planck and KiDS-1000. We
demonstrate the capacity of CMB weak lensing cross-correlations
to set constraints on either the redshift or shear calibration
by analysing a previously unused high-redshift KiDS galaxy
sample (1.2 < z$_{B}$ < 2), with the cross-correlation detected
at a significance of 7{\ensuremath{\sigma}}. This analysis
provides an independent assessment for the accuracy of redshift
measurements in a regime that is challenging to calibrate
directly owing to known incompleteness in spectroscopic surveys.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...649A.146R},
 altmetric = {94822852},
 archiveprefix = {arXiv},
 arxiv = {2011.11613},
 author = {{Robertson}, Naomi Clare and {Alonso}, David and {Harnois-D{\'e}raps}, Joachim and {Darwish}, Omar and {Kannawadi}, Arun and {Amon}, Alexandra and {Asgari}, Marika and {Bilicki}, Maciej and {Calabrese}, Erminia and {Choi}, Steve K. and {Devlin}, Mark J. and {Dunkley}, Jo and {Dvornik}, Andrej and {Erben}, Thomas and {Ferraro}, Simone and {Fortuna}, Maria Cristina and {Giblin}, Benjamin and {Han}, Dongwon and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Hill}, J. Colin and {Hilton}, Matt and {Ho}, Shuay-Pwu P. and {Hoekstra}, Henk and {Hubmayr}, Johannes and {Hughes}, John P. and {Joachimi}, Benjamin and {Joudaki}, Shahab and {Knowles}, Kenda and {Kuijken}, Konrad and {Madhavacheril}, Mathew S. and {Moodley}, Kavilan and {Miller}, Lance and {Namikawa}, Toshiya and {Nati}, Federico and {Niemack}, Michael D. and {Page}, Lyman A. and {Partridge}, Bruce and {Schaan}, Emmanuel and {Schillaci}, Alessandro and {Schneider}, Peter and {Sehgal}, Neelima and {Sherwin}, Blake D. and {Sif{\'o}n}, Crist{\'o}bal and {Staggs}, Suzanne T. and {Tr{\"o}ster}, Tilman and {van Engelen}, Alexander and {Valentijn}, Edwin and {Wollack}, Edward J. and {Wright}, Angus H. and {Xu}, Zhilei},
 bibtex_show = {true},
 custom_keywords = {major},
 doi = {10.1051/0004-6361/202039975},
 eid = {A146},
 eprint = {2011.11613},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, large-scale structure of Universe, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {May},
 pages = {A146},
 primaryclass = {astro-ph.CO},
 title = {{Strong detection of the CMB lensing and galaxy weak lensing cross-correlation from ACT-DR4, Planck Legacy, and KiDS-1000}},
 volume = {649},
 year = {2021}
}

@article{2021A&A...649A..88T,
 abbr = {A&A},
 abstract = {{We present constraints on extensions to the standard cosmological model
of a spatially flat Universe governed by general relativity, a
cosmological constant ({\ensuremath{\Lambda}}), and cold dark
matter (CDM) by varying the spatial curvature
{\ensuremath{\Omega}}$_{K}$, the sum of the neutrino masses
{\ensuremath{\sum}}m$_{{\ensuremath{\nu}}}$, the dark energy
equation of state parameter w, and the Hu-Sawicki f(R) gravity
f$_{R0}$ parameter. With the combined 3 {\texttimes} 2 pt
measurements of cosmic shear from the Kilo-Degree Survey
(KiDS-1000), galaxy clustering from the Baryon Oscillation
Spectroscopic Survey (BOSS), and galaxy-galaxy lensing from the
overlap between KiDS-1000, BOSS, and the spectroscopic 2-degree
Field Lensing Survey, we find results that are fully consistent
with a flat {\ensuremath{\Lambda}}CDM model with
{\ensuremath{\Omega}}$_{K}$ =
0.011$_{{\ensuremath{-}}0.057}$$^{+0.054}$,
{\ensuremath{\sum}}m$_{{\ensuremath{\nu}}}$ < 1.76 eV (95\% CL),
and w = {\ensuremath{-}}0.99$_{{\ensuremath{-}}0.13}$$^{+0.11}$.
The f$_{R0}$ parameter is unconstrained in our fully non-linear
f(R) cosmic shear analysis. Considering three different model
selection criteria, we find no clear preference for either the
fiducial flat {\ensuremath{\Lambda}}CDM model or any of the
considered extensions. In addition to extensions to the flat
{\ensuremath{\Lambda}}CDM parameter space, we also explore
restrictions to common subsets of the flat
{\ensuremath{\Lambda}}CDM parameter space by fixing the
amplitude of the primordial power spectrum to the Planck best-
fit value, as well as adding external data from supernovae and
lensing of the cosmic microwave background (CMB). Neither the
beyond-{\ensuremath{\Lambda}}CDM models nor the imposed
restrictions explored in this analysis are able to resolve the
{\ensuremath{\sim}}3{\ensuremath{\sigma}} tension in S$_{8}$
between the 3 {\texttimes} 2 pt constraints and the Planck
temperature and polarisation data, with the exception of wCDM,
where the S$_{8}$ tension is resolved. The tension in the wCDM
case persists, however, when considering the joint S$_{8}$
{\ensuremath{-}} w parameter space. The joint flat
{\ensuremath{\Lambda}}CDM CMB lensing and 3 {\texttimes} 2 pt
analysis is found to yield tight constraints on
{\ensuremath{\Omega}}$_{m}$ =
0.307$_{{\ensuremath{-}}0.013}$$^{+0.008}$,
{\ensuremath{\sigma}}$_{8}$ =
0.769$_{{\ensuremath{-}}0.010}$$^{+0.022}$, and S$_{8}$ =
0.779$_{{\ensuremath{-}}0.013}$$^{+0.013}$.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...649A..88T},
 altmetric = {93571849},
 archiveprefix = {arXiv},
 arxiv = {2010.16416},
 author = {{Tr{\"o}ster}, Tilman and {Asgari}, Marika and {Blake}, Chris and {Cataneo}, Matteo and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Joachimi}, Benjamin and {Lin}, Chieh-An and {S{\'a}nchez}, Ariel G. and {Wright}, Angus H. and {Bilicki}, Maciej and {Bose}, Benjamin and {Crocce}, Martin and {Dvornik}, Andrej and {Erben}, Thomas and {Giblin}, Benjamin and {Glazebrook}, Karl and {Hoekstra}, Henk and {Joudaki}, Shahab and {Kannawadi}, Arun and {K{\"o}hlinger}, Fabian and {Kuijken}, Konrad and {Lidman}, Chris and {Lombriser}, Lucas and {Mead}, Alexander and {Parkinson}, David and {Shan}, HuanYuan and {Wolf}, Christian and {Xia}, Qianli},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202039805},
 eid = {A88},
 eprint = {2010.16416},
 journal = {Astronomy and Astrophysics},
 keywords = {cosmology: observations, cosmological parameters, gravitational lensing: weak, large-scale structure of Universe, dark energy, methods: statistical, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {May},
 pages = {A88},
 primaryclass = {astro-ph.CO},
 title = {{KiDS-1000 Cosmology: Constraints beyond flat {\ensuremath{\Lambda}}CDM}},
 volume = {649},
 year = {2021}
}

@article{2021A&A...649A..81N,
 abbr = {A&A},
 abstract = {{We present a catalog of quasars with their corresponding redshifts
derived from the photometric Kilo-Degree Survey (KiDS) Data
Release 4. We achieved it by training machine learning (ML)
models, using optical ugri and near-infrared ZYJHK$_{s}$ bands,
on objects known from Sloan Digital Sky Survey (SDSS)
spectroscopy. We define inference subsets from the 45 million
objects of the KiDS photometric data limited to 9-band
detections, based on a feature space built from magnitudes and
their combinations. We show that projections of the high-
dimensional feature space on two dimensions can be successfully
used, instead of the standard color-color plots, to investigate
the photometric estimations, compare them with spectroscopic
data, and efficiently support the process of building a catalog.
The model selection and fine-tuning employs two subsets of
objects: those randomly selected and the faintest ones, which
allowed us to properly fit the bias versus variance trade-off.
We tested three ML models: random forest (RF), XGBoost (XGB),
and artificial neural network (ANN). We find that XGB is the
most robust and straightforward model for classification, while
ANN performs the best for combined classification and redshift.
The ANN inference results are tested using number counts, Gaia
parallaxes, and other quasar catalogs that are external to the
training set. Based on these tests, we derived the minimum
classification probability for quasar candidates which provides
the best purity versus completeness trade-off: p(QSO$_{cand}$) >
0.9 for r < 22 and p(QSO$_{cand}$) > 0.98 for 22 < r < 23.5. We
find 158 000 quasar candidates in the safe inference subset (r <
22) and an additional 185 000 candidates in the reliable
extrapolation regime (22 < r < 23.5). Test-data purity equals
97\% and completeness is 94\%; the latter drops by 3\% in the
extrapolation to data fainter by one magnitude than the training
set. The photometric redshifts were derived with ANN and modeled
with Gaussian uncertainties. The test-data redshift error (mean
and scatter) equals 0.009 {\ensuremath{\pm}} 0.12 in the safe
subset and {\ensuremath{-}}0.0004 {\ensuremath{\pm}} 0.19 in the
extrapolation, averaged over a redshift range of 0.14 < z < 3.63
(first and 99th percentiles). Our success of the extrapolation
challenges the way that models are optimized and applied at the
faint data end. The resulting catalog is ready for cosmology and
active galactic nucleus (AGN) studies.
\textbackslash\textbackslashA copy of the catalog is only
available at the CDS via anonymous ftp to <A
href=``http://cdsarc.u-strasbg.fr/''>cdsarc.u-strasbg.fr</A>
(ftp://130.79.128.5) or via <A
href=``http://cdsarc.u-strasbg.fr/viz-
bin/cat/J/A+A/649/A81''>http://cdsarc.u-strasbg.fr/viz-
bin/cat/J/A+A/649/A81</A> \textbackslash\textbackslashWe
publicly release the catalog at <A href=``https://kids.strw.leid
enuniv.nl/DR4/quasarcatalog.php''>https://kids.strw.leidenuniv.n
l/DR4/quasarcatalog.php</A> and the code at <A
href=``https://github.com/snakoneczny/kids-
quasars''>github.com/snakoneczny/kids-quasars</A>}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...649A..81N},
 altmetric = {93249875},
 archiveprefix = {arXiv},
 arxiv = {2010.13857},
 author = {{Nakoneczny}, S.~J. and {Bilicki}, M. and {Pollo}, A. and {Asgari}, M. and {Dvornik}, A. and {Erben}, T. and {Giblin}, B. and {Heymans}, C. and {Hildebrandt}, H. and {Kannawadi}, A. and {Kuijken}, K. and {Napolitano}, N.~R. and {Valentijn}, E.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202039684},
 eid = {A81},
 eprint = {2010.13857},
 journal = {Astronomy and Astrophysics},
 keywords = {methods: data analysis, methods: observational, catalogs, surveys, quasars: general, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {May},
 pages = {A81},
 primaryclass = {astro-ph.CO},
 title = {{Photometric selection and redshifts for quasars in the Kilo-Degree Survey Data Release 4}},
 volume = {649},
 year = {2021}
}

@article{2021MNRAS.502.4048K,
 abbr = {MNRAS},
 abstract = {{METACALIBRATION is a state-of-the-art technique for measuring weak
gravitational lensing shear from well-sampled galaxy images. We
investigate the accuracy of shear measured with METACALIBRATION
from fitting elliptical Gaussians to undersampled galaxy images.
In this case, METACALIBRATION introduces aliasing effects
leading to an ensemble multiplicative shear bias about 0.01 for
Euclid and even larger for the Roman Space Telescope, well
exceeding the missions' requirements. We find that this aliasing
bias can be mitigated by computing shapes from weighted moments
with wider Gaussians as weight functions, thereby trading bias
for a slight increase in variance of the measurements. We show
that this approach is robust to the point-spread function in
consideration and meets the stringent requirements of Euclid for
galaxies with moderate to high signal-to-noise ratios. We
therefore advocate METACALIBRATION as a viable shear measurement
option for weak lensing from upcoming space missions.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021MNRAS.502.4048K},
 altmetric = {92182062},
 archiveprefix = {arXiv},
 arxiv = {2010.04164},
 author = {{Kannawadi}, Arun and {Rosenberg}, Erik and {Hoekstra}, Henk},
 bibtex_show = {true},
 custom_keywords = {first},
 doi = {10.1093/mnras/stab211},
 eprint = {2010.04164},
 journal = {Monthly Notices of the Royal Astronomical Society},
 keywords = {gravitational lensing: weak, methods: observational, cosmology: observations, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {April},
 number = {3},
 pages = {4048-4063},
 primaryclass = {astro-ph.IM},
 selected = {true},
 title = {{Mitigating the effects of undersampling in weak lensing shear estimation with metacalibration}},
 volume = {502},
 year = {2021}
}

@article{2021A&A...647A.185G,
 abbr = {A&A},
 abstract = {{We present measurements of f$_{h}$, the ratio of the aligned components
of the projected halo and galaxy ellipticities, for a sample of
central galaxies using weak gravitational lensing data from the
Kilo-Degree Survey (KiDS). Using a lens galaxy shape estimation
that is more sensitive to outer galaxy regions, we find f$_{h}$
= 0.50 {\ensuremath{\pm}} 0.20 for our full sample and f$_{h}$ =
0.55 {\ensuremath{\pm}} 0.19 for an intrinsically red sub-sample
(that therefore has a higher stellar mass), rejecting the
hypothesis that round halos and/or galaxies are not aligned with
their parent halo at 2.5{\ensuremath{\sigma}} and
2.9{\ensuremath{\sigma}}, respectively. We quantify the 93.4\%
purity of our central galaxy sample using numerical simulations
and overlapping spectroscopy from the Galaxy and Mass Assembly
survey. This purity ensures that the interpretation of our
measurements is not complicated by the presence of a significant
fraction of satellite galaxies. Restricting our central galaxy
ellipticity measurement to the inner isophotes, we find f$_{h}$
= 0.34 {\ensuremath{\pm}} 0.17 for our red sub-sample,
suggesting that the outer galaxy regions are more aligned with
their dark matter halos than the inner regions. Our results are
in agreement with previous studies and suggest that lower mass
halos are rounder and/or less aligned with their host galaxy
than samples of more massive galaxies, studied in galaxy groups
and clusters.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...647A.185G},
 altmetric = {99778344},
 archiveprefix = {arXiv},
 arxiv = {2102.03549},
 author = {{Georgiou}, Christos and {Hoekstra}, Henk and {Kuijken}, Konrad and {Bilicki}, Maciej and {Dvornik}, Andrej and {Erben}, Thomas and {Giblin}, Benjamin and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {de Jong}, Jelte T.~A. and {Kannawadi}, Arun and {Schneider}, Peter and {Schrabback}, Tim and {Shan}, Huan Yuan and {Wright}, Angus H.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/201937405},
 eid = {A185},
 eprint = {2102.03549},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, galaxies: general, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {March},
 pages = {A185},
 primaryclass = {astro-ph.GA},
 title = {{Halo shapes constrained from a pure sample of central galaxies in KiDS-1000}},
 volume = {647},
 year = {2021}
}

@article{2021A&A...647A.124H,
 abbr = {A&A},
 abstract = {{We present redshift distribution estimates of galaxies selected from the
fourth data release of the Kilo-Degree Survey over an area of
{\ensuremath{\sim}}1000 deg$^{2}$ (KiDS-1000). These redshift
distributions represent one of the crucial ingredients for weak
gravitational lensing measurements with the KiDS-1000 data. The
primary estimate is based on deep spectroscopic reference
catalogues that are re-weighted with the help of a self-
organising map (SOM) to closely resemble the KiDS-1000 sources,
split into five tomographic redshift bins in the photometric
redshift range 0.1 < z$_{B}$ {\ensuremath{\leq}} 1.2. Sources
are selected such that they only occupy that volume of nine-
dimensional magnitude-space that is also covered by the
reference samples (`gold' selection). Residual biases in the
mean redshifts determined from this calibration are estimated
from mock catalogues to be {\ensuremath{\lesssim}}0.01 for all
five bins with uncertainties of {\ensuremath{\sim}}0.01. This
primary SOM estimate of the KiDS-1000 redshift distributions is
complemented with an independent clustering redshift approach.
After validation of the clustering-z on the same mock catalogues
and a careful assessment of systematic errors, we find no
significant bias of the SOM redshift distributions with respect
to the clustering-z measurements. The SOM redshift distributions
re-calibrated by the clustering-z represent an alternative
calibration of the redshift distributions with only slightly
larger uncertainties in the mean redshifts of
{\ensuremath{\sim}}0.01 {\ensuremath{-}} 0.02 to be used in
KiDS-1000 cosmological weak lensing analyses. As this includes
the SOM uncertainty, clustering-z are shown to be fully
competitive on KiDS-1000 data.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...647A.124H},
 altmetric = {86841898},
 archiveprefix = {arXiv},
 arxiv = {2007.15635},
 author = {{Hildebrandt}, H. and {van den Busch}, J.~L. and {Wright}, A.~H. and {Blake}, C. and {Joachimi}, B. and {Kuijken}, K. and {Tr{\"o}ster}, T. and {Asgari}, M. and {Bilicki}, M. and {de Jong}, J.~T.~A. and {Dvornik}, A. and {Erben}, T. and {Getman}, F. and {Giblin}, B. and {Heymans}, C. and {Kannawadi}, A. and {Lin}, C. -A. and {Shan}, H. -Y.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202039018},
 eid = {A124},
 eprint = {2007.15635},
 journal = {Astronomy and Astrophysics},
 keywords = {cosmology: observations, gravitational lensing: weak, galaxies: photometry, surveys, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics},
 month = {March},
 pages = {A124},
 primaryclass = {astro-ph.CO},
 title = {{KiDS-1000 catalogue: Redshift distributions and their calibration}},
 volume = {647},
 year = {2021}
}

@article{2021A&A...646A.175L,
 abbr = {A&A},
 abstract = {{We performed an internal-consistency test of the KiDS+VIKING-450 (KV450)
cosmic shear analysis with a colour-based split of source
galaxies. Utilising the same measurements and calibrations for
both sub-samples, we inspected the characteristics of the shear
measurements and the performance of the calibration pipelines.
On the modelling side, we examined the observational nuisance
parameters, specifically those for the redshift calibration and
intrinsic alignments, using a Bayesian analysis with dedicated
test parameters. We verified that the current nuisance
parameters are sufficient for the KV450 data to capture residual
systematics, with slight deviations seen in the second and the
third redshift tomographic bins. Our test also showcases the
degeneracy between the inferred amplitude of intrinsic
alignments and the redshift uncertainties in low redshift
tomographic bins. The test is rather insensitive to the
background cosmology and, therefore, can be implemented before
any cosmological inference is made.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...646A.175L},
 altmetric = {89300972},
 archiveprefix = {arXiv},
 arxiv = {2009.00367},
 author = {{Li}, Shun-Sheng and {Kuijken}, Konrad and {Hoekstra}, Henk and {Hildebrandt}, Hendrik and {Joachimi}, Benjamin and {Kannawadi}, Arun},
 bibtex_show = {true},
 custom_keywords = {major},
 doi = {10.1051/0004-6361/202039254},
 eid = {A175},
 eprint = {2009.00367},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, methods: statistical, surveys, cosmology: observations, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {February},
 pages = {A175},
 primaryclass = {astro-ph.CO},
 title = {{KiDS+VIKING-450: An internal-consistency test for cosmic shear tomography with a colour-based split of source galaxies}},
 volume = {646},
 year = {2021}
}

@article{2021A&A...646A.140H,
 abbr = {A&A},
 abstract = {{We present a joint cosmological analysis of weak gravitational lensing
observations from the Kilo-Degree Survey (KiDS-1000), with
redshift-space galaxy clustering observations from the Baryon
Oscillation Spectroscopic Survey (BOSS) and galaxy-galaxy
lensing observations from the overlap between KiDS-1000, BOSS,
and the spectroscopic 2-degree Field Lensing Survey. This
combination of large-scale structure probes breaks the
degeneracies between cosmological parameters for individual
observables, resulting in a constraint on the structure growth
parameter S$_{8}$ = {\ensuremath{\sigma}}$_{8}${\ensuremath{\sqr
t{}}}({\ensuremath{\Omega}}$_{m}$/0.3) =
0.766$_{-0.014}$$^{+0.020}$, which has the same overall
precision as that reported by the full-sky cosmic microwave
background observations from Planck. The recovered S$_{8}$
amplitude is low, however, by 8.3 {\ensuremath{\pm}} 2.6\%
relative to Planck. This result builds from a series of
KiDS-1000 analyses where we validate our methodology with
variable depth mock galaxy surveys, our lensing calibration with
image simulations and null-tests, and our optical-to-near-
infrared redshift calibration with multi-band mock catalogues
and a spectroscopic-photometric clustering analysis. The
systematic uncertainties identified by these analyses are folded
through as nuisance parameters in our cosmological analysis.
Inspecting the offset between the marginalised posterior
distributions, we find that the S$_{8}$-difference with Planck
is driven by a tension in the matter fluctuation amplitude
parameter, {\ensuremath{\sigma}}$_{8}$. We quantify the level of
agreement between the cosmic microwave background and our large-
scale structure constraints using a series of different metrics,
finding differences with a significance ranging between
{\ensuremath{\sim}}3{\ensuremath{\sigma}}, when considering the
offset in S$_{8}$, and
{\ensuremath{\sim}}2{\ensuremath{\sigma}}, when considering the
full multi-dimensional parameter space.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...646A.140H},
 altmetric = {86841902},
 archiveprefix = {arXiv},
 arxiv = {2007.15632},
 author = {{Heymans}, Catherine and {Tr{\"o}ster}, Tilman and {Asgari}, Marika and {Blake}, Chris and {Hildebrandt}, Hendrik and {Joachimi}, Benjamin and {Kuijken}, Konrad and {Lin}, Chieh-An and {S{\'a}nchez}, Ariel G. and {van den Busch}, Jan Luca and {Wright}, Angus H. and {Amon}, Alexandra and {Bilicki}, Maciej and {de Jong}, Jelte and {Crocce}, Martin and {Dvornik}, Andrej and {Erben}, Thomas and {Fortuna}, Maria Cristina and {Getman}, Fedor and {Giblin}, Benjamin and {Glazebrook}, Karl and {Hoekstra}, Henk and {Joudaki}, Shahab and {Kannawadi}, Arun and {K{\"o}hlinger}, Fabian and {Lidman}, Chris and {Miller}, Lance and {Napolitano}, Nicola R. and {Parkinson}, David and {Schneider}, Peter and {Shan}, HuanYuan and {Valentijn}, Edwin A. and {Verdoes Kleijn}, Gijs and {Wolf}, Christian},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202039063},
 eid = {A140},
 eprint = {2007.15632},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, methods: data analysis, methods: statistical, surveys, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {February},
 pages = {A140},
 primaryclass = {astro-ph.CO},
 selected = {true},
 title = {{KiDS-1000 Cosmology: Multi-probe weak gravitational lensing and spectroscopic galaxy clustering constraints}},
 volume = {646},
 year = {2021}
}

@article{2021A&A...646A.129J,
 abbr = {A&A},
 abstract = {{We present the methodology for a joint cosmological analysis of weak
gravitational lensing from the fourth data release of the ESO
Kilo-Degree Survey (KiDS-1000) and galaxy clustering from the
partially overlapping Baryon Oscillation Spectroscopic Survey
(BOSS) and the 2-degree Field Lensing Survey (2dFLenS). Cross-
correlations between BOSS and 2dFLenS galaxy positions and
source galaxy ellipticities have been incorporated into the
analysis, necessitating the development of a hybrid model of
non-linear scales that blends perturbative and non-perturbative
approaches, and an assessment of signal contributions by
astrophysical effects. All weak lensing signals were measured
consistently via Fourier-space statistics that are insensitive
to the survey mask and display low levels of mode mixing. The
calibration of photometric redshift distributions and
multiplicative gravitational shear bias has been updated, and a
more complete tally of residual calibration uncertainties was
propagated into the likelihood. A dedicated suite of more than
20 000 mocks was used to assess the performance of covariance
models and to quantify the impact of survey geometry and spatial
variations of survey depth on signals and their errors. The
sampling distributions for the likelihood and the
{\ensuremath{\chi}}$^{2}$ goodness-of-fit statistic have been
validated, with proposed changes for calculating the effective
number of degrees of freedom. The prior volume was explicitly
mapped, and a more conservative, wide top-hat prior on the key
structure growth parameter S$_{8}$ = {\ensuremath{\sigma}}$_{8}$
({\ensuremath{\Omega}}$_{m}$/0.3)$^{1/2}$ was introduced. The
prevalent custom of reporting S$_{8}$ weak lensing constraints
via point estimates derived from its marginal posterior is
highlighted to be easily misinterpreted as yielding
systematically low values of S$_{8}$, and an alternative
estimator and associated credible interval are proposed. Known
systematic effects pertaining to weak lensing modelling and
inference are shown to bias S$_{8}$ by no more than 0.1 standard
deviations, with the caveat that no conclusive validation data
exist for models of intrinsic galaxy alignments. Compared to the
previous KiDS analyses, S$_{8}$ constraints are expected to
improve by 20\% for weak lensing alone and by 29\% for the joint
analysis.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...646A.129J},
 altmetric = {85277048},
 archiveprefix = {arXiv},
 arxiv = {2007.01844},
 author = {{Joachimi}, B. and {Lin}, C. -A. and {Asgari}, M. and {Tr{\"o}ster}, T. and {Heymans}, C. and {Hildebrandt}, H. and {K{\"o}hlinger}, F. and {S{\'a}nchez}, A.~G. and {Wright}, A.~H. and {Bilicki}, M. and {Blake}, C. and {van den Busch}, J.~L. and {Crocce}, M. and {Dvornik}, A. and {Erben}, T. and {Getman}, F. and {Giblin}, B. and {Hoekstra}, H. and {Kannawadi}, A. and {Kuijken}, K. and {Napolitano}, N.~R. and {Schneider}, P. and {Scoccimarro}, R. and {Sellentin}, E. and {Shan}, H.~Y. and {von Wietersheim-Kramsta}, M. and {Zuntz}, J.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202038831},
 eid = {A129},
 eprint = {2007.01844},
 journal = {Astronomy and Astrophysics},
 keywords = {cosmology: miscellaneous, gravitational lensing: weak, large-scale structure of Universe, methods: data analysis, methods: analytical, methods: statistical, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics},
 month = {February},
 pages = {A129},
 primaryclass = {astro-ph.CO},
 title = {{KiDS-1000 methodology: Modelling and inference for joint weak gravitational lensing and spectroscopic galaxy clustering analysis}},
 volume = {646},
 year = {2021}
}

@article{2021A&A...646A.124H,
 abbr = {A&A},
 abstract = {{Weak lensing by large-scale structure is a powerful probe of cosmology
if the apparent alignments in the shapes of distant galaxies can
be accurately measured. Most studies have therefore focused on
improving the fidelity of the shape measurements themselves, but
the preceding step of object detection has been largely ignored.
In this paper, we study the impact of object detection for a
Euclid-like survey and show that it leads to biases that exceed
requirements for the next generation of cosmic shear surveys. In
realistic scenarios, the blending of galaxies is an important
source of detection bias. We find that METADETECTION is able to
account for blending, leading to average multiplicative biases
that meet requirements for Stage IV surveys, provided a
sufficiently accurate model for the point spread function is
available. Further work is needed to estimate the performance
for actual surveys. Combined with sufficiently realistic image
simulations, this provides a viable way forward towards accurate
shear estimates for Stage IV surveys.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...646A.124H},
 altmetric = {92182045},
 archiveprefix = {arXiv},
 arxiv = {2010.04178},
 author = {{Hoekstra}, Henk and {Kannawadi}, Arun and {Kitching}, Thomas D.},
 bibtex_show = {true},
 custom_keywords = {first},
 doi = {10.1051/0004-6361/202038998},
 eid = {A124},
 eprint = {2010.04178},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, large-scale structure of Universe, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {February},
 pages = {A124},
 primaryclass = {astro-ph.CO},
 selected = {true},
 title = {{Accounting for object detection bias in weak gravitational lensing studies}},
 volume = {646},
 year = {2021}
}

@article{2021A&A...646A..73S,
 abbr = {A&A},
 abstract = {{Cosmological simulations predict that galaxies are embedded into
triaxial dark matter haloes, which appear approximately
elliptical in projection. Weak gravitational lensing allows us
to constrain these halo shapes and thereby test the nature of
dark matter. Weak lensing has already provided robust detections
of the signature of halo flattening at the mass scales of groups
and clusters, whereas results for galaxies have been somewhat
inconclusive. Here we combine data from five weak lensing
surveys (NGVSLenS, KiDS/KV450, CFHTLenS, CS82, and RCSLenS,
listed in order of most to least constraining) in order to
tighten observational constraints on galaxy-scale halo
ellipticity for photometrically selected lens samples. We
constrain f$_{h}$, the average ratio between the aligned
component of the halo ellipticity and the ellipticity of the
light distribution, finding f$_{h}$ =
0.303$_{-0.079}$$^{+0.080}$ for red lens galaxies and f$_{h}$ =
0.217$_{-0.159}$$^{+0.160}$ for blue lens galaxies when assuming
elliptical Navarro-Frenk-White density profiles and a linear
scaling between halo ellipticity and galaxy ellipticity. Our
constraints for red galaxies constitute the currently most
significant (3.8{\ensuremath{\sigma}}) systematics-corrected
detection of the signature of halo flattening at the mass scale
of galaxies. Our results are in good agreement with expectations
from the Millennium Simulation that apply the same analysis
scheme and incorporate models for galaxy-halo misalignment.
Assuming these misalignment models and the analysis assumptions
stated above are correct, our measurements imply an average dark
matter halo ellipticity for the studied red galaxy samples of
⟨|ϵ$_{h}$|⟩ = 0.174 {\ensuremath{\pm}} 0.046, where |ϵ$_{h}$| =
(1 - q)/(1 + q) relates to the ratio q = b/a of the minor and
major axes of the projected mass distribution. Similar
measurements based on larger upcoming weak lensing data sets can
help to calibrate models for intrinsic galaxy alignments, which
constitute an important source of systematic uncertainty in
cosmological weak lensing studies.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...646A..73S},
 altmetric = {91601904},
 archiveprefix = {arXiv},
 arxiv = {2010.00311},
 author = {{Schrabback}, Tim and {Hoekstra}, Henk and {Van Waerbeke}, Ludovic and {van Uitert}, Edo and {Georgiou}, Christos and {Asgari}, Marika and {C{\^o}t{\'e}}, Patrick and {Cuillandre}, Jean-Charles and {Erben}, Thomas and {Ferrarese}, Laura and {Gwyn}, Stephen D.~J. and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Kannawadi}, Arun and {Kuijken}, Konrad and {Leauthaud}, Alexie and {Makler}, Martin and {Mei}, Simona and {Miller}, Lance and {Raichoor}, Anand and {Schneider}, Peter and {Wright}, Angus},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202037670},
 eid = {A73},
 eprint = {2010.00311},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, galaxies: halos, dark matter, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies},
 month = {February},
 pages = {A73},
 primaryclass = {astro-ph.CO},
 title = {{Tightening weak lensing constraints on the ellipticity of galaxy-scale dark matter haloes}},
 volume = {646},
 year = {2021}
}

@article{2021A&A...645A.105G,
 abbr = {A&A},
 abstract = {{We present weak lensing shear catalogues from the fourth data release of
the Kilo-Degree Survey, KiDS-1000, spanning 1006 square degrees
of deep and high-resolution imaging. Our `gold-sample' of
galaxies, with well-calibrated photometric redshift
distributions, consists of 21 million galaxies with an effective
number density of 6.17 galaxies per square arcminute. We
quantify the accuracy of the spatial, temporal, and flux-
dependent point-spread function (PSF) model, verifying that the
model meets our requirements to induce less than a
0.1{\ensuremath{\sigma}} change in the inferred cosmic shear
constraints on the clustering cosmological parameter S$_{8}$ =
{\ensuremath{\sigma}}$_{8}$
{\ensuremath{\sqrt{}}}{\ensuremath{\Omega}}$_{m}$/0.3.. Through
a series of two-point null-tests, we validate the shear
estimates, finding no evidence for significant non-lensing
B-mode distortions in the data. The PSF residuals are detected
in the highest-redshift bins, originating from object selection
and/or weight bias. The amplitude is, however, shown to be
sufficiently low and within our stringent requirements. With a
shear-ratio null-test, we verify the expected redshift scaling
of the galaxy-galaxy lensing signal around luminous red
galaxies. We conclude that the joint KiDS-1000 shear and
photometric redshift calibration is sufficiently robust for
combined-probe gravitational lensing and spectroscopic
clustering analyses.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...645A.105G},
 altmetric = {85277045},
 archiveprefix = {arXiv},
 arxiv = {2007.01845},
 author = {{Giblin}, Benjamin and {Heymans}, Catherine and {Asgari}, Marika and {Hildebrandt}, Hendrik and {Hoekstra}, Henk and {Joachimi}, Benjamin and {Kannawadi}, Arun and {Kuijken}, Konrad and {Lin}, Chieh-An and {Miller}, Lance and {Tr{\"o}ster}, Tilman and {van den Busch}, Jan Luca and {Wright}, Angus H. and {Bilicki}, Maciej and {Blake}, Chris and {de Jong}, Jelte and {Dvornik}, Andrej and {Erben}, Thomas and {Getman}, Fedor and {Napolitano}, Nicola R. and {Schneider}, Peter and {Shan}, HuanYuan and {Valentijn}, Edwin},
 bibtex_show = {true},
 custom_keywords = {major},
 doi = {10.1051/0004-6361/202038850},
 eid = {A105},
 eprint = {2007.01845},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, large-scale structure of Universe, cosmological parameters, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {January},
 pages = {A105},
 primaryclass = {astro-ph.CO},
 title = {{KiDS-1000 catalogue: Weak gravitational lensing shear measurements}},
 volume = {645},
 year = {2021}
}

@article{2021A&A...645A.104A,
 abbr = {A&A},
 abstract = {{We present cosmological constraints from a cosmic shear analysis of the
fourth data release of the Kilo-Degree Survey (KiDS-1000), which
doubles the survey area with nine-band optical and near-infrared
photometry with respect to previous KiDS analyses. Adopting a
spatially flat standard cosmological model, we find S$_{8}$ = {\
ensuremath{\sigma}}$_{8}$({\ensuremath{\Omega}}$_{m}$/0.3)$^{0.5
}$ = 0.759$_{-0.021}$$^{+0.024}$ for our fiducial analysis,
which is in 3{\ensuremath{\sigma}} tension with the prediction
of the Planck Legacy analysis of the cosmic microwave
background. We compare our fiducial COSEBIs (Complete Orthogonal
Sets of E/B-Integrals) analysis with complementary analyses of
the two-point shear correlation function and band power spectra,
finding the results to be in excellent agreement. We investigate
the sensitivity of all three statistics to a number of
measurement, astrophysical, and modelling systematics, finding
our S$_{8}$ constraints to be robust and dominated by
statistical errors. Our cosmological analysis of different
divisions of the data passes the Bayesian internal consistency
tests, with the exception of the second tomographic bin. As this
bin encompasses low-redshift galaxies, carrying insignificant
levels of cosmological information, we find that our results are
unchanged by the inclusion or exclusion of this sample.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2021A&A...645A.104A},
 altmetric = {86841900},
 archiveprefix = {arXiv},
 arxiv = {2007.15633},
 author = {{Asgari}, Marika and {Lin}, Chieh-An and {Joachimi}, Benjamin and {Giblin}, Benjamin and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Kannawadi}, Arun and {St{\"o}lzner}, Benjamin and {Tr{\"o}ster}, Tilman and {van den Busch}, Jan Luca and {Wright}, Angus H. and {Bilicki}, Maciej and {Blake}, Chris and {de Jong}, Jelte and {Dvornik}, Andrej and {Erben}, Thomas and {Getman}, Fedor and {Hoekstra}, Henk and {K{\"o}hlinger}, Fabian and {Kuijken}, Konrad and {Miller}, Lance and {Radovich}, Mario and {Schneider}, Peter and {Shan}, HuanYuan and {Valentijn}, Edwin},
 bibtex_show = {true},
 custom_keywords = {major},
 doi = {10.1051/0004-6361/202039070},
 eid = {A104},
 eprint = {2007.15633},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, methods: observational, cosmology: observations, large-scale structure of Universe, cosmological parameters, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {January},
 pages = {A104},
 primaryclass = {astro-ph.CO},
 title = {{KiDS-1000 cosmology: Cosmic shear constraints and comparison between two point statistics}},
 volume = {645},
 year = {2021}
}

@article{2020A&A...642A.158B,
 abbr = {A&A},
 abstract = {{The physics of gravity on cosmological scales affects both the rate of
assembly of large-scale structure and the gravitational lensing
of background light through this cosmic web. By comparing the
amplitude of these different observational signatures, we can
construct tests that can distinguish general relativity from its
potential modifications. We used the latest weak gravitational
lensing dataset from the Kilo-Degree Survey, KiDS-1000, in
conjunction with overlapping galaxy spectroscopic redshift
surveys, BOSS and 2dFLenS, to perform the most precise existing
amplitude-ratio test. We measured the associated E$_{G}$
statistic with 15 - 20\% errors in five {\ensuremath{\Delta}}z =
0.1 tomographic redshift bins in the range 0.2 < z < 0.7 on
projected scales up to 100 h$^{-1}$ Mpc. The scale-independence
and redshift-dependence of these measurements are consistent
with the theoretical expectation of general relativity in a
Universe with matter density {\ensuremath{\Omega}}$_{m}$ = 0.27
{\ensuremath{\pm}} 0.04. We demonstrate that our results are
robust against different analysis choices, including schemes for
correcting the effects of source photometric redshift errors,
and we compare the performance of angular and projected galaxy-
galaxy lensing statistics.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2020A&A...642A.158B},
 altmetric = {83194846},
 archiveprefix = {arXiv},
 arxiv = {2005.14351},
 author = {{Blake}, Chris and {Amon}, Alexandra and {Asgari}, Marika and {Bilicki}, Maciej and {Dvornik}, Andrej and {Erben}, Thomas and {Giblin}, Benjamin and {Glazebrook}, Karl and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Joachimi}, Benjamin and {Joudaki}, Shahab and {Kannawadi}, Arun and {Kuijken}, Konrad and {Lidman}, Chris and {Parkinson}, David and {Shan}, HuanYuan and {Tr{\"o}ster}, Tilman and {van den Busch}, Jan Luca and {Wolf}, Christian and {Wright}, Angus H.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202038505},
 eid = {A158},
 eprint = {2005.14351},
 journal = {Astronomy and Astrophysics},
 keywords = {dark energy, large-scale structure of Universe, gravitational lensing: weak, surveys, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {October},
 pages = {A158},
 primaryclass = {astro-ph.CO},
 title = {{Testing gravity using galaxy-galaxy lensing and clustering amplitudes in KiDS-1000, BOSS, and 2dFLenS}},
 volume = {642},
 year = {2020}
}

@article{2020A&A...642A..83D,
 abbr = {A&A},
 abstract = {{We simultaneously present constraints on the stellar-to-halo mass
relation for central and satellite galaxies through a weak
lensing analysis of spectroscopically classified galaxies. Using
overlapping data from the fourth data release of the Kilo-Degree
Survey (KiDS), and the Galaxy And Mass Assembly survey (GAMA),
we find that satellite galaxies are hosted by halo masses that
are 0.53 {\ensuremath{\pm}} 0.39 dex (68\% confidence,
3{\ensuremath{\sigma}} detection) smaller than those of central
galaxies of the same stellar mass (for a stellar mass of
log(M$_{{\ensuremath{\star}}}$/M$_{{\ensuremath{\odot}}}$) =
10.6). This is consistent with galaxy formation models, whereby
infalling satellite galaxies are preferentially stripped of
their dark matter. We find consistent results with similar
uncertainties when comparing constraints from a standard
azimuthally averaged galaxy-galaxy lensing analysis and a two-
dimensional likelihood analysis of the full shear field. As the
latter approach is somewhat biased due to the lens
incompleteness and as it does not provide any improvement to the
precision when applied to actual data, we conclude that stacked
tangential shear measurements are best-suited for studies of the
galaxy-halo connection.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2020A&A...642A..83D},
 altmetric = {84448276},
 archiveprefix = {arXiv},
 arxiv = {2006.10777},
 author = {{Dvornik}, Andrej and {Hoekstra}, Henk and {Kuijken}, Konrad and {Wright}, Angus H. and {Asgari}, Marika and {Bilicki}, Maciej and {Erben}, Thomas and {Giblin}, Benjamin and {Graham}, Alister W. and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Hopkins}, Andrew M. and {Kannawadi}, Arun and {Lin}, Chieh-An and {Taylor}, Edward N. and {Tr{\"o}ster}, Tilman},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202038693},
 eid = {A83},
 eprint = {2006.10777},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, methods: statistical, surveys, galaxies: halos, large-scale structure of Universe, dark matter, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {October},
 pages = {A83},
 primaryclass = {astro-ph.CO},
 title = {{KiDS+GAMA: The weak lensing calibrated stellar-to-halo mass relation of central and satellite galaxies}},
 volume = {642},
 year = {2020}
}

@article{2020arXiv200813154V,
 abstract = {{We present a sample of luminous red-sequence galaxies to study the
large-scale structure in the fourth data release of the Kilo-
Degree Survey. The selected galaxies are defined by a red-
sequence template, in the form of a data-driven model of the
colour-magnitude relation conditioned on redshift. In this work,
the red-sequence template is built using the broad-band
optical+near infrared photometry of KiDS-VIKING and the
overlapping spectroscopic data sets. The selection process
involves estimating the red-sequence redshifts, assessing the
purity of the sample, and estimating the underlying redshift
distributions of redshift bins. After performing the selection,
we mitigate the impact of survey properties on the observed
number density of galaxies by assigning photometric weights to
the galaxies. We measure the angular two-point correlation
function of the red galaxies in four redshift bins, and
constrain the large scale bias of our red-sequence sample
assuming a fixed $\Lambda$CDM cosmology. We find consistent
linear biases for two luminosity-threshold samples (dense and
luminous). We find that our constraints are well characterized
by the passive evolution model.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2020arXiv200813154V},
 archiveprefix = {arXiv},
 arxiv = {2008.13154},
 author = {{Vakili}, Mohammadjavad and {Hoekstra}, Henk and {Bilicki}, Maciej and {Fortuna}, Maria-Cristina and {Kuijken}, Konrad and {Wright}, Angus H. and {Asgari}, Marika and {Brown}, Michael and {Dombrovskij}, Elisabeth and {Erben}, Thomas and {Giblin}, Benjamin and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Johnston}, Harry and {Joudaki}, Shahab and {Kannawadi}, Arun},
 bibtex_show = {true},
 doi = {10.48550/arXiv.2008.13154},
 eid = {arXiv:2008.13154},
 eprint = {2008.13154},
 journal = {arXiv e-prints},
 keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {August},
 pages = {arXiv:2008.13154},
 primaryclass = {astro-ph.CO},
 title = {{Clustering of red-sequence galaxies in the fourth data release ofthe Kilo-Degree Survey}},
 year = {2020}
}

@article{2020A&A...640L..14W,
 abbr = {A&A},
 abstract = {{We present updated cosmological constraints for the KiDS+VIKING-450
cosmic shear data set (KV450) estimated through redshift
distributions and photometric samples defined using self-
organising maps (SOMs). Our fiducial analysis finds marginal
posterior constraints of S$_{8}$ {\ensuremath{\equiv}}
{\ensuremath{\sigma}}$_{8}$ {\ensuremath{\Omega}}$_{m}$/0.3 =
0.716$_{-0.038}$$^{+0.043}$, which are smaller but otherwise
consistent with previous works that have applied this data set
(|{\ensuremath{\Delta}}S$_{8}$| = 0.023). We analysed additional
samples and redshift distributions set up in three ways: (1) by
excluding certain spectroscopic surveys during redshift
calibration; (2) by excluding lower-confidence spectroscopic
redshifts in redshift calibration; and (3) by considering only
those photometric sources which are jointly calibrated by at
least three spectroscopic surveys. In all cases, the method
utilised here has been proven to be robust: we find a maximal
deviation from our fiducial analysis of
|{\ensuremath{\Delta}}S$_{8}$| {\ensuremath{\leq}} 0.011 for all
samples defined and analysed using our SOM. To demonstrate the
reduction in systematic biases found within our analysis, we
highlight our results when performing redshift calibration
without the DEEP2 spectroscopic data set. In this case, we find
marginal posterior constraints of S$_{8}$ =
0.707$_{-0.042}$$^{+0.046}$; this is a difference, with respect
to the fiducial, that is both significantly smaller and in the
opposite direction with regard to the equivalent shift from
previous works. These results suggest that our improved
cosmological parameter estimates are not sensitive to
pathological misrepresentations of photometric sources by the
spectroscopy used for direct redshift calibration and,
therefore, that this systematic effect cannot be responsible for
the observed difference between S$_{8}$ estimates made with
KV450 and Planck CMB probes.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2020A&A...640L..14W},
 altmetric = {81769364},
 archiveprefix = {arXiv},
 arxiv = {2005.04207},
 author = {{Wright}, Angus H. and {Hildebrandt}, Hendrik and {van den Busch}, Jan Luca and {Heymans}, Catherine and {Joachimi}, Benjamin and {Kannawadi}, Arun and {Kuijken}, Konrad},
 bibtex_show = {true},
 custom_keywords = {major},
 doi = {10.1051/0004-6361/202038389},
 eid = {L14},
 eprint = {2005.04207},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, cosmology: observations, surveys, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {August},
 pages = {L14},
 primaryclass = {astro-ph.CO},
 title = {{KiDS+VIKING-450: Improved cosmological parameter constraints from redshift calibration with self-organising maps}},
 volume = {640},
 year = {2020}
}

@article{2020A&A...640A..59L,
 abbr = {A&A},
 abstract = {{Context. Several semi-analytic models (SAMs) try to explain how galaxies
form, evolve, and interact inside the dark matter large-scale
structure. These SAMs can be tested by comparing their
predictions for galaxy-galaxy-galaxy lensing (G3L), which is
weak gravitational lensing around galaxy pairs, with
observations. \textbackslash Aims: We evaluate the SAMs by
Henriques et al. (2015, MNRAS, 451, 2663, hereafter H15) and by
Lagos et al. (2012, MNRAS, 426, 2142, hereafter L12), which were
implemented in the Millennium Run, by comparing their
predictions for G3L to observations at smaller scales than
previous studies and also for pairs of lens galaxies from
different populations. \textbackslash Methods: We compared the
G3L signal predicted by the SAMs to measurements in the overlap
of the Galaxy And Mass Assembly survey (GAMA), the Kilo-Degree
Survey (KiDS), and the VISTA Kilo-degree Infrared Galaxy survey
(VIKING) by splitting lens galaxies into two colour and five
stellar-mass samples. Using an improved G3L estimator, we
measured the three-point correlation of the matter distribution
with ``mixed lens pairs'' with galaxies from different samples,
and with ``unmixed lens pairs'' with galaxies from the same
sample. \textbackslash Results: Predictions by the H15 SAM for
the G3L signal agree with the observations for all colour-
selected samples and all but one stellar-mass-selected sample
with 95\% confidence. Deviations occur for lenses with stellar
masses below 9.5 h$^{-2}$ M$_{{\ensuremath{\odot}}}$ at scales
below 0.2 h$^{-1}$ Mpc. Predictions by the L12 SAM for stellar-
mass selected samples and red galaxies are significantly higher
than observed, while the predicted signal for blue galaxy pairs
is too low. \textbackslash Conclusions: The L12 SAM predicts
more pairs of low stellar mass and red galaxies than the H15 SAM
and the observations, as well as fewer pairs of blue galaxies.
This difference increases towards the centre of the galaxies'
host halos. Likely explanations are different treatments of
environmental effects by the SAMs and different models of the
initial mass function. We conclude that G3L provides a stringent
test for models of galaxy formation and evolution.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2020A&A...640A..59L},
 altmetric = {81536909},
 archiveprefix = {arXiv},
 arxiv = {2005.02419},
 author = {{Linke}, Laila and {Simon}, Patrick and {Schneider}, Peter and {Erben}, Thomas and {Farrow}, Daniel J. and {Heymans}, Catherine and {Hildebrandt}, Hendrik and {Hopkins}, Andrew M. and {Kannawadi}, Arun and {Napolitano}, Nicola R. and {Sif{\'o}n}, Crist{\'o}bal and {Wright}, Angus H.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/202038355},
 eid = {A59},
 eprint = {2005.02419},
 journal = {Astronomy and Astrophysics},
 keywords = {gravitational lensing: weak, cosmology: observations, large-scale structure of Universe, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {August},
 pages = {A59},
 primaryclass = {astro-ph.CO},
 title = {{KiDS+VIKING+GAMA: Testing semi-analytic models of galaxy evolution with galaxy-galaxy-galaxy lensing}},
 volume = {640},
 year = {2020}
}

@article{2020A&A...638L...1J,
 abbr = {A&A},
 abstract = {{We present a combined tomographic weak gravitational lensing analysis of
the Kilo Degree Survey (KV450) and the Dark Energy Survey
(DES-Y1). We homogenize the analysis of these two public cosmic
shear datasets by adopting consistent priors and modeling of
nonlinear scales, and determine new redshift distributions for
DES-Y1 based on deep public spectroscopic surveys. Adopting
these revised redshifts results in a 0.8{\ensuremath{\sigma}}
reduction in the DES-inferred value for S$_{8}$, which
decreases to a 0.5{\ensuremath{\sigma}} reduction when including
a systematic redshift calibration error model from mock DES data
based on the MICE2 simulation. The combined KV450+DES-Y1
constraint on S$_{8}$ = 0.762$_{-0.024}$$^{+0.025}$ is in
tension with the Planck 2018 constraint from the cosmic
microwave background at the level of 2.5{\ensuremath{\sigma}}.
This result highlights the importance of developing methods to
provide accurate redshift calibration for current and future
weak-lensing surveys.}},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2020A&A...638L...1J},
 altmetric = {62604871},
 archiveprefix = {arXiv},
 arxiv = {1906.09262},
 author = {{Joudaki}, S. and {Hildebrandt}, H. and {Traykova}, D. and {Chisari}, N.~E. and {Heymans}, C. and {Kannawadi}, A. and {Kuijken}, K. and {Wright}, A.~H. and {Asgari}, M. and {Erben}, T. and {Hoekstra}, H. and {Joachimi}, B. and {Miller}, L. and {Tr{\"o}ster}, T. and {van den Busch}, J.~L.},
 bibtex_show = {true},
 doi = {10.1051/0004-6361/201936154},
 eid = {L1},
 eprint = {1906.09262},
 journal = {Astronomy and Astrophysics},
 keywords = {cosmology: observations, galaxies: photometry, gravitational lensing: weak, surveys, Astrophysics - Cosmology and Nongalactic Astrophysics},
 month = {June},
 pages = {L1},
 primaryclass = {astro-ph.CO},
 title = {{KiDS+VIKING-450 and DES-Y1 combined: Cosmology with cosmic shear}},
 volume = {638},
 year = {2020}
}

@article{2020A&A...638C...2E,
 abbr = {A&A},
 adsnote = {Provided by the SAO/NASA Astrophysics Data System},
 adsurl = {https://ui.adsabs.harvard.edu/abs/2020A&A...638C...2E},
 altmetric = {83528298},
 author = {{Euclid Collaboration} and {Paykari}, P. and {Kitching}, T. and {Hoekstra}, H. and {Azzollini}, R. and {Cardone}, V.~F. and {Cropper}, M. and {Duncan}, C.~A.~J. and {Kannawadi}, A. and {Miller}, L. and {Aussel}, H. and {Conti}, I.~F. and {Auricchio}, N. and {Baldi}, M. and {Bardelli}, S. and {Biviano}, A. and {Bonino}, D. and {Borsato}, E. and {Bozzo}, E. and {Branchini}, E. and {Brau-Nogue}, S. and {Brescia}, M. and {Brinchmann}, J. and {Burigana}, C. and {Camera}, S. and {Capobianco}, V. and {Carbone}, C. and {Carretero}, J. and {Casas}, S. and {Castander}, F.~J. and {Castellano}, M. and {Cavuoti}, S. and {Charles}, Y. and {Cledassou}, R. and {Colodro-Conde}, C. and {Congedo}, G. and {Conselice}, C. and {Conversi}, L. and {Copin}, Y. and {Coupon}, J. and {Courtois}, H.~M. and {Da Silva}, A. and {Dupac}, X. and {Fabbian}, G. and {Farrens}, S. and {Ferreira}, P.~G. and {Fosalba}, P. and {Fourmanoit}, N. and {Frailis}, M. and {Fumana}, M. and {Galeotta}, S. and {Garilli}, B. and {Gillard}, W. and {Gillis}, B.~R. and {Giocoli}, C. and {Graci{\'a}-Carpio}, J. and {Grupp}, F. and {Hormuth}, F. and {Ili{\'c}}, S. and {Israel}, H. and {Jahnke}, K. and {Keihanen}, E. and {Kermiche}, S. and {Kilbinger}, M. and {Kirkpatrick}, C.~C. and {Kubik}, B. and {Kunz}, M. and {Kurki-Suonio}, H. and {Lacasa}, F. and {Laureijs}, R. and {Le Mignant}, D. and {Ligori}, S. and {Lilje}, P.~B. and {Lloro}, I. and {Maciaszek}, T. and {Maiorano}, E. and {Marggraf}, O. and {Markovic}, K. and {Martinelli}, M. and {Martinet}, N. and {Marulli}, F. and {Massey}, R. and {Mauri}, N. and {Medinaceli}, E. and {Mei}, S. and {Mellier}, Y. and {Meneghetti}, M. and {Metcalf}, R.~B. and {Moresco}, M. and {Moscardini}, L. and {Munari}, E. and {Neissner}, C. and {Nichol}, R.~C. and {Niemi}, S. and {Nutma}, T. and {Padilla}, C. and {Paltani}, S. and

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