About

Matias Carrasco Kind is a faculty member at the University of Illinois at Urbana-Champaign, with positions including Faculty in Residence at the Gies College of Business and Affiliate Professor at the National Center for Supercomputing Applications. His educational background includes a Ph.D. and M.S. in Astrophysics from the University of Illinois at Urbana-Champaign, and a B.S. in Astronomy from Pontificia Universidad Catolica de Chile. His research focuses on astrophysics and data science, with significant contributions to photometric redshift estimation, galaxy clustering, and machine learning applications in astronomy. Carrasco Kind has held various research roles, including Research Assistant Professor of Astronomy and Senior Research Scientist at NCSA, and has been involved in developing innovative methods for analyzing large-scale astronomical data, such as probabilistic photometric redshifts and self-organizing maps. His work emphasizes the integration of advanced computational techniques with astrophysical research, contributing to the field's understanding of cosmic structures and the development of tools for petascale astronomy.

Research topics

• Astrophysics
• Physics
• Astronomy
• Computer Science
• Artificial Intelligence
• Chemistry
• Psychology

Selected publications

• Dark Energy Survey Year 3: Blue shear

  Physical review. D/Physical review. D. · 2026-02-17 · 7 citations

  preprintOpen access

  Modeling the intrinsic alignment (IA) of galaxies poses a challenge to weak lensing analyses. The Dark Energy Survey is expected to be less impacted by IA when limited to blue, star-forming galaxies. The cosmological parameter constraints from this blue cosmic shear sample are stable to IA model choice, unlike passive galaxies in the full DES Y3 sample, the goodness-of-fit is improved and the $Ω_{m}$ and $S_8$ better agree with the cosmic microwave background. Mitigating IA with sample selection, instead of flexible model choices, can reduce uncertainty in $S_8$ by a factor of 1.5.

  PublisherOA PDFDOI

• Biasing from galaxy trough and peak profiles with the DES Y3 redMaGiC galaxies and the weak lensing mass map

  Monthly Notices of the Royal Astronomical Society · 2026-01-05

  preprintOpen access

  ABSTRACT We measure the correspondence between the distribution of galaxies and matter around troughs and peaks in the projected galaxy density, by comparing redMaGiC galaxies ($0.15< z<0.65$) to weak lensing mass maps from the Dark Energy Survey (DES) Y3 data release. We obtain stacked profiles, as a function of angle $\theta$, of the galaxy density contrast $\delta _{\rm g}$ and the weak lensing convergence $\kappa$, in the vicinity of these identified troughs and peaks, referred to as ‘void’ and ‘cluster’ superstructures. The ratio of the profiles depend mildly on $\theta$, indicating good consistency between the profile shapes. We model the amplitude of this ratio using a function $F(\boldsymbol{\eta }, \theta)$ that depends on cosmological parameters $\boldsymbol{\eta }$, scaled by the galaxy bias. We construct templates of $F(\boldsymbol{\eta }, \theta)$ using a suite of N-body (Gower Street) simulations forward-modelled with DES Y3-like noise and systematics. We discuss and quantify the caveats of using a linear bias model to create galaxy maps from the simulation dark matter shells. We measure the galaxy bias in three lens tomographic bins (near to far): $2.32^{+0.86}_{-0.27}, 2.18^{+0.86}_{-0.23}, 1.86^{+0.82}_{-0.23}$ for voids, and $2.46^{+0.73}_{-0.27}, 3.55^{+0.96}_{-0.55}, 4.27^{+0.36}_{-1.14}$ for clusters, assuming the best-fitting Planck cosmology. Similar values with $\sim 0.1\sigma$ shifts are obtained assuming the mean DES Y3 cosmology. The biases from troughs and peaks are broadly consistent, although a larger bias is derived for peaks, which is also larger than those measured from the DES Y3 $3\times 2$-point analysis. This method shows an interesting avenue for measuring field-level bias that can be applied to future lensing surveys.

  PublisherOA PDFDOI

• Constraining the Stellar-to-Halo Mass Relation with Galaxy Clustering and Weak Lensing from DES Year 3 Data

  The Open Journal of Astrophysics · 2026-01-08

  articleOpen access

  We develop a framework to study the relation between the stellar mass of a galaxy and the total mass of its host dark matter halo using galaxy clustering and galaxy-galaxy lensing measurements. We model a wide range of scales, roughly from to , using a theoretical framework based on the Halo Occupation Distribution and data from Year 3 of the Dark Energy Survey (DES) dataset. The new advances of this work include: 1) the generation and validation of a new stellar mass-selected galaxy sample in the range of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mo>log</mml:mo> <mml:msub> <mml:mi>M</mml:mi> <mml:mo>⋆</mml:mo> </mml:msub> <mml:mi>/</mml:mi> <mml:msub> <mml:mi>M</mml:mi> <mml:mo>⊙</mml:mo> </mml:msub> <mml:mo>∼</mml:mo> <mml:mn>9.6</mml:mn> </mml:mrow> </mml:math> to <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mo>∼</mml:mo> <mml:mn>11.5</mml:mn> </mml:mrow> </mml:math> ; 2) the joint-modeling framework of galaxy clustering and galaxy-galaxy lensing that is able to describe our stellar mass-selected sample deep into the 1-halo regime; and 3) stellar-to-halo mass relation (SHMR) constraints from this dataset. In general, our SHMR constraints agree well with existing literature with various weak lensing measurements. We constrain the free parameters in the SHMR functional form <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mo>log</mml:mo> <mml:msub> <mml:mi>M</mml:mi> <mml:mo>⋆</mml:mo> </mml:msub> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:msub> <mml:mi>M</mml:mi> <mml:mi>h</mml:mi> </mml:msub> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo>=</mml:mo> <mml:mo>log</mml:mo> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mi>ϵ</mml:mi> <mml:msub> <mml:mi>M</mml:mi> <mml:mn>1</mml:mn> </mml:msub> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo>+</mml:mo> <mml:mi>f</mml:mi> <mml:mrow> <mml:mo stretchy="true" form="prefix">[</mml:mo> <mml:mo>log</mml:mo> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:msub> <mml:mi>M</mml:mi> <mml:mi>h</mml:mi> </mml:msub> <mml:mi>/</mml:mi> <mml:msub> <mml:mi>M</mml:mi> <mml:mn>1</mml:mn> </mml:msub> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo stretchy="true" form="postfix">]</mml:mo> </mml:mrow> <mml:mo>−</mml:mo> <mml:mi>f</mml:mi> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> </mml:mrow> </mml:math> , with <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mi>f</mml:mi> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mi>x</mml:mi> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo>≡</mml:mo> <mml:mo>−</mml:mo> <mml:mo>log</mml:mo> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mrow> <mml:mi>α</mml:mi> <mml:mi>x</mml:mi> </mml:mrow> </mml:msup> <mml:mo>+</mml:mo> <mml:mn>1</mml:mn> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo>+</mml:mo> <mml:mi>δ</mml:mi> <mml:msup> <mml:mrow> <mml:mo stretchy="true" form="prefix">[</mml:mo> <mml:mo>log</mml:mo> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mn>1</mml:mn> <mml:mo>+</mml:mo> <mml:mo>exp</mml:mo> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:mi>x</mml:mi> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo stretchy="true" form="postfix">]</mml:mo> </mml:mrow> <mml:mi>γ</mml:mi> </mml:msup> <mml:mi>/</mml:mi> <mml:mrow> <mml:mo stretchy="true" form="prefix">[</mml:mo> <mml:mn>1</mml:mn> <mml:mo>+</mml:mo> <mml:mo>exp</mml:mo> <mml:mrow> <mml:mo stretchy="true" form="prefix">(</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mi>x</mml:mi> </mml:mrow> </mml:msup> <mml:mo stretchy="true" form="postfix">)</mml:mo> </mml:mrow> <mml:mo stretchy="true" form="postfix">]</mml:mo> </mml:mrow> </mml:mrow> </mml:math> , to be <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mo>log</mml:mo> <mml:msub> <mml:mi>M</mml:mi> <mml:mn>1</mml:mn> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mn>11.506</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.404</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.325</mml:mn> </mml:mrow> </mml:msubsup> </mml:mrow> </mml:math> , <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mo>log</mml:mo> <mml:mi>ϵ</mml:mi> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:msubsup> <mml:mn>1.632</mml:mn> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.181</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.306</mml:mn> </mml:mrow> </mml:msubsup> </mml:mrow> </mml:math> , <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"> <mml:mrow> <mml:mi>α

  PublisherDOI

• Interacting dark sector within ETHOS: Cosmological constraints from SPT cluster abundance with DES and HST weak lensing data

  Physical review. D/Physical review. D. · 2025-04-24 · 1 citations

  articleOpen access

  We use galaxy cluster abundance measurements from the South Pole Telescope enhanced by multicomponent matched filter confirmation and complemented with mass information obtained using weak-lensing data from Dark Energy Survey Year 3 (DES Y3) and targeted Hubble Space Telescope observations for probing deviations from the cold dark matter paradigm. Concretely, we consider a class of dark sector models featuring interactions between dark matter (DM) and a dark radiation (DR) component within the framework of the effective theory of structure formation (ETHOS). We focus on scenarios that lead to power suppression over a wide range of scales, and thus can be tested with data sensitive to large scales, as realized, for example, for DM–DR interactions following from an unbroken non-Abelian <a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mi>S</a:mi><a:mi>U</a:mi><a:mo stretchy="false">(</a:mo><a:mi>N</a:mi><a:mo stretchy="false">)</a:mo></a:math> gauge theory (interaction rate with power-law index <e:math xmlns:e="http://www.w3.org/1998/Math/MathML" display="inline"><e:mi>n</e:mi><e:mo>=</e:mo><e:mn>0</e:mn></e:math> within the ETHOS parametrization). Cluster abundance measurements are mostly sensitive to the amount of DR interacting with DM, parametrized by the ratio of DR temperature to the cosmic microwave background (CMB) temperature, <g:math xmlns:g="http://www.w3.org/1998/Math/MathML" display="inline"><g:msub><g:mi>ξ</g:mi><g:mi>DR</g:mi></g:msub><g:mo>=</g:mo><g:msub><g:mi>T</g:mi><g:mi>DR</g:mi></g:msub><g:mo>/</g:mo><g:msub><g:mi>T</g:mi><g:mi>CMB</g:mi></g:msub></g:math>. We find an upper limit <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:msub><i:mi>ξ</i:mi><i:mi>DR</i:mi></i:msub><i:mo>&lt;</i:mo><i:mn>17</i:mn><i:mo>%</i:mo></i:math> at 95% credibility. When the cluster data are combined with Planck 2018 CMB data along with baryon acoustic oscillation (BAO) measurements we find <k:math xmlns:k="http://www.w3.org/1998/Math/MathML" display="inline"><k:msub><k:mi>ξ</k:mi><k:mi>DR</k:mi></k:msub><k:mo>&lt;</k:mo><k:mn>10</k:mn><k:mo>%</k:mo></k:math>, corresponding to a limit on the abundance of interacting DR that is around 3 times tighter than that from CMB + BAO data alone. We also discuss the complementarity of weak lensing informed cluster abundance studies with probes sensitive to smaller scales, explore the impact on our analysis of massive neutrinos, and comment on a slight preference for the presence of a nonzero interacting DR abundance, which enables a physical solution to the <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:msub><m:mi>S</m:mi><m:mn>8</m:mn></m:msub></m:math> tension.

  PublisherOA PDFDOI

• High-Significance Detection of Correlation Between the Unresolved Gamma-Ray Background and the Large Scale Cosmic Structure

  Lancaster EPrints (Lancaster University) · 2025-01-17

  preprintOpen access

  Our understanding of the $γ$-ray sky has improved dramatically in the past decade, however, the unresolved $γ$-ray background (UGRB) still has a potential wealth of information about the faintest $γ$-ray sources pervading the Universe. Statistical cross-correlations with tracers of cosmic structure can indirectly identify the populations that most characterize the $γ$-ray background. In this study, we analyze the angular correlation between the $γ$-ray background and the matter distribution in the Universe as traced by gravitational lensing, leveraging more than a decade of observations from the Fermi-Large Area Telescope (LAT) and 3 years of data from the Dark Energy Survey (DES). We detect a correlation at signal-to-noise ratio of 8.9. Most of the statistical significance comes from large scales, demonstrating, for the first time, that a substantial portion of the UGRB aligns with the mass clustering of the Universe as traced by weak lensing. Blazars provide a plausible explanation for this signal, especially if those contributing to the correlation reside in halos of large mass ($\sim 10^{14} M_{\odot}$) and account for approximately 30-40 % of the UGRB above 10 GeV. Additionally, we observe a preference for a curved $γ$-ray energy spectrum, with a log-parabolic shape being favored over a power-law. We also discuss the possibility of modifications to the blazar model and the inclusion of additional $gamma$-ray sources, such as star-forming galaxies or particle dark matter.

  OA PDFDOI

• Multiprobe cosmology from the abundance of SPT clusters and DES galaxy clustering and weak lensing

  Physical review. D/Physical review. D. · 2025-03-14 · 7 citations

  articleOpen access

  Cosmic shear, galaxy clustering, and the abundance of massive halos each probe the large-scale structure of the Universe in complementary ways. We present cosmological constraints from the joint analysis of the three probes, building on the latest analyses of the lensing-informed abundance of clusters identified by the South Pole Telescope (SPT) and of the auto- and cross-correlation of galaxy position and weak lensing measurements (<a:math xmlns:a="http://www.w3.org/1998/Math/MathML" display="inline"><a:mn>3</a:mn><a:mo>×</a:mo><a:mn>2</a:mn><a:mi>pt</a:mi></a:math>) in the Dark Energy Survey (DES). We consider the cosmological correlation between the different tracers and we account for the systematic uncertainties that are shared between the large-scale lensing correlation functions and the small-scale lensing-based cluster mass calibration. Marginalized over the remaining <c:math xmlns:c="http://www.w3.org/1998/Math/MathML" display="inline"><c:mi mathvariant="normal">Λ</c:mi></c:math> cold dark matter (<f:math xmlns:f="http://www.w3.org/1998/Math/MathML" display="inline"><f:mi mathvariant="normal">Λ</f:mi><f:mi>CDM</f:mi></f:math>) parameters (including the sum of neutrino masses) and 52 astrophysical modeling parameters, we measure <i:math xmlns:i="http://www.w3.org/1998/Math/MathML" display="inline"><i:msub><i:mi mathvariant="normal">Ω</i:mi><i:mi mathvariant="normal">m</i:mi></i:msub><i:mo>=</i:mo><i:mn>0.300</i:mn><i:mo>±</i:mo><i:mn>0.017</i:mn></i:math> and <m:math xmlns:m="http://www.w3.org/1998/Math/MathML" display="inline"><m:msub><m:mi>σ</m:mi><m:mn>8</m:mn></m:msub><m:mo>=</m:mo><m:mn>0.797</m:mn><m:mo>±</m:mo><m:mn>0.026</m:mn></m:math>. Compared to constraints from primary cosmic microwave background (CMB) anisotropies, our constraints are only 15% wider with a probability to exceed of 0.22 (<o:math xmlns:o="http://www.w3.org/1998/Math/MathML" display="inline"><o:mn>1.2</o:mn><o:mi>σ</o:mi></o:math>) for the two-parameter difference. We further obtain <q:math xmlns:q="http://www.w3.org/1998/Math/MathML" display="inline"><q:msub><q:mi>S</q:mi><q:mn>8</q:mn></q:msub><q:mo>≡</q:mo><q:msub><q:mi>σ</q:mi><q:mn>8</q:mn></q:msub><q:mo stretchy="false">(</q:mo><q:msub><q:mi mathvariant="normal">Ω</q:mi><q:mi mathvariant="normal">m</q:mi></q:msub><q:mo>/</q:mo><q:mn>0.3</q:mn><q:msup><q:mo stretchy="false">)</q:mo><q:mn>0.5</q:mn></q:msup><q:mo>=</q:mo><q:mn>0.796</q:mn><q:mo>±</q:mo><q:mn>0.013</q:mn></q:math> which is lower than the measurement at the <w:math xmlns:w="http://www.w3.org/1998/Math/MathML" display="inline"><w:mn>1.6</w:mn><w:mi>σ</w:mi></w:math> level. The combined SPT cluster, DES <y:math xmlns:y="http://www.w3.org/1998/Math/MathML" display="inline"><y:mn>3</y:mn><y:mo>×</y:mo><y:mn>2</y:mn><y:mi>pt</y:mi></y:math>, and datasets mildly prefer a nonzero positive neutrino mass, with a 95% upper limit <ab:math xmlns:ab="http://www.w3.org/1998/Math/MathML" display="inline"><ab:mo>∑</ab:mo><ab:msub><ab:mi>m</ab:mi><ab:mi>ν</ab:mi></ab:msub><ab:mo>&lt;</ab:mo><ab:mn>0.25</ab:mn><ab:mtext> </ab:mtext><ab:mtext> </ab:mtext><ab:mi>eV</ab:mi></ab:math> on the sum of neutrino masses. Assuming a <cb:math xmlns:cb="http://www.w3.org/1998/Math/MathML" display="inline"><cb:mi>w</cb:mi><cb:mi>CDM</cb:mi></cb:math> model, we constrain the dark energy equation of state parameter <eb:math xmlns:eb="http://www.w3.org/1998/Math/MathML" display="inline"><eb:mi>w</eb:mi><eb:mo>=</eb:mo><eb:mo>−</eb:mo><eb:mn>1.1</eb:mn><eb:msubsup><eb:mn>5</eb:mn><eb:mrow><eb:mo>−</eb:mo><eb:mn>0.17</eb:mn></eb:mrow><eb:mrow><eb:mo>+</eb:mo><eb:mn>0.23</eb:mn></eb:mrow></eb:msubsup></eb:math> and when combining with primary CMB anisotropies, we recover <gb:math xmlns:gb="http://www.w3.org/1998/Math/MathML" display="inline"><gb:mi>w</gb:mi><gb:mo>=</gb:mo><gb:mo>−</gb:mo><gb:mn>1.2</gb:mn><gb:msubsup><gb:mn>0</gb:mn><gb:mrow><gb:mo>−</gb:mo><gb:mn>0.09</gb:mn></gb:mrow><gb:mrow><gb:mo>+</gb:mo><gb:mn>0.15</gb:mn></gb:mrow></gb:msubsup></gb:math>, a <ib:math xmlns:ib="http://www.w3.org/1998/Math/MathML" display="inline"><ib:mn>1.7</ib:mn><ib:mi>σ</ib:mi></ib:math> difference with a cosmological constant. The precision of our results highlights the benefits of multiwavelength multiprobe cosmology and our analysis paves the way for upcoming joint analyses of next-generation datasets.

  PublisherOA PDFDOI

• Dark Energy Survey Year 6 Results: Clustering-redshifts and importance sampling of Self-Organised-Maps $n(z)$ realizations for $3\times2$pt samples

  arXiv (Cornell University) · 2025-01-01

  articleOpen access

  International audience

  PublisherOA PDF

• High-significance detection of correlation between the unresolved gamma-ray background and the large-scale cosmic structure

  Journal of Cosmology and Astroparticle Physics · 2025-06-01 · 3 citations

  articleOpen access

  Abstract Our understanding of the γ -ray sky has improved dramatically in the past decade, however, the unresolved γ -ray background (UGRB) still has a potential wealth of information about the faintest γ -ray sources pervading the Universe. Statistical cross-correlations with tracers of cosmic structure can indirectly identify the populations that most characterize the γ -ray background. In this study, we analyze the angular correlation between the γ -ray background and the matter distribution in the Universe as traced by gravitational lensing, leveraging more than a decade of observations from the Fermi -Large Area Telescope (LAT) and 3 years of data from the Dark Energy Survey (DES). We detect a correlation at signal-to-noise ratio of 8.9. Most of the statistical significance comes from large scales, demonstrating, for the first time, that a substantial portion of the UGRB aligns with the mass clustering of the Universe as traced by weak lensing. Blazars provide a plausible explanation for this signal, especially if those contributing to the correlation reside in halos of large mass (∼ 10 14 M ⊙ ) and account for approximately 30–40% of the UGRB above 10 GeV. Additionally, we observe a preference for a curved γ -ray energy spectrum, with a log-parabolic shape being favored over a power-law. We also discuss the possibility of modifications to the blazar model and the inclusion of additional γ -ray sources, such as star-forming galaxies, misalinged active galactic nuclei, or particle dark matter.

  PublisherDOI

• Dark energy survey year 3 results: cosmology from galaxy clustering and galaxy–galaxy lensing in harmonic space

  Monthly Notices of the Royal Astronomical Society · 2024-11-30 · 18 citations

  articleOpen access

  ABSTRACT We present the joint tomographic analysis of galaxy-galaxy lensing and galaxy clustering in harmonic space (HS), using galaxy catalogues from the first three years of observations by the Dark Energy Survey (DES Y3). We utilize the redMaGiC and MagLim catalogues as lens galaxies and the metacalibration catalogue as source galaxies. The measurements of angular power spectra are performed using the pseudo-$C_\ell$ method, and our theoretical modelling follows the fiducial analyses performed by DES Y3 in configuration space, accounting for galaxy bias, intrinsic alignments, magnification bias, shear magnification bias and photometric redshift uncertainties. We explore different approaches for scale cuts based on non-linear galaxy bias and baryonic effects contamination. Our fiducial covariance matrix is computed analytically, accounting for mask geometry in the Gaussian term, and including non-Gaussian contributions and super-sample covariance terms. To validate our HS pipelines and covariance matrix, we used a suite of 1800 log-normal simulations. We also perform a series of stress tests to gauge the robustness of our HS analysis. In the $\Lambda$CDM model, the clustering amplitude $S_8 =\sigma _8(\Omega _m/0.3)^{0.5}$ is constrained to $S_8 = 0.704\pm 0.029$ and $S_8 = 0.753\pm 0.024$ (68 per cent C.L.) for the redMaGiC and MagLim catalogues, respectively. For the wCDM, the dark energy equation of state is constrained to $w = -1.28 \pm 0.29$ and $w = -1.26^{+0.34}_{-0.27}$, for redMaGiC and MagLim catalogues, respectively. These results are compatible with the corresponding DES Y3 results in configuration space and pave the way for HS analyses using the DES Y6 data.

  PublisherDOI

• SPT clusters with DES and HST weak lensing. II. Cosmological constraints from the abundance of massive halos

  Physical review. D/Physical review. D. · 2024-10-03 · 62 citations

  articleOpen access

  In these two papers, the authors use mock maps to establish a method for studying the abundance and calibrating the weak-lensing based mass of galaxy clusters. They set up a likelihood function, thus obtaining cosmological constraints from a sample of 1,005 clusters detected with the South Pole Telescope, in combination with further cluster data from the Dark Energy Survey, the Wide-field Infrared Survey Explorer, and the Hubble Space Telescope.

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Frequent coauthors

• L. N. da Costa

  Laboratório Interinstitucional de e-Astronomia

  1998 shared

• D. Gruen

  1898 shared

• A. Carnero Rosell

  1882 shared

• E. Bertin

  Orange (France)

  1874 shared

• M. A. G. Maia

  Laboratório Interinstitucional de e-Astronomia

  1453 shared

• R. Miquel

  Institute for High Energy Physics

  1403 shared

• J. Gschwend

  Laboratório Interinstitucional de e-Astronomia

  1353 shared

• K. Kuehn

  Netherlands Institute for Radio Astronomy

  1316 shared

Labs

• Disruption LabPI

Education

• PhD, Astronomy

  University of Illinois at Urbana-Champaign

  2014

Awards & honors

• Deloitte Foundation Center for Business Analytics Scholar, U…