Showing papers by "IFAE published in 2021"
TL;DR: In this article, the population of 47 compact binary mergers detected with a false-alarm rate of 0.614 were dynamically assembled, and the authors found that the BBH rate likely increases with redshift, but not faster than the star formation rate.
Abstract: We report on the population of 47 compact binary mergers detected with a false-alarm rate of 0.01 are dynamically assembled. Third, we estimate merger rates, finding RBBH = 23.9-+8.614.3 Gpc-3 yr-1 for BBHs and RBNS = 320-+240490 Gpc-3 yr-1 for binary neutron stars. We find that the BBH rate likely increases with redshift (85% credibility) but not faster than the star formation rate (86% credibility). Additionally, we examine recent exceptional events in the context of our population models, finding that the asymmetric masses of GW190412 and the high component masses of GW190521 are consistent with our models, but the low secondary mass of GW190814 makes it an outlier.
468 citations
Stanford University1, Fermilab2, University of Wisconsin-Madison3, University of Southern California4, University of Texas at Austin5, Carnegie Mellon University6, Princeton University7, Texas A&M University8, Autonomous University of Madrid9, Rutgers University10, Max Planck Society11, Ohio State University12, University of Pennsylvania13, University of São Paulo14, University College London15, University of Illinois at Urbana–Champaign16, IFAE17, INAF18, Indian Institute of Technology, Hyderabad19, Santa Cruz Institute for Particle Physics20, University of Michigan21, University of Queensland22, Smithsonian Institution23, University of Arizona24, Macquarie University25, National Center for Supercomputing Applications26, University of Sussex27, University of Southampton28, Brandeis University29, Oak Ridge National Laboratory30
TL;DR: This analysis fully incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and marginalizes over uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk.
Abstract: We perform a comprehensive study of Milky Way (MW) satellite galaxies to constrain the fundamental properties of dark matter (DM). This analysis fully incorporates inhomogeneities in the spatial distribution and detectability of MW satellites and marginalizes over uncertainties in the mapping between galaxies and DM halos, the properties of the MW system, and the disruption of subhalos by the MW disk. Our results are consistent with the cold, collisionless DM paradigm and yield the strongest cosmological constraints to date on particle models of warm, interacting, and fuzzy dark matter. At 95% confidence, we report limits on (i) the mass of thermal relic warm DM, mWDM>6.5 keV (free-streaming length, λfs≲10h-1 kpc), (ii) the velocity-independent DM-proton scattering cross section, σ0 2.9×10-21 eV (de Broglie wavelength, λdB≲0.5 kpc). These constraints are complementary to other observational and laboratory constraints on DM properties.
164 citations
TL;DR: In this article, the ATLAS particle-flow reconstruction method is used to reconstruct the topo-clusters of the proton-proton collision data with a center-of-mass energy of 13$ TeV collected by the LHC.
Abstract: Jet energy scale and resolution measurements with their associated uncertainties are reported for jets using 36-81 fb$^{-1}$ of proton-proton collision data with a centre-of-mass energy of $\sqrt{s}=13$ TeV collected by the ATLAS detector at the LHC. Jets are reconstructed using two different input types: topo-clusters formed from energy deposits in calorimeter cells, as well as an algorithmic combination of charged-particle tracks with those topo-clusters, referred to as the ATLAS particle-flow reconstruction method. The anti-$k_t$ jet algorithm with radius parameter $R=0.4$ is the primary jet definition used for both jet types. Jets are initially calibrated using a sequence of simulation-based corrections. Next, several $\textit{in situ}$ techniques are employed to correct for differences between data and simulation and to measure the resolution of jets. The systematic uncertainties in the jet energy scale for central jets ($|\eta| 2.5$ TeV). The relative jet energy resolution is measured and ranges from ($24 \pm 1.5$)% at 20 GeV to ($6 \pm 0.5$)% at 300 GeV.
131 citations
IFAE1
TL;DR: In this article, the LIGO-Virgo data were analyzed to test a hypothesis that the data contains more than one population of black holes, and a maximum likelihood analysis including a population of astrophysical black holes with a truncated power-law mass function whose merger rate follows from star formation rate was performed.
Abstract: We analyse the LIGO-Virgo data, including the recently released GWTC-2 dataset, to test a hypothesis that the data contains more than one population of black holes. We perform a maximum likelihood analysis including a population of astrophysical black holes with a truncated power-law mass function whose merger rate follows from star formation rate, and a population of primordial black holes for which we consider log-normal and critical collapse mass functions. We find that primordial black holes alone are strongly disfavoured by the data, while the best fit is obtained for the template combining astrophysical and primordial merger rates. Alternatively, the data may hint towards two different astrophysical black hole populations. We also update the constraints on primordial black hole abundance from LIGO-Virgo observations finding that in the $2-400 M_{\odot}$ mass range, they must comprise less than 0.2% of dark matter.
109 citations
University of Texas at Austin1, Université Paris-Saclay2, Goethe University Frankfurt3, Korea Institute for Advanced Study4, Université de Sherbrooke5, Canadian Institute for Advanced Research6, Graz University of Technology7, Spanish National Research Council8, École Normale Supérieure9, École Polytechnique Fédérale de Lausanne10, Eindhoven University of Technology11, University of Copenhagen12, IFAE13, University of Grenoble14, Max Planck Society15, University of Chile16, University of Minnesota17, Indian Institute of Technology Bombay18, Aix-Marseille University19, Cornell University20, Universidade Federal do ABC21
TL;DR: For a snapshot of the most recent developments in the field, and to identify outstanding challenges and emerging opportunities, the Quantum Materials Roadmap collection as mentioned in this paper is a collection of experts in each discipline sharing their viewpoint and articulate their vision for quantum materials.
Abstract: In recent years, the notion of "Quantum Materials" has emerged as a powerful unifying concept across diverse fields of science and engineering, from condensed-matter and cold-atom physics to materials science and quantum computing. Beyond traditional quantum materials such as unconventional superconductors, heavy fermions, and multiferroics, the field has significantly expanded to encompass topological quantum matter, two-dimensional materials and their van der Waals heterostructures, Moire materials, Floquet time crystals, as well as materials and devices for quantum computation with Majorana fermions. In this Roadmap collection we aim to capture a snapshot of the most recent developments in the field, and to identify outstanding challenges and emerging opportunities. The format of the Roadmap, whereby experts in each discipline share their viewpoint and articulate their vision for quantum materials, reflects the dynamic and multifaceted nature of this research area, and is meant to encourage exchanges and discussions across traditional disciplinary boundaries. It is our hope that this collective vision will contribute to sparking new fascinating questions and activities at the intersection of materials science, condensed matter physics, device engineering, and quantum information, and to shaping a clearer landscape of quantum materials science as a new frontier of interdisciplinary scientific inquiry.
102 citations
TL;DR: In this article, a catalog of 4195 optically confirmed galaxy clusters detected with signal-to-noise ratio >4 in 13,211 deg2 of sky surveyed by the Atacama Cosmology Telescope (ACT) is presented.
Abstract: We present a catalog of 4195 optically confirmed Sunyaev–Zel’dovich (SZ) selected galaxy clusters detected with signal-to-noise ratio >4 in 13,211 deg2 of sky surveyed by the Atacama Cosmology Telescope (ACT). Cluster candidates were selected by applying a multifrequency matched filter to 98 and 150 GHz maps constructed from ACT observations obtained from 2008 to 2018 and confirmed using deep, wide-area optical surveys. The clusters span the redshift range 0.04 1 clusters, and a total of 868 systems are new discoveries. Assuming an SZ signal versus mass-scaling relation calibrated from X-ray observations, the sample has a 90% completeness mass limit of M500c > 3.8 × 1014 Me, evaluated at z = 0.5, for clusters detected at signal-to-noise ratio >5 in maps filtered at an angular scale of 2 4. The survey has a large overlap with deep optical weak-lensing surveys that are being used to calibrate the SZ signal mass-scaling relation, such as the Dark Energy Survey (4566 deg2), the Hyper Suprime-Cam Subaru Strategic Program (469 deg2), and the Kilo Degree Survey (825 deg2). We highlight some noteworthy objects in the sample, including potentially projected systems, clusters with strong lensing features, clusters with active central galaxies or star formation, and systems of multiple clusters that may be physically associated. The cluster catalog will be a useful resource for future cosmological analyses and studying the evolution of the intracluster medium and galaxies in massive clusters over the past 10 Gyr.
100 citations
TL;DR: In this paper, the authors describe the muon reconstruction and identification efficiency obtained by the ATLAS experiment for 139.5 million collision data collected between 2015 and 2018 during Run 2 of the LHC, and show that the improved and newly developed algorithms were deployed to preserve high muon identification efficiency with a low misidentification rate and good momentum resolution.
Abstract: This article documents the muon reconstruction and identification efficiency obtained by the ATLAS experiment for 139 $$\hbox {fb}^{-1}$$
fb
-
1
of pp collision data at $$\sqrt{s}=13$$
s
=
13
TeV collected between 2015 and 2018 during Run 2 of the LHC. The increased instantaneous luminosity delivered by the LHC over this period required a reoptimisation of the criteria for the identification of prompt muons. Improved and newly developed algorithms were deployed to preserve high muon identification efficiency with a low misidentification rate and good momentum resolution. The availability of large samples of $$Z\rightarrow \mu \mu $$
Z
→
μ
μ
and $$J/\psi \rightarrow \mu \mu $$
J
/
ψ
→
μ
μ
decays, and the minimisation of systematic uncertainties, allows the efficiencies of criteria for muon identification, primary vertex association, and isolation to be measured with an accuracy at the per-mille level in the bulk of the phase space, and up to the percent level in complex kinematic configurations. Excellent performance is achieved over a range of transverse momenta from 3 GeV to several hundred GeV, and across the full muon detector acceptance of $$|\eta |<2.7$$
|
η
|
<
2.7
.
86 citations
TL;DR: In this paper, the authors provide an updated assessment of the power of the Cherenkov Telescope Array (CTA) to search for thermally produced dark matter at the TeV scale via the associated gamma-ray signal from pair-annihilating dark matter particles in the region around the Galactic centre.
Abstract: We provide an updated assessment of the power of the Cherenkov Telescope Array (CTA) to search for thermally produced dark matter at the TeV scale, via the associated gamma-ray signal from pair-annihilating dark matter particles in the region around the Galactic centre. We find that CTA will open a new window of discovery potential, significantly extending the range of robustly testable models given a standard cuspy profile of the dark matter density distribution. Importantly, even for a cored profile, the projected sensitivity of CTA will be sufficient to probe various well-motivated models of thermally produced dark matter at the TeV scale. This is due to CTA's unprecedented sensitivity, angular and energy resolutions, and the planned observational strategy. The survey of the inner Galaxy will cover a much larger region than corresponding previous observational campaigns with imaging atmospheric Cherenkov telescopes. CTA will map with unprecedented precision the large-scale diffuse emission in high-energy gamma rays, constituting a background for dark matter searches for which we adopt state-of-the-art models based on current data. Throughout our analysis, we use up-to-date event reconstruction Monte Carlo tools developed by the CTA consortium, and pay special attention to quantifying the level of instrumental systematic uncertainties, as well as background template systematic errors, required to probe thermally produced dark matter at these energies.
70 citations
TL;DR: In this article, the authors search for gravitational-wave signals produced by cosmic strings in the Advanced LIGO and Virgo full O3 dataset and obtain results for the first time that kink-kink collisions do not yield a detection.
Abstract: We search for gravitational-wave signals produced by cosmic strings in the Advanced LIGO and Virgo full O3 dataset Search results are presented for gravitational waves produced by cosmic string loop features such as cusps, kinks, and, for the first time, kink-kink collisions A template-based search for short-duration transient signals does not yield a detection We also use the stochastic gravitational-wave background energy density upper limits derived from the O3 data to constrain the cosmic string tension Gμ as a function of the number of kinks, or the number of cusps, for two cosmic string loop distribution models Additionally, we develop and test a third model that interpolates between these two models Our results improve upon the previous LIGO-Virgo constraints on Gμ by 1 to 2 orders of magnitude depending on the model that is tested In particular, for the one-loop distribution model, we set the most competitive constraints to date: Gμ≲4×10^{-15} In the case of cosmic strings formed at the end of inflation in the context of grand unified theories, these results challenge simple inflationary models
62 citations
TL;DR: EuclidEmulator2 as mentioned in this paper is a fast and accurate predictor for the nonlinear correction of the matter power spectrum in the eight-dimensional parameter space of w0waCDM+∑mν models between redshift z = 0 and z = 3 for spatial scales within the range 0.01hMpc−1.
Abstract: We present a new, updated version of the EuclidEmulator (called EuclidEmulator2), a fast and accurate predictor for the nonlinear correction of the matter power spectrum. 2 per cent level accurate emulation is now supported in the eight-dimensional parameter space of w0waCDM+∑mν models between redshift z = 0 and z = 3 for spatial scales within the range 0.01hMpc−1≤k≤10hMpc−1. In order to achieve this level of accuracy, we have had to improve the quality of the underlying N-body simulations used as training data: (i) we use self-consistent linear evolution of non-dark matter species such as massive neutrinos, photons, dark energy, and the metric field, (ii) we perform the simulations in the so-called N-body gauge, which allows one to interpret the results in the framework of general relativity, (iii) we run over 250 high-resolution simulations with 30003 particles in boxes of 1(h−1 Gpc)3 volumes based on paired-and-fixed initial conditions, and (iv) we provide a resolution correction that can be applied to emulated results as a post-processing step in order to drastically reduce systematic biases on small scales due to residual resolution effects in the simulations. We find that the inclusion of the dynamical dark energy parameter wa significantly increases the complexity and expense of creating the emulator. The high fidelity of EuclidEmulator2 is tested in various comparisons against N-body simulations as well as alternative fast predictors such as HALOFIT, HMCode, and CosmicEmu. A blind test is successfully performed against the Euclid Flagship v2.0 simulation. Nonlinear correction factors emulated with EuclidEmulator2 are accurate at the level of 1 per cent or better for 0.01hMpc−1≤k≤10hMpc−1 and z ≤ 3 compared to high-resolution dark-matter-only simulations. EuclidEmulator2 is publicly available at https://github.com/miknab/EuclidEmulator2.
61 citations
TL;DR: In this paper, the Higgs boson properties in the four-lepton decay channel (where lepton = e, mu) were studied using 139 fb(-1) of proton-proton collision data recorded at v s =13 TeV by the ATLAS experiment at the Lar...
Abstract: Higgs boson properties are studied in the fourlepton decay channel (where lepton = e, mu) using 139 fb(-1) of proton-proton collision data recorded at v s =13 TeV by the ATLAS experiment at the Lar ...
IFAE1, Brookhaven National Laboratory2, Stanford University3, Argonne National Laboratory4, Duke University5, Ohio State University6, University of Pennsylvania7, State University of Campinas8, University of Manchester9, SLAC National Accelerator Laboratory10, California Institute of Technology11, University of Chicago12, Spanish National Research Council13, Princeton University14, University of Edinburgh15, University of São Paulo16, Fermilab17, Autonomous University of Madrid18, Institute of Cosmology and Gravitation, University of Portsmouth19, Institut d'Astrophysique de Paris20, University of Sussex21, University College London22, University of La Laguna23, University of Illinois at Urbana–Champaign24, National Center for Supercomputing Applications25, University of Nottingham26, INAF27, University of Queensland28, Indian Institute of Technology, Hyderabad29, Ludwig Maximilian University of Munich30, Santa Cruz Institute for Particle Physics31, University of Oslo32, University of Michigan33, University of Cambridge34, University of Geneva35, Max Planck Society36, Smithsonian Institution37, University of Arizona38, Texas A&M University39, Catalan Institution for Research and Advanced Studies40, University of Wisconsin-Madison41, Carnegie Mellon University42, University of Southampton43, Oak Ridge National Laboratory44
TL;DR: In this paper, the authors present and characterize the galaxy shape catalogue from the first 3 years of the DES observations, over an effective area of 4143 deg2 of the southern sky.
Abstract: We present and characterize the galaxy shape catalogue from the first 3 yr of Dark Energy Survey (DES) observations, over an effective area of 4143 deg2 of the southern sky. We describe our data analysis process and our self-calibrating shear measurement pipeline metacalibration, which builds and improves upon the pipeline used in the DES Year 1 analysis in several aspects. The DES Year 3 weak-lensing shape catalogue consists of 100 204 026 galaxies, measured in the riz bands, resulting in a weighted source number density of neff = 5.59 gal arcmin-2 and corresponding shape noise σe = 0.261. We perform a battery of internal null tests on the catalogue, including tests on systematics related to the point spread function (PSF) modelling, spurious catalogue B-mode signals, catalogue contamination, and galaxy properties.
TL;DR: In this paper, a search for charged Higgs bosons decaying into W±W± or W±Z bosons is performed, involving experimental signatures with two leptons of the same charge, or three or four lepton with a variety of charge combinations, missing transverse momentum and jets.
Abstract: A search for charged Higgs bosons decaying into W±W± or W±Z bosons is performed, involving experimental signatures with two leptons of the same charge, or three or four leptons with a variety of charge combinations, missing transverse momentum and jets. A data sample of proton-proton collisions at a centre-of-mass energy of 13 TeV recorded with the ATLAS detector at the Large Hadron Collider between 2015 and 2018 is used. The data correspond to a total integrated luminosity of 139 fb−1. The search is guided by a type-II seesaw model that extends the scalar sector of the Standard Model with a scalar triplet, leading to a phenomenology that includes doubly and singly charged Higgs bosons. Two scenarios are explored, corresponding to the pair production of doubly charged H±± bosons, or the associated production of a doubly charged H±± boson and a singly charged H± boson. No significant deviations from the Standard Model predictions are observed. H±± bosons are excluded at 95% confidence level up to 350 GeV and 230 GeV for the pair and associated production modes, respectively. [Figure not available: see fulltext.]
TL;DR: In this article, a search for supersymmetric partners of quarks and gluons (squarks, gluinos) in final states containing jets and missing transverse momentum, but no electrons or muons, is presented.
Abstract: A search for the supersymmetric partners of quarks and gluons (squarks and gluinos) in final states containing jets and missing transverse momentum, but no electrons or muons, is presented. The data used in this search were recorded by the ATLAS experiment in proton-proton collisions at a centre-of-mass energy of $\sqrt{s}$ = 13 TeV during Run 2 of the Large Hadron Collider, corresponding to an integrated luminosity of 139 fb$^{-1}$. The results are interpreted in the context of various $R$-parity-conserving models where squarks and gluinos are produced in pairs or in association and a neutralino is the lightest supersymmetric particle. An exclusion limit at the 95% confidence level on the mass of the gluino is set at 2.30 TeV for a simplified model containing only a gluino and the lightest neutralino, assuming the latter is massless. For a simplified model involving the strong production of mass-degenerate first- and second-generation squarks, squark masses below 1.85 TeV are excluded if the lightest neutralino is massless. These limits extend substantially beyond the region of supersymmetric parameter space excluded previously by similar searches with the ATLAS detector.
University of Cambridge1, Spanish National Research Council2, University of Michigan3, Fermilab4, University of Arizona5, California Institute of Technology6, University of Chicago7, Stanford University8, University of Hawaii9, Ohio State University10, Argonne National Laboratory11, University of Wisconsin-Madison12, University of Pennsylvania13, SLAC National Accelerator Laboratory14, Carnegie Mellon University15, University of La Laguna16, University of Illinois at Urbana–Champaign17, National Center for Supercomputing Applications18, University of Manchester19, University of California, Berkeley20, Santa Cruz Institute for Particle Physics21, University College London22, IFAE23, University of Geneva24, Brookhaven National Laboratory25, Duke University26, University of São Paulo27, Autonomous University of Madrid28, Institute of Cosmology and Gravitation, University of Portsmouth29, Institut d'Astrophysique de Paris30, University of Sussex31, INAF32, Indian Institute of Technology, Hyderabad33, University of Oslo34, University of Queensland35, Smithsonian Institution36, Lowell Observatory37, Macquarie University38, Catalan Institution for Research and Advanced Studies39, Princeton University40, University of Southampton41, Oak Ridge National Laboratory42, Max Planck Society43, Ludwig Maximilian University of Munich44
TL;DR: In this article, a fiducial covariance matrix model for the combined 2-point function analysis of the Dark Energy Survey Year 3 (DES-Y3) dataset is presented.
Abstract: We describe and test the fiducial covariance matrix model for the combined 2-point function analysis of the Dark Energy Survey Year 3 (DES-Y3) dataset. Using a variety of new ansatzes for covariance modelling and testing we validate the assumptions and approximations of this model. These include the assumption of a Gaussian likelihood, the trispectrum contribution to the covariance, the impact of evaluating the model at a wrong set of parameters, the impact of masking and survey geometry, deviations from Poissonian shot-noise, galaxy weighting schemes and other, sub-dominant effects. We find that our covariance model is robust and that its approximations have little impact on goodness-of-fit and parameter estimation. The largest impact on best-fit figure-of-merit arises from the so-called $f_{\mathrm{sky}}$ approximation for dealing with finite survey area, which on average increases the $\chi^2$ between maximum posterior model and measurement by $3.7\%$ ($\Delta \chi^2 \approx 18.9$). Standard methods to go beyond this approximation fail for DES-Y3, but we derive an approximate scheme to deal with these features. For parameter estimation, our ignorance of the exact parameters at which to evaluate our covariance model causes the dominant effect. We find that it increases the scatter of maximum posterior values for $\Omega_m$ and $\sigma_8$ by about $3\%$ and for the dark energy equation of state parameter by about $5\%$.
University of Texas at Austin1, Université Paris-Saclay2, Goethe University Frankfurt3, Korea Institute for Advanced Study4, Canadian Institute for Advanced Research5, Université de Sherbrooke6, Graz University of Technology7, Spanish National Research Council8, École Normale Supérieure9, École Polytechnique Fédérale de Lausanne10, Eindhoven University of Technology11, University of Copenhagen12, IFAE13, University of Grenoble14, Max Planck Society15, University of Chile16, University of Minnesota17, Indian Institute of Technology Bombay18, Aix-Marseille University19, Cornell University20, Universidade Federal do ABC21
TL;DR: The Quantum Materials Roadmap collection as discussed by the authors provides a snapshot of the most recent developments in the field, and identifies outstanding challenges and emerging opportunities in quantum materials science, as well as an overview of the current state of the art.
Abstract: In recent years, the notion of Quantum Materials has emerged as a powerful unifying concept across diverse fields of science and engineering, from condensed-matter and cold atom physics to materials science and quantum computing. Beyond traditional quantum materials such as unconventional superconductors, heavy fermions, and multiferroics, the field has significantly expanded to encompass topological quantum matter, two-dimensional materials and their van der Waals heterostructures, Moire materials, Floquet time crystals, as well as materials and devices for quantum computation with Majorana fermions. In this Roadmap collection we aim to capture a snapshot of the most recent developments in the field, and to identify outstanding challenges and emerging opportunities. The format of the Roadmap, whereby experts in each discipline share their viewpoint and articulate their vision for quantum materials, reflects the dynamic and multifaceted nature of this research area, and is meant to encourage exchanges and discussions across traditional disciplinary boundaries. It is our hope that this collective vision will contribute to sparking new fascinating questions and activities at the intersection of materials science, condensed matter physics, device engineering, and quantum information, and to shaping a clearer landscape of quantum materials science as a new frontier of interdisciplinary scientific inquiry.
TL;DR: In this paper, the authors present catalogues of stellar masses, star formation rates, and ancillary stellar population parameters for galaxies spanning $0 2.6$ and show evidence of a bend in the relation at low redshifts.
Abstract: We present catalogues of stellar masses, star formation rates, and ancillary stellar population parameters for galaxies spanning $0 2.6$, we see evidence of a bend in the relation at low redshifts ($z<0.45$). This suggests evolution in both the normalisation and shape of the SFR-$M_\star$ relation since cosmic noon. It is significant that we only clearly see this bend when combining our new DEVILS measurements with consistently derived values for lower redshift galaxies from the Galaxy And Mass Assembly (GAMA) survey: this shows the power of having consistent treatment for galaxies at all redshifts.
Spanish National Research Council1, Ohio State University2, University of La Laguna3, University of Wisconsin-Madison4, University of Arizona5, University of Oslo6, University of Michigan7, University of São Paulo8, Fermilab9, Stanford University10, Autonomous University of Madrid11, Institut d'Astrophysique de Paris12, Pierre-and-Marie-Curie University13, University of Sussex14, University of Manchester15, University College London16, University of Illinois at Urbana–Champaign17, IFAE18, Indian Institute of Technology, Hyderabad19, University of Chicago20, University of Pennsylvania21, California Institute of Technology22, University of Cambridge23, University of Geneva24, University of Queensland25, University of California, Santa Cruz26, Ludwig Maximilian University of Munich27, Max Planck Society28, Harvard University29, Lowell Observatory30, Macquarie University31, Texas A&M University32, Princeton University33, Carnegie Mellon University34, University of Southampton35, Oak Ridge National Laboratory36
TL;DR: In this paper, the authors investigate the potential gains in cosmological constraints from the combination of galaxy clustering and galaxy-galaxy lensing by optimizing the lens galaxy sample selection using information from DES Year 3 data and assuming the DES Year 1 metacalibration sample for the sources.
Abstract: We investigate potential gains in cosmological constraints from the combination of galaxy clustering and galaxy-galaxy lensing by optimizing the lens galaxy sample selection using information from Dark Energy Survey (DES) Year 3 data and assuming the DES Year 1 metacalibration sample for the sources. We explore easily reproducible selections based on magnitude cuts in i-band as a function of (photometric) redshift, zphot, and benchmark the potential gains against those using the well-established redMaGiC [E. Rozo et al., Mon. Not. R. Astron. Soc. 461, 1431 (2016)MNRAA40035-871110.1093/mnras/stw1281] sample. We focus on the balance between density and photometric redshift accuracy, while marginalizing over a realistic set of cosmological and systematic parameters. Our optimal selection, the MagLim sample, satisfies i<4zphot+18 and has ∼30% wider redshift distributions but ∼3.5 times more galaxies than redMaGiC. Assuming a wCDM model (i.e. with a free parameter for the dark energy equation of state) and equivalent scale cuts to mitigate nonlinear effects, this leads to 40% increase in the figure of merit for the pair combinations of ωm, w, and σ8, and gains of 16% in σ8, 10% in ωm, and 12% in w. Similarly, in ΛCDM, we find an improvement of 19% and 27% on σ8 and ωm, respectively. We also explore flux-limited samples with a flat magnitude cut finding that the optimal selection, i<22.2, has ∼7 times more galaxies and ∼20% wider redshift distributions compared to MagLim, but slightly worse constraints. We show that our results are robust with respect to the assumed galaxy bias and photometric redshift uncertainties with only moderate further gains from increased number of tomographic bins or the inclusion of bin cross-correlations, except in the case of the flux-limited sample, for which these gains are more significant.
Stanford University1, University of Arizona2, Ohio State University3, INAF4, Argonne National Laboratory5, University of Pennsylvania6, Ludwig Maximilian University of Munich7, University of Manchester8, University of Wisconsin-Madison9, University of California, Berkeley10, University of Chicago11, University of Michigan12, University of Cambridge13, IFAE14, University of Geneva15, Carnegie Mellon University16, Brookhaven National Laboratory17, Duke University18, Max Planck Society19, Fermilab20, University of Edinburgh21, University of São Paulo22, Autonomous University of Madrid23, Institut d'Astrophysique de Paris24, University of Sussex25, University College London26, Spanish National Research Council27, University of Illinois at Urbana–Champaign28, University of Queensland29, Indian Institute of Technology, Hyderabad30, Santa Cruz Institute for Particle Physics31, University of Oslo32, Smithsonian Institution33, Macquarie University34, Texas A&M University35, Princeton University36, University of Southampton37, Oak Ridge National Laboratory38, National Center for Supercomputing Applications39, Institute of Cosmology and Gravitation, University of Portsmouth40
TL;DR: This analysis is an important advance in both optical cluster cosmology and multiprobe analyses of upcoming wide imaging surveys and finds improved constraints on cosmological parameters as well as on the cluster observable-mass scaling relation.
Abstract: We present the first joint analysis of cluster abundances and auto or cross-correlations of three cosmic tracer fields: galaxy density, weak gravitational lensing shear, and cluster density split by optical richness. From a joint analysis (4×2pt+N) of cluster abundances, three cluster cross-correlations, and the auto correlations of the galaxy density measured from the first year data of the Dark Energy Survey, we obtain ωm=0.305-0.038+0.055 and σ8=0.783-0.054+0.064. This result is consistent with constraints from the DES-Y1 galaxy clustering and weak lensing two-point correlation functions for the flat νΛCDM model. Consequently, we combine cluster abundances and all two-point correlations from across all three cosmic tracer fields (6×2pt+N) and find improved constraints on cosmological parameters as well as on the cluster observable-mass scaling relation. This analysis is an important advance in both optical cluster cosmology and multiprobe analyses of upcoming wide imaging surveys.
TL;DR: In this article, a measurement of light-by-light scattering based on Pb+Pb collision data recorded by the ATLAS experiment during Run 2 of the LHC is described.
Abstract: This paper describes a measurement of light-by-light scattering based on Pb+Pb collision data recorded by the ATLAS experiment during Run 2 of the LHC. The study uses 2.2 nb$^{−1}$ of integrated luminosity collected in 2015 and 2018 at $ \sqrt{s_{\mathrm{NN}}} $ = 5.02 TeV. Light-by-light scattering candidates are selected in events with two photons produced exclusively, each with transverse energy $ {E}_{\mathrm{T}}^{\gamma } $> 2.5 GeV, pseudorapidity |η$_{γ}$| 5 GeV, and with small diphoton transverse momentum and diphoton acoplanarity. The integrated and differential fiducial cross sections are measured and compared with theoretical predictions. The diphoton invariant mass distribution is used to set limits on the production of axion-like particles. This result provides the most stringent limits to date on axion-like particle production for masses in the range 6–100 GeV. Cross sections above 2 to 70 nb are excluded at the 95% CL in that mass interval.[graphic not available: see fulltext]
TL;DR: In this article, the anomalous magnetic moment of electron (a e ) and muon (a μ ) was explained in terms of an Aligned 2-Higgs Doublet Model with right-handed neutrinos.
University of Southampton1, University of Lyon2, Smithsonian Institution3, University of Pennsylvania4, University of Queensland5, Institute of Cosmology and Gravitation, University of Portsmouth6, University of Granada7, University of Chicago8, Australian National University9, University of Auvergne10, Duke University11, University of Texas at Austin12, University of São Paulo13, Fermilab14, Autonomous University of Madrid15, Institut d'Astrophysique de Paris16, University College London17, SLAC National Accelerator Laboratory18, Stanford University19, University of La Laguna20, Spanish National Research Council21, University of Illinois at Urbana–Champaign22, National Center for Supercomputing Applications23, IFAE24, INAF25, Indian Institute of Technology, Hyderabad26, Santa Cruz Institute for Particle Physics27, University of Oslo28, California Institute of Technology29, University of Michigan30, Ohio State University31, Lawrence Berkeley National Laboratory32, Macquarie University33, Lowell Observatory34, Texas A&M University35, Radcliffe Institute for Advanced Study36, Catalan Institution for Research and Advanced Studies37, University of Wisconsin-Madison38, University of Cambridge39, Princeton University40, University of Sussex41, Complutense University of Madrid42, Oak Ridge National Laboratory43, Max Planck Society44
TL;DR: In this paper, the authors examined the host galaxies of SNe Ia in the Dark Energy Survey three-year spectroscopically-confirmed cosmological sample, obtaining photometry in a series of local apertures centred on the SN, and for the global host galaxy.
Abstract: Analyses of type Ia supernovae (SNe Ia) have found puzzling correlations between their standardised luminosities and host galaxy properties: SNe Ia in high-mass, passive hosts appear brighter than those in lower-mass, star-forming hosts. We examine the host galaxies of SNe Ia in the Dark Energy Survey three-year spectroscopically-confirmed cosmological sample, obtaining photometry in a series of ‘local’ apertures centred on the SN, and for the global host galaxy. We study the differences in these host galaxy properties, such as stellar mass and rest-frame U − R colours, and their correlations with SN Ia parameters including Hubble residuals. We find all Hubble residual steps to be >3σ in significance, both for splitting at the traditional environmental property sample median and for the step of maximum significance. For stellar mass, we find a maximal local step of 0.098 ± 0.018 mag; ∼0.03 mag greater than the largest global stellar mass step in our sample (0.070 ± 0.017 mag). When splitting at the sample median, differences between local and global U − R steps are small, both ∼0.08 mag, but are more significant than the global stellar mass step (0.057 ± 0.017 mag). We split the data into sub-samples based on SN Ia light curve parameters: stretch (x1) and colour (c), finding that redder objects (c > 0) have larger Hubble residual steps, for both stellar mass and U − R, for both local and global measurements, of ∼0.14 mag. Additionally, the bluer (star-forming) local environments host a more homogeneous SN Ia sample, with local U − R r.m.s. scatter as low as 0.084 ± 0.017 mag for blue (c < 0) SNe Ia in locally blue U − R environments.
TL;DR: In this paper, the authors studied the production of GWs in strongly supercooled cosmological phase transitions in gauge theories and derived the scaling of the GW source from two-bubble lattice simulations.
Abstract: We study production of gravitational waves (GWs) in strongly supercooled cosmological phase transitions in gauge theories. We extract from two-bubble lattice simulations the scaling of the GW source, and use it in many-bubble simulations in the thin-wall limit to estimate the resulting GW spectrum. We find that in presence of the gauge field the GW source decays with bubble radius as $$\propto R^{-3}$$
after collisions. This leads to a GW spectrum that follows $$\Omega _{\mathrm{GW}} \propto \omega ^{2.3}$$
at low frequencies and $$\Omega _{\mathrm{GW}} \propto \omega ^{-2.9}$$
at high frequencies, marking a significant deviation from the popular envelope approximation.
TL;DR: In this article, the spectral energy distributions were modeled as a linear combination of continuum and emission-line templates and computed its Bayes evidence, integrating over the linear combinations, and the correlation between the UV luminosity and the O II line was measured using the 66 available bands with the zCOSMOS spectroscopic sample, and used as a prior which constrains the relative flux between continuum and line templates.
Abstract: We present – and make publicly available – accurate and precise photometric redshifts in the ACS footprint from the COSMOS field for objects with iAB ≤ 23. The redshifts are computed using a combination of narrow-band photometry from PAUS, a survey with 40 narrow bands spaced at 100A˚ intervals covering the range from 4500 to 8500A˚, and 26 broad, intermediate, and narrow bands covering the UV, visible and near-infrared spectrum from the COSMOS2015 catalogue. We introduce a new method that models the spectral energy distributions as a linear combination of continuum and emission-line templates and computes its Bayes evidence, integrating over the linear combinations. The correlation between the UV luminosity and the O II line is measured using the 66 available bands with the zCOSMOS spectroscopic sample, and used as a prior which constrains the relative flux between continuum and emission-line templates. The flux ratios between the O II line and Hα, Hβ and OIII are similarly measured and used to generate the emission-line templates. Comparing to public spectroscopic surveys via the quantity Δz ≡ (zphoto − zspec)/(1 + zspec), we find the photometric redshifts to be more precise than previous estimates, with σ68(Δz) ≈ (0.003, 0.009) for galaxies at magnitude iAB ∼ 18 and iAB ∼ 23, respectively, which is three times and 1.66 times tighter than COSMOS2015. Additionally, we find the redshifts to be very accurate on average, yielding a median of the Δz distribution compatible with |median(Δz)| ≤ 0.001 at all redshifts and magnitudes considered. Both the added PAUS data and new methodology contribute significantly to the improved results. The catalogue produced with the technique presented here is expected to provide a robust redshift calibration for current and future lensing surveys, and allows one to probe galaxy formation physics in an unexplored luminosity-redshift regime, thanks to its combination of depth, completeness, and excellent redshift precision and accuracy.
University of Cambridge1, Argonne National Laboratory2, Stanford University3, SLAC National Accelerator Laboratory4, University of Pennsylvania5, Ohio State University6, Duke University7, Brookhaven National Laboratory8, Fermilab9, Carnegie Mellon University10, University of Edinburgh11, University of Manchester12, Max Planck Society13, Ludwig Maximilian University of Munich14, University of Illinois at Urbana–Champaign15, National Center for Supercomputing Applications16, University of Oxford17, University of Geneva18, Complutense University of Madrid19, Santa Cruz Institute for Particle Physics20, California Institute of Technology21, ETH Zurich22, IFAE23, University of São Paulo24, Institute of Cosmology and Gravitation, University of Portsmouth25, Institut d'Astrophysique de Paris26, University College London27, Spanish National Research Council28, University of La Laguna29, INAF30, University of Michigan31, Indian Institute of Technology, Hyderabad32, University of Arizona33, University of Oslo34, University of Chicago35, Autonomous University of Madrid36, University of Queensland37, Smithsonian Institution38, Texas A&M University39, Radcliffe Institute for Advanced Study40, Princeton University41, Catalan Institution for Research and Advanced Studies42, University of Wisconsin-Madison43, University of Southampton44, Oak Ridge National Laboratory45, University of Sussex46
TL;DR: In this article, a hierarchical Bayesian scheme was proposed to jointly fit the source population and cosmological parameters, and the results were validated by an end-to-end analysis using simulated GW $h(t)$ data and posterior samples generated from Bayesian samplers used for GW parameter estimation.
Abstract: Knowledge of the shape of the mass spectrum of compact objects can be used to help break the degeneracy between the mass and redshift of the gravitational wave (GW) sources and thus can be used to infer cosmological parameters in the absence of redshift measurements obtained from electromagnetic observations. In this paper, we study extensively different aspects of this approach, including its computational limits and achievable accuracy. Focusing on ground-based detectors with current and future sensitivities, we first perform the analysis of an extensive set of simulated data using a hierarchical Bayesian scheme that jointly fits the source population and cosmological parameters. We consider a population model (power-law plus Gaussian) which exhibits characteristic scales (extremes of the mass spectrum, presence of an accumulation point modeled by a Gaussian peak) that allow an indirect estimate of the source redshift. Our analysis of this catalog highlights and quantifies the tight interplay between source population and cosmological parameters, as well as the influence of initial assumptions (whether formulated on the source or cosmological parameters). We then validate our results by an ``end-to-end'' analysis using simulated GW $h(t)$ data and posterior samples generated from Bayesian samplers used for GW parameter estimation, thus mirroring the analysis chain used for observational data for the first time in literature. Our results then lead us to re-examine the estimation of ${H}_{0}$ obtained with GWTC-1 in Abbott et al. [LIGO Scientific, Virgo Collaborations, Astrophys. J. 909, 218 (2021)], and we show explicitly how population assumptions impact the final ${H}_{0}$ result. Together, our results underline the importance of inferring source population and cosmological parameters simultaneously (and not separately as is often assumed). The only exception, as we discuss, is if an electromagnetic counterpart was to be observed for all the BBH events; then, the population assumptions have less impact on the estimation of cosmological parameters.
TL;DR: In this paper, a search for heavy resonances decaying into a pair of Z bosons leading to either an electron or a muon is presented, where the results are interpreted as upper limits on the production cross section of a spin-0 or spin-2 resonance.
Abstract: A search for heavy resonances decaying into a pair of Z bosons leading to $\ell ^+\ell ^-\ell '^+\ell '^-$ and $\ell ^+\ell ^-
u {{\bar{
u }}}$ final states, where $\ell $ stands for either an electron or a muon, is presented. The search uses proton–proton collision data at a centre-of-mass energy of 13 TeV collected from 2015 to 2018 that corresponds to the integrated luminosity of 139 $\mathrm {fb}^{-1}$ recorded by the ATLAS detector during Run 2 of the Large Hadron Collider. Different mass ranges spanning 200 GeV to 2000 GeV for the hypothetical resonances are considered, depending on the final state and model. In the absence of a significant observed excess, the results are interpreted as upper limits on the production cross section of a spin-0 or spin-2 resonance. The upper limits for the spin-0 resonance are translated to exclusion contours in the context of Type-I and Type-II two-Higgs-doublet models, and the limits for the spin-2 resonance are used to constrain the Randall–Sundrum model with an extra dimension giving rise to spin-2 graviton excitations.
Carnegie Mellon University1, University of Arizona2, University of Pennsylvania3, University of Michigan4, Ohio State University5, Autonomous University of Madrid6, University of Manchester7, University of California, Santa Cruz8, University of Cambridge9, IFAE10, Spanish National Research Council11, Stanford University12, ETH Zurich13, University of Geneva14, University College London15, Ludwig Maximilian University of Munich16, Max Planck Society17, University of Chicago18, Duke University19, University of Edinburgh20, University of São Paulo21, Fermilab22, Argonne National Laboratory23, Pierre-and-Marie-Curie University24, Institut d'Astrophysique de Paris25, University of La Laguna26, National Center for Supercomputing Applications27, University of Queensland28, Lowell Observatory29, Macquarie University30, Texas A&M University31, University of Illinois at Urbana–Champaign32, Princeton University33, University of Sussex34, University of Southampton35, Brandeis University36, Oak Ridge National Laboratory37
TL;DR: In this article, the authors constrain the feedback strength of baryons jointly with cosmology using weak lensing and galaxy clustering observables (3$\times$2pt) of DES Year 1 data in combination with external information from baryon acoustic oscillations (BAO) and Planck cosmic microwave background polarization.
Abstract: Measurements of large-scale structure are interpreted using theoretical predictions for the matter distribution, including potential impacts of baryonic physics. We constrain the feedback strength of baryons jointly with cosmology using weak lensing and galaxy clustering observables (3$\times$2pt) of Dark Energy Survey (DES) Year 1 data in combination with external information from baryon acoustic oscillations (BAO) and Planck cosmic microwave background polarization. Our baryon modeling is informed by a set of hydrodynamical simulations that span a variety of baryon scenarios; we span this space via a Principal Component (PC) analysis of the summary statistics extracted from these simulations. We show that at the level of DES Y1 constraining power, one PC is sufficient to describe the variation of baryonic effects in the observables, and the first PC amplitude ($Q_1$) generally reflects the strength of baryon feedback. With the upper limit of $Q_1$ prior being bound by the Illustris feedback scenarios, we reach $\sim 20\%$ improvement in the constraint of $S_8=\sigma_8(\Omega_{\rm m}/0.3)^{0.5}=0.788^{+0.018}_{-0.021}$ compared to the original DES 3$\times$2pt analysis. This gain is driven by the inclusion of small-scale cosmic shear information down to 2.5$\arcmin$, which was excluded in previous DES analyses that did not model baryonic physics. We obtain $S_8=0.781^{+0.014}_{-0.015}$ for the combined DES Y1+Planck EE+BAO analysis with a non-informative $Q_1$ prior. In terms of the baryon constraints, we measure $Q_1=1.14^{+2.20}_{-2.80}$ for DES Y1 only and $Q_1=1.42^{+1.63}_{-1.48}$ for DESY1+Planck EE+BAO, allowing us to exclude one of the most extreme AGN feedback hydrodynamical scenario at more than $2 \sigma$.
TL;DR: In this article, a search for pair production of third-generation scalar leptoquarks decaying into a top quark and a τ-lepton is presented based on a dataset of pp collisions at s = 13 TeV recorded with the ATLAS detector during Run 2 of the Large Hadron Collider, corresponding to an integrated luminosity of 139 fb−1.
Abstract: A search for pair production of third-generation scalar leptoquarks decaying into a top quark and a τ-lepton is presented The search is based on a dataset of pp collisions at s = 13 TeV recorded with the ATLAS detector during Run 2 of the Large Hadron Collider, corresponding to an integrated luminosity of 139 fb−1 Events are selected if they have one light lepton (electron or muon) and at least one hadronically decaying τ -lepton, or at least two light leptons In addition, two or more jets, at least one of which must be identified as containing b-hadrons, are required Six final states, defined by the multiplicity and flavour of lepton candidates, are considered in the analysis Each of them is split into multiple event categories to simultaneously search for the signal and constrain several leading backgrounds The signal-rich event categories require at least one hadronically decaying τ-lepton candidate and exploit the presence of energetic final-state objects, which is characteristic of signal events No significant excess above the Standard Model expectation is observed in any of the considered event categories, and 95% CL upper limits are set on the production cross section as a function of the leptoquark mass, for different assumptions about the branching fractions into tτ and bν Scalar leptoquarks decaying exclusively into tτ are excluded up to masses of 143 TeV while, for a branching fraction of 50% into tτ, the lower mass limit is 122 TeV [Figure not available: see fulltext]
TL;DR: In this article, a broken power law model was adopted to place 95% confidence level upper limits simultaneously on the gravitational-wave energy density at 25 Hz from unresolved compact binary mergers and strong first-order phase transitions.
Abstract: We place constraints on the normalized energy density in gravitational waves from first-order strong phase transitions using data from Advanced LIGO and Virgo's first, second, and third observing runs First, adopting a broken power law model, we place 95% confidence level upper limits simultaneously on the gravitational-wave energy density at 25 Hz from unresolved compact binary mergers, ${\mathrm{\ensuremath{\Omega}}}_{\mathrm{CBC}}l61\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}9}$, and strong first-order phase transitions, ${\mathrm{\ensuremath{\Omega}}}_{\mathrm{BPL}}l44\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}9}$ The inclusion of the former is necessary since we expect this astrophysical signal to be the foreground of any detected spectrum We then consider two more complex phenomenological models, limiting at 25 Hz the gravitational-wave background due to bubble collisions to ${\mathrm{\ensuremath{\Omega}}}_{\mathrm{pt}}l50\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}9}$ and the background due to sound waves to ${\mathrm{\ensuremath{\Omega}}}_{\mathrm{pt}}l58\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}9}$ at 95% confidence level for phase transitions occurring at temperatures above ${10}^{8}\text{ }\text{ }\mathrm{GeV}$