Hasil untuk "Geophysics. Cosmic physics"

E. Komatsu, J. Dunkley, J. Dunkley et al.

The Wilkinson Microwave Anisotropy Probe (WMAP) 5-year data provide stringent limits on deviations from the minimal, six-parameter Λ cold dark matter model. We report these limits and use them to constrain the physics of cosmic inflation via Gaussianity, adiabaticity, the power spectrum of primordial fluctuations, gravitational waves, and spatial curvature. We also constrain models of dark energy via its equation of state, parity-violating interaction, and neutrino properties, such as mass and the number of species. We detect no convincing deviations from the minimal model. The six parameters and the corresponding 68% uncertainties, derived from the WMAP data combined with the distance measurements from the Type Ia supernovae (SN) and the Baryon Acoustic Oscillations (BAO) in the distribution of galaxies, are: Ωbh2 = 0.02267+0.00058−0.00059, Ωch2 = 0.1131 ± 0.0034, ΩΛ = 0.726 ± 0.015, ns = 0.960 ± 0.013, τ = 0.084 ± 0.016, and at k = 0.002 Mpc-1. From these, we derive σ8 = 0.812 ± 0.026, H0 = 70.5 ± 1.3 km s-1 Mpc−1, Ωb = 0.0456 ± 0.0015, Ωc = 0.228 ± 0.013, Ωmh2 = 0.1358+0.0037−0.0036, zreion = 10.9 ± 1.4, and t0 = 13.72 ± 0.12 Gyr. With the WMAP data combined with BAO and SN, we find the limit on the tensor-to-scalar ratio of r 1 is disfavored even when gravitational waves are included, which constrains the models of inflation that can produce significant gravitational waves, such as chaotic or power-law inflation models, or a blue spectrum, such as hybrid inflation models. We obtain tight, simultaneous limits on the (constant) equation of state of dark energy and the spatial curvature of the universe: −0.14 < 1 + w < 0.12(95%CL) and −0.0179 < Ωk < 0.0081(95%CL). We provide a set of “WMAP distance priors,” to test a variety of dark energy models with spatial curvature. We test a time-dependent w with a present value constrained as −0.33 < 1 + w0 < 0.21 (95% CL). Temperature and dark matter fluctuations are found to obey the adiabatic relation to within 8.9% and 2.1% for the axion-type and curvaton-type dark matter, respectively. The power spectra of TB and EB correlations constrain a parity-violating interaction, which rotates the polarization angle and converts E to B. The polarization angle could not be rotated more than −5.°9 < Δα < 2.°4 (95% CL) between the decoupling and the present epoch. We find the limit on the total mass of massive neutrinos of ∑mν < 0.67 eV(95%CL), which is free from the uncertainty in the normalization of the large-scale structure data. The number of relativistic degrees of freedom (dof), expressed in units of the effective number of neutrino species, is constrained as Neff = 4.4 ± 1.5 (68%), consistent with the standard value of 3.04. Finally, quantitative limits on physically-motivated primordial non-Gaussianity parameters are −9 < flocalNL < 111 (95% CL) and −151 < fequilNL < 253 (95% CL) for the local and equilateral models, respectively.

J. Frieman, M. Turner, D. Huterer

Ten years ago, the discovery that the expansion of the universe is accelerating put in place the last major building block of the present cosmological model, in which the universe is composed of 4% baryons, 20% dark matter, and 76% dark energy. At the same time, it posed one of the most profound mysteries in all of science, with deep connections to both astrophysics and particle physics. Cosmic acceleration could arise from the repulsive gravity of dark energy—for example, the quantum energy of the vacuum—or it may signal that general relativity (GR) breaks down on cosmological scales and must be replaced. We review the present observational evidence for cosmic acceleration and what it has revealed about dark energy, discuss the various theoretical ideas that have been proposed to explain acceleration, and describe the key observational probes that will shed light on this enigma in the coming years.

J. Bernal, L. Verde, A. Riess

We perform a comprehensive cosmological study of the H0 tension between the direct local measurement and the model-dependent value inferred from the Cosmic Microwave Background. With the recent measurement of H0 this tension has raised to more than 3 σ. We consider changes in the early time physics without modifying the late time cosmology. We also reconstruct the late time expansion history in a model independent way with minimal assumptions using distance measurements from Baryon Acoustic Oscillations and Type Ia Supernovae, finding that at z < 0.6 the recovered shape of the expansion history is less than 5% different than that of a standard ΛCDM model. These probes also provide a model insensitive constraint on the low-redshift standard ruler, measuring directly the combination rsh where H0 = h × 100 Mpc−1km/s and rs is the sound horizon at radiation drag (the standard ruler), traditionally constrained by CMB observations. Thus rs and H0 provide absolute scales for distance measurements (anchors) at opposite ends of the observable Universe. We calibrate the cosmic distance ladder and obtain a model-independent determination of the standard ruler for acoustic scale, rs. The tension in H0 reflects a mismatch between our determination of rs and its standard, CMB-inferred value. Without including high-ℓ Planck CMB polarization data (i.e., only considering the ``recommended baseline" low-ℓ polarisation and temperature and the high ℓ temperature data), a modification of the early-time physics to include a component of dark radiation with an effective number of species around 0.4 would reconcile the CMB-inferred constraints, and the local H0 and standard ruler determinations. The inclusion of the ``preliminary" high-ℓ Planck CMB polarisation data disfavours this solution.

T. I. C. M. G. Aartsen, R. Abbasi, M. Ackermann et al.

The observation of electromagnetic radiation from radio to $\gamma$-ray wavelengths has provided a wealth of information about the universe. However, at PeV (10$^{15}$ eV) energies and above, most of the universe is impenetrable to photons. New messengers, namely cosmic neutrinos, are needed to explore the most extreme environments of the universe where black holes, neutron stars, and stellar explosions transform gravitational energy into non-thermal cosmic rays. The discovery of cosmic neutrinos with IceCube has opened this new window on the universe. In this white paper, we present an overview of a next-generation instrument, IceCube-Gen2, which will sharpen our understanding of the processes and environments that govern the universe at the highest energies. IceCube-Gen2 is designed to: 1) Resolve the high-energy neutrino sky from TeV to EeV energies; 2) Investigate cosmic particle acceleration through multi-messenger observations; 3) Reveal the sources and propagation of the highest energy particles in the universe; 4) Probe fundamental physics with high-energy neutrinos. IceCube-Gen2 will increase the annual rate of observed cosmic neutrinos by a factor of ten compared to IceCube, and will be able to detect sources five times fainter than its predecessor. Furthermore, through the addition of a radio array, IceCube-Gen2 will extend the energy range by several orders of magnitude compared to IceCube. Construction will take 8 years and cost about \$350M. The goal is to have IceCube-Gen2 fully operational by 2033. IceCube-Gen2 will play an essential role in shaping the new era of multi-messenger astronomy, fundamentally advancing our knowledge of the high-energy universe. This challenging mission can be fully addressed only in concert with the new survey instruments across the electromagnetic spectrum and gravitational wave detectors which will be available in the coming years.

Euclid Collaboration Y. Mellier, Abdurro’uf, J. Barroso et al.

The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. is a medium-class mission in the Cosmic Vision 2015--2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14\,000\,deg$^2$ of extragalactic sky. In addition to accurate weak lensing and clustering measurements that probe structure formation over half of the age of the Universe, its primary probes for cosmology, these exquisite data will enable a wide range of science. This paper provides a high-level overview of the mission, summarising the survey characteristics, the various data-processing steps, and data products. We also highlight the main science objectives and expected performance.

M. Kamionkowski, A. Riess

Over the past decade, the disparity between the value of the cosmic expansion rate determined directly from measurements of distance and redshift and that determined instead from the standard Lambda cold dark matter (ΛCDM) cosmological model, calibrated by measurements from the early Universe, has grown to a level of significance requiring a solution. Proposed systematic errors are not supported by the breadth of available data (and unknown errors untestable by lack of definition). Simple theoretical explanations for this Hubble tension that are consistent with the majority of the data have been surprisingly hard to come by, but in recent years, attention has focused increasingly on models that alter the early or pre-recombination physics of ΛCDM as the most feasible. Here, we describe the nature of this tension and emphasize recent developments on the observational side. We then explain why early-Universe solutions are currently favored and the constraints that any such model must satisfy. We discuss one workable example, early dark energy, and describe how it can be tested with future measurements. Given an assortment of more extended recent reviews on specific aspects of the problem, the discussion is intended to be fairly general and understandable to a broad audience. Expected final online publication date for the Annual Review of Nuclear and Particle Science, Volume 73 is September 2023. Please see http://www.annualreviews.org/page/journal/pubdates for revised estimates.

Ilaria Cazzaniga, Ana I. Dogliotti, Susanne Kratzer et al.

The use of high-resolution data in aquatic applications increased significantly in the last decade with the launch of decametre-scale optical sensors. More recently, commercial very-high resolution (VHR) sensors, offering finer spatial and temporal resolutions, have shown the potential of complementing data from high-resolution missions. Planet SuperDove (SD), with a band-setting similar to the Copernicus Sentinel-2 MultiSpectral Instrument (S2-MSI), a 3-m spatial resolution and quasi-daily revisiting time, show the potential for widening water monitoring applications to smaller water basins, and finer-scale phenomena. However, the uncertainties in SD products need to be quantified, to assess their fitness-for-purpose for these applications. This work aims to provide uncertainty estimates for SD-derived aquatic remote sensing reflectance (RRS) in different water types, benefitting from the radiometric measurements of the AERONET-OC network. RRS was derived from both Surface Reflectance (SR) products, distributed by Planet, or from data processed with ACOLITE. The comparability between SD and S2-MSI products was also assessed comparing RRS and Rayleigh-corrected reflectance (RRC) from S2-MSI and SD. The results indicate generally low performance across all bands for both SD RRS products, except in the most turbid waters, and highlight the lack of a publicly available robust atmospheric correction processor for SD data for most optical water types. The comparison to S2-MSI shows promising results only when comparing RRC values, but differences still suggest issues associated with calibration and radiometry of the SD sensors. The results also highlight the need for a harmonization strategy to ensure consistent integration of these datasets within multi-source monitoring systems.

Antoine Hochet, Florian Sévellec, Nicolas Kolodziejczyk

Abstract Anthropogenic climate change is projected to intensify the global hydrological cycle, posing substantial risks to human societies. However, monitoring these changes through direct observations remains challenging, particularly over the oceans. Since long‐term shifts in the hydrological cycle are expected to alter ocean salinity distribution, understanding the processes governing its evolution is essential. Salinity distribution is known to result from a balance between freshwater fluxes, which broaden the distribution, and mixing processes, which narrow it. Using a novel diagnostic based on the mean salinity variance budget applied to the Estimating the Circulation and Climate of the Ocean (ECCO), we estimate that the large‐scale salinity flux—primarily driven by the seasonal cycle—contributes approximately 23% to this mixing. Our framework also enables us to understand the regional balances, and to identify the regions where these balances are most significant. Our results suggest that accurately representing the seasonal salinity cycle in ocean and climate models is important for simulating the ocean salinity distribution.

Elana Resnick, Elana Resnick, Anders Lundkvist et al.

The Community Coordinated Modeling Center (CCMC) at NASA Goddard Space Flight Center has developed comprehensive resources and initiatives to support the Heliophysics Big Year (HBY) during the approach to solar maximum. This paper details the CCMC’s extensive outreach efforts from October 2023 through December 2024, engaging diverse audiences including the general public, educators, and scientific communities. Key activities included partnerships with the Intrepid Museum and American Museum of Natural History, educational presentations reaching over 1,000 physics educators, and specialized workshops for high school teachers. The paper also highlights significant technological enhancements to the CCMC’s visualization capabilities, specifically the improved Integrated Space Weather Analysis (ISWA) system with its global synchronization features and specialized layout options. Additionally, we discuss the collaborative development of OpenSpace, a versatile 3D visualization tool that integrates data from observations, simulations, and space missions to support public engagement through planetarium shows and educational initiatives. Through these combined efforts, the CCMC has established multiple pathways for audiences to engage with heliophysics research and better understand space weather phenomena during this period of heightened solar activity.

Xianqi Meng, Yuefeng Zhao, Kaifa Cao et al.

Remote sensing image change captioning (RSICC) aims to generate textual descriptions of changes between bitemporal images. However, accurately describing fine-grained changes while capturing interscale relationships as well as distinguishing real changes from spurious changes (e.g., illumination, seasonal variations) are still major challenges for current methods. To address these issues, we propose DualFocus-CapNet, a novel model tailored for RSICC. DualFocus-CapNet employs a dual-stream architecture, where each stream is dedicated to processing a distinct pair of bitemporal features. Crucially, we introduce a scale-wise progressive convolution (ScalePro Conv) that employs a progressive scale-specific approach to decompose remote sensing features into pixel-level variations, regional continuities, and linear structures. Unlike conventional parallel multiscale processing methods, ScalePro Conv adopts a serial progressive structure to establish interscale relationships, thereby avoiding the fragmentation of feature information. Then, the bi-directional difference guided transformer (BDiGTrans) is proposed to eliminate interference from spurious changes by dynamically masking invariant regions and extracting bidirectional differential features. Furthermore, the cross-temporal adaptive fusion module (CTAF) is introduced to dynamically balance bitemporal features using learnable gating to enhance change discrimination and robust caption generation. Comprehensive experiments on the benchmark datasets LEVIR-CC and WHU-CDC show that our DualFocus-CapNet surpasses state-of-the-art change captioning methods in various evaluation metrics.

E. Madge, Enrico Morgante, Cristina Puchades-Ibáñez et al.

In recent years, several pulsar timing array collaborations have reported first hints for a stochastic gravitational wave background at nano-Hertz frequencies. Here we elaborate on the possibility that this signal comes from new physics that leads to the generation of a primordial stochastic gravitational wave background. We propose a set of simple but concrete models that can serve as benchmarks for gravitational waves sourced by cosmological phase transitions, domain wall networks, cosmic strings, axion dynamics, or large scalar fluctuations. These models are then confronted with pulsar timing data and with cosmological constraints. With only a limited number of free parameters per model, we are able to identify viable regions of parameter space and also make predictions for future astrophysical and laboratory tests that can help with model identification and discrimination.

T. Bringmann, Paul Frederik Depta, T. Konstandin et al.

Gravitational waves from a first-order cosmological phase transition, at temperatures at the MeV-scale, would arguably be the most exciting explanation of the common red spectrum reported by the NANOGrav collaboration, not the least because this would be direct evidence of physics beyond the standard model. Here we perform a detailed analysis of whether such an interpretation is consistent with constraints on the released energy deriving from big bang nucleosynthesis and the cosmic microwave background. We find that a phase transition in a completely secluded dark sector with sub-horizon sized bubbles is strongly disfavoured with respect to the more conventional astrophysical explanation of the putative gravitational wave signal in terms of supermassive black hole binaries. On the other hand, a phase transition in a dark sector that subsequently decays, before the time of neutrino decoupling, remains an intriguing possibility to explain the data. From the model-building perspective, such an option is easily satisfied for couplings with the visible sector that are small enough to evade current collider and astrophysical constraints. The first indication that could eventually corroborate such an interpretation, once the observed common red spectrum is confirmed as a nHz gravitational wave background, could be the spectral tilt of the signal. In fact, the current data already show a very slight preference for a spectrum that is softer than what is expected from the leading astrophysical explanation.

W. Freedman, B. Madore

One of the most exciting and pressing issues in cosmology today is the discrepancy between some measurements of the local Hubble constant and other values of the expansion rate inferred from the observed temperature and polarization fluctuations in the cosmic microwave background (CMB) radiation. Resolving these differences holds the potential for the discovery of new physics beyond the standard model of cosmology: Lambda Cold Dark Matter (ΛCDM), a successful model that has been in place for more than 20 years. Given both the fundamental significance of this outstanding discrepancy, and the many-decades-long effort to increase the accuracy of the extragalactic distance scale, it is critical to demonstrate that the local measurements are convincingly free from residual systematic errors. We review the progress over the past quarter century in measurements of the local value of the Hubble constant, and discuss remaining challenges. Particularly exciting are new data from the James Webb Space Telescope (JWST), for which we present an overview of our program and first results. We focus in particular on Cepheids and the Tip of the Red Giant Branch (TRGB) stars, as well as a relatively new method, the JAGB (J-Region Asymptotic Giant Branch) method, all methods that currently exhibit the demonstrably smallest statistical and systematic uncertainties. JWST is delivering high-resolution near-infrared imaging data to both test for and to address directly several of the systematic uncertainties that have historically limited the accuracy of extragalactic distance scale measurements (e.g., the dimming effects of interstellar dust, chemical composition differences in the atmospheres of stars, and the crowding and blending of Cepheids contaminated by nearby previously unresolved stars). For the first galaxy in our program, NGC 7250, the high-resolution JWST images demonstrate that many of the Cepheids observed with the Hubble Space Telescope (HST) are significantly crowded by nearby neighbors. Avoiding the more significantly crowded variables, the scatter in the JWST near-infrared (NIR) Cepheid PL relation is decreased by a factor of two compared to those from HST, illustrating the power of JWST for improvements to local measurements of H 0. Ultimately, these data will either confirm the standard model, or provide robust evidence for the inclusion of additional new physics.

Ali Saeibehrouzi, Soroush Abolfathi, Petr Denissenko et al.

Abstract Flow through a granular, natural porous media can erode it chemically by dissolving and thus shrinking the solid particles, or mechanically, by removing them. The two‐way interplay between the transport of fluids and dissolved solutes and alteration of the porous structure and hence the medium's transport properties is of interest to processes ranging from subsurface energy storage to contamination in groundwater. Here, we conduct a quantitative pore‐scale analysis through a combination of numerical simulations and microfluidic experiments. We find that erosion enhances solute dispersion at low Pe (diffusion‐dominated) and diminishes it at high Pe. Residence time distribution reveals that mechanical erosion tends to induce non‐Fickian transport more than chemical erosion, which we attribute to the differences in their effects on pore size distribution.

Lan Wang, Xuwei Bao, Guanghua Chen et al.

Abstract Typhoon Haikui (2023) brought an unprecedented rainstorm to Fuzhou, with a rainfall record of 360.4 mm in 12 hr and an instantaneous rain rate of 234 mm hr−1. This study investigates the evolution of precipitation microphysics during this short‐term period. High rain rates exceeding 100 mm hr−1 along with large mass‐weighted diameter Dm were predominantly observed in the first 3 hr (Stage I), while the next 9 hr (Stage II) experienced less than 100 mm hr−1. At the onset of Stage I, it is warm‐cloud processes that mainly contributed to the increased rain rate, yet the rain rates hardly exceeded 200 mm hr−1. Approximately 1 hr later, a rain rate of 234 mm hr−1 occurred due to a joint contribution of ice‐ and warm‐cloud processes, characterized by the increased horizontal reflectivity throughout the troposphere. Moreover, this study provides a new insight into the correlation between rainfall intensity and convective intensity.

Na Liu, Guodong Wu, Yonggui Huang et al.

In large-scale multimodal remote sensing data archives, the application of cross-modal technology to achieve fast retrieval between different modalities has attracted great attention. In this article, we focus on cross-modal retrieval technology between remote sensing images and text. At present, there is still a large heterogeneity problem in the semantic information extracted from different modal data in the remote sensing field, which leads to the inability to effectively utilize intraclass similarities and interclass differences in the hash learning process, ultimately resulting in low cross-modal retrieval accuracy. In addition, supervised learning-based methods require a large number of labeled training samples, which limits the large-scale application of hash-based cross-modal retrieval technology in the remote sensing field. To address this problem, this article proposes a new unsupervised cross-autoencoder contrast hashing method for RS retrieval. This method constructs an end-to-end deep hashing model, which mainly includes a feature extraction module and a hash representation module. The feature extraction module is mainly responsible for extracting deep semantic information from different modal data and sends the different modal semantic information to the hash representation module through the intermediate layer to learn and generate binary hash codes. In the hashing module, we introduce a new multiobjective loss function to increase the expression of intramodal and intermodal semantic consistency through multiscale semantic similarity constraints and contrastive learning and add a cross-autoencoding module to reconstruct and compare hash features to reduce the loss of semantic information during the learning process. This article conducts a large number of experiments on the UC Merced Land dataset and the RSICD dataset. The experimental results of these two popular benchmark datasets show that the proposed CACH method outperforms the most advanced unsupervised cross-modal hashing methods in RS.

Marcus Saraiva, Ana Muller, Alexandre Maul

Model-based seismic inversion is a key technique in reservoir characterization, but traditional methods face significant limitations, such as relying on 1D average stationary wavelets and assuming an unrealistic lateral resolution. To address these challenges, we propose a Geophysics-Informed Neural Network (GINN) that integrates deep learning with seismic modeling. This novel approach employs a Deep Convolutional Neural Network (DCNN) to simultaneously estimate Point Spread Functions (PSFs) and acoustic impedance (IP). PSFs are divided into zero-phase and residual components to ensure geophysical consistency and to capture fine details. We used synthetic data from the SEAM Phase I Earth Model to train the GINN for 100 epochs (approximately 20 minutes) using a 2D UNet architecture. The network's inputs include positional features and a low-frequency impedance (LF-IP) model. A self-supervised loss function combining Mean Squared Error (MSE) and Structural Similarity Index Measure (SSIM) was employed to ensure accurate results. The GINN demonstrated its ability to generate high-resolution IP and realistic PSFs, aligning with expected geological features. Unlike traditional 1D wavelets, the GINN produces PSFs with limited lateral resolution, reducing noise and improving accuracy. Future work will aim to refine the training process and validate the methodology with real seismic data.

Chun-Hao To, Shivam Pandey, E. Krause et al.

Upcoming cosmic shear analyses will precisely measure the cosmic matter distribution at low redshifts. At these redshifts, the matter distribution is affected by galaxy formation physics, primarily baryonic feedback from star formation and active galactic nuclei. Employing measurements from the Magneticum and IllustrisTNG simulations and a dark matter + baryon (DMB) halo model, this paper demonstrates that Sunyaev-Zel'dovich (SZ) effect observations of galaxy clusters, whose masses have been calibrated using weak gravitational lensing, can constrain the baryonic impact on cosmic shear with statistical and systematic errors subdominant to the measurement errors of DES-Y3 and LSST-Y1, with systematic errors on S8 and Ω m reaching 10% and 50% of the statistical errors, respectively. For LSST-Y6 and Roman surveys, these systematic errors increase to 150% and 100% of the statistical errors, indicating the necessity for further model developments for future surveys. We further dissect the contributions from different scales and halos with different masses to cosmic shear, highlighting the dominant role of SZ clusters at scales critical for cosmic shear analyses. These findings suggest a promising avenue for future joint analyses of Cosmic Microwave Background (CMB) and lensing surveys.

Giorgi Arsenadze, Andrea Caputo, Xucheng Gan et al.

The cosmic microwave background (CMB) spectrum is an extraordinary tool for exploring physics beyond the Standard Model. The exquisite precision of its measurement makes it particularly sensitive to small effects caused by hidden sector interactions. In particular, CMB spectral distortions can unveil the existence of dark photons which are kinetically coupled to the standard photon. In this work, we use the COBE-FIRAS dataset to derive accurate and robust limits on photon-to-dark-photon oscillations for a large range of dark photon masses, from 10−10 to 10−4 eV. We consider in detail the redshift dependence of the bounds, computing CMB distortions due to photon injection/removal using a Green’s function method. Our treatment improves on previous results, which had set limits studying energy injection/removal into baryons rather than photon injection/removal, or ignoring the redshift evolution of distortions. The difference between our treatment and previous ones is particularly noticeable in the predicted spectral shape of the distortions, a smoking gun signature for photon-to-dark-photon oscillations. The characterization of the spectral shape is crucial for future CMB missions, which could improve the present sensitivity by orders of magnitude, exploring regions of the dark photon parameter space that are otherwise difficult to access .

Ankita Budhraja, W. Waalewijn

Energy correlators characterize the asymptotic energy flow in scattering events produced at colliders, from which the microscopic physics of the scattering can be deduced. This view of collisions is akin to analyses of the Cosmic Microwave Background, and a range of promising phenomenological applications of energy correlators have been identified, including the study of hadronization, the deadcone effect, measuring $\alpha_s$ and the top quark mass. While $N$-point energy correlators are interesting to study for larger values of $N$, their evaluation is computationally intensive, scaling like $M^N/N!$, where $M$ is the number of particles. In this Letter, we develop a fast, approximate method for their evaluation exploiting that correlations at a given angular scale are insensitive to effects at other (widely-separated) scales. This implies that the energy correlator can be computed on (sub)jets, effectively reducing M. Furthermore, we utilize a dynamical (sub)jet radius that allows us to obtain reliable results without restricting the angular scales being probed. For concreteness we focus on the projected energy correlator, which projects onto the largest separation between the $N$ directions. E.g.~for $N=7$ we find a speed up of up to four orders of magnitude, depending on the desired accuracy. We also consider the possibility of raising the energy to a power higher than one in the energy correlator, which has been proposed to reduce soft sensitivity, and further cuts back the required computation time. These higher-power correlators are not collinear safe, but as a byproduct our approach suggests a natural method to regularize them, such that they can be described using perturbation theory. This letter is accompanied by a public code that implements our method.