{"total":16,"items":[{"citing_arxiv_id":"2606.26576","ref_index":162,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detectors for CLASS-W2: The second 90 GHz telescope of the Cosmology Large Angular Scale Surveyor","primary_cat":"astro-ph.IM","submitted_at":"2026-06-25T03:52:30+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A new 296-detector 90 GHz TES bolometer array for CLASS achieves uniform properties, 16 μK√s NET, 0.37 optical efficiency, and a 41% mapping speed boost after addressing blue-leak radiation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.22302","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting cosmic anisotropy with the Pantheon+ compilation","primary_cat":"astro-ph.CO","submitted_at":"2026-06-21T02:05:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Re-analysis of Pantheon+ supernovae finds no statistically compelling evidence for intrinsic cosmic anisotropy; reported signals are subsample-dependent and attributed to data distribution artifacts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00219","ref_index":70,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"21cmEMUv3: a hybrid diffusion-LSTM emulator of 21cmFAST summary observables","primary_cat":"astro-ph.CO","submitted_at":"2026-05-29T18:00:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"21cmEMUv3 emulates the cylindrical 21cm power spectrum via score-based diffusion and six other 21cmFAST observables via LSTM networks at sub-percent accuracy, then uses the emulator to infer a lower limit on soft-band X-ray luminosity from HERA data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.23489","ref_index":36,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A comparison between Galactic magnetic field models and polarized synchrotron emission with C-BASS at 4.76 GHz and S-PASS at 2.3 GHz","primary_cat":"astro-ph.GA","submitted_at":"2026-05-22T10:51:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Comparison of Galactic magnetic field models to polarized synchrotron observations shows good agreement on angles but poor match on intensity, indicating local foreground structures must be incorporated.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19953","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing String-Theory-Inspired Topologies of the Early Universe through CMB Temperature and Polarization Anisotropies","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T15:05:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reexamination of Planck CMB data finds a possible spatial-parity-breaking signal consistent with six extra dimensions compactified toroidally at the GUT scale before inflation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16917","ref_index":85,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Rapid ASKAP Continuum Survey VII: Spectra and Polarisation In Cutouts of Extragalactic Sources (SPICE-RACS) Second Data Release -- Unveiling the Magnetised Sky","primary_cat":"astro-ph.GA","submitted_at":"2026-05-16T10:13:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"SPICE-RACS DR2 delivers the largest single Faraday rotation measure catalog from a radio survey, with 250,000-340,000 RMs across most of the sky at median uncertainty of 2 rad m^{-2}.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.01023","ref_index":3,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Formation and Redshift Evolution of Dark Matter Spikes","primary_cat":"astro-ph.CO","submitted_at":"2026-05-01T18:35:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Stellar gravitational heating reduces dark matter spike overdensities by 2-4 orders of magnitude and drives the inner slope to γ_χ ≈ 1.5 within a few Gyrs, remaining above NFW cusps.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Any robust interpretation of indirect dark matter signals from galactic nuclei must account for this evolution. I. INTRODUCTION The existence of dark matter (DM) is firmly established through its gravitational effects across a wide range of physical scales, from the cosmic microwave background [1, 2] and galaxy clustering to the rotation curves of galax- ies [3, 4] (see [5, 6] for reviews). On sub-parsec scales, however, the distribution of DM in the vicinity of super- massive black holes (SMBHs) remains poorly constrained. Measurements of stellar orbits near SagittariusA⋆ show no evidence for an enclosed DM mass comparable to the black hole mass, placing upper limits on the DM den- sity profile at sub-pc scales [7, 8]."},{"citing_arxiv_id":"2604.14088","ref_index":88,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"BROOM: a python package for model-independent analysis of microwave astronomical data","primary_cat":"astro-ph.CO","submitted_at":"2026-04-15T17:04:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"BROOM is a Python package that applies ILC and GILC techniques for model-independent separation of CMB, SZ, and foreground signals in microwave data along with diagnostic and simulation utilities.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"We now proceed to present the results of a validation run of theBROOMpackage in the following section. 4 Validation and results In this section, we present the results of a validation run covering most of the functional- ities of theBROOMpackage. The analysis is divided into two parts: the first one focuses on full-sky observations, representative of satellite CMB experiments (e.g. WMAP [23, 88], Planck[31, 89], LiteBIRD [90], PICO [91, 92]), while the second targets partial-sky measure- ments characteristic of ground-based experiments (e.g. POLARBEAR [93, 94], ACT [95, 96], SPT [3, 97], BICEP/Keck [16, 98], SO [14, 99]). For both cases, we run the complete analysis pipeline provided by the package, including the generation of tailored simulations, the appli-"},{"citing_arxiv_id":"2601.14222","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting the Matter Creation Process: Observational Constraints on Gravitationally Induced Dark Energy and the Hubble Tension","primary_cat":"astro-ph.CO","submitted_at":"2026-01-20T18:32:34+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Gravitationally induced particle creation models fit cosmological data as well as ΛCDM and reduce the Hubble tension from 4.3σ to 2.4–3σ.","context_count":1,"top_context_role":"baseline","top_context_polarity":"baseline","context_text":"tive equation of state parameter of dark energy (pre- liminary analysis for choosing the priors) within the PC1 model. For reference and comparison we will use the flat (zero curvature) ΛCDM model, see Fig. 1 for the marginalized posteriors of its background parameters h≡ H0 100 km−1 s Mpc (dimensionless Hubble constant) and Ω m0 usingCC+BAO+SN+SH0ES+CMBas the dataset combination. [1] C. L. Bennettet al.(WMAP), Astrophys. J. Suppl.208, 20 (2013), arXiv:1212.5225 [astro-ph.CO]. [2] N. Aghanimet al.(Planck), Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]. [3] N. Aghanimet al.(Planck), Astron. Astrophys.641, A1 (2020), arXiv:1807.06205 [astro-ph.CO]. [4] S. Aiolaet al."},{"citing_arxiv_id":"2511.18657","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"How Complex is Dark Energy? A Bayesian Analysis of CPL Extensions with Recent DESI BAO Measurements","primary_cat":"astro-ph.CO","submitted_at":"2025-11-23T23:56:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian evidence from DESI BAO plus CMB and SN data favors the standard CPL evolving dark energy model over both simpler constant-w and more complex higher-order extensions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2411.07970","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"MUltiplexed Survey Telescope (MUST) Science White Paper I: Overview of Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys","primary_cat":"astro-ph.CO","submitted_at":"2024-11-12T17:51:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MUST is a planned 6.5m Stage-V spectroscopic survey telescope targeting 100M+ galaxies and quasars to z~5.5 for large-scale structure cosmology studies.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"from the CfA Redshift Survey in 1982 [1, 2], spectroscopic mapping of large-scale structures (LSS) has accumulated more than 30 million redshifts of nearby and distant galax- ies. This monumental achievement has contributed signifi- cantly to the establishment of the current cosmological model ΛCDM, along with other cosmological probes, i.e., cosmic microwave background (CMB; [3, 4]), Type-Ia supernovae (SN; [5-7]), or measurements of weak lensing (e.g., [8, 9]). For two decades (2000-2020), major experiments such as the Sloan Digital Sky Survey (SDSS; [10]), followed by the on- going (2021-2026) survey from the Dark Energy Spectro- scopic Instrument1) (DESI; [11]), have mapped the 3D uni- verse at low and intermediate redshift (z≲3)."},{"citing_arxiv_id":"2211.04492","ref_index":78,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Hubble Tension and Early Dark Energy","primary_cat":"astro-ph.CO","submitted_at":"2022-11-08T19:00:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":2.0,"formal_verification":"none","one_line_summary":"The Hubble tension between local and early-universe expansion-rate measurements may be resolved by early dark energy that speeds up expansion before recombination while satisfying existing constraints.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"CMB results. The first effort to determine H0 from the CMB was in 2000 (77), but the results were not constraining because these initial measurements lacked enough information about the higher peaks in the CMB power spectrum to fix ωm and ωb. This was accomplished with NASA's Wilkinson Anisotropy Probe (WMAP), which arrived at H0 = 69.3± 0.8 km sec−1 Mpc−1 (78) for their final mission value for the Hubble pa- rameter (improving upon their first-year result, H0 = 73 ± 5 km sec −1 Mpc−1 (79)).1 Subsequently, the European Space Agency's Planck satellite (4) provided power spectra to multipole moments ℓ∼ 2500, as opposed to ℓ∼ 800 from WMAP, finding H0 = 67.4± 0.5 km sec−1 Mpc−1. These measurements have then been complemented at even smaller an-"},{"citing_arxiv_id":"1907.08010","ref_index":81,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological searches for the neutrino mass scale and mass ordering","primary_cat":"astro-ph.CO","submitted_at":"2019-07-18T12:03:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Thesis summarizing an upper limit of 0.12 eV on the neutrino mass sum, bias calibration via CMB lensing cross-correlations, and tighter limits plus stronger normal-ordering preference in non-phantom dynamical dark energy models.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Meanwhile, evidence for the existence of dark components in our Universe kept growing. 1A number of other CMB experiments were launched during those and subsequent years, but it is fair to say that two stand out particularly among the others: the Wilkinson Microwave Anisotropy Probe (WMAP), operating between 2001 and 2010, played a crucial role in definitely establishing the current concordance ΛCDM model [79-81]. ThePlanck satellite has instead mapped the CMB sky to exquisite accuracy and is currently providing the tightest constraints on cosmological parameters from a single experiment [82-90]. 8 Chapter 2. Standard Models and what lies beyond In the 1970s, seminal works by Vera Rubin [91-95], along with upper limits on the amplitude of temperature anisotropies in the CMB, provided strong support for the existence of the DM"},{"citing_arxiv_id":"1907.04473","ref_index":86,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"CMB-S4 Science Case, Reference Design, and Project Plan","primary_cat":"astro-ph.IM","submitted_at":"2019-07-10T01:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Presents the science case, reference design, and project plan for the CMB-S4 ground-based CMB experiment.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"For the second category the signatures qualitatively depend on the mass of the additional degrees of freedom (fields). Additional light degrees of freedom can fluctuate significantly and may have large self-interactions. Heavy degrees of freedom do not fluctuate appreciably, but may come into existence by quantum fluctuations and decay into inflaton quanta, generating non-Gaussian correlations [85, 86, 29, 87]. Alternatively, they may become excited by the dynamics of the inflaton and their backreaction on the inflationary dynamics may lead to non-Gaussian correlations [88, 89, 90, 91]. Constraints on non-Gaussianity are often expressed in terms of the correlator of three scalar modes, described by the bispectrum BR(k1, k2, k3), defined through ⟨R(k1)R(k2)R(k3)⟩ = (2π)3δ(k1 + k2 + k3)BR(k1, k2, k3) ."},{"citing_arxiv_id":"1807.06211","ref_index":269,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Planck 2018 results. X. Constraints on inflation","primary_cat":"astro-ph.CO","submitted_at":"2018-07-17T04:05:09+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Updated Planck CMB measurements give ns = 0.9649 ± 0.0042, r < 0.056, confirm flatness at 0.4 percent, and show no evidence for scale-dependent features or non-slow-roll dynamics in the inflaton potential.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1807.06209","ref_index":42,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Planck 2018 results. VI. Cosmological parameters","primary_cat":"astro-ph.CO","submitted_at":"2018-07-17T04:05:07+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Final Planck CMB data confirms the flat 6-parameter ΛCDM model with Ω_c h² = 0.120 ± 0.001, Ω_b h² = 0.0224 ± 0.0001, n_s = 0.965 ± 0.004, τ = 0.054 ± 0.007, H_0 = 67.4 ± 0.5 km/s/Mpc, and no strong evidence for extensions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}