{"total":12,"items":[{"citing_arxiv_id":"2606.27812","ref_index":207,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Unraveling the Imprints of Fluctuation-dynamo on the Intracluster Medium with the SKA","primary_cat":"astro-ph.GA","submitted_at":"2026-06-26T07:54:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"MHD simulations indicate that SKA-Mid Band 5a can detect filamentary polarized emission from ICM magnetic fields at high resolution and sensitivity, allowing inference of turbulence driving scales.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25537","ref_index":139,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing the Fundamental Nature of Particle Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2026-06-24T08:13:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Review summarizing radio searches for WIMP and ALP dark matter with SKA precursors and forecasts for SKA-Low and SKA-Mid telescopes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.22431","ref_index":120,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"An Interplay Between Fractional Calculus and Holographic Dark Energy","primary_cat":"gr-qc","submitted_at":"2026-06-21T10:44:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Introduces Fractional Holographic Dark Energy (FHDE) via fractionally corrected entropy from a modified Wheeler-DeWitt equation and studies its late-time cosmology, field reconstructions, and extensions to modified gravity theories.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"The general K-essence Lagrangian may be written as Lkq =f kq(φ)F(X)−V(φ).(3.41) Standard quintessence is recovered by settingfkq(φ) = 1and F(X) = X. The principal motivation for K-essence is that late-time accelerated expansion - and, in other contexts, inflation - can be driven through non-standard kinetic structure alone, without the need for a potential. Following [120], we adopt a general kinetic LagrangianP (φ,Xkq), depending on the 26 Chapter 3. Fractionalswirlto Holographic Dark Energy Model Figure 3.10: Redshift evolution of the K- essence kinetic energyXkq. Figure 3.11: Redshift evolution of the K- essence coupling functionfkq(φ). scalar fieldφand the kinetic variableXkq =−˙φ2 kq/2. The corresponding action is"},{"citing_arxiv_id":"2606.21839","ref_index":12,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Observational Constraints on $f(Q,T)$ Gravity in the Presence of DBI-Essence Scalar Field","primary_cat":"gr-qc","submitted_at":"2026-06-20T02:12:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Derives background solutions for linear f(Q,T)=αQ+βT plus DBI field and reports MCMC posteriors from Hubble, BAO, and SNIa data that are consistent with late-time constraints.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11065","ref_index":4,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"CMB Birefringence from Vacuum Interfaces","primary_cat":"hep-th","submitted_at":"2026-05-11T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"CMB polarization rotation emerges as a Pancharatnam phase localized at dark sector vacuum interfaces, independent of redshift, frequency, and the presence of light axions.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"ground,\" Nature Rev. Phys. 4, no.7, 452-469 (2022) [arXiv:2202.13919 [astro-ph.CO]]. [2] M. C. Huang and P. Sikivie, \"The Structure of Axionic Domain Walls,\" Phys. Rev. D 32, 1560 (1985). [3] D. Harari and P. Sikivie, \"Effects of a Nambu-Goldstone boson on the polarization of radio galaxies and the cosmic microwave background,\" Phys. Lett. B 289, 67-72 (1992). [4] S. M. Carroll, \"Quintessence and the rest of the world,\" Phys. Rev. Lett. 81, 3067-3070 (1998) [arXiv:astro-ph/9806099 [astro-ph]]. [5] A. Lue, L. M. Wang and M. Kamionkowski, \"Cosmological signature of new parity violating interactions,\" Phys. Rev. Lett. 83, 1506-1509 (1999) [arXiv:astro-ph/9812088 [astro-ph]]. [6] M. Pospelov, A. Ritz and C. Skordis, \"Pseudoscalar perturbations and polariza-"},{"citing_arxiv_id":"2605.08465","ref_index":11,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"How to augment cosmic shear measurements with radio polarimetry of galaxies?","primary_cat":"astro-ph.CO","submitted_at":"2026-05-08T20:31:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A Gaussian statistical model of galaxy shapes and radio polarizations yields unbiased, minimum-variance estimators for cosmic shear, intrinsic alignment, and line-of-sight rotation that are accurate to first order.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"com/mnras/article-pdf/474/1/460/22141968/stx2750.pdf]. [9] W. W. Yin, L. Dai, J. Huang, L. Ji and S. Ferraro,New Probe of Cosmic Birefringence Using Galaxy Polarization and Shapes,Phys. Rev. Lett.134(2025) 161001 [2402.18568]. [10] S. M. Carroll, G. B. Field and R. Jackiw,Limits on a Lorentz and Parity Violating Modification of Electrodynamics,Phys. Rev. D41(1990) 1231. [11] S. M. Carroll,Quintessence and the Rest of the World: Suppressing Long-Range Interactions, Phys. Rev. Lett.81(1998) 3067 [astro-ph/9806099]. [12] A. Lue, L. Wang and M. Kamionkowski,Cosmological Signature of New Parity-Violating Interactions, Phys. Rev. Lett.83(1999) 1506 [astro-ph/9812088]. [13] A. Arvanitaki, S. Dimopoulos, S. Dubovsky, N. Kaloper and J."},{"citing_arxiv_id":"2604.17441","ref_index":35,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A short course in general relativity","primary_cat":"gr-qc","submitted_at":"2026-04-19T13:43:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"Lecture notes that derive the nonlinear Einstein field equations from the gravitational action and apply them to black holes, cosmology, and gravitational waves at the advanced undergraduate level.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.02124","ref_index":41,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the Physical Nature of the Scalar Mode Mass in the Jordan frame of a Metric $f(R)$ gravity","primary_cat":"gr-qc","submitted_at":"2026-03-02T17:42:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The scalar mode mass in Jordan-frame metric f(R) gravity must exceed the Hubble scale by several orders of magnitude.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2509.08787","ref_index":26,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Parity Violation in Galaxy Shapes: Primordial Non-Gaussianity","primary_cat":"astro-ph.CO","submitted_at":"2025-09-10T17:15:21+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The parity-odd intrinsic alignment power spectrum probes the collapsed limit of the parity-odd primordial trispectrum and can tighten constraints on parity-violating PNG when bias parameters are calibrated from N-body simulations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Cahn, Measurement of parity-odd modes in the large-scale 4-point correlation function of Sloan Digital Sky Survey Baryon Oscillation Spectroscopic Survey twelfth data release CMASS and LOWZ galaxies, Mon. Not. Roy. Astron. Soc.522, 5701 (2023), arXiv:2206.03625 [astro-ph.CO]. [25] A. Krolewski, S. May, K. Smith, and H. Hopkins, No evidence for parity violation in BOSS, JCAP2024, 044 (2024), arXiv:2407.03397 [astro-ph.CO]. [26] O. H. E. Philcox and J. Ereza, Could sample variance be responsible for the parity-violating signal seen in the Baryon Oscillation Spectroscopic Survey?, Philosophical Transactions of the Royal Society of London Series A383, 20240034 (2025), arXiv:2401.09523 [astro-ph.CO]. [27] Z. Slepian, A. Krolewski, A. Greco, S. May, W. Ortola Leonard, F. Kamalinejad, J."},{"citing_arxiv_id":"2211.04492","ref_index":111,"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":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"1907.04473","ref_index":260,"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":"The signal from kSZ in galaxy clustering alone is plotted in orange and the combination of everything in blue. We see that even in the absence of an informative prior, the constraining power is twice that of DESI alone. For a sufficiently tight prior on τg, the CMB-S4 data alone can surpass DESI RSD measurements. modes, producing characteristic T B and EB cross-correlations in the CMB maps [259, 260]. Even though there is no firm theoretical prediction for the size of this effect,6 if observed, it would be a clear \"smoking-gun\" evidence for physics beyond the Standard Model, in the form of a new scalar field. Previous studies have constrained both a uniform rotation angle α, as well as anisotropic rotation described by a power spectrum. The current tightest bound on the uniform rotation angle is α < 0."},{"citing_arxiv_id":"1705.11098","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Modified Gravity Theories on a Nutshell: Inflation, Bounce and Late-time Evolution","primary_cat":"gr-qc","submitted_at":"2017-05-31T13:41:52+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Modified gravity theories supply viable mathematical frameworks for inflation, bounces, and dark energy eras that match observational data.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Then, we need to require F ′(R)> 0. (20) We should note that from the viewpoint of the field theory, the grav iton becomes ghost in the antigravity region. It should be noted that the de Sitter or anti-de Sitter space solutio n in (9) corresponds to the extremum of the potential V (σ ). In fact, we find, dV (σ ) dA = F ′′(A) F ′(A)3 (−AF ′(A) + 2F (A)) . (21) Therefore, if Eq. (9) is satisfied, the scalar field σ should be on the local maximum or local minimum of the potential and σ can be a constant. When the condition (9) is satisfied, the mass give n by (18) has the following form: m2 σ = 3 2F ′(A) ( −A + F ′(A) F ′′(A) ) . (22) Therefore, in the case that the condition (20) for avoiding the ant igravity holds true, the mass squared m2"}],"limit":50,"offset":0}