{"total":15,"items":[{"citing_arxiv_id":"2607.01226","ref_index":156,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Intertwined Constraints in Extended Cosmologies: Dark Energy, Curvature, Neutrinos, and Inflation","primary_cat":"astro-ph.CO","submitted_at":"2026-07-01T17:57:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Dynamical dark energy remains preferred across extended models while curvature, neutrino mass and inflation parameters show strong model dependence, with no resolution of the H0 tension.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"[153]DESIcollaboration,Extended dark energy analysis using DESI DR2 BAO measurements, Phys. Rev. D112(2025) 083511 [2503.14743]. [154] M. Cortˆ es and A.R. Liddle,Interpreting DESI's evidence for evolving dark energy,JCAP12 (2024) 007 [2404.08056]. - 87 - [155] D. Shlivko and P.J. Steinhardt,Assessing observational constraints on dark energy,Phys. Lett. B855(2024) 138826 [2405.03933]. [156] O. Luongo and M. Muccino,Model-independent cosmographic constraints from DESI 2024, Astron. Astrophys.690(2024) A40 [2404.07070]. [157] I.D. Gialamas, G. H¨ utsi, K. Kannike, A. Racioppi, M. Raidal, M. Vasar et al.,Interpreting DESI 2024 BAO: Late-time dynamical dark energy or a local effect?,Phys. Rev. D111 (2025) 043540 [2406.07533]. [158] H. Wang and Y."},{"citing_arxiv_id":"2606.30903","ref_index":49,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Cosmological Concordance in an Especially Opaque Universe: A Tentative Cosmological Detection of Physical Neutrino Mass in $\\Lambda$CDM","primary_cat":"astro-ph.CO","submitted_at":"2026-06-29T20:49:45+00:00","verdict":"REJECT","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Imposing a high prior on τ = 0.11 ± 0.006 produces a 2σ positive neutrino mass sum of 0.10 eV and restores concordance between CMB and DESI data inside ΛCDM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.30713","ref_index":36,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Galaxy Power Spectrum at Two-Loop Order: Implications for Weak Lensing Surveys and New Physics","primary_cat":"astro-ph.CO","submitted_at":"2026-06-29T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Two-loop EFT galaxy power spectrum achieves per-mille agreement with simulations to k=0.85 h/Mpc and yields three times narrower unbiased σ8 errors than linear theory.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21518","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Are Cosmological Data Excluding Sterile Neutrinos or Only the Fully Thermalized Limit?","primary_cat":"astro-ph.CO","submitted_at":"2026-06-19T15:15:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Cosmological observations constrain the effective abundance of light sterile neutrinos tightly while allowing non-fully-thermalized realizations to remain viable across LambdaCDM and CPL models.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05853","ref_index":54,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reconstructing dark energy with fewer assumptions","primary_cat":"astro-ph.CO","submitted_at":"2026-06-04T08:27:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bin-wise uncorrelated reconstruction from DESI/SDSS BAO and Pantheon+/Union3.1/DES-Dovekie supernovae yields dark energy density peaking then declining and equation of state oscillating with phantom crossing near z~0.7, consistent across datasets at moderate significance.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Ishak and L. Medina-Varela, Persistent and serious challenge to the LCDM throne: Evidence for dynamical dark energy rising from combinations of different types of datasets (2025), arXiv:2507.22856 [astro-ph.CO]. [53] R. E. Keeley, A. Shafieloo, and W. L. Matthewson, Could We Be Fooled about Phantom Crossing? (2025), arXiv:2506.15091 [astro-ph.CO]. [54] D. A. Kessler, L. A. Escamilla, S. Pan, and E. Di Valentino, One-parameter dynamical dark energy: Hints for oscillations (2025), arXiv:2504.00776 [astro- ph.CO]. [55] D. H. Lee, W. Yang, E. Di Valentino, S. Pan, and C. van de Bruck, Shape of dark energy: Constraining its evolution with a general parametrization, Phys. Rev. D113, 063554 (2026), arXiv:2507."},{"citing_arxiv_id":"2606.05005","ref_index":124,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Neutrino mass constraints in interacting dark energy models after DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-06-03T15:26:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Upper bounds on total neutrino mass in four phenomenological interacting dark energy models are derived from DESI DR2 BAO plus CMB and SNIa data, showing strong dependence on the interaction term form and statistical preference for models that tighten the bound below the oscillation lower limit.","context_count":1,"top_context_role":"background","top_context_polarity":"unclear","context_text":"14744 [astro-ph.CO]. [121] S.-H. Zhou, T.-N. Li, G.-H. Du, J.-Q. Jiang, J.-F. Zhang, and X. Zhang, Phys. Rev. D112, 123532 (2025), arXiv:2509.10836 [astro-ph.CO]. [122] G. S. Nair, A. Chakraborty, L. Amendola, and S. Das, (2025), arXiv:2512.08752 [astro-ph.CO]. [123] A. Chudaykin, M. M. Ivanov, and O. H. E. Philcox, (2025), arXiv:2511.20757 [astro-ph.CO]. [124] S. D'Onofrio, S. Odintsov, and T. Schiavone, (2025), arXiv:2511.06924 [gr-qc]. [125] R. K. Sharma and J. Lesgourgues, JCAP02, 034 (2026), arXiv:2510.15835 [astro-ph.CO]. [126] G.-H. Du, T.-N. Li, P.-J. Wu, J.-F. Zhang, and X. Zhang, (2025), arXiv:2507.16589 [astro-ph.CO]. [127] W. Giar` e, O. Mena, E. Specogna, and E. Di Valentino, Phys. Rev. D112, 103520 (2025), arXiv:2507."},{"citing_arxiv_id":"2605.28644","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Exploring non-Poisson satellite occupation in HOD models and its impact on 2- and 3-point galaxy clustering","primary_cat":"astro-ph.CO","submitted_at":"2026-05-27T15:50:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Replacing Poisson satellite occupation with Conway-Maxwell-Poisson in HOD models produces up to 10% shifts in small-scale projected clustering and 30% in counts-in-cylinders but under 2% change in tree-level bispectrum at k_max=0.3.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21436","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Euclid preparation: Testing multi-field inflation with galaxy power spectrum and bispectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T17:26:36+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Validates redshift-space power spectrum and bispectrum analysis on Abacus-PNG mocks to recover unbiased f_NL constraints for Euclid spectroscopic sample.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Appendix D: Additional results from individual and combined statistics For the same analysis settings as in Sect. 5.4.2, we present addi- tional plots, which complement those shown earlier. Article number, page 27 of 30 A&A proofs:manuscript no. main Table C.1.hoices for priors on cosmological and nuisance parameters. Parameter Prior Cosmology hU [0.6,0.8 ] ωc U[0.085,0.165] 109 ×A s U[1,3.2] fNL U[−500,500] Bias b1 U[0.9,5] b2 U[−20,20] bG2 U[−20,20] bΓ3 U[−20,20] Counter-Term c0 h h−2 Mpc2i N \u0010 0,100 2 \u0011 c2 h h−2 Mpc2i N \u0010 0,100 2 \u0011 c4 h h−2 Mpc2i N \u0010 0,100 2 \u0011 c6 h h−4 Mpc4i N \u0010 0,100 2 \u0011 cB VDG U[−50,50] Shot-Noise s0 N \u0010 0,2 2 \u0011 s02 h h−2 Mpc2i N \u0010 0,10 2 \u0011 s2 h h−2 Mpc2i N \u0010 0,10 2 \u0011 s4 h h−2 Mpc2i"},{"citing_arxiv_id":"2605.20748","ref_index":57,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing late-time deviations from $\\Lambda$CDM with a quadratic dark energy expansion","primary_cat":"astro-ph.CO","submitted_at":"2026-05-20T05:49:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"The QDEE model fits combined cosmological datasets better than Lambda CDM, shifts the Hubble constant higher, and shows strong Bayesian evidence in its favor.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13298","ref_index":28,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Probing nonlinear structure formation beyond $\\Lambda$CDM with the LSS bootstrap: a joint power spectrum and bispectrum analysis","primary_cat":"astro-ph.CO","submitted_at":"2026-05-13T10:12:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First MCMC constraints on LSS bootstrap parameters yield ~7% precision on linear growth modifications and ~57% on quadratic kernel modifications from BOSS data, improving to 1% and 25% with larger simulations.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"Nonetheless, they rest on the choice of a particular cosmological model. By contrast, the LSS Bootstrap offers a complementary, model-independent framework that enables an efficient exploration of a wide class of theories beyondΛCDM. We apply our pipeline both on observational data from the BOSS survey [27] and on mock galaxy catalogs constructed from the 'PT Challenge' simulations [28], which cover substantially larger volumes. In doing so, we can evaluate the range of constraints on new physics that can be derived from present-day data and from the measurements attainable by a futuristic survey. The paper is organized as follows. In Sec. II, we review the Large-Scale Structure (LSS) Bootstrap and introduce the model-independent parameters used to detect possible departures from theΛCDM framework."},{"citing_arxiv_id":"2605.05114","ref_index":22,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Effective Field Theory of Large Scale Structure and Newtonian Motion Gauges","primary_cat":"astro-ph.CO","submitted_at":"2026-05-06T16:45:33+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A Newtonian Motion Gauge found via Einstein-Boltzmann solver maps linear dynamics with scale-dependent growth and GR corrections to Newtonian equations, enabling consistent nonlinear EFT calculations that are transformed back for accuracy in real and redshift space.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Gil-Mar' ın, \"The Cosmological Analysis of the SDSS/BOSS data from the Effective Field Theory of Large-Scale Structure,\"JCAP05(2020) 005,arXiv:1909.05271 [astro-ph.CO]. [21] S.-F. Chen, Z. Vlah, and M. White, \"A new analysis of galaxy 2-point functions in the BOSS survey, including full-shape information and post-reconstruction BAO,\"JCAP02no. 02, (2022) 008,arXiv:2110.05530 [astro-ph.CO]. [22] T. Simon, P. Zhang, and V. Poulin, \"Cosmological inference from the EFTofLSS: the eBOSS QSO full-shape analysis,\"JCAP07(2023) 041,arXiv:2210.14931 [astro-ph.CO]. [23] O. H. E. Philcox and M. M. Ivanov, \"BOSS DR12 full-shape cosmology: ΛCDM constraints from the large-scale galaxy power spectrum and bispectrum monopole,\"Phys. Rev. D105no. 4, (2022)"},{"citing_arxiv_id":"2604.25171","ref_index":9,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Multi-tracers, multi-surveys: a joint Fisher analysis of DESI+PFS","primary_cat":"astro-ph.CO","submitted_at":"2026-04-28T03:20:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A joint multi-tracer Fisher analysis of DESI and PFS cross-spectra calibrates bias parameters from data, improving forecasted constraints on fσ8 by 33%, neutrino mass by 80%, and Ωm by 49% compared to single-tracer baselines.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":", 5, 6], full-shape EFT analyses have improved LSS con- straints on, for example, neutrino masses [7-9], primordial non-Gaussianity [10-12], early - 1 - dark energy [13-15], clustering dark energy [16], interacting dark energy [17], ultra-light ax- ions [18] and dark-sector interactions [19, 20]. More recently, the DESI collaboration [21-23] and independent reanalyses [9, 12, 24-26] applied this framework to DESI DR1 data, report- ing evidence for dynamical dark energy and-when combined with CMB data-a preference for the normal neutrino mass hierarchy over the inverted hierarchy. Sharpeningσ(M ν)from galaxy clustering is therefore a pressing goal, as the neutrino mass constraint is currently the most prior-sensitive quantity in EFT full-shape analyses."},{"citing_arxiv_id":"2604.08895","ref_index":48,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"FolpsD: combining EFT and phenomenological approaches for joint power spectrum and bispectrum analyses","primary_cat":"astro-ph.CO","submitted_at":"2026-04-10T02:59:01+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"FolpsD combines EFT power spectrum and tree-level bispectrum with damping to enable joint analyses that improve cosmological constraints from DESI-like galaxy mocks by up to 30% on As and omega_cdm while extending the usable k-range without significant biases for LRG samples.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"analysis at one loop from the Effective Field Theory of Large-Scale Structure,JCAP05 (2024) 059, [2206.08327]. [46] Z. Lu, T. Simon and P. Zhang,Preference for evolving dark energy in light of the galaxy bispectrum,2503.04602. [47] S. Novell Masot et al.,Full-Shape analysis of the power spectrum and bispectrum of DESI DR1 LRG and QSO samples,JCAP06(2025) 005, [2503.09714]. [48] A. Chudaykin, M. M. Ivanov and O. H. E. Philcox,Reanalyzing DESI DR1: 1. LCDM Constraints from the Power Spectrum and Bispectrum,2507.13433. [49] A. Chudaykin, M. M. Ivanov and O. H. E. Philcox,Reanalyzing DESI DR1: 2. Constraints on Dark Energy, Spatial Curvature, and Neutrino Masses,2511.20757. [50] A. Chudaykin, M. M. Ivanov and O. H. E. Philcox,Reanalyzing DESI DR1: 3."},{"citing_arxiv_id":"2603.10787","ref_index":105,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Measuring neutrino mass in light of ACT DR6 and DESI DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-03-11T14:00:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New ACT and DESI data yield model-dependent upper limits on sum of neutrino masses, with holographic dark energy giving the tightest bounds and a consistent preference for degenerate hierarchy.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Chen, A. Chudaykin, M. Maus, and O. H. E. Philcox, (2026), arXiv:2601.16165 [astro-ph.CO]. [102] G. Franco Abell' an, (2026), arXiv:2601.04312 [astro-ph.CO]. [103] A. Ladeira, R. C. Nunes, S. Pan, and W. Yang, (2026), arXiv:2601.02077 [astro-ph.CO]. [104] G. S. Nair, A. Chakraborty, L. Amendola, and S. Das, (2025), arXiv:2512.08752 [astro-ph.CO]. [105] A. Chudaykin, M. M. Ivanov, and O. H. E. Philcox, (2025), arXiv:2511.20757 [astro-ph.CO]. [106] S. D'Onofrio, S. Odintsov, and T. Schiavone, (2025), arXiv:2511.06924 [gr-qc]. [107] R. K. Sharma and J. Lesgourgues, (2025), arXiv:2510.15835 [astro-ph.CO]. [108] S. Barua and S. Desai, Phys. Dark Univ. 51, 102229 (2026), arXiv:2508.16238 [astro-ph.CO]."},{"citing_arxiv_id":"2601.02077","ref_index":49,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Joint Constraints on Neutrinos and Dynamical Dark Energy in Minimally Modified Gravity","primary_cat":"astro-ph.CO","submitted_at":"2026-01-05T12:58:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The w†VCDM model shows a statistically significant preference for late-time quintessence-phantom crossing dark energy, raises the Hubble constant, and satisfies neutrino mass and Neff constraints from current cosmological datasets.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Nunes, Robust evidence for dynamical dark energy from DESI galaxy-CMB lensing cross-correlation and geometric probes, JCAP09, 084, arXiv:2505.24465 [astro-ph.CO]. [48] A. Chudaykin, M. M. Ivanov, and O. H. E. Philcox, Reanalyzing DESI DR1: 2. Constraints on Dark En- ergy, Spatial Curvature, and Neutrino Masses (2025), arXiv:2511.20757 [astro-ph.CO]. [49] A. Reeves, S. Ferraro, A. Nicola, and A. Refregier, Mul- tiprobe constraints on early and late time dark energy (2025), arXiv:2510.06114 [astro-ph.CO]. [50] M. Ishak and L. Medina-Varela, Persistent and serious challenge to the ΛCDM throne: Evidence for dynamical dark energy rising from combinations of different types of datasets (2025), arXiv:2507."}],"limit":50,"offset":0}