{"total":13,"items":[{"citing_arxiv_id":"2606.23651","ref_index":114,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting the 'Lensing is Low' Problem with UNIONS","primary_cat":"astro-ph.CO","submitted_at":"2026-06-22T17:36:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"New UNIONS galaxy-galaxy lensing data around CMASS galaxies indicates no significant lensing is low problem, with joint HOD fits to GGL and GC favoring a slightly lower matter power spectrum amplitude than Planck.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18437","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Impact of inhomogeneous curvature on growth rate measurements from magnitude fluctuations","primary_cat":"astro-ph.CO","submitted_at":"2026-06-16T19:40:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Full-GR simulations find that inhomogeneous curvature produces only sub-dominant systematic offsets in growth-rate measurements from magnitude fluctuations at z ≲ 0.2 relative to current statistical errors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.30579","ref_index":94,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Mapping the Universe as a Bianchi I cosmology with Gaia data","primary_cat":"astro-ph.CO","submitted_at":"2026-05-28T21:12:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Gaia quasar proper motions show a significant quadrupole signal matching an axisymmetric Bianchi I anisotropy model, but the amplitude does not increase with redshift as the model requires and the inferred local shear exceeds expectations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.29806","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The observer power spectrum for lightcone statistics, integrated relativistic observables and wide angle effects","primary_cat":"astro-ph.CO","submitted_at":"2026-05-28T11:52:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Introduces the observer power spectrum as a diagonal Fourier-space statistic for lightcone observables by transforming over observer positions rather than sources.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.28817","ref_index":61,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Fewer simulations, sharper covariances: Reducing mock covariance noise with Zeldovich approximation control variates","primary_cat":"astro-ph.CO","submitted_at":"2026-05-27T17:59:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Control variates with Zeldovich mocks reduce covariance matrix variance by up to an order of magnitude on large scales in DESI-like mocks.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.06021","ref_index":57,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Testing parity with composite-field spectra of BOSS and DESI luminous red galaxies","primary_cat":"astro-ph.CO","submitted_at":"2026-04-07T16:19:34+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"No evidence for cosmological parity violation is found in the first kurto-spectrum analysis of BOSS DR12 and DESI DR1 luminous red galaxies.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"where we chose Heaviside-step-function as the smoothing window function: W(k) = 1 2 \u0014 1−tanh \u0012 αln k kmax \u0013\u0015 ,(2.17) withα= 50andk max = 0.45hMpc −1, which filters out the comoving scales smaller than R∼7h −1 Mpc. 2.2 FKP estimator for parity-odd kurto spectra In order to analyse data from spectroscopic galaxy surveys, namely BOSS and DESI, and in anal- ogy with the skew-spectrum analysis of ref. [57], we extend the estimators developed in ref. [54], which measure the kurto spectra in periodic box simulations using Fast Fourier Transforms, to a formulation suitable for survey data that accounts for survey geometry and observational systematics. To this end, we construct an equivalent of Feldman-Kaiser-Peacock [FKP; 58] estimators for the power spectrum, bispectrum, and skew spectra, by introducing a weighted fluctuation"},{"citing_arxiv_id":"2512.17865","ref_index":101,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining primordial non-Gaussianity from DESI DR1 quasars and Planck PR4 CMB Lensing","primary_cat":"astro-ph.CO","submitted_at":"2025-12-19T18:14:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Cross-correlation of DESI DR1 quasars with Planck PR4 CMB lensing constrains local f_NL to 2^{+28}_{-34} (p=1.6) or 6^{+20}_{-24} (p=1.0), tightening previous limits by 35%.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.07236","ref_index":93,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Counting voids and filaments: Betti Curves as a Powerful Probe for Cosmology","primary_cat":"astro-ph.CO","submitted_at":"2025-12-08T07:33:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Betti curves from persistent homology of large-scale structure provide complementary cosmological constraints on ns, sigma8, and Om, with tighter bounds when analyzed jointly with the power spectrum.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.05467","ref_index":59,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Combined tracer analysis for DESI 2024 BAO","primary_cat":"astro-ph.CO","submitted_at":"2025-08-07T15:06:22+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Combining LRG and ELG tracers with bias weighting improves BAO constraints by 11% on alpha_iso and 7% on alpha_AP in DESI DR1 data for the 0.8<z<1.1 bin.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2411.12022","ref_index":83,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI 2024 VII: Cosmological Constraints from the Full-Shape Modeling of Clustering Measurements","primary_cat":"astro-ph.CO","submitted_at":"2024-11-18T20:03:35+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI DR1 full-shape clustering yields Ω_m = 0.2962 ± 0.0095 and σ_8 = 0.842 ± 0.034 in flat ΛCDM, tightening to H_0 = 68.40 ± 0.27 km/s/Mpc with CMB and DESY3, while favoring w_0 > -1, w_a < 0 and limiting neutrino mass sum to < 0.071 eV.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"The power spectrum measurements are obtained from the galaxy catalogs (\"data\") and from synthetically-generated catalogs with random distribution of points (\"ran- doms\") to which we assign the same selection as for the data, including assigning weights (to points) that account for systematic corrections, and those that implement the Feldman- Kaiser-Peacock (FKP) optimal weighting scheme [83]. We also use the random catalog to compute the window matrix [84, 85] that relates the measured power spectrum multipoles to the theory power spectrum prediction. Data and random catalogs are constructed as described in [66]; they are both masked for the presence of bright objects, lack of or bad imaging data and spectroscopic observations, and target priorities."},{"citing_arxiv_id":"2411.12021","ref_index":91,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI 2024 V: Full-Shape Galaxy Clustering from Galaxies and Quasars","primary_cat":"astro-ph.CO","submitted_at":"2024-11-18T20:03:34+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI DR1 full-shape galaxy clustering constrains Omega_m = 0.296 ± 0.010, H0 = 68.63 ± 0.79 km/s/Mpc, and sigma_8 = 0.841 ± 0.034, consistent with LambdaCDM and Planck.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"The effects of these issues are combined into a weight column in the data and random catalogues, intended for use in summary statistics calculations, such as the two-point statistics. The number density of the DESI DR1 sample varies significantly with both redshift and the number of overlapping tiles, due to fibre assignment incompleteness. Therefore, 'FKP' weights [91] designed to maximise the signal-to-noise ratio of clustering measurements at the BAO scale in relation to such number density variations, are included in all two-point calculations. For a full description of the weight calculations, see [83]. In Section 5, we will discuss in detail each potential source of systematic and how to mitigate them in the Full-Shape analysis."},{"citing_arxiv_id":"2407.03397","ref_index":30,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"No evidence for parity violation in BOSS","primary_cat":"astro-ph.CO","submitted_at":"2024-07-03T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"New statistics applied to BOSS data show the reported parity violation signal is consistent with zero after accounting for eight-point correlation function mismatch between data and mocks.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2404.03000","ref_index":75,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars","primary_cat":"astro-ph.CO","submitted_at":"2024-04-03T18:41:49+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI measures BAO scales in six redshift bins with 0.52% combined precision using 5.7 million objects, detecting the signal at up to 9.1 sigma and finding larger scales than Planck LCDM at z<0.8.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"effects of all of those issues are combined into a weight column in the data and random catalogs, meant to be used for any subsequent calculations (i.e., both for reconstruction and two-point statistics). The number density of the DR1 DESI samples varies strongly with both redshift and the number of overlapping tiles (due to assignment completeness). Thus, 'FKP'6 weights, inspired by [75], that are meant to maximize the signal to noise of clustering measurements at the BAO scale with respect to such number density variations are also included in all two-point calculations. Their calculation is fully detailed in [67]. In what follows, we provide brief details on the properties of each sample, providing further context for the statistics of each sample that are presented in Table 2."}],"limit":50,"offset":0}