{"total":26,"items":[{"citing_arxiv_id":"2607.08044","ref_index":52,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Catching Disguised Transients with ASTRANet: Anomaly-Aware Spectroscopic Classification and Conformal Calibration","primary_cat":"astro-ph.IM","submitted_at":"2026-07-09T01:40:10+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"ASTRANet combines a redshift-free spectral classifier, a 16-score anomaly detector, and conformal prediction to identify and calibrate uncertainty for out-of-taxonomy astronomical transients.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.07329","ref_index":56,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Beyond traditional emission-line diagnostics: using autoencoders to uncover active galactic nuclei in DESI spectra","primary_cat":"astro-ph.GA","submitted_at":"2026-07-08T12:21:19+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":5.5,"formal_verification":"none","one_line_summary":"SPENDER autoencoder plus k-d tree nearest-neighbor classification on DESI spectra identifies AGN and broad-line AGN at accuracies 0.952 and 0.965, recovering sources missed by single-line diagnostics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.06844","ref_index":220,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"First detection of ultra-fast outflows in a quiescent galaxy","primary_cat":"astro-ph.GA","submitted_at":"2026-07-07T22:33:16+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First detection of an ultra-fast outflow (v≈0.07c) in a quiescent galaxy quenched ~9 Gyr ago, suggesting AGN winds can maintain quiescence independent of global star formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.31486","ref_index":109,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A simulation-based analytic model of radio galaxies II: self-consistent radiative losses","primary_cat":"astro-ph.GA","submitted_at":"2026-06-30T11:00:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Including radiative losses in analytic models of high-redshift radio galaxies reduces predicted radio and X-ray luminosities compared to models that neglect them.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.30633","ref_index":109,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"GIGA-Lens 2.0: Strong-Lens Modeling on Multiple GPU Nodes","primary_cat":"astro-ph.CO","submitted_at":"2026-06-29T17:57:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"GIGA-Lens 2.0 scales strong gravitational lens modeling across up to 128 GPU nodes and demonstrates it on 100 simulated systems plus one real DESI lens.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28559","ref_index":86,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"DESI DR2 Reference Mocks: Clustering results from UCHUU ELGs and QSOs","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T19:22:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Mock catalogs for DESI DR2 ELGs and QSOs are constructed via modified subhalo abundance matching on the Uchuu simulation to reproduce observed number density and clustering statistics.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28501","ref_index":106,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"A hierarchical Bayesian framework for cosmology using Type 1 AGN variability","primary_cat":"astro-ph.CO","submitted_at":"2026-06-26T18:00:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A hierarchical Bayesian framework that uses the empirical anti-correlation between AGN variability amplitude and luminosity to infer cosmological parameters from moderate-baseline light curves via importance reweighting.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24651","ref_index":44,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Measuring local primordial non-Gaussianity from the clustering of DESI DR1 LRGs and QSOs","primary_cat":"astro-ph.CO","submitted_at":"2026-06-23T14:45:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Reports first config-space f_NL measurement from DESI DR1 LRG/QSO 2pcf, yielding joint f_NL = -3^{+12}_{-12} at 68% CL using simulation-based modeling and imaging systematics mitigation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18581","ref_index":39,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"DESI Data Release 2 ELGs: Property-dependent subsamples, imaging systematics, and clustering","primary_cat":"astro-ph.CO","submitted_at":"2026-06-17T01:09:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Property-dependent systematic weights derived separately on ELG subsamples, with separate DES footprint treatment, mitigate spurious clustering in ~10% of subsamples but are not optimal for the full sample.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00992","ref_index":194,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Understanding the Broad-line Region of Active Galactic Nuclei with Photoionization. II. Slim disks, Self-shadowing, and BLR sizes","primary_cat":"astro-ph.GA","submitted_at":"2026-05-31T04:15:31+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Slim-disk self-shadowing plus accretion-rate-dependent BLR density enhancement explains the observed offsets of high-Eddington AGNs below the canonical R-L relation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.28903","ref_index":5,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"The energy conditions and model selection in the local Universe","primary_cat":"astro-ph.CO","submitted_at":"2026-05-27T16:08:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Local HII galaxy and cosmic chronometer data favor the Rh=ct universe over ΛCDM at 92% vs 8% likelihood, with Rh=ct satisfying all energy conditions while ΛCDM violates the strong energy condition at z≲2.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.02463","ref_index":18,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmic-web quenching with DESI DR1: T-Web environments and mass-dependent red/blue classification","primary_cat":"astro-ph.GA","submitted_at":"2026-04-02T18:50:07+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Stellar mass primarily drives galaxy quenching in DESI DR1, with cosmic web environment as a secondary modulator strongest in knots at lower redshifts.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"colour-mass diagrams with Otsu thresholds, and the evolution of red/blue fractions across environments. Finally, Section 5 summarises our conclusions and outlines future prospects with upcoming DESI data releases. 2 Data 2.1 DESI DR1 galaxy samples We use spectroscopic galaxy samples from the first public data release of the Dark Energy Spectroscopic Instrument [18], selected from the standard DESI clustering catalogs [19]. Our analysis employs three tracer populations: luminous red galaxies (LRGs), emission-line galaxies (ELGs), and the Bright Galaxy Survey (BGS). These tracers span different redshift ranges, galaxy types, and large-scale bias, enabling a comparative study of galaxy evolution across cosmic-web environments."},{"citing_arxiv_id":"2601.21432","ref_index":17,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"Cosmological analysis of the DESI DR1 Lyman alpha 1D power spectrum","primary_cat":"astro-ph.CO","submitted_at":"2026-01-29T09:08:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DESI DR1 Lyman-alpha data yields Δ²★=0.379±0.032 and n★=-2.309±0.019 at k★=0.009 km⁻¹s and z=3, sharpening N_eff, α_s, and β_s constraints by factors of 1.18-1.90 when combined with other probes.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Spectroscopic Survey (BOSS [12]) expanded this number to≃160 000 over five years, and the extended Baryon Oscillation Spectroscopic Survey (eBOSS [13]) further increased it to ≃210 000 over six years. This number rose dramatically with the advent of the Dark Energy Spectroscopic Instrument survey (DESI [14]). Remarkably, DESI measured≃55 000 Lyα forests [15, 16] within the Early Data Release (EDR [17]), which contains observations from the six-month Survey Validation period (SV [18]) and the first two months of the main survey. In this work, we analyzeP 1D measurements [19, 20] from the first DESI data release (DR1 [21]), which includes 450 000 Lyαforests obtained during the first year of main survey observations combined with the SV data. Within the ΛCDM model and several of its extensions, there is no significant loss of"},{"citing_arxiv_id":"2512.07236","ref_index":10,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"2511.01803","ref_index":13,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"DESI DR2 Galaxy Luminosity Functions","primary_cat":"astro-ph.GA","submitted_at":"2025-11-03T18:03:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"DESI DR2 yields galaxy luminosity functions showing non-power-law faint-end behavior and bright-end deviations, with good North-South agreement and reduced errors compared to GAMA.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2510.19149","ref_index":73,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"$H_0$ Without the Sound Horizon (or Supernovae): A 2% Measurement in DESI DR1","primary_cat":"astro-ph.CO","submitted_at":"2025-10-22T00:46:39+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A heuristic power-spectrum rescaling applied to DESI DR1 BAO data plus CMB acoustic scale anchor yields H0 values of 69.2 to 70.3 km/s/Mpc at sub-2% precision across three independent late-time datasets.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.05467","ref_index":67,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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 -1, wa < 0) at 3.1 sigma with CMB and 2.8-4.2 sigma when including supernovae.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"measured in photometric surveys (e.g., [16]), though the precision obtained for a given number of tracers is much higher with spectroscopic redshifts. DESI is designed specifically to enable a spectroscopic BAO survey of un- precedented power and efficiency [17], as shown in its sur- vey validation [18] based on the early data release [19]. In its first year of observations [20], DESI already achieved BAO measurements competitive with those of all previ- ous surveys combined [21, 22]. Now, with redshifts of more than 30 million galaxies and quasars, and Ly α for- est spectra of more than 820,000 quasars, the DESI DR2 sample is by far the largest spectroscopic galaxy sample to date. The BAO technique (reviewed in §4 of [23]), which is"},{"citing_arxiv_id":"2411.12022","ref_index":50,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"dataset","top_context_polarity":"use_dataset","context_text":"In addition to systematics related to theoretical modeling, we quantify several fur- ther potential systematic effects using mock catalogues. These mocks are built from the AbacusSummit suite of simulations [116, 117] with a galaxy-halo connection prescription based on halo occupation distribution (HOD) models calibrated on the DESI Early Data Re- lease [50] which are described in [118-120]. We have identified and studied seven sources of systematic effects that could bias our cosmological constraints: i) theoretical modeling men- tioned above [69], ii) description of the galaxy-halo connection [73], iii) assumptions related to the fiducial cosmology [79], iv) imaging systematics due to inhomogeneities in the target"},{"citing_arxiv_id":"2411.12021","ref_index":113,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"dataset","top_context_polarity":"use_dataset","context_text":"dark time tracers we used the extended HOD framework implemented in theAbacusHOD code [111] and for bright time tracers we used a halo tabulation method to fit HODs for different absolute magnitude threshold samples [112]. We produced a first generation of theAbacusmocks (calledAbacus-1) that is based on a very early version of the DESI early data release (DESI-EDR [113]) to find the best fit HOD model. Having this version early allowed us to start testing the analysis pipeline as we were collecting more data. For dark time tracers, the HOD parameters were found by fitting the galaxy two-point correlation function averaged in angular bins at small scales. More details about the HOD models can be found in [114]. Satellite galaxies were distributed using NFW"},{"citing_arxiv_id":"2404.03002","ref_index":73,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"paper_title":"DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations","primary_cat":"astro-ph.CO","submitted_at":"2024-04-03T18:41:51+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First-year DESI BAO data are consistent with flat LambdaCDM and, when combined with CMB, show a 2.5-3.9 sigma preference for evolving dark energy (w0 > -1, wa < 0) that strengthens with certain supernova datasets.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"a sample of stellar targets is being observed to a high density in an overlapping Milky Way Survey [71] to explore the stellar evolution and kinematics of the Milky Way. For cosmology, DESI is designed to impose stringent constraints on both the expansion history and the growth rate of large scale structure. Promising detections of the BAO feature at the few percent level [72] from the DESI early data release [73] have confirmed that DESI is on target to meet the top-level science requirements on BAO measurements. Specifically, DESI will tightly constrain matter density in the universe, the equation of state of dark energy, spatial curvature, the amplitude of primordial fluctuations, and neutrino mass. It will also sharply test modifications to the general theory of relativity proposed to explain the accelerated"},{"citing_arxiv_id":"2404.03000","ref_index":39,"ref_count":1,"confidence":0.9,"is_internal_anchor":false,"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":"background","top_context_polarity":"background","context_text":"5 × 10−4 h3 Mpc−3, for a sample with 100% fiber assignment completeness. Thus, the DR1 number density is roughly constant at 3 × 10−4 h3 Mpc−3, averaged over the DR1 footprint, as can be seen in the light green curve in Figure 1. The sample was defined using k-corrected r-band absolute magnitudes from [78, 79] and a correction for evolution that is linear in redshift (matching that used for [39]). The cuts make the sample a close match to both the LRG number density (for a complete sample) at z = 0.4 and the clustering amplitude, as can be seen by comparing to the red curve in Figure 1 and the P0 entries in Table 2. The density is high enough to make shot-noise a minor contribution to the BGS statistical uncertainty in the DR1 two-point measurements at BAO scales."}],"limit":50,"offset":0}