{"total":12,"items":[{"citing_arxiv_id":"2607.08192","ref_index":26,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"CARPP: Parametric Radiative-Transfer Fitting of Molecular Cores from Dust Continuum Data","primary_cat":"astro-ph.GA","submitted_at":"2026-07-09T07:46:44+00:00","verdict":"ACCEPT","verdict_confidence":"HIGH","novelty_score":6.0,"formal_verification":"none","one_line_summary":"CARPP recovers seven core parameters from multi-band dust continuum via layered radiative transfer, achieving <20% average relative error under a stated noise-resolution criterion and classifying TMC-1C as near-critical Bonnor-Ebert and Ori2-2 as power-law collapsing.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.07489","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Chemical diversity of dense cores in Orion B: The role of the environment","primary_cat":"astro-ph.GA","submitted_at":"2026-07-08T14:49:40+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"PCA of 25 molecular lines across 1001 Orion B cores reveals that chemical diversity is driven by column density, the FUV-to-density ratio G0/n, and freeze-out signatures tied to mean density.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.02353","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Tracing grain growth in the forming prestellar core L1506C with 3D modeling of Herschel, IRAM, and CFHT observations","primary_cat":"astro-ph.GA","submitted_at":"2026-07-02T15:59:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"3D modeling of L1506C with THEMIS 2 dust model shows evolved grains needed in densest regions, indicating early grain growth in prestellar phase.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.00872","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Kolmogorov turbulence across multi-fractal gas in Polaris Flare","primary_cat":"astro-ph.GA","submitted_at":"2026-07-01T12:36:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Reveals a pristine scale-invariant 3D Kolmogorov turbulence cascade in the Polaris Flare with an analytical mapping showing the apparent transition arises from projection and density fractal dimension changes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25291","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Formation of a Protostellar Multiple System via Rotational Fragmentation","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T01:49:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Multi-scale observations of dense core G205.46-14.56-N2 show a quadruple protostellar system whose symmetry, outflows, and kinematics match simulations of rotational fragmentation, providing the first claimed evidence for this pathway in high-order multiples.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25158","ref_index":42,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Early phases of star formation with SKAO: synchrotron emission from dense starless cores in molecular clouds","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T20:45:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"SKAO will enable detection of synchrotron emission from prestellar cores to probe their magnetic field properties in nearby star-forming regions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.19694","ref_index":68,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"PMO Polaris CO survey. II. Where is the dust?","primary_cat":"astro-ph.GA","submitted_at":"2026-06-18T01:46:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Linear decomposition of Planck dust maps using PMO CO and EBHIS HI surveys attributes 20-40% of dust to CO gas, negligible amounts to broad warm HI, and significant fractions to narrow cold HI and CO-dark molecular gas at boundaries.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.16796","ref_index":141,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A HINSA view of cosmic-ray ionization in IC 348 and NGC 1333: evidence for a strong low-energy cosmic-ray disparity","primary_cat":"astro-ph.GA","submitted_at":"2026-06-15T14:38:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"HINSA observations show CRIR decreasing with H2 column density in both clouds, with IC 348 values an order of magnitude above NGC 1333, modeled as an order-of-magnitude difference in low-energy CR populations from local acceleration sources.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13123","ref_index":49,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Grain alignment and dust evolution physics with polarisation (GRADE-POL). II. On the physical basis of Serkowski and super-Serkowski polarisation spectra","primary_cat":"astro-ph.GA","submitted_at":"2026-06-11T09:50:18+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04713","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Statistical analysis of the relative orientations between filaments and magnetic fields using Herschel and Planck data in star-forming regions","primary_cat":"astro-ph.GA","submitted_at":"2026-06-03T10:46:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Low-column-density filaments align parallel to magnetic fields while high-column-density wide filaments align perpendicular, with transition at roughly 0.8-8 x 10^21 cm^-2; projection effects analyzed statistically.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21101","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"B-Fields and Star Formation across Scales with TRAO (B-FROST): CO Abundances, Dynamics and Relative Orientations in the Translucent High Latitude Cloud MBM12","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T12:30:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Observational study of MBM12 shows CO-to-H2 conversion factor near galactic average with density-dependent variations, high virial parameters decreasing at small scales, broken power-law mass-size relations indicating external pressure, and magnetic field orientation transition at N(H2) = 4.5e21 cm-","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":": B-FROST: B-Fields and Star Formation across Scales with TRAO Fig. 2.Spatial variation in the 250µm dust opacity in MBM12, κ1200, derived from the ratio ofτ 1200 andA K, accounting for vari- able molecular gas fraction. The conversion assumes an extinction curve withR V =3.1, andN(H)/A K =1.67×10 22 cm−2 mag−1 (Cardelli et al. 1989; Bohlin et al. 1978; Lewis et al. 2022). Contours ofκ 1200 =[0.16,0.18,0.2,0.22,0.24] cm 2 g−1 are overplotted. platform (Lombardi & Alves 2001; Lombardi 2009)5. We chose a control field close to MBM12, and a smoothing FWHM of 5 ′, and a pixel size of 2.5 ′. We then convolved and reprojected the τ1200 map to the same grid and used Eq. 4 to produce the spatial variation inκ 1200 (Fig. 2). We also took spatial variations inf mol into account (App."},{"citing_arxiv_id":"2605.20835","ref_index":33,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T07:26:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Oblique filament collisions lead to gravitational collapse of the compressed cloud when post-collision |gravitational energy| exceeds kinetic plus thermal plus magnetic energies, with lower angles and lower velocities favoring hub-filament formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}