{"total":14,"items":[{"citing_arxiv_id":"2605.20622","ref_index":175,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Connecting CGM enrichment with Lyman alpha emitters at 2.9 < z < 6.7","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T02:15:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Blind MUSE search detects 156 LAEs at 2.9<z<6.7 with 34 C IV and 14 Mg II absorber associations, indicating low-mass galaxies enrich the CGM.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.26702","ref_index":1,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"SRGA J115215.0$-$510656: an unusual long-period eclipsing dwarf nova with disc wind signatures","primary_cat":"astro-ph.SR","submitted_at":"2026-04-29T14:10:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"SRGA J115215.0-510656 is a long-period U Gem-type dwarf nova with eclipses, a K3 secondary, and disc wind signatures in its outburst spectra.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24431","ref_index":43,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"CSST Preparations: Galaxy Completeness and S\\'ersic Profile Fitting across the Wide, Deep, and Extreme Fields","primary_cat":"astro-ph.GA","submitted_at":"2026-04-27T12:58:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Mock CSST images yield 95% completeness limits of 26.3-28.5 mag for point sources and 24.4-27.1 mag for galaxies, with fainter objects showing systematic overestimates in magnitude, size, and surface brightness and underestimates in Sersic index and axis ratio.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"tems (B/T=0) andn=4 for purely bulge-dominated sys- tems (B/T=1). The upper limit ofnis therefore 4. The axis ratioqand position angle (PA) are computed in the same manner: q=q disk (1−B/T)+q bulge B/T(2) and PA=PA disk (1−B/T)+PA bulge B/T.(3) The intrinsic effective radius (R e) is then determined nu- merically through isophotal analysis withPythonpackage Photutils[43], using elliptical isophotes defined by the de- rivedqand PA. Based on the resulting structural parameters, the surface brightness at the effective radius,Ie, is computed 2) https://csst-tb.bao.ac.cn/code/csst-sims/csst msc sim Ziqi Ma, et al. Sci. China-Phys. Mech. Astron.January (2024) V ol. xxx No. xx000000-4 analytically. The final single-S'ersic surface brightness profile"},{"citing_arxiv_id":"2604.20195","ref_index":115,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Photometric Super-Resolution for Improving Galaxy Morphological Measurements using Conditional Generative Adversarial Networks","primary_cat":"astro-ph.IM","submitted_at":"2026-04-22T05:23:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Neo, a cGAN, super-resolves HSC images to HST-like quality and improves galaxy morphological parameter accuracy by factors of 2-10.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19674","ref_index":7,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Resolved UV-Optical HST Imaging and Spectral Energy Distribution Modeling of Nearby BAT Active Galactic Nuclei","primary_cat":"astro-ph.GA","submitted_at":"2026-04-21T16:54:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"HST-resolved SEDs for seven nearby BAT AGN show host-galaxy contamination biases accretion-disk temperature by ~2 eV, extinction by ~2.2 mag, bolometric luminosity by ~0.57 dex, and X-ray bolometric corrections by ~0.66 dex relative to Swift/UVOT data.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"extended features that are not visible in the Swift/UVOT data. The difference in the UV magnitude of the central point source, as measured from the Swift and HST data, increases from left to right and is listed in Table 2. T able 1.Sample Properties. BAT ID Counterpart NamezlogM BH logL 2−10 keV logL bol logλ Edd Spectral Type (1) (2) (3) (4) (5) (6) (7) (8) 1189 NGC7603 0.023 8.59 43.62 45.34 -1.95 Sy1 335 UGC3478 0.012 6.06 42.29 43.26 -0.84 Sy1.5 34 UGC524 0.036 7.62 42.71 44.44 -1.49 Sy1.5 134 NGC985 0.043 8.11 43.76 44.98 -1.32 Sy1.5 925 VIIZw142 0.063 7.43 43.15 44.61 -1.07 Sy1.5 130 Mrk1044 0.016 6.45 42.23 44.04 -0.58 Sy1 549 IC2921 0.043 7.70 42.82 44.29 -1.058 Sy1.5 Note- (1)Swift/BAT ID (W."},{"citing_arxiv_id":"2604.18696","ref_index":13,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Other red dots: A possible GLIMPSE of normal AGB stars at Cosmic Noon through extreme lensing","primary_cat":"astro-ph.GA","submitted_at":"2026-04-20T18:00:10+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Four faint red point sources near critical curves in JWST images of Abell S1063 are interpreted as extremely magnified AGB stars and a yellow supergiant at cosmic noon.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16619","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Evidence for Environmental Stripping in the Coma Cluster","primary_cat":"astro-ph.GA","submitted_at":"2026-04-17T18:15:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Globular cluster deficits in several Coma galaxies, revealed by Voronoi density maps and asymmetry tests, provide evidence for environmental stripping.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"41(0.07) 0.45 -0.08(0.15) 6.3 edge NGC 4874 274.2 LEDA 44616 -20.29 32(8) 0.24(0.06) 0.44 -0.46(0.14) 3.8 NGC 4874 319.5 IC 3976 -20.28 38(7) 0.30(0.05) 0.44 -0.33(0.11) 5.8 edge NGC 4874 401.6 NGC 4875 -20.13 43(9) 0.38(0.08) 0.44 -0.12(0.18) 4.8 NGC 4874 189.2 LEDA 44792 -20.11 57(12) 0.51(0.11) 0.43 0.18(0.25) 4.7 NGC 4889 428.1 LEDA 44809 -20.05 73(10) 0.70(0.09) 0.43 0.61(0.22) 7.3 NGC 4889 463.0 LEDA 44723 -19.79 20(6) 0.24(0.07) 0.44 -0.45(0.17) 3.2 NGC 4889 360.1 LEDA 44656 -19.77 62(13) 0.77(0.16) 0.44 0.75(0.37) 4.7 NGC 4874 166.0 Note-Systems passing the detection criterionZ≥3; quoted uncertainties are 1σ. ter population (e.g., NGC 4876). These variations high- light the complex, overlapping nature of GCS in the"},{"citing_arxiv_id":"2604.15089","ref_index":6,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"An FUor-like Outbursting Class I Protostar in NGC 7538","primary_cat":"astro-ph.SR","submitted_at":"2026-04-16T14:49:26+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A deeply embedded Class I protostar in NGC 7538 underwent an FUor-like outburst lasting years, detected through WISE mid-IR light curves showing rapid rise, peak, and slow fade.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.09897","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Study of HH 270 with the James Webb Space Telescope","primary_cat":"astro-ph.SR","submitted_at":"2026-04-10T20:49:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"JWST, Subaru, and ALMA observations of HH 270 identify a new collimated jet closer to the source and show interactions between the shock-excited jet and the molecular outflow.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.06380","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Wonderful World of Binary Stars","primary_cat":"astro-ph.SR","submitted_at":"2026-04-07T19:08:09+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Student teams at an ESO school obtained spectroscopic and photometric data on binary stars and blue stragglers, confirming alignment due to tides, cluster membership via abundances, delta Scuti pulsation, and a binary central star in a planetary nebula.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.01326","ref_index":19,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Calibrating Photometric Mid-Infrared Star Formation Rates for JWST","primary_cat":"astro-ph.GA","submitted_at":"2026-04-01T19:08:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Rest-frame 6-8um MIRI luminosity provides broken power-law SFR calibrations with 0.2-0.3 dex scatter and UV+IR composites at 0.15 dex, supporting robust use above log M* ~9 up to z~3.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.20460","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Coma Physics of an Interstellar Object: JWST Spatial-Spectral Mapping of 3I/ATLAS","primary_cat":"astro-ph.EP","submitted_at":"2026-03-20T19:40:35+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":"2602.02702","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Connecting the Dots: UV-Bright Companions of Little Red Dots as Lyman-Werner Sources Enabling Direct Collapse Black Hole Formation","primary_cat":"astro-ph.GA","submitted_at":"2026-02-02T19:13:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"UV-bright companions to Little Red Dots provide Lyman-Werner fluxes of J21 ~ 10^2.5-10^5 that can suppress H2 cooling and enable direct collapse to massive black holes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.08931","ref_index":13,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Expanding the High-z Supernova Frontier: \"Wide-Area\" JWST Discoveries from the First Two Years of COSMOS-Web","primary_cat":"astro-ph.HE","submitted_at":"2026-01-13T19:10:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST difference imaging from COSMOS-Web and PRIMER has yielded 68 high-redshift supernovae including a core-collapse event at z>3 and a Type Ia at z>2, demonstrating the feasibility of wide-area time-domain searches in the early universe.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}