{"total":15,"items":[{"citing_arxiv_id":"2607.01129","ref_index":97,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Tilting at the Turnover: Modeling the Faint-End of the UV Luminosity Function Behind Abell s1063 with JWST","primary_cat":"astro-ph.GA","submitted_at":"2026-07-01T16:14:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Using lensed JWST data behind Abell S1063, the UVLF at z~6-11 is fit with gradual quadratic turnover, yielding no evidence for turnover to M_UV=-13.5 at z=6, exclusion limits on turnover models, and lower bounds showing faint galaxies contribute >50% of UV luminosity density and ~64% of ionizing pho","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25070","ref_index":84,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"A Look at Eight Outbursts of Comet 7P/Pons-Winnecke","primary_cat":"astro-ph.EP","submitted_at":"2026-06-23T18:24:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Analysis of eight 2021 outbursts on comet 7P/Pons-Winnecke using ground-based photometry yields ejecta masses of 10^5-10^6 kg and normalized rates comparable to several other comets but discrepant with 67P spacecraft data.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21808","ref_index":46,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the stellar parameter dependence of the combined Fe I and Fe II chromospheric emission-line in the wings of the Ca II K line","primary_cat":"astro-ph.SR","submitted_at":"2026-06-20T00:05:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Observational analysis of 21 giant stars shows Fe I+Fe II blend emission proportional to Ca II K with matching Teff power-law exponent and a slope break in the flux ratio at log g ≈ 2.5.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18751","ref_index":51,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Dust colour, phase behaviour, and Monte Carlo modelling of interstellar comet 3I/ATLAS from 4 au pre- to 4 au post-perihelion","primary_cat":"astro-ph.EP","submitted_at":"2026-06-17T06:54:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Multi-band photometry and Monte Carlo modeling of interstellar comet 3I/ATLAS yield a dust size distribution with power-law index -3.5 and a phase curve showing opposition surge of 0.1-0.4 mag distinct from Solar System comets.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02984","ref_index":54,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Dust On, Dust Off: HST Observations of the Newly Dormant Jupiter Co-orbital Comet P/2023 V6 (PANSTARRS)","primary_cat":"astro-ph.EP","submitted_at":"2026-06-02T00:43:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"New HST observations of P/2023 V6 (PANSTARRS) document its transition to dormancy and yield a diameter estimate of approximately 340 meters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00218","ref_index":49,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Prospects of resolving and localising individual supermassive black hole binaries with pulsar timing arrays: the host ranking challenge","primary_cat":"astro-ph.GA","submitted_at":"2026-05-29T18:00:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations forecast 21-51% probability of resolving individual SMBH binaries with PTAs in 0-10 years, with localization areas containing ~190k early-type galaxies on average and a ranking method that excludes roughly half the candidates when galaxy properties are available.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19375","ref_index":75,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"AMPM II. A Lunar-Mass Primordial Black Hole Microlensing Candidate in the Milky Way Halo","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T05:20:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A ~60-minute microlensing event is interpreted via Bayesian modeling as a ~0.03 Earth-mass primordial black hole in the Milky Way dark-matter halo.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18976","ref_index":67,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Bulgeless Evolution And the Rise of Discs (BEARD) I. Physical drivers of the mass-size relation for Milky Way-like galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-05-18T18:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bulgeless galaxies trace the upper envelope of the mass-R1 relation with scatter driven by central stellar density and the spatial configuration of mergers rather than their number.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.24111","ref_index":53,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Morphological Identification and Study of Radio Galaxies from LoTSS DR2. III. The Multiwavelength Analysis of Winged Radio Galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-04-27T07:07:56+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Multiwavelength study of 621 winged radio galaxies shows XRGs are radio-luminous with frequent backflow signatures while ZRGs link to lower jet power and environmental perturbations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"whereM ∗/Lr−band is the stellar mass-to-light ratio in solar units andg−ris the rest-frame color (AB mag- nitudes). The zero point (−0.456) includes a−0.15 dex correction relative to a diet Salpeter IMF, consis- tent with a Chabrier IMF. Ther-band luminosity was then computed asLr−band = 10−0.4(Mr−Mr,⊙), adopting Mr,⊙ = 4.65in the AB system (C. N. A. Willmer 2018). We restricted the sample to sources with0.3≤g−r≤ 1.5, encompassing typical early-type galaxies (0.6-1.0), slightly earlier spirals (0.3-0.6), and red ellipticals with dust or metallicity effects (up to 1.5) (M. R. Blanton et al. 2005; M. Fukugita et al. 2007). Objects outside this range were excluded due to possible dust reddening, photometric errors, or other uncertainties."},{"citing_arxiv_id":"2604.22932","ref_index":102,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Characterization of the Volatile Properties of 133P/Elst-Pizarro and Other Main-Belt Comets with JWST and Ground-Based Observations","primary_cat":"astro-ph.EP","submitted_at":"2026-04-24T18:05:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JWST observations of 133P/Elst-Pizarro yield water outgassing rates of (1.9 ± 0.6) × 10^25 and (1.4 ± 0.4) × 10^25 molecules/s at true anomalies 8° and 37.4°, with hypervolatile depletion Q(CO2)/Q(H2O) < 0.009 and an average log(Afrho/Q(H2O)) = -24.6 ± 0.2 across three MBCs.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"using separate detectors fed by a dichroic. Each detec- tor is 2040×2048 pixels in size, but with pixel scales of 0.′′0313 pixel −1 and 0.′′0630 pixel −1 for the F200W and F277W images, respectively. These different scales provide angular fields of view of 63.′′9×64.′′1 (F200W im- ages) and 128.′′5×129. ′′0 (F277W images), respectively. When observing a Solar spectrum (C. N. A. Willmer 2018), the F200W and F277W filters (spanning wave- lengths between 1.725µm to 2.260µm, and 2.367µm to 3.220µm, respectively) are characterized by effec- tive wavelengths of 1.97µm and 2.74µm, respectively (M. S. P. Kelley et al. 2023). The 4-point INTRAMOD- ULEBOX dither pattern was used to enable mitigation of detector artifacts and cosmic rays, with one exposure"},{"citing_arxiv_id":"2604.22931","ref_index":86,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Emerging Diversity Among the Main-Belt Comets: Insights from JWST and Ground-Based Observations of 457P/Lemmon-PANSTARRS","primary_cat":"astro-ph.EP","submitted_at":"2026-04-24T18:04:51+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"457P shows dust activity without detectable H2O, CO, CO2, or CH3OH, with Q(H2O) < 2e24 molecules/s, indicating it may be more volatile-depleted than other main-belt comets.","context_count":1,"top_context_role":"dataset","top_context_polarity":"use_dataset","context_text":"multaneously with a dichroic and two separate detec- tors. Each detector has a field of view 2040×2048 pixels in size. The pixel scales are different, however, 0.′′0313 pixel −1 and 0.′′0630 pixel −1 for the F200W and F277W images, respectively, for an angular field of view of 63.′′9×64.′′1 for F200W images and 128.′′5×129.′′0 for F277W images. For the Solar spectrum as reported by C. N. A. Willmer (2018), the F200W and F277W filters (covering wavelengths between 1.725µm to 2.260µm, and between 2.367µm to 3.220µm, respectively) ob- tain effective wavelengths of 1.97µm and 2.74µm, re- spectively (M. S. P. Kelley et al. 2023). Each of four exposures was obtained using the 4-point INTRAMOD- ULEBOX dither pattern to mitigate detector artifacts and any cosmic ray strikes."},{"citing_arxiv_id":"2604.19975","ref_index":280,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The FUor Mass Distribution Matches the Solar Neighborhood IMF: Evidence for a Universal Eruptive Phase","primary_cat":"astro-ph.SR","submitted_at":"2026-04-21T20:34:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FUor masses inferred from Keplerian line broadening in H-band spectra match the solar neighborhood IMF, indicating a universal eruptive phase during star formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16792","ref_index":179,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Role of Cluster Environments in Quiescent Galaxy Stellar Halo Assembly","primary_cat":"astro-ph.GA","submitted_at":"2026-04-18T02:39:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"High-mass quiescent galaxies in clusters assemble more luminous stellar halos than field galaxies while low-mass cluster galaxies assemble less luminous ones over 0.1 < z < 1.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"05mag/arcsec 2 in inner regions (2Re, first vertical black line in Figure 4) to∼1mag/arcsec 2 in the outermost regions of profiles (10Re, second vertical black line in Figure 4). Extracted profileµvalues (AB magnitudes/arcsecond 2) are corrected for cosmological surface brightness dimming (µ∝(1 +z) −3 when using AB magnitudes; Whitney et al. 2020). We use absolute solar magnitudes ingrizybands from Willmer (2018) to convertµvalues intoL ⊙/pc2 units. Additionally, we convert the major axis profiles that are given byGalPRIMEinto circularized profiles viaR= √ ab, where 8 local = 24.3 mag/arcsecond2 RBCG = 51 (309 kpc) Pixels Masked = 24.3% 2\" 1 2 4 6 8 10 20 22 24 26 28 30 32 [mag/arcsec2] Lhalo: -7.1% BG Extracted Profile SimGal Model local = 26.4 mag/arcsecond2"},{"citing_arxiv_id":"2604.16727","ref_index":85,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Metallicity Gradient of Sagittarius Dwarf Spheroidal Galaxy Prior to Infall Constrained by S-PLUS Observations of its Tidal Stream","primary_cat":"astro-ph.GA","submitted_at":"2026-04-17T22:02:24+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The Sagittarius dwarf progenitor had a metallicity gradient of roughly -0.3 dex per kpc prior to infall.","context_count":1,"top_context_role":"other","top_context_polarity":"background","context_text":"2007; S. Hasselquist et al. 2021). However, a self- consistent chemodynamical model of this interplay still does not exist. Apart from these stellar population differences be- tween the remaining core of Sgr and its leading and 16 Assuming this galaxy'sV-band absolute magnitudeM V = −13.27 (S. R. Majewski et al. 2003),M V,⊙ = +4.81 for the Sun (C. N. A. Willmer 2018), and a mass-to-light ratio of 2, which is appropriate for non-star-forming systems (e.g., J. D. Simon 2019). 17 [X/Y] = log (N X/NY)⋆ −log (N X/NY)⊙, whereN X (NY) is the number density of atoms of element X (Y) for a given star (⋆) relative to the Sun (⊙). trailing arms, many authors have reported chemical vari- ations within the stream itself (M."},{"citing_arxiv_id":"2601.16191","ref_index":41,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"On the Missing Red Giants near the Galactic Center","primary_cat":"astro-ph.GA","submitted_at":"2026-01-22T18:43:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Tidal stripping fails to explain missing bright red giants near Sgr A* as loss-cone diffusion scales too weakly with stellar radius compared to the rapid drop in red-giant lifetimes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}