{"total":30,"items":[{"citing_arxiv_id":"2606.26075","ref_index":46,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Glossy Silicate Clouds on the Scorched Dayside of LTT9779b","primary_cat":"astro-ph.EP","submitted_at":"2026-06-24T17:50:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First statistically significant detection of dayside silicate clouds on a Neptunian-mass exoplanet, with CO and CO2 detections and C/O ratio of 0.984 from JWST spectra.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24114","ref_index":152,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Kepler Image-Subtracted Light Curves and Variable Star Catalog of NGC 6819","primary_cat":"astro-ph.SR","submitted_at":"2026-06-23T04:01:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Kepler image-subtracted photometry yields 81,498 light curves and a catalog of 87 periodic variable candidates in NGC 6819, including 26 newly discovered ones.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23774","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"C, N, O, S, and photochemistry in a temperate giant planet orbiting a late M dwarf","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T18:00:00+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Transit spectrum of TOI-6894b indicates 3-10x solar metallicity with solar C/O, N/O, and S/O ratios, similar to Jupiter and Saturn.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21855","ref_index":158,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The panchromatic JWST dayside spectrum of WASP-121 b reveals a refractory-rich formation","primary_cat":"astro-ph.EP","submitted_at":"2026-06-20T03:23:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Panchromatic JWST spectrum of WASP-121 b detects SiO and measures refractory-to-volatile ratios 3x stellar, consistent with mixed solid-gas accretion or migration with continued solid accretion.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17218","ref_index":27,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Transit Timing Variations in TESS: A Catalog from the First Five Years","primary_cat":"astro-ph.EP","submitted_at":"2026-06-15T19:05:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First TESS TTV catalog from 175 multi-TOI systems detects significant variations in 20 systems (13 new), showing 2:1 resonance pile-up unlike Kepler's 3:2.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12010","ref_index":57,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The 35-Myr old infant planet TOI-837 b has a mildly misaligned orbit","primary_cat":"astro-ph.EP","submitted_at":"2026-06-10T12:33:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"TOI-837 b has a true obliquity of 25.9+7.5-6.3 deg, the first planet younger than 100 Myr with accessible ψ incompatible with an aligned orbit, favoring primordial disc torque followed by disc-driven migration.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09973","ref_index":39,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Stellar Obliquities of Young Systems, Atmospheres Undergoing Contraction and Escape (SOYSAUCE) II: a 135 Myr planet on an aligned orbit with transit timing variations","primary_cat":"astro-ph.EP","submitted_at":"2026-06-08T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Validation of a 135 Myr, 3.6 R_E transiting planet with aligned obliquity and TTV evidence for a near-resonant companion.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.07511","ref_index":47,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"GJ 3929 b as the First Complete Rocky Worlds DDT Data Set","primary_cat":"astro-ph.EP","submitted_at":"2026-06-05T17:59:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Complete four-observation JWST dataset for GJ 3929 b yields 118±22 ppm eclipse depth, consistent with bare rock while allowing thin atmospheres and ruling out only thick CO2 cases at >3σ.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04875","ref_index":151,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Model Selection Criterion for Multidimensional Gaussian Processes: Application to Radial Velocities","primary_cat":"astro-ph.IM","submitted_at":"2026-06-03T13:38:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Introduces MGIC_rv, an information criterion that combines conditional RV likelihood with an effective parameter count for selecting multi-GP models focused on radial velocities.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.03740","ref_index":92,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"KRONOS I: The $1{-}2.8\\mu$m JWST Transmission Spectrum of the 23 Myr V1298 Tau c","primary_cat":"astro-ph.EP","submitted_at":"2026-06-02T14:55:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST NIRISS/SOSS data yield a transmission spectrum of the 23 Myr V1298 Tau c showing H2O absorption and an atmospheric metallicity of 14.8^{+56}_{-12} times solar, lower than mature planets of similar mass.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"each for a 1,000 step burn-in period followed by a 2,500 step sampling period. 3.2.Test Case 1: Masking Spot Crossing Events As the first and most conservative approach, we masked the apparent SCEs in each light curve. The full light curve modelF obs is therefore simply Fobs,1 (t) =T(θ, t)×S(θ, t).(2) No new parameters beyond those listed in Section 3.1 are required. Here, we usedbatman(L. Kreidberg 2015) for the transit modelT(θ, t). We identified the affected regions by eye as relative flux values that deviate from the expected smooth, lower floor of the transit, and were agnostic to whether such deviations could be from one or more individual starspot crossings. We identified and masked integrations 658- 850, 970-1300, 1370-1450, and 1550-1700 in both the"},{"citing_arxiv_id":"2606.02140","ref_index":7,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"AstroSkyFlow: an astronomical sky image flow simulator for time domain survey validation and machine learning","primary_cat":"astro-ph.IM","submitted_at":"2026-06-01T12:07:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"AstroSkyFlow generates simulated time-series astronomical images with realistic noise and variability, outperforming SkyMaker in noise and PSF reproduction while recovering injected signals such as exoplanet transits and asteroid trails.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00787","ref_index":86,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Pan-Pacific Planet Search -- IX. A menagerie of companions orbiting evolved stars","primary_cat":"astro-ph.EP","submitted_at":"2026-05-30T16:08:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Resolves six speculative companions into one giant planet, one eccentric brown dwarf, two low-mass stars, and two stars with no detectable companions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00177","ref_index":21,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Magnesium Silicate Clouds in the Atmosphere of HD 209458b from a Rule-Based Tree-Structured Data Reduction","primary_cat":"astro-ph.EP","submitted_at":"2026-05-29T14:00:29+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST MIRI/LRS data combined with archival observations detect magnesium silicate clouds (likely Mg2SiO4) in HD 209458b at 1-10 mbar with ~0.1 micron particles using a new rule-based data reduction approach.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.29428","ref_index":45,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"DELOS: Detecting Shallow Transits in Kepler Photometry Using a Contrastive-Learning Framework","primary_cat":"astro-ph.EP","submitted_at":"2026-05-28T06:22:22+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"DELOS applies contrastive learning to phase-folded light curves to detect shallow intermediate-to-long period transits, reporting 15.5% and 11.25% gains in combined precision-recall over BLS and TLS in low-SNR tests plus 3-80x speedups.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19000","ref_index":29,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Exoplanets in ancient stellar populations: occurrence constraints and hot-Jupiter candidates in the Galactic halo","primary_cat":"astro-ph.EP","submitted_at":"2026-05-18T18:19:30+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Hot Jupiter occurrence in the Galactic halo is low at ~0.13% with no significant difference between in-situ and accreted populations, well below disk rates.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16499","ref_index":49,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Revised Mass and Period for the Habitable Zone super-Earth GJ 3378b: A Planet Straddling the Cosmic Shoreline","primary_cat":"astro-ph.EP","submitted_at":"2026-05-15T18:00:14+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Joint radial-velocity analysis revises GJ 3378b's period to 21.45 days and minimum mass to 2.3 Earth masses, placing the habitable-zone planet near the cosmic shoreline.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15003","ref_index":56,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"JWST COMPASS Program: The 3--5$\\mu$m transmission spectrum of LTT 1445 A b","primary_cat":"astro-ph.EP","submitted_at":"2026-05-14T16:05:17+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST NIRSpec observations of LTT 1445 A b yield a featureless 3-5μm transmission spectrum, limiting atmospheric metallicity to ≳350× solar under grey-cloud models.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"curves fromEureka!as we have done in previous COM- PASS papers. We first iteratively trim 3σoutliers from a 50 point rolling median three times and trim the ini- tial 200 points (∼12 minutes) from the light curves to remove any initial ramps in the observation. We then fit the white light curve with a combination of an as- trophysical model usingbatman(Kreidberg 2015) with transit depth (R p/R∗), time of transit (T 0), inclination (i), and ratio of the semi-major axis to the stellar ra- dius (a/R∗) as free parameters, and a systematic model of the form S=p 1 +p 2 ×T+p 3 ×X+p 4 ×Y,(1) wherep N are free parameters,Tis the array of times, andXandYare arrays of the positions of the trace to be consistent with the simplest noise model that we"},{"citing_arxiv_id":"2605.05468","ref_index":48,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A single power law for the TRAPPIST-1 flare distribution across four orders of magnitude in energy","primary_cat":"astro-ph.SR","submitted_at":"2026-05-06T21:48:44+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"TRAPPIST-1 flares follow a single power law N(≥E_TESS) ∝ E_TESS^{-0.753} from 10^{29} to 10^{33} erg after sensitivity corrections and bandpass conversion.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05068","ref_index":39,"ref_count":2,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The NUV transit of XO-3 b","primary_cat":"astro-ph.EP","submitted_at":"2026-05-06T16:02:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"NUV transit depth of XO-3b measured at 0.1371 with 22-minute late center; X-ray data yield mass-loss rate ~10^4 g/s; bow-shock model predicts early rather than late transit.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Furthermore, computer simulations are needed to explore the circulation patterns and heating that can lead to aerosol formation and destruction patterns - which could produce SiO signatures - in the unique environment of this eccentric hot Jupiter. 7.ACKNOWLEDGEMENTS Software:Lightkurve(Lightkurve Collaboration et al. 2018),Julietand its dependencies (Kreidberg 2015; Es- pinoza et al. 2019; Speagle 2020),exoplanetand its dependencies (Foreman-Mackey et al. 2021; Foreman-Mackey et al. 2021; Foreman-Mackey et al. 2017b; Agol et al. 2020; Kumar et al. 2019; Astropy Collaboration et al. 2013, 2018; Luger et al. 2019) This work has made use of data from the European Space Agency (ESA) missionGaia(https://www.cosmos."},{"citing_arxiv_id":"2605.04936","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Horizontal transport as a source of disequilibrium chemistry on the nightside of a hot exoplanet","primary_cat":"astro-ph.EP","submitted_at":"2026-05-06T14:04:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST data on NGTS-10A b shows nightside CH4 depletion caused by day-to-night horizontal transport rather than vertical mixing or non-solar abundances.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04149","ref_index":49,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"TOI-159 b: an eccentric hot-Jupiter planet around a young, pulsating $\\gamma$ Doradus star","primary_cat":"astro-ph.EP","submitted_at":"2026-05-05T18:00:04+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"TOI-159 b is confirmed as the hottest known eccentric hot Jupiter (e = 0.24) with a 13-sigma Keplerian detection around a young gamma Doradus star, including a preliminary low-resolution transmission spectrum.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02036","ref_index":66,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"JWST unveils a high mean molecular weight atmosphere for mini-Neptune TOI-1130b: Evidence for formation beyond the water ice line","primary_cat":"astro-ph.EP","submitted_at":"2026-05-03T20:04:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The atmosphere of TOI-1130b shows high metallicity, low C/O, and elevated mean molecular weight consistent with ex-situ formation beyond the water ice line.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.23929","ref_index":77,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Uncovering the Rapidly Evolving Orbits of the Dynamic TOI-201 System","primary_cat":"astro-ph.EP","submitted_at":"2026-04-27T01:11:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"TOI-201 has three planets whose co-transiting configuration will end in 200 years due to Kozai-Lidov oscillations driven by mutual inclinations.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"model is based on the one developed in (75) to jointly model RVs andHipparcos-Gaiaastrometry, implementing modifications for handling multiplanet systems from (76). To our knowledge, TOI- 201 c is the first substellar companion to be detected simultaneously in RV, transit, and astrometry data. To incorporate the transit data in this model, we use thebatmanpackage (77) to generate transit models. Since this model assumes Keplerian dynamics, we cannot straightforwardly account for TTVs arising from inter-planet interactions. These effects have no impact on the astrometry at the level of precision; so for the sake of simplicity, we restrict the included photometric data to a single transit each for TOI-201 b and TOI-201 c."},{"citing_arxiv_id":"2604.19179","ref_index":61,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A tidally detached super Neptune on a strongly misaligned retrograde orbit","primary_cat":"astro-ph.EP","submitted_at":"2026-04-21T07:44:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"TOI-1710 b has a true obliquity of 149 degrees indicating retrograde motion, favoring high-eccentricity migration via planet-planet scattering and Kozai-Lidov cycles for this tidally detached super-Neptune.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.18579","ref_index":56,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The T16 Planet Hunt: 10,000 New Planet Candidates from TESS Cycle 1 and the Confirmation of a Hot Jupiter Around TIC 183374187","primary_cat":"astro-ph.EP","submitted_at":"2026-04-20T17:59:06+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A transit search on TESS Cycle 1 full-frame images produced 10,091 new planet candidates down to T=16 mag, more than doubling the known TESS total, with one hot Jupiter confirmed by radial velocity.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"cur at characteristic periods and ephemerides across a given CCD, therefore, when a period bin is overly pop- ulated and the associated candidates also share similar transit times, we remove those signals as likely system- atics. For all remaining candidates, we fit a planetary tran- sit model to the remaining light curves using theBATMAN package (Kreidberg 2015). Any candidate whose best fit planetary radius exceeds 2.5R J is discarded as a likely EB. This threshold is intentionally generous, additional large radius false positives are filtered later in the man- ual vetting step. TheBATMANfit performed here is a fast, initial fit that is applied to all candidates that pass our filters up to this stage. This initial fit often fails, lead-"},{"citing_arxiv_id":"2604.05907","ref_index":41,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Transit Timing and Transmission Spectrum of Hot Jupiter WASP-43 b from a decade of Multi-band Transit Follow-up Observations","primary_cat":"astro-ph.EP","submitted_at":"2026-04-07T14:10:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"New transit observations of WASP-43 b yield no evidence of orbital decay while revealing major challenges in combining multi-instrument data for atmospheric retrievals.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"11 availableJWSTlight curves reduced byEureka!v1 (Bell et al. 2022) from Bell et al. (2024). 3.TRANSITFIT LIGHT-CURVE MODELING To determine the planetary parameters of WASP-43 b, we usedTransitFit, a Python package designed for fit- ting multi-filter and multi-epoch exoplanet transit ob- servations simultaneously (Hayes et al. 2024). The pack- age employs the transit model frombatman(Kreidberg 2015) and utilizes dynamic nested sampling routines fromdynesty(Speagle 2020) to derive the parameters. As mentioned in Section 2, we utilized a large number of light curves from both ground-based and space-based observations. To mitigate issues related to computer memory, we divided the light curve data into four dis- tinct groups: Ground-based,HST,TESS, andJWST"},{"citing_arxiv_id":"2604.05570","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Investigation of Transit Timing and an Optical Transmission Spectrum of the Hot Jupiter WASP-11 b","primary_cat":"astro-ph.EP","submitted_at":"2026-04-07T08:13:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"New transit data for WASP-11 b over 16 years shows no orbital decay or TTV signals from other planets, with a transmission spectrum exhibiting a strong Rayleigh scattering slope possibly from the atmosphere or contamination.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"TESSJulian Date (BTJD) to Barycentric Julian Date (BJDTDB) by adding 2,457,000. 3.LIGHT-CURVE MODELING To derive the planetary parameters of WASP- 11 b/HAT-P-10 b, we employedTransitFit, a Python package designed for the simultaneous fitting of multi- filter and multi-epoch exoplanet transit observations (Hayes et al. 2024). This package utilizes thebatman transit model (Kreidberg 2015) and thedynestydy- namic nested sampling routines (Speagle 2020) to esti- mate system parameters. The transit light curves were divided into two groups: ground-based andTESS. For both datasets, each individual light curve was detrended 2 https://archive.stsci.edu/ 4 T able 2.The details of WASP-11 b/HAT-P-10 b transit observations obtained with the SPEARNET telescopes."},{"citing_arxiv_id":"2604.05305","ref_index":28,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Scientific Validation of the SPARC4 Pipeline: Multi-band Imaging, Polarimetry, and Photometric Time Series for Improved Characterization of Transiting Exoplanets","primary_cat":"astro-ph.EP","submitted_at":"2026-04-07T01:20:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The SPARC4 pipeline delivers 0.02% photometric and ~0.02% polarimetric precision on transiting exoplanet observations and refines planetary parameters through joint modeling with TESS or K2 data.","context_count":1,"top_context_role":"other","top_context_polarity":"unclear","context_text":"1 SPARC4 z band HATS-23 57072.8527(7) 2.1605160(50) 6.1 0.4 −0.3 0.159(20) 81.0 +0.9 −0.6 0.3728 0.3215 Bento et al. (2017) 58654.3462(11) 2.1605122(21) 8.7±1.8 0.099(16) 86.3±2.9 0.8(4) 0.4(4) only TESS data 58654.3463(11) 2.1605120(13) 7.20±0.18 0.1145(15) 83.92±0.270.70(25) 0.50(31)TESS+SP ARC4 58654.34689(18) FIXED 7.16±0.15 0.1133(26) 83.71±0.22 0.26(28) 0.8(4) 1.0±0.2 SPARC4 g band 58654.34618(8) FIXED 6.95±0.17 0.1143(16) 83.81±0.24 0.97(23) 0.30(27) 1.0±0.1 SPARC4 r band 58654.34652(11) FIXED 7.66±0.17 0.1097(23) 84.57±0.24 0.54(27) 0.52(35) 1.1±0.1 SPARC4 i band 58654.34529(18) FIXED 7.48±0.19 0.1102(27) 84.30±0.27 0.48(32) 0.64(40) 1.2±0.1 SPARC4 z band HATS-24 57038.4733(4) 1.3484954(13) 4.67 +0."},{"citing_arxiv_id":"2604.05049","ref_index":83,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Super-Solar Metallicity and Tentative Evidence for Photochemistry on WASP-96b from JWST and Ground-Based VLT Transmission Spectroscopy","primary_cat":"astro-ph.EP","submitted_at":"2026-04-06T18:01:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"WASP-96b shows super-solar metallicity of 2-6x stellar, roughly stellar C/O, tentative SO2 consistent with photochemistry, and an optical slope from scattering aerosols, supporting core-accretion formation beyond the water snowline.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"q2NRS2 U[0, 1] 0.35 +0.23 −0.29 Note-q1 and q2 refer to the Kipping (2013) re-parameterization of the quadratic limb-darkening law.T 0 is fit as the NIRISS mid-transit time and also propagated here to the epoch of the NIRSpec transit. We use the flexiblejulietpackage (Espinoza et al. 2019) to jointly fit the transit and RV datasets. The transit model usesbatman(Kreidberg 2015), assum- ing a circular orbit (Hellier et al. 2014) and with the orbital period,P, mid transit time (fixed to be that of the NIRISS/SOSS transit),T 0, scaled planet radius, Rp/R∗, impact parameter,b, scaled semi-major axis, a/R∗, and the two parameters of the Kipping (2013) parameterization of the quadratic limb-darkening law, q1 andq 2, as free parameters."},{"citing_arxiv_id":"2602.18553","ref_index":65,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"POSEIDON I: The Dynamical Origins of Transiting Neptunes","primary_cat":"astro-ph.EP","submitted_at":"2026-02-20T19:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"New obliquity measurements for two Neptunes update the sample distribution to favor aligned systems plus a random component, resembling that of more massive planets and implying shared dynamical origins.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}