{"total":19,"items":[{"citing_arxiv_id":"2606.24114","ref_index":154,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":29,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"2606.23551","ref_index":57,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Observing a 542-day transiting giant with large TTVs: The 2025 transit of HIP 41378 f and new constraints on the outer system","primary_cat":"astro-ph.EP","submitted_at":"2026-06-22T16:25:34+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"darkening coefficients (q 1,q 2) as free parameters. Gaussian pri- ors were imposed on these parameters based on the results of Lund et al. (2019) and Grouffal et al. (in press). Priors on the limb-darkening coefficients were computed using the PyLDTk package (Husser et al. 2013; Parviainen & Aigrain 2015), adopt- ing theq 1,q 2 parameterization introduced by Kipping (2013). For each instrument and observing campaign, an additional jit- ter term was included, to account for white noise, and added in quadrature to the photometric uncertainties. We applied an over- sample factor to the K2 observations to match the overall ca- dence of the datasets (⪅2 mins). The light-curves were modeled using the thebatmanpackage (Kreidberg et al."},{"citing_arxiv_id":"2606.18355","ref_index":88,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Revisiting the Exo-Mercury Candidate GJ 367 b with ESPRESSO and a Self-Consistent Tidal Distortion Model","primary_cat":"astro-ph.EP","submitted_at":"2026-06-16T18:03:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Revised mass of 0.503 M_Earth and radius of 0.736 R_Earth for GJ 367 b give a density of 6.9 g cm^{-3} and an iron fraction of 50-70% via new tidal and composition modeling.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"A&A, 602, A88, doi: 10.1051/0004-6361/201630153 Barragán, O., Gandolfi, D., Dai, F., et al. 2018, A&A, 612, A95, doi: 10.1051/0004-6361/201732217 Benz, W., Anic, A., Horner, J., & Whitby, J. A. 2007, Space Science Reviews, 132, 189, doi: 10.1007/s11214-007-9284-1 Benz, W., Slattery, W. L., & Cameron, A. G. W. 1988, Icarus, 74, 516, doi: 10.1016/0019-1035(88)90118-2 Berger, T. A., Huber, D., van Saders, J. L., et al. 2020, AJ, 159, 280, doi: 10.3847/1538-3881/159/6/280 Berger, T. A., Schlieder, J. E., & Huber, D. 2023, arXiv e-prints, arXiv:2301.11338, doi: 10.48550/arXiv.2301.11338 Betancourt, M. 2017, arXiv e-prints, arXiv:1701.02434, doi: 10.48550/arXiv.1701.02434 Boley, K. M., Panero, W. R., Unterborn, C."},{"citing_arxiv_id":"2606.17218","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"2606.09973","ref_index":42,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"2606.04875","ref_index":100,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"2605.28719","ref_index":253,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Homogeneous Catalog of Rossiter-McLaughlin Systems: Distinct $e$-$\\lambda$ Trends in Three Gas-Giant Mass Regimes","primary_cat":"astro-ph.EP","submitted_at":"2026-05-27T16:39:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Homogeneous reanalysis of 145 single-star RM systems reveals mass-dependent e-λ trends: sub-Saturns eccentric and misaligned, Jupiters misaligned only when circular, and super-Jupiters aligned at all eccentricities.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Accordingly, we treat these as hitherto under-explored degrees of freedom and search for empirical structure in thee-ψplane, recognizing thateandψneed not rise and fall together but can retain specific,correlatedimprints of distinct dynamical pathways. A range of statistical techniques can be used to infer eccentricity from the photo-eccentric effect (R. I. Daw- son & J. A. Johnson 2012; D. M. Kipping 2013), es- timate mutual inclinations from multiplicity statistics (J. J. Lissauer et al. 2011; S. Tremaine & S. Dong 2012), transit-duration distributions (D. C. Fabrycky et al. 2014), and transit-timing and transit-duration variations (TTVs/TDVs, W. Zhu et al. 2018; S. C. Mill- holland et al. 2021). Simultaneously, line-of-sight stellar obliquity (i⋆) can be constrained fromvsini ⋆ statistics"},{"citing_arxiv_id":"2605.19000","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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":"2605.12324","ref_index":121,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"An Ultra-Short Period Super-Earth and a Sub-Neptune Orbiting the K dwarf TOI-4311","primary_cat":"astro-ph.EP","submitted_at":"2026-05-12T16:07:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"TOI-4311 hosts a 0.99-day super-Earth (1.38 R_earth, 4.5 M_earth) and 15-day sub-Neptune (2.47 R_earth), plus a candidate 38-day planet, with the dense inner planet potentially challenging formation theories given the host's galactic population.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.08544","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Bayesian Doppler Imaging: Simultaneous Inference of Surface Maps and Geometric Parameters","primary_cat":"astro-ph.EP","submitted_at":"2026-05-08T23:10:07+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A fully Bayesian pixel-based Doppler imaging framework uses Gaussian Process priors and Hamiltonian Monte Carlo to simultaneously infer surface maps and geometric parameters from spectral data.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"obtained by integrating over the nonlinear parameters: p(a|d) = Z p(a|d,θ)p(θ|d)dθ.(30) Since the integral is analytically intractable, we ap- proximate it using the MCMC samples{θ (s)}Nsamples s=1 . Substituting the empirical measurep(θ|d)≈ 1 Nsamples PNsamples s=1 δ(θ−θ (s)) into Eq. (30) yields the Monte Carlo approximation p(a|d)≈ 1 Nsamples NsamplesX s=1 p(a|d,θ (s)),(31) i.e., a finite mixture of Gaussians weighted uniformly by the MCMC samples. While this mixture does not collapse to a single Gaus- sian, its moments are readily computed. In particular, the posterior mean and variance of the surface map are approximated by ¯µ:=E[a|d]≈ 1 Nsamples NsamplesX s=1 µ(s) a|d,(32) Var[a|d]≈ 1 Nsamples × NsamplesX s=1 \u0002 Σ(s)"},{"citing_arxiv_id":"2605.05068","ref_index":35,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"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":"Limb Darkening Toolkit (LDTK, Parviainen & Aigrain 2015) using XO-3 stellar parameters from Stassun et al. (2017) and Bonomo et al. (2017), and the XMM-Newton OM response files for UVM2. The toolkit returned quadratic NUV LDCsu 1=1.553,u 2=-0.641. For the second fit, we introduced quadratic optical LDCs as free parameters in the model, using theQuadLimbDarkprior distribution fromexoplanet. This distribution is based on the Kipping (2013) quadratic limb darkening law, and provides an uninformative prior. This added two parameters to the joint model, which only applied to the optical transits (TESS and ISAS). We conducted a third fit with both the optical and NUV LDCs as free parameters. However, we do not include these results because freeing the NUV LDCs did not improve the goodness-of-fit statistics and merely increased the"},{"citing_arxiv_id":"2605.04149","ref_index":50,"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":"2604.19179","ref_index":62,"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":53,"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":"the first transit), the planet-to-star radius ratio, the scaled semi-major axis (a/R ⋆), the orbital inclination, and the two limb-darkening coefficients. We use the quadratic limb-darkening law first introduced by Kopal (1950): I(µ)/I(1) = 1−u 1(1−µ)−u 2(1−µ) 2,(4) whereµ= cos(θ) andθis the angle between the line of sight and the local stellar surface normal. We adopt the parameterization of Kipping (2013), which redefines the limb-darkening coefficients as q1 = (u1 +u 2)2,(5) and q2 = u1 2(u1 +u 2) ,(6) allowing uniform priors while ensuring physically mean- ingful combinations ofu 1 andu 2. We assume circular or- bits (e= 0) for all candidates. TheBATMANlight curves are computed using a supersampling factor of 3 and an exposure time of 30 minutes, matching the cadence of"},{"citing_arxiv_id":"2604.06595","ref_index":36,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"An Aligned Very-Low-Mass Star Orbiting an M dwarf and Obliquity Patterns Across Giant Planets, Brown Dwarfs, and Binary Stars","primary_cat":"astro-ph.EP","submitted_at":"2026-04-08T02:27:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First obliquity measurement in an M dwarf binary shows alignment, with tentative evidence that aligned orbits around cool stars and wide separations also hold for brown dwarfs and binaries.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"vided by the orbital semi-major axis ((R ∗ +R c)/a), cosine of the orbital inclination (cosi c), RV semi- amplitude (K), two parameters related to eccentricity and argument of periastron (√ecosωand √esinω), the sky-projectedspin-orbitangle(λ)andtheprojectedstel- lar rotational velocity (vsini). For the photometry, we adopted a quadratic limb-darkening law for the TESS data (Kipping 2013) but a linear law for the ground- based RBO light curve, given its low-cadence and lim- ited data points. Since the TESS simple aperture pho- tometry has uncorrected light dilution effect due to the large pixel size (21′′pixel−1), we fitted a contaminating flux ratioF C/(FC +F T ), whereF T andF C are the flux of the target and nearby contaminating sources."},{"citing_arxiv_id":"2604.06388","ref_index":28,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Determining the Host Stars of Planets in Binary Star Systems with Asterodensity Profiling: Investigating the Canonical Radius Gap","primary_cat":"astro-ph.EP","submitted_at":"2026-04-07T19:19:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Probabilistic host-star assignments via asterodensity profiling suggest the exoplanet radius gap is less empty in binary systems once possible circumsecondary planets are included.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"whether planets in binary systems mostly orbit the pri- mary star, the secondary star, or a mix of both. Therefore, it is necessary to identify the host star to measure accurate planet properties. One method for doing so relies on the asterodensity profiling technique, whereby the density of a planet's host star can be es- timated from transit fitting (Seager & Mall' en-Ornelas 2003; Kipping 2014). If there are independent estimates of the stellar densities in a binary, than the asteroden- sity estimate should be consistent with the star that is hosting the planet (e.g. Sliski & Kipping 2014; Barclay et al. 2015; Torres et al. 2015; Gaidos et al. 2016; Lester et al. 2022; Eastman et al. 2023). Other methods for determining the host star include spatially resolving the"},{"citing_arxiv_id":"2604.05049","ref_index":80,"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":"q1TESS U[0, 1] 0.34 +0.05 −0.05 q2TESS U[0, 1] 0.14 +0.10 −0.18 q1SOSS1 U[0, 1] 0.14 +0.01 −0.01 q2SOSS1 U[0, 1] 0.46 +0.13 −0.14 q1SOSS2 U[0, 1] 0.29 +0.02 −0.02 q2SOSS2 U[0, 1] 0.58 +0.10 −0.10 q1NRS1 U[0, 1] 0.05 +0.01 −0.01 q2NRS1 U[0, 1] 0.11 +0.08 −0.15 q1NRS2 U[0, 1] 0.04 +0.01 −0.01 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."},{"citing_arxiv_id":"2602.18553","ref_index":63,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"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}