{"total":35,"items":[{"citing_arxiv_id":"2607.01095","ref_index":32,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Automatic detection of solar filament oscillations I: Multi-scale spectral pipeline","primary_cat":"astro-ph.SR","submitted_at":"2026-07-01T15:48:58+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"A multi-scale spectral pipeline using deep learning filament detection automatically identifies 91 oscillatory events in two weeks of 2014 GONG data, recovering known events and finding new ones with periods 20-126 min.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2607.00921","ref_index":143,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Spatially resolved optical and mid-infrared spectroscopy of SDSS1335+0728: implications for the origin of the Ansky event","primary_cat":"astro-ph.GA","submitted_at":"2026-07-01T13:24:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Spatially resolved spectroscopy shows SDSS1335+0728 has a three-zone ionisation structure, optically thin dust, and sustained low-level nuclear activity for at least 1500 years, implying the Ansky event is a faint transient in an already accreting low-mass SMBH.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.30280","ref_index":155,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Multi-year Ground-Based Survey Photometry of Active Comet 103P/Hartley 2 and Centaur (2060) Chiron: A Tale of Two Comets in the Pre-LSST Era","primary_cat":"astro-ph.EP","submitted_at":"2026-06-29T13:23:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reports asymmetric heliocentric activity slopes for 103P/Hartley 2 and exponential outburst decay plus flattening phase curves for Chiron from ATLAS, ZTF, and LCO photometry.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.29653","ref_index":34,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Pulsed Infrared Emission from Magnetar 4U 0142+61 Detected by JWST","primary_cat":"astro-ph.HE","submitted_at":"2026-06-28T23:46:34+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST timing observation detects pulsed IR emission from magnetar 4U 0142+61 matching its spin period, with flux 22.9±0.6 μJy and ~10% pulsed fraction lower limit.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.28446","ref_index":49,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Domain-Informed Multi-View Self-Distillation for Astronomical Light-Curve Representation Learning with JEPA","primary_cat":"astro-ph.IM","submitted_at":"2026-06-26T08:35:55+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A JEPA-based model with domain-informed multi-view self-distillation learns light-curve representations that outperform hand-crafted features on 15 of 16 StarEmbed metrics and adapts competitively to other irregular time-series datasets.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26411","ref_index":56,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"A Spitzer Space Telescope Exploration Science Program to Search for Y Dwarf Variability","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T22:10:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Spitzer mid-IR monitoring of all known Y dwarfs yields variability fractions of 35-75% that, when combined with L/T dwarf data, weakly support condensate cloud variations as the driver of brown dwarf variability.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26358","ref_index":29,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Predictions of Transiting Exoplanet Confirmations from Rubin LSST Surveys","primary_cat":"astro-ph.EP","submitted_at":"2026-06-24T20:13:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"Simulations predict very limited transiting exoplanet confirmations from LSST due to observing cadence constraints, with only a few possible in DDF for hot planets on M dwarfs.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25517","ref_index":16,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Unveiling the nature of barium stars. I. Asteroseismic masses and the evolutionary link between Ba dwarfs and giants","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T07:50:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Asteroseismic masses average 1.29 Msun for Ba dwarfs versus 1.96 Msun for Ba giants, supporting main-sequence accretion evolution from dwarfs to giants, though models fail to match the observed [hs/ls] ratio.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"2013, (2) Shejeelammal et al. 2020, (3) Roriz et al. 2025, (4) de Castro et al. 2016, (5) Komiya et al. 2007, (6) Barbuy et al. 1992, (7) Tomkin & Lambert 1979, (8) Sneden et al. 1981, (9) Smiljanic et al. 2007, (10) Masseron et al. 2010, (11) Andrievsky et al. 2002, (12) Zacs 1994, (13) Katime Santrich et al. 2013, (14) Yang et al. 2024, (15) Karinkuzhi et al. 2018, (16) Smith 1984, (17) Jorissen 1988, (18) Karinkuzhi & Goswami 2014, (19) Karinkuzhi & Goswami 2015, (20) Dimoffet al. 2024, (21) Tomkin et al. 1976, (22) Deming 1978, (23) Kong et al. 2018b, (24) Merle et al. 2016, (25) Liang et al. 2003, (26) Luck 2017, (27) Soubiran & Girard 2005, (28) Gustafsson et al. 1999, (29) Shi et al. 2004, (30) Edvardsson et al."},{"citing_arxiv_id":"2606.12532","ref_index":139,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"TESS detection of periodic brightness variations during the rise of classical nova PGIR22akgylf","primary_cat":"astro-ph.SR","submitted_at":"2026-06-10T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Detection of a 0.1802-day periodic signal in TESS photometry of slow-rising nova PGIR22akgylf interpreted as orbital modulation from binary distortion of the envelope during common-envelope interaction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11972","ref_index":110,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"$^{13}$CO and potential variability in $\\beta$ Pictoris b with GRAVITY+","primary_cat":"astro-ph.EP","submitted_at":"2026-06-10T11:51:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"GRAVITY+ observations yield a 12CO/13CO ratio of 91^{+24}_{-17} in β Pictoris b consistent with solar/ISM values and a tentative 1.4% atmospheric variability amplitude.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09072","ref_index":124,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"CORALIE radial-velocity search for companions around evolved stars (CASCADES) V. Three planetary companions and achievable precision","primary_cat":"astro-ph.EP","submitted_at":"2026-06-08T06:14:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Three massive planets detected around HD125136 (2.26 MJup, 850 d) and HD127195 (0.66 and 0.78 MJup, 535 d and 834 d) via Bayesian Keplerian modeling of CORALIE RV series; one additional signal attributed to activity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.08519","ref_index":30,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Photometric light curves analysis of SU UMa-type dwarf novae: the case of RZ LMi and KV Dra","primary_cat":"astro-ph.SR","submitted_at":"2026-06-07T08:56:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"New photometry of RZ LMi and KV Dra detects superhumps during superoutbursts, determines periods and amplitudes, clarifies ER UMa and WZ Sge subclassifications, and measures a 0.0586-day orbital period for KV Dra.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.07230","ref_index":152,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Study of photometric and spectral variability of the roAp star HD~210684","primary_cat":"astro-ph.SR","submitted_at":"2026-06-05T12:53:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Observational analysis of HD210684 yields rotational period 5.02188 d, magnetic obliquity 77°, and main-sequence age ~1.45 Gyr from photometry, LSD magnetic measurements, and MESA/GYRE modeling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05521","ref_index":47,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Kinematic Study of Wolf-Rayet Stars at the Galactic Center I: Binary Candidates and Constraints on the Binary Fraction","primary_cat":"astro-ph.GA","submitted_at":"2026-06-03T23:52:15+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"30-year kinematic monitoring of 27 Galactic center Wolf-Rayet stars identifies five binary candidates and infers a binary fraction of 0.56 ± 0.18.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05343","ref_index":198,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraining Orbital Eccentricity of a Supermassive Black Hole Binary Candidate PKS 2131-0211","primary_cat":"astro-ph.HE","submitted_at":"2026-06-03T18:35:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian fitting of an eccentric Keplerian orbit to the radio light curve of PKS 2131-021 gives e = 0.053 ± 0.015 without red noise but favors a circular orbit plus DRW noise with e < 0.15.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.01823","ref_index":47,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A 0.03 Hz Radio Quasi-periodic Oscillation During the 2025 Flare of GRS 1915+105","primary_cat":"astro-ph.HE","submitted_at":"2026-06-01T07:39:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A recurring 0.03 Hz radio QPO was detected in the 2025 flare of GRS 1915+105 at >5.9 sigma in one epoch, identical across S- and X-bands and prior years, indicating an intrinsic accretion-jet timescale.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.29428","ref_index":76,"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":"2605.22702","ref_index":52,"ref_count":2,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Follow the wobble: Statistical methods to detect astrometric binary asteroids in Gaia FPR","primary_cat":"astro-ph.EP","submitted_at":"2026-05-21T16:44:52+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Refined statistical pipeline on Gaia FPR residuals detects 343 binary asteroid candidates, with 88% fewer false positives in noise simulations and overlaps with 9 known binaries.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17005","ref_index":190,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Red novae, their progenitors, and remnants","primary_cat":"astro-ph.SR","submitted_at":"2026-05-16T14:06:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":2.0,"formal_verification":"none","one_line_summary":"A synthesis of observational data on red novae as stellar merger events, including outburst properties, progenitor diversity, and long-term remnants.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12024","ref_index":48,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"An eclipsing CEMP candidate discovered in a search for dwarf carbon stars in post-common envelope binaries","primary_cat":"astro-ph.SR","submitted_at":"2026-05-12T12:11:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"The first eclipsing CEMP candidate is identified in a 1.224-day binary, with 3.5% of dwarf carbon stars showing short-period variability consistent with tidally locked post-common envelope systems and supporting wind capture for carbon enhancement.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.10610","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"On the origin of variability in $\\alpha$ Cygni variable $\\epsilon$ Ori (HD 37128) using TESS observations and modelling","primary_cat":"astro-ph.SR","submitted_at":"2026-05-11T14:09:11+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Linear stability analysis and non-linear hydrodynamical simulations link the stochastic low-frequency variability of ε Ori to strange-mode instabilities that excite finite-amplitude pulsations.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"from Sectors 6 and 32 were analysed separately, accounting for small mean-flux differences and the two-year gap between obser- vations. The fluxes were converted to the magnitude scale using 𝑚=−2.5 log 10 (flux), after which the mean magnitude was sub- tracted. To study the time series in the frequency domain, Lomb- Scargleperiodograms(Lomb1976;Scargle1982;VanderPlas2018) were computed, as they are well suited for unevenly spaced data. The resulting light curves exhibit amplitude scatters of roughly 40 mmaginSector06andabout15mmaginSector32.Thebrightness in millimagnitudes as a function of Barycentric TESS Julian Date (BTJD)aredisplayedintheleftpanelsofFig.1forSectors06and32. The corresponding periodograms, shown as a function of frequency"},{"citing_arxiv_id":"2605.09340","ref_index":89,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"GSC 08227-00723: An Unusually Large PSH Excess AH Pic Candidate","primary_cat":"astro-ph.SR","submitted_at":"2026-05-10T05:41:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"GSC 08227-00723 is classified as a new AH Pic-type nova-like variable with recurrent stunted outbursts and an exceptionally large positive superhump excess of approximately 0.19.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06517","ref_index":97,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The 2MIG isolated AGNs. 3. Optical--IR variability and dust reverberation in the NLSy1 galaxies Mrk~42 and Mrk~493","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T16:26:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Optical-MIR lags of 39.1 days and 79.4 days are measured in Mrk 42 and Mrk 493, yielding dust reverberation radii of 0.032 pc and 0.065 pc with R_dust/R_BLR ratios of approximately 6-7.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.05303","ref_index":143,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Multi-wavelength outburst activity from EP J174942.2-384834: a very faint X-ray transient discovered by Einstein Probe","primary_cat":"astro-ph.HE","submitted_at":"2026-05-06T18:00:02+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"EP J174942.2-384834 is classified as a very faint X-ray transient black hole candidate based on its hard X-ray spectra, optical/UV brightening correlated with X-rays, and lack of radio emission.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04818","ref_index":4,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"AGILE detection of transient {\\gamma}-ray emission from the region of the supergiant fast X-ray transient source IGR J17354-3255","primary_cat":"astro-ph.HE","submitted_at":"2026-05-06T12:07:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"AGILE archival data reveal gamma-ray flares from a source matching IGR J17354-3255, with orbital phase correlation supporting physical association and high-energy emission from SFXTs.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"7800 307.3 0.5 48.1 55055.5 - 55074.5 7900 343.1 11.1 16.8 55074.5 - 55084.5 8200 3.1 5.3 9.5 55090.5 - 55104.5 8300 10.1 -6.5 15.9 55104.5 - 55119.5 Spinning - - - 55197.0 - 60309.0 Notes.The columns show: (1) AGILE observation block (OB) num- ber for pointing-mode observations; (2-3) Galactic coordinates (l,b) of the pointing centroids (in degrees); (4) distance of the pointing from IGR J17354−3255; (5) observation time interval in MJD. We selected a total of 1993 days of data, 174 of which in pointing mode and 1819 in spinning mode that maximise the exposure on the source. 4. AGILE/GRID data analysis and results We performed the analysis of AGILE/GRIDγ-ray data using the FM3.119 on-ground background event filter, instrument re-"},{"citing_arxiv_id":"2605.04179","ref_index":67,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Multiwavelength Characterization of a New Magnetic Cataclysmic Variable 2CXO J050740.7-091337","primary_cat":"astro-ph.HE","submitted_at":"2026-05-05T18:17:41+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"2CXO J0507 is a polar-type magnetic cataclysmic variable featuring a white dwarf with B ≈ 30 MG and an orbital period of 2.34 hours, identified through multiwavelength archival and follow-up data.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"We performed the search for periodicity in the resulting light curve, using theastropyimplementation 7 of the Lomb-Scargle periodogram (Lomb 1976; Scargle 1982). To evaluate the significance of the peaks in the peri- odogram, we performed 4000 bootstrap simulations to determine the false-alarm probability corresponding to 1, 2 and 3σsignificance levels (VanderPlas 2018). We used a bootstrap technique to quantify the uncertainty of the detected period (Boldin et al. 2013). We ran- domly redistributed the fluxes within their Gaussian un- certainties and generated 10 000 simulated light curves. 6 https://docs.astropy.org/en/latest/api/astropy.stats. sigma clip.html 7 https://docs.astropy.org/en/stable/timeseries/lombscargle."},{"citing_arxiv_id":"2605.03323","ref_index":130,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Search for High Frequency Oscillations in TESS Cycle 7","primary_cat":"astro-ph.SR","submitted_at":"2026-05-05T03:25:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"A homogeneous search of TESS Cycle 7 20-second cadence light curves identifies 73 rapid oscillators (24 white dwarfs, 31 hot subdwarfs, 18 A-F stars) with measured frequencies and amplitudes after vetting.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"odograms, none were identified as genuine targets of in- terest, except for two previously known pulsating white dwarfs from A. D. Romero et al. (2022). We therefore adopted FAP≤0.0001 to retain a high-quality sample while keeping the candidate-vetting process efficient. 3 https://archive.stsci.edu/ Furthermore, to mitigate the effect of the sampling window function (J. T. VanderPlas 2018), we calculated the periodogram of the window function for each target, and removed a fraction of frequencies most severely af- fected by the sampling effect. In practice, we removed 0.5% of frequencies with the highest power in the win- dow function periodogram, and this effectively removed the frequencies below 50 d −1, while minimizing the im-"},{"citing_arxiv_id":"2605.02216","ref_index":61,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Search for Variability of Ultracool Dwarfs with the Zwicky Transient Facility","primary_cat":"astro-ph.SR","submitted_at":"2026-05-04T04:39:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"ZTF data yielded 32 robust ultracool dwarf rotation periods including 12 new detections, with a trend of decreasing periods toward later spectral types in dwarfs older than 100 Myr.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"riods, and ZTF provides sufficiently long temporal cov- erage, the primary limitation in period determination arises from the sampling cadence. For ground-based time-domain surveys, the daily cadence imposes a sig- nificant challenge to period reliability. Daily aliases are a well-known issue arising from the sampling behavior in time-series data (J. T. VanderPlas 2018). In contrast, most current variability studies of brown dwarfs rely on observations with shorter baselines but much higher cadence sampling, which can serve as an independent check on the reliability of our period measurements. We searched the published literature for counterparts to our sample in order to assess the accuracy of our 8 https://doi."},{"citing_arxiv_id":"2605.00372","ref_index":61,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Random Polarization Position Angle Behaviors across Bursts of Repeating Fast Radio Bursts","primary_cat":"astro-ph.HE","submitted_at":"2026-05-01T03:22:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Repeating FRBs show Gaussian-distributed intrinsic PAs with no periodicity, explained by stochastic magnetospheric axis wandering in an extended rotating vector model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.27503","ref_index":78,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Detection of optical quasi-periodic oscillation in the blazar 3C 454.3","primary_cat":"astro-ph.HE","submitted_at":"2026-04-30T06:51:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Detection of a persistent ~433-day optical QPO in blazar 3C 454.3 at 2.53σ significance using Lomb-Scargle, WWZ, and PDM methods, with a new test for seasonal gaps.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"in spurious peaks in the LSP. When applying LSP to a dataset with gaps, it is vital to take into account its failure modes, i.e., the largest peak in the LSP may not correspond to the true frequency but to some har- monic or alias of it. These effects related to the window function's structure should always be considered. Nev- ertheless, as mentioned in VanderPlas (2018), doing so does not guarantee that the true peak is always identi- fied; however, it is still preferable than simply assuming that the highest peak in the periodogram is the correct one. The relevant tests and their results are as follows: 1)Harmonic test:We tested whether the 433-day peak could be a harmonic of a longer true period by evaluating the Lomb-Scargle power at the harmonic"},{"citing_arxiv_id":"2604.22144","ref_index":42,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Short timescale variation in the submillimeter flux of Sagittarius A*","primary_cat":"astro-ph.GA","submitted_at":"2026-04-24T01:31:49+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Sgr A* exhibits a white-noise-like flat variability regime in its 340 GHz flux on timescales below 2.3 to 6.3 minutes, transitioning to red-noise-like behavior at longer timescales, with no evidence for narrow periodic signals.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20814","ref_index":51,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Search for Rotation Measure Flare Candidates in Repeating Fast Radio Bursts","primary_cat":"astro-ph.HE","submitted_at":"2026-04-22T17:44:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A search of repeating FRBs identifies RM flare candidates in FRB 20121102A, FRB 20201124A, and FRB 20180916B, suggesting such events may be common and tied to dynamic magneto-ionic environments.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2603.05586","ref_index":88,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"The TESS All-Sky Rotation Survey: Periods for 1,046,317 Stars Within 500 pc","primary_cat":"astro-ph.SR","submitted_at":"2026-03-05T19:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The TESS All-Sky Rotation Survey provides periods for 1,046,317 stars within 500 pc, with an estimated 93% being true rotation periods, and includes a method to correct half-period aliases.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.23392","ref_index":17,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Revisiting the Reported Period of FRB 20201124A Using MCMC Methods","primary_cat":"astro-ph.HE","submitted_at":"2025-12-29T11:28:10+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"An MCMC-based period search method recovers previously reported candidate periods in FRB 20201124A observations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2405.12324","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Robust 1-norm periodograms for analysis of noisy non-Gaussian time series with irregular cadences: Application to VLBI astrometry of quasars","primary_cat":"astro-ph.IM","submitted_at":"2024-05-20T18:47:25+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A 1-norm robust periodogram is introduced for non-Gaussian irregular time series and applied to 259 quasars, identifying 49 with quasi-periodic signals above 3σ.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}