# Ledger

One row per approach. Every run's per-target results are in the coverage store (`coverage.db`); each approach's method
is its docstring, and its calls are in the recipes of `README.md`.

## Searched

| Approach | Data | Result |
|---|---|---|
| Curved drift tracks, radio | Breakthrough Listen GBT: cached H I and OH channels of 13 stars; every coarse channel of 15 L- and S-band cadences on the eight nearest stars (GJ 406, 699, 411, 447, 273, 1111, 628, 876) | 7322 curved hits in the cached channels, none recurring in a second ON scan and absent from the OFFs; 5558 ON scan-channels of the nearest stars searched and the 366 cadence-channels where an ON hit recurred judged against their OFFs: no curved hit only in ON scans against 9 only in OFF scans (`bl_curved_nearest`) |
| Narrowband drift, radio | Breakthrough Listen: TRAPPIST-1, GJ 273, 24 cadences at H I and OH | stopped; nothing beyond the published turboSETI results |
| Rest-frame line tracks, radio | Breakthrough Listen L band, 230 cadences; H I and OH in the CMB, Solar System and stellar frames | 2037 tests with uniform p; low-p hits are zero-drift or off-source carriers |
| Planet-frame line tracks, radio | Breakthrough Listen TESS C and X band, 12 TOI hosts | 140 tests; none with every ON scan above every OFF |
| Frequency hopping and combs, radio | cached Breakthrough Listen cadences | none on a target alone |
| Lines in sky fibres | SDSS DR17 BOSS and eBOSS spPlates: all 3853 plates, 381943 sky-fibre spectra | every peak and dip at 6 sigma that passes the mask, airglow and width tests is kept with its count of other sky fibres at 3 sigma, so both sharing rules and every later test apply to both signs alike: under the two-fibre rule 3217 clean peaks and 4108 clean dips (970 and 1479 at 8 sigma), 762 and 1813 of them fixed to a fibre at other positions on other plates; the redshift test, with H alpha required beside a strong line and the [O III] doublet at a flux ratio of 1.5-5, marks 156 fibres against 4 among the dips and 11.6 +- 3.5 with the wavelengths shuffled: 154 galaxies at z 0.016-1.069 (median 0.44), six of them seen twice on different plates or nights, 122 with a Legacy Surveys source of median r 23.1, and two Galactic fibres; spectra holding clean lines of both signs set aside 10 peaks and 10 dips at 8 sigma, leaving 485 peaks and 336 dips, with Legacy Surveys sources within 1.5 arcsec at 181 of the 480 peaks the catalogue covers against 21 at positions 30 arcsec north and at 10 of 330 dips against 28, so 162 peaks are single lines of galaxies and the other 323 fall short of the dips by 13 to 31 +- 33; read in every spCFrame, 359 peaks and 241 dips persist (galaxy lines 179 of 188), 25 and 37 are single-exposure events and 1 and 16 one camera's, and net of counterparts 202 persistent peaks stand against 253 persistent dips (-52 +- 29); one line recurs at one position on two or more plate-nights at 37 peak positions against 3 dip positions, among them 4732.6 A in the SDSS-RM field on 54 plate-nights, which the stack of its 94 spectra shows resolved (287 km/s) and without companion lines, Ly alpha at z 2.893, and [O III] 5007 of the z 0.5525 galaxy on 7; the strongest persistent peak is [O III] 4959 of the planetary nebula Abell 31; between 6 and 8 sigma the dips outnumber the peaks (1899 against 1571), so the comparison is drawn at 8 sigma; the median 8 sigma line flux is 8.0e-17 erg/s/cm2, 37 W through 10 m aimed at Earth from 10 pc, and with 0.68 of lines recovered the fibres' 0.093 deg2 bound such transmitters to fewer than 850 per square degree, and those steady through the exposures to fewer than 790; the one-fibre rule gives 188 peaks against 236 to 245 dips; every peak and dip with its tests, counterparts and frame verdicts is in papers/sky_fibres/data (`sdss_sky_fibres_shared2`, `sdss_sky_fibres`) |
| Laser lines, Gaia RVS | 2363 FGK stars within 75 pc | none above the null; a line at the threshold carries a median 2.9e-15 erg/s/cm2, 1.2e20 W isotropic or 7e4 W through 10 m aimed at Earth at the median star, from each star's residual noise and G_RVS flux |
| Laser lines, HARPS | M and K dwarfs, transit-zone stars, 97 sun-like stars within 30 pc | none above the null |
| Laser lines, ESPRESSO, UVES, FEROS | sun-like stars within 50 pc | no recurring group above the null; of the steady peaks above it, ESPRESSO's six lie within the neighbour model's own dip and its seventh (6961.5 A) where seven other stars carry model residuals; FEROS's nine sit in one night's exposures, eight of them the night of 2018-03-22 at one detector wavelength, and its tenth where 25 other stars carry residuals; one UVES group left, a cosmic ray on a low-S/N pseudo-continuum peak |
| Laser lines, SOPHIE | OHP archive: 1465 F to M dwarfs within 50 pc with high-resolution spectra on three or more nights, with the second fibre | no recurring group above the null; the one steady peak above it, 33 Peg at 3950.65 A between Ca II K and H, lies where 29 other stars carry residuals of their neighbour models (`laser_sophie`) |
| Laser lines, GALAH DR4 | 699 spectra of 621 dwarfs within 100 pc, each shifted to the star's rest frame | 35 isolated emission-like peaks above the absorption-like null in 33 stars, all in camera I, whose null (21) sits far below the other cameras' (86-205) and whose continuum carries 36 emission-like peaks above S/N 20 against one absorption-like; 26 stars explained by the exposure's other fibres, the same fibre's other runs of the night, the star's other spectra or a peak narrower than three quarters of the instrument's width, the other 7 in their raw HERMES frames from the AAT archive: in six observations of three or four exposures the fibre holds no light in every exposure near the peak's column and single exposures hold charge there, one event of them on the trace with light's width as 0.4-7 per cent of the single-exposure events across 11-37 fibres of the same frames are, and the S/N 1687 peak, in an observation of one exposure, is charge 2.2 px from the fibre's trace (Findings); threshold median 1.3e-15 erg/s/cm2 a camera, 3e4 W through 10 m at the median star and 50 W at the nearest (4.3 pc) |
| Laser lines, APOGEE DR17 | 3370 dwarfs within 100 pc, combined spectra and 14178 visits | none above the null; threshold median 1.6e-16 erg/s/cm2 from the combined spectrum's S/N and 2MASS H, 1.1e19 W isotropic, 2e4 W through 10 m at 1.6 um |
| Laser lines, DESI DR1 | 7718 stars within 100 pc | coadds of two or more exposures explained; 4749 single-exposure stars (62 per cent) need a second epoch; threshold median 2.1e-16 erg/s/cm2 a camera, 5e3 W through 10 m at the median star, 300 W within 20 pc and 5 W at the nearest (3.6 pc) |
| Laser lines, LAMOST MRS | 14400 stars within 100 pc | 18 features in single stars against 17 by chance, mostly in two of 22-238 exposures; read in every exposure of every night of their stars, all 19 are one or two pixels wide above half their excess against an instrumental FWHM of 5.6-6.5 pixels, so they are detector pixels and not light through the spectrograph, and besides that six sit on masked, variance-inflated or dead pixels, eight have exposures whose peaks lie more than half a resolution element apart, four fill one night and none of the star's other nights, and three are single exposures of nights whose other exposures are flat; the strongest, 241 sigma in three exposures of one night, is a block of pixels at 1800 times the continuum beside it with the pipeline's variance inflated a thousandfold; per-exposure threshold median 3.0e-15 erg/s/cm2, 6e4 W through 10 m at the median star (`laser_lamost_mrs`) |
| Laser lines, CARMENES DR1 | 362 M dwarfs | none once every epoch and every star is registered in its own frame |
| Laser lines, ultraviolet | StarCAT, COS, IUE, FUSE, and STIS after 2004 (4206 exposures of 867 stars) | steady stellar lines in line-crowded spectra only; the seven Arcturus features sit at the brightest flux within 10 A of them, as windows between the absorption lines of a blanketed K-giant spectrum do, at the wavelengths of V II, Cr II, Mn II, Fe II and Co II lines (three within 0.3 km/s), three shared at z > 5 by one other star each; 0.1-7 W through a 10 m aperture aimed at Earth within 5 pc, the beam 0.005 au wide at 2 pc |
| Short-lived elements | Tc, Pm, Pa, Pu, Am and Cm in HARPS, UVES, FEROS and ESPRESSO spectra of sun-like stars within 50 pc | 9 of 2262 tests below p 0.01 against 22.6 expected (a Poisson probability of 0.001 for so few: the nulls are conservative, the p values thinning at both ends because the scatter criterion keeps lines whose scores lie beyond 3 sigma in 1.3-2.8 per cent of cases against the random wavelengths' 1.5-3.6), all shared blends or one double star; Tc I limits 1.6-5.3 mA, A(Tc) < 0.69 for solar-type stars with HARPS and ESPRESSO on Korg curves of growth from A -1 to 3.5, which is 1.7e19 kg of Tc-99 in a solar convective envelope, the product of fissioning 6.6e20 kg of U-235, several thousand times the Earth's uranium, so the limit reaches system-scale disposal and not a planet's |
| Periodic spectral modulation | Borra and Trottier's 234 SDSS stars in SDSS, LAMOST and DESI | no modulation at 1.6465e-13 s |
| Industrial gases | K2-18 b's MIRI transmission spectrum | consistent with zero, too noisy to test |
| Mid-infrared excess | AllWISE, 170 FGK stars from Breakthrough Listen sessions | a debris disk, a blend and a catalogued excess |
| Fully enclosed stars | 36603 AllWISE sources red in W2-W3 | the 72 moving dark sources lie in clouds or among young stars |
| Dark companions | Gaia DR3 orbits (279) and proper-motion anomalies (195) | median bounds 0.3-0.4 per cent of the companion's light at 300 K; the four 3-sigma excesses among the anomalies are a diffraction spike, an M0 photosphere, 56 Per's white-dwarf companion and HD 59099's AllWISE photometry, 0.11 mag brighter at 12 um than the All-Sky release of the same exposures where the sample's two releases agree to 0.007 mag, its All-Sky excess +0.02 mag |
| SPHEREx spectra | Project Hephaistos candidates; Contardo and Hogg's 53 excess stars | background galaxies, a radio source, warm dust and red companions; JWST (Project Hephaistos IV, 2026) resolves the galaxies within about 1 arcsec of candidates D and E, the two whose SPHEREx spectra place the excess in a galaxy here; the fits from 1.6 to 5 um reach components above about 400 K only |
| Cold shells, 30-100 K | 27394 stars within 50 pc against AKARI | 35 matches against 26 by chance: clouds and known young disks |
| Habitable-zone stacks | WISE and DASCH at 178 hosts within 100 pc | intercepted fraction below 1.5e-5 at 300 K |
| Pulsars as megastructure hosts | 1978 timed pulsars against AllWISE | no ring-like counterpart |
| Vanished POSS I stars | 5893 infrared counterparts | four red sources, none detected at W3; a source of R 19 enclosed at 200-600 K would reach W3 11.1-11.6 or W2 14-17, inside AllWISE's and CatWISE's limits, so the test covers enclosures of the catalogue's sources at those temperatures |
| Radio from inactive stars | VLASS, LoTSS-DR2 and RACS-low against nearby stars | at the chance-alignment rate; the two brightest coincidences, 52.6 mJy at 0.34 arcsec from Gaia DR3 2906691964510880128 and 81 mJy at 1.2 arcsec from Gaia DR3 1283261877869284096, are background radio galaxies, the first by a steady steep spectrum from 0.86 to 3 GHz (alpha -0.5 to -0.7) that no star gives, the second resolved by LoTSS (9 x 7 arcsec at 144 MHz) with a second WISE source beside the star (`vlass_quiet_radio_stars`) |
| Circular polarisation | V-LoTSS, RACS-low2 Stokes V, MWA | pulsars, active stars and published brown-dwarf candidates |
| Linear polarisation above the synchrotron ceiling | NVSS (VIII/65): 26973 sources above 10 mJy with polarised flux above 6 mJy | the Rician-debiased polarised fraction's lower bound at three sigma against 0.72, the most incoherent synchrotron gives: median fraction 0.058, 99th percentile 0.51; 23 above the ceiling, every one with a polarised flux at or above its total flux (debiased fractions 0.98-2.97), which no component can have and which the diffuse polarised emission of the field explains, the sources lying in Fornax A's lobes, on the Galactic plane in Cygnus, Cassiopeia and Aquila and in other extended fields, so the catalogue's polarised fluxes are the field's where the Stokes I component is small; none at a pulsar; the Rician errors alone would put 0.6 sources above the ceiling (`nvss_polarisation_ceiling`) |
| 21 cm lines, HI4PI | 27723 stars within 50 pc, two rest frames, and blind | at the noise and cold-hydrogen rates |
| Lines below the ionospheric cutoff | Wind/WAVES 1995-2021, STEREO-A and -B | none outside spacecraft and terrestrial lines; RAD1 measured only 32 to 38 of its 256 channels in nearly every minute of every year and the archive interpolates the rest, so every RAD1 line of the full-channel test was a measured channel above interpolated neighbours; at the measured channels alone, 2020 holds 26 persistent lines, all plasma-line and auroral below 500 kHz and none above 700 kHz (`wind_rad1_2020`); RAD2's channel scatter is 2.4 per cent of the galactic background, so a 5 sigma line in its 20 kHz channel is 2e-16 W/m2, 6e7 W isotropic at 1 au and 2e18 W at 1 pc, and STEREO's 50 kHz channels reach about 2e-15 W/m2; 64 per cent of RAD2's band and 52 per cent of STEREO's lie inside the terrestrial service bands, where a line is assigned to the service |
| Sidereal persistence | e-Callisto in Greenland, Norway, Alaska and Australia | nothing at two stations beyond bright-source transits |
| Solar-gravitational-lens receivers | RACS and VLASS at 119 antipodes | one on-track source against four at controls |
| Stars in planetary-radar beams | JPL radar astrometry 1968-2025 | 813 stars in the beams of 825 radar pings, the nearest at 48.9 ly behind 2017 SL16 (Arecibo, 2019 September); the first replies are due in 2117 (`radar_beam_stars`) |
| Reply windows | transit-zone stars within 45 ly in Breakthrough Listen | GJ 169 only: rest-frame lowest p 0.032, S band in occupied allocations; L-band curved tracks leave two lone hits at 1424.51 and 1424.64 MHz in the one ON scan of 2016 August 26, the -66 and +66 kHz sidebands of a carrier at 1424.5787 MHz that switched on for two minutes with sidebands at -121 and +121 kHz as well, all drifting at +0.55 to +0.65 Hz/s where a source fixed on the sky drifts at -0.11 Hz/s; the carrier recurs on that drift in the scans of Hip21932 and Hip20897 17 and 12 minutes earlier (S/N 7.6 and 8.1, within 140 Hz of the extrapolation), so it is a transmitter in the sidelobes with a drifting oscillator (`curved_gj169_l`) |
| Fresh transit-zone entrants | Gaia DR3: the 40,499 stars within 100 pc and 5 deg of the ecliptic with proper motions, their motion in ecliptic latitude, joined to Hipparcos, the coverage store and the Breakthrough Listen target list | 2,352 see Earth transit the Sun now, and 7 enter the zone within the next century, the nearest Gaia DR3 35227046884571776 at 3.8 pc in 2042; a list for the tests that look at the zone, with Wolf 359 and 89 Leo searched in radio (`etz_fresh_entrants`) |
| Pulsar antipodes | 45116 stars near 100 pulsar antipodes | none at p below 0.01 in the coverage store |
| High-energy sources | 2626 Gaia sources within 20 pc against eRASS1 and 4FGL | flare stars and active binaries; gamma-ray coincidences at the chance rate |
| TeV neutrinos | IceCube tracks at 271 systems within 10 pc | consistent with background |
| Millimetre flares | 66 SPT-3G flare stars | X-ray active stars and late-M emission-line dwarfs |
| Narrowband millimetre lines | ALMA pipeline cubes, 96 spectra of 20 stars within 20 pc | none at 6 sigma in 87130 channels; 464 of 480 injected 8-sigma lines recovered |
| Long-period radio transients | 16 published LPTs against Gaia DR3 at their localisations | ten white-dwarf binaries, X-ray outbursts or rotators; no star at the DM distance beyond chance at the other six |
| X-ray periodicities | Chandra and XMM-Newton within 10-20 pc | at the chance rate |
| Ultraviolet pulses | GALEX and HST photon lists within 10 pc | flare peaks and chance; one isolated 100 ms near-UV brightening of GJ 725 A, 7 photons against 0.2, clean of detector and field events, fixed to the star in rebuilt detector coordinates; a census of 116 GALEX NUV eclipses finds 98 isolated 7-photon bursts, the mapped ones recurring at the detector's edge, and none on a catalogued star matching GJ 725 A's (`galex_burst_census`); the visit is the star's only one with a photon list, its two all-sky visits having none in the public bucket, and GJ 725 B in the same visit holds 3 photons in its busiest 100 ms against 0.1 expected; the nine photon clusters at false-alarm probability below 0.01 among 147 star-eclipses of 51 stars against 4.8 expected are five events, two of them counted once per component of G 272-61 and Wolf 424, on Wolf 359, Ross 128, Wolf 424, G 272-61 and GJ 725 A, every one a flare star, so they are flares |
| Glints | Kepler and TESS candidate periods; TESS 20 s within 30 pc; asteroid light curves | at the chance rate; the per-cadence scatter after detrending is 780 ppm (Kepler short cadence), 1600 ppm (TESS two-minute) and 3000 ppm (TESS 20 s), so a 5 sigma flash is 0.4 to 1.5 per cent of the star, a perfect flat reflector of 3-8e15 m2 reflecting the star's disc; the four quiet cadences required on each side pass a flash in white noise with probability 0.69, and the package's end-to-end test of the Kepler detector recovers 0.62 of isolated 10 sigma flashes; the one-to-three-cadence window covers spinning reflectors whose beam crosses the observer in minutes, not orbit-locked mirrors whose glints last 1.5 to 6 hours |
| Hollow planets around old stars | Exoplanet Archive: 627 planets with measured masses at 3 sigma and bulk density below 1 g/cm^3 | escape parameter Lambda against host age: the lowest Lambda belongs to young planets (V1298 Tau c and d, HIP 67522 b, Kepler-51 c, 17-300 Myr), as evaporation predicts; of 379 around stars of 3 Gyr or more none is below 10, the lowest Kepler-223 e at 10.5 (`exoplanet_hollow`) |
| Nightside light | 63 ultra-short-period rocky planets | none above 3 sigma; median limit 102 ppm, which is 21 times the starlight the median planet intercepts, (R_p/2a)^2 = 0.5-33 ppm, so the limits bound only light of a non-stellar source, 4e21 W at the median (2e20 to 1e23) |
| Clarke exobelts | 461 Kepler planets | none; median limit 117 ppm six planetary radii out |
| Clarke exobelts beyond 30 days | Kepler DR25 long-cadence light curves of the 331 candidate and confirmed planets below 2 Earth radii beyond 30 d on 322 FGK dwarfs (4000-6500 K, log g 4 or above, Kp 16 or brighter), where tides leave a planet unlocked and its synchronous orbit lies inside the Hill sphere | shoulders k Rp/v beyond contact, k 3-90 within half the Hill radius, against random phases: 284 planets measured in 893 planet-k tests, no null phase above z 5; 7 planets above z 4, 2 of them above 5 on both sides (KOI-4371.01 at 7.5, KOI-3436.01 at 7.2); against a null detrended as the transit is, with the light curve's own contacts and transit times, all 7 fall to z -0.9 to 2.2, every catalogue duration among them short of the light curve's (KOI-4371.01 8.6 h against 11.1; KOI-3436.01 5.0 h against 24.8, its transit times spread by 735 min); 3-sigma shoulder limits at k = 6 of 55 ppm best and 215 ppm median (`exobelts_kepler_long`) |
| Transit shapes | 1116 Kepler and 255 TESS rejects | eclipsing binaries, variables and smooth dips; the eclipse on a blue supergiant is TOI-796.01, a 1.6 mmag dip at 0.81 d on a star whose radius puts that orbit inside it, a pulsation or a blended binary and a TFOP false alarm |
| Timing steps | 1810 Kepler candidates; 2939 LMC Cepheids | known timing variations and chance |
| Impulsive period changes | Holczer et al. (2016) Kepler transit times: 1810 KOIs with 20 or more good transits | a two-segment ephemeris continuous at a break scanned over the transits against the best sinusoid and the quadratic, the kink's gain in chi-square less the extra parameter's log N as its evidence: 6 kinks above 10 over both at 5 sigma in the period change; each candidate's own sinusoid at a random phase with first-order autoregressive noise of its residual scatter (60 draws) is beaten by two, KOI-2217.01 and Kepler-142 b, and both kinks rest on the series' last transits, KOI-2217.01's on its final two (-143 and -175 min after 35 within 50) and Kepler-142 b's on its final one (-44.5 +- 6 min), so with any one transit left out the evidence falls below 10 and none remains; KOI-984.01's and KOI-3692.01's kinks sit inside their sinusoidal timing variations (`impulsive_period_changes`) |
| Century-scale dimming | DASCH, 300 sun-like stars | two trends, both inconsistent between plate series |
| Dimming in survey photometry | TESS, Hipparcos epochs, Hipparcos to Gaia, Gaia epochs, Gaia alerts, NEOWISE | explained, or at the rate of control stars |
| Polarised reflectors | 819 stars within 50 pc | 4 polarised beyond the interstellar expectation with no explanation, three of them on one photoelectric measurement each from Heiles' compilation (1630-4540 ppm at 3.9-4.8 sigma); the fourth, HD 101805 (F8V, 34 pc, 3.9 Gyr), reads 223 ppm at 9 deg on one night, rising from 172 ppm in R to 314 in B, where the nine stars measured at the ppm level nearer than 35 pc within 22 deg read 12-45 ppm, five of them at 72-88 deg; the far infrared leaves too little dust to scatter that much light and hot dust polarises by 30 ppm or less, more in the red (Marshall et al. 2016), while a cloudlet in front of it would have to end within 2.7 pc of its sightline and carry a field turned 63-79 deg from its surroundings'; its 2026 Gemini/GHOST spectra measure the gas in front of it from 2027 July |
| Intrinsic polarisation of quiet dwarfs | the Panopoulou et al. (2025) compilation (J/ApJS/276/15): 37210 stars with Stokes q and u, Gaia EDR3 identifiers and distances, 29442 unflagged with five or more neighbours within 3 deg and 20 per cent in distance, 28704 of them judged within their own catalogues | the residual Stokes vector against the neighbours' mean over its error and the field's scatter: above 3 sigma in 8.3 per cent against 7.4 with the measurements reassigned among neighbours, above 5 in 1.2 against 0.9; four dwarfs within 200 pc at 5 sigma with residuals above 0.1 per cent and five times the field's scatter, discordant in angle or in an unpolarised field: HD 142832 (0.42 per cent) sits in the Lupus 1 field of Alves and Franco (2006) at the cloud's distance, Dachs SMC 2-61 (1.65 per cent, RUWE 8.9, an X-ray source) is a binary or a blend in a crowded SMC field, and two rested on single old catalogue entries: HD 127769 (A7V at 187 pc, 1.3 per cent at 43 deg in Heiles 2000 against the field's 0.4 per cent at 87 deg) is interstellar after all, since Gaia gives it A_G 0.32 where its nearer neighbours have none and Planck's 353 GHz dust at its position is polarised at 18 per cent with a field that predicts starlight at 52 deg and 1.9 per cent for the full column, the measured 43 deg and 1.3 per cent sitting on that sightline; and HD 31435, an F9/G0 at 100 pc, 8-9 Gyr old at the turnoff, read at 5.48 +- 0.15 per cent and 47 deg in Johnson V on the Lowell 42-inch in 1977 November and listed by name in Table 2 of Moneti et al. (1984), whose other 93 stars of that run read below 0.4 per cent within 130 pc and rise with reddening beyond; no other polarimetry of it exists in 135 VizieR catalogues; Gaia gives E(BP-RP) 0.00 and B-V 0.565 against an intrinsic 0.58, WISE sees the photosphere to 22 um, TESS, K2 and Hipparcos are flat to 0.03 per cent, RUWE 0.99 and a proper-motion anomaly of 20 +- 32 m/s allow no companion, Gaia's 17 velocities over 920 d are constant to 1 km/s, and the Harvard plates show no dimming around 1977 against matched stars on the same plates; the angle matches the field's 46-66 deg behind the cloud, and HD 283904, a reddened A2 star of the same brightness 5 arcmin away at 214 pc with A_G 1.3 and the 1.527 um interstellar band in its APOGEE spectrum, would read near that value; Planck's 353 GHz polarisation at the position (6-8 per cent, read from the HEALPix map by HTTP range) predicts 49-54 deg for starlight behind the column, against the measured 47, and 2.3-2.8 per cent for its amount (P_353 over 5.4 MJy/sr), half the measured value, so a swap needs an efficiently polarising sightline; the star's Gaia XP spectrum against 40 unreddened twins is flat to 0.3 per cent from 400 to 700 nm and 0.5 per cent high at 800-900 nm, within the twins' spread, which excludes a tenth of the light reflected from aluminium or a dielectric and leaves a grey reflector; Pan-STARRS profiles against three stars of like brightness in the same frames show no excess light at 2-13 arcsec in any filter, so no extended reflector beyond 100 AU either, and with WISE inside 10 AU and Gaia's image statistics between, a reflector has no distance left; so the 1977 entry is a wrong star on a one-in-twenty sightline, and one measurement of both stars decides (`intrinsic_polarisation`) |
| Imaging survey candidates | Gemini/NICI and NaCo | bound companions, background stars and field dwarfs |
| Phase-space clustering | 2977 wide binaries in the coverage store | only the likeness of co-natal stars |
| Orbital poles against the Galactic plane | Gaia DR3 nss_two_body_orbit astrometric solutions (Orbital, OrbitalAlternative, OrbitalTargetedSearch, AstroSpectroSB1) with Thiele-Innes elements, 125786, joined to binary_masses: 1361 companions whose lower mass bound lies below 0.08 Msun (74 with the upper bound below 0.2) against 87382 with lower bounds above 0.2 | each orbit's inclination and the two candidate nodes from the elements, the fraction with either candidate pole within 15 deg of a Galactic pole (3.4 per cent for one isotropic pole, 6.3 for the stellar set's two): possibly substellar 6.2 per cent (84 of 1361) against the stellar set's 6.3 reweighted to the same Galactic latitudes (p 0.59); the strict set 9 of 74 against 4.7 +- 2.1 at that size (p 0.04), the one reading of a small set among several (`orbital_poles_galactic`) |
| Asteroid spins, surfaces and radar | LCDB, Gaia DR3 reflectance spectra, radar albedos | known fast rotators, no solar-cell surface, no specular reflector |
| Area-to-mass ratios | 301 small bodies with non-gravitational terms | three light bodies: 2008 GO98, 'Oumuamua and the dark comet 2016 NJ33 |
| Exact commensurability | 2393 planet pairs in the NASA Exoplanet Archive | none within 1e-5 of a small-integer ratio; 5 within 1e-4 against 3.4, the closest in the librating chains of TOI-1136, Kepler-223 and HD 110067 |
| Light without mass | 42 Gaia DR3 astrometric orbits within 100 pc with HARPS or HIRES velocities | 9 photocentre orbits the velocities exclude: close companions (HD 80883, HD 163441, HD 105113B), a long-period companion (HD 217850), HD 223238's 61-day period beside the scanning law, and blended double-lined stars, the two whose velocities scatter by 0.5-0.9 km/s being pairs Gaia itself sees: Gaia DR3 1754663916181432704 shows two image peaks in 51 per cent of its transits and 792549013757246976 had a neighbour's spectrum deblended from 10 of its 29 RVS transits, so their orbits are photocentres of resolved pairs and their velocities are blends; none with warm W3 excess |
| Cold shells, 10-30 K | 27394 stars within 50 pc against Planck PCCS2, PGCC and AKARI 140-160 um | matches at the chance rate of shifted positions; the strongest would need more than the star's luminosity: cold clumps and cirrus |
| Joint anomaly across methods | 223 targets with rank-calibrated p values from two or more of seven families of runs | no star beyond chance: the strongest, Gaia DR3 5730371484020807808 (elements 0.05, glints 0.05), at 0.86 of the family-shuffled maxima; most runs give no p yet |
| Lasers in line cores | the steady peaks of the HARPS, ESPRESSO, FEROS and UVES runs inside chromospheric and Balmer cores | 6 unresolved peaks above the core null, all in Balmer and He I lines 17-100 km/s from their centres where the neighbour template dips; none in the Ca II H and K or Na D cores |
| Warm dust without pollution at white dwarfs | DESI DR1's 45053 white-dwarf spectra (zpix) joined on Data Lab to unWISE and Gaia DR3: 6627 with unWISE matches, 1434 detected in W1 and W2 with parallaxes at 5 sigma | the white dwarfs' own G - W1 and G - W2 against BP - RP as the photosphere locus (scatter 0.33 mag): 13 exceed it at 5 sigma in both bands, 5 of them unblended with excess black bodies at 900-1500 K, every one 1.6-3.3 mag above the photosphere in W1, the excess of an unresolved brown dwarf rather than the 0.3-1 mag of a dust disc; their DESI spectra against the pipeline's templates constrain Ca II K only to 40-430 mA (G 17.2-19.5), so no accretion test reaches the 50 mA level, and no disc-like excess appears in a sample whose W2 detections confine it to the nearest and brightest white dwarfs (`desi_wd_dust_pollution`) |
| Cold excess around white dwarfs | 16676 white dwarfs within 100 pc (Gentile Fusillo et al. 2021) against AllWISE | 25 with W3 or W4 above the photosphere at 3 sigma and W1-W2 photospheric; the strongest are an extended plane source, an optical ghost, single-exposure detections and cirrus at LSPM J0543+3637 |
| Bodies hotter than sunlight allows | 74609 NEOWISE thermal fits with a free beaming parameter (68500 objects) | 8 fits below eta 0.6 at 2 sigma, each at one epoch, the lowest pinned at the fit's floor; no object below it at every fitted epoch |
| Flux in discrete levels | TESS 20 s light curves of the stars within 30 pc (1806 sectors) | 2096 steps between adjacent 30-minute medians at 7 sigma with transitions of 2 minutes or less, 149 of them common to three or more stars of a sector and 1134 of flares, rises whose light falls by half its jump within the next half hour and the steps down within three hours after them; the 826 left split 504 up and 322 down on 347 light curves, and none holds three levels each revisited, 11 holding two, among them BY Dra's spotted and flaring pair and HD 72946, 10 arcsec from the brighter HD 72945 (`tess20_levels`) |
| Nova ellipsoids | T CrB's 1866 and 1946 eruptions (916 pc, Gaia DR3); Gaia DR3 stars within 100 pc on either ellipsoid in the TESS years, 2-minute light curves of sectors 1-99 | stars of G 6 or fainter observed at their arrival (2 sigma of the parallax-set date): 1946, 180 stars, 593 capped lone flashes against 555.8 from the same sectors and 260 light curves with a flash against 286.1; 1866, 211 stars, 417 against 419.1 and 199 against 211.3; the raw counts' excess (1400) comes from saturated stars brighter than G 6 (`tcrb_nova_ellipsoid`); eight more eruptions by the same test, stars at arrival with capped lone flashes against expectation and light curves with a flash against expectation: GK Per 1901, 203 stars, 469 against 508 and 225 against 254; V603 Aql 1918, 184, 391 against 383 and 191 against 203; RR Pic 1925, 152, 241 against 254 and 112 against 119; DQ Her 1934, 145, 254 against 285 and 120 against 138; CP Pup 1942, 176, 426 against 432 and 200 against 218; V1500 Cyg 1975, 148, 585 against 461 and 274 against 267, the count's excess carried by a few light curves with several flashes each, chiefly TIC 307985337 (158 in its 20 window sectors, a G 9 binary with RUWE 44 whose flashes vary sector by sector) and TIC 219861041 (RUWE 34, an astrometric and spectroscopic binary with a 7 km/s velocity amplitude), active binaries whose flares and systematics track the sectors, not the arrival; SN 1572, 201, 528 against 506 and 238 against 259; SN 1604, 280, 647 against 749 and 319 against 360 (`nova_ellipsoid_gkper` to `nova_ellipsoid_sn1604`) |
| Earth-transit-zone stars at opposition | TESS sectors 42-46 2-minute light curves of Gaia DR3 stars within 100 pc and 0.27 deg of the ecliptic (766 star-sectors) and 1500 control star-sectors 1-5 deg off it | 27 transit windows (6.5 hours either side of opposition) observed: no lone flash against 0.37 expected from the same stars outside the windows and no brightening against 1.12; the 111 control windows hold 7 lone flashes against 4.82 (`tess_etz_opposition`); sectors 70-72 add 12 windows on 12 stars with 1 lone flash against 0.53 expected and no brightening against 0.64, the 129 control windows holding 3 against 4.6 (`tess_etz_opposition_70_72`); sectors 91-92, the ecliptic pointings after 72, add 8 windows on 8 stars with 1 lone flash (5.1 sigma, TIC 135070915, sector 91) against 0.26 expected and no brightening against 0.03, the 74 control windows holding 2 against 1.37 (`tess_etz_opposition_91_92`) |
| Top-hat flares | 1806 TESS 20 s light curves of stars within 30 pc | 256 brightenings with sharp symmetric edges that a box fits better than a flare, against 263 dips of the same shape: the rate of instrumental steps |
| Clockwork flares | Yang and Liu (2019) Kepler flare catalogue: 2304 stars with 10 or more flares | de Jager's H from 0.5 d to a third of each span with 20 harmonics; the 40 highest against 20 draws of other stars' flare times in the same quarters, which keep Kepler's gaps: 22 beat every draw away from rotation, one a burst in three cycles, 2 at the quarter or downlink spacing, none an eclipsing binary, and 19 phase-locked with a scatter of 0.004-0.017 of the period (KIC 7838383 at 49.91 d from 16 of 30 cycles, KIC 9267997 at 22.24 d, the rest at 0.5-3 d near the cadence floor), none below the 1e-3 of a clock; the two long clocks on fast rotators are beats: KIC 7838383 rotates at 1.0472 d with a second spot period at 1.0685 d, which beat at 52 d, and KIC 7746984 at 0.7398 and 0.7377 d, which beat at 268 d with the flare clock at its half, the flare rate following the visibility of the active regions as the two spot groups drift past each other (`kepler_clockwork_flares`) |
| Superflare deficit among planet hosts | Yang et al. (2023) TESS flare catalogue (J/A+A/669/A15): 60810 flares with energies on 11131 of 264643 two-minute targets, with the TESS objects of interest (PC, CP, KP) and the confirmed planets' stars: 83 flaring hosts with 332 flares above 1e33 erg against 11048 flaring non-hosts | each host's ten nearest non-hosts in temperature, radius, distance and sectors drawn 2000 times: the hosts' fraction of flares above 1e34 erg among those above 1e33 is 0.283 against 0.350 +- 0.060 (p of a deficit 0.14), and 48 per cent of the hosts carry a flare above 1e34 against 48 +- 4 per cent of the draws; a two-sample test of the pooled energies gives p 0.009 (medians 10^33.56 and 10^33.72 erg), carried by the few hosts with many flares, so the draws over stars are the reading (`superflare_deficit`) |
| Clockwork flares, TESS | Yang et al. (2023) TESS flare catalogue: 1426 stars with 10 or more of 60810 flares | the same H-test from 0.2 d to a third of each span, against other stars' flare times in the same 13.7 d orbits: 9 of the highest 40 beat every draw, 8 of them bursts in one or two cycles at the 240 d spacing of TESS's year-long pointings and TIC 457100137 at 1.213 d with a phase scatter of 0.0087, 30 times the 2 min cadence floor and above a clock's 1e-3 (`tess_clockwork_flares`) |
| Fission-product abundances | 50742 GALAH DR4 stars with clean Zr, Mo, Ru, Ba, Nd and Eu | fission-like patterns rarer than the mirror at every threshold (71 against 230 above 5 sigma), the strongest single-element outliers in cool stars; 23 FGK dwarfs carry Mo and Ru, all of them 4800-4880 K at [Fe/H] +0.1 to +0.4 with errors of 0.11-0.28 dex and none beyond 2.5 sigma from solar in either element, so the thin envelopes where pollution shows are barely sampled and hold no signal to read (`fission_galah`) |
| NEOs on unreachable orbits | JPL Small-Body Database near-Earth objects in the delivery model's empty cells | 24 retrograde, all at e 0.74 or more; none retrograde below e 0.3; one near-circular orbit inside 0.75 AU above 25 deg (2025 LP) within the Atira population; 12 above 60 deg below e 0.25, reachable through Kozai cycles |
| CNO-processed unevolved dwarfs | APOGEE DR17: 31351 dwarfs with log g above 4.2, Teff 4800-6500 K, [Fe/H] above -0.3 and unflagged C and N | [C/N] against the dwarf locus in Teff and [Fe/H] (scatter 0.096 dex): 91 nitrogen-rich at 5 sigma and no carbon-rich mirror; 57 of the 91 are Gaia DR3 binaries against 28 per cent of random dwarfs, the mark of transfer from an evolved companion or blended spectra, and 78 carry binary, s-process, sodium, rotation, evolution or Teff-edge flags; the 13 that carry none all carry ASPCAP's VMICRO_WARN, the microturbulence grid-edge warning that biases the carbon and nitrogen read from the CN bands in dwarfs, seven with TEFF_WARN or STAR_WARN as well, so the nitrogen excess is the pipeline's (`apogee_cno_dwarfs`) |
| Herded stars | APOGEE DR17 dwarfs within 100 pc with their own radial velocities and Gaia astrometry (6044 with 3D velocity errors below 0.5 km/s) | 903 pairs within 10 pc and 1 km/s in 31 groups, the largest the Hyades (62 members); [Fe/H] spreads above 0.2 dex among members within 600 K of each other only in the Hyades' coolest M dwarfs, at the pipeline's temperature edge, and in one metal-poor pair 540 K apart (-1.22, -0.94) (`apogee_herded_stars`) |
| Coherent hyperbolic meteor streams | Global Meteor Network trajectories 2018-2026: 3.58 million orbits, 40753 sporadic meteors hyperbolic at 3 sigma | incoming asymptotes and v_inf from each orbit, neighbours within 1 deg and 3 km/s against the 10 deg density: 35 meteors below p 1e-4 in 10 groups, 8 of them IAU shower members with overestimated speeds (PER, ORI, ETA, XIP); the largest, 16 meteors from 2022-2026 at solar longitudes 80-214 on one asymptote (ecliptic 134.5, -1.6; RA 136.5, Dec +15.0) at 12 km/s, is matched by a 16-member group in one of three realisations of a 1.5 per cent speed overestimate shared by the elliptic sporadics (74000 simulated), while 15 realisations thinned to the observed 40753 at 1.0-2.0 per cent give 3-31 meteors below p 1e-4 and groups of up to 14; SonotaCo's independent 353231 orbits hold 1 meteor on the asymptote against 0.16 from the local density and about 1.6 a real stream would give; no star within 100 pc shares its velocity on its line (`gmn_hyperbolic_streams`); the focal-line test of the 12 km/s asymptote, whose members Earth's gravity would spread along loci reaching +-52 deg of latitude, half of them south, as Earth crosses the line near solar longitude 134.5: the Aug 3-11 loci hold 529 meteors against a mean of 16 on 11 control asymptotes, but 510 of them north where the Perseids (204 tagged) and the apex sporadics sit and 19 south against 10 by chance, so the excess is the speed-overestimated shower population and not a stream (`gmn_focal_line`) |
| Cosmic-ray doublets | Pierre Auger Phase One, 2635 events above 32 EeV (2004-2020) | pairs within 2 deg: 8 within 10 days against a time-permuted mean of 5.7 (p 0.21) and 2 within a day against 0.56 (p 0.11); no triplet within 30 days (0.34 expected); one pair's circle holds Kapteyn's Star at 3.9 pc, its members 1.8 and 2.1 deg from it, beyond the 0.9 deg resolution (`auger_doublets`) |
| Cosmic-ray doublets, open data | Pierre Auger open data 2024 (a tenth of the events): 2355 inclined showers and 22751 from the 1500 m array | inclined: 7 pairs within 2 deg and 10 days against 5.1 permuted, 2 within a day against 0.50, no triplet; 1500 m array: 569 against 559, 69 within a day against 57 (p 0.08), 349 triplets within 30 days against 361 (`auger_doublets_inclined`, `auger_doublets_sd1500`) |
| Self-luminous asteroids | ATLAS phase curves (VizieR VII/288): 39239 of 127012 with phases below 7 and above 25 deg | slopes over 5-30 deg from H, G1, G2 (median 0.0277 mag/deg); 221 pinned at the flattest the model allows (0.0179), with median residuals of 0.28 mag from rotation; 107 of them have literature albedos, 0.03-0.74, none above 0.8 (`atlas_self_luminous`) |
| Centrifugal habitats | LCDB frequency-diameter table, 8854 asteroids | strength needed above the gravity spin limit (2.33 h at 2000 kg/m^3): no kilometre body under 10 minutes or needing 100 kPa; of 8 bodies of 0.3 km or more needing over 1 kPa, 2019 MA2 (0.49 km from H, 2.62 min, quality 2) needs 97 kPa, within a monolith's strength, and 2008 RA106 (3.7 km, 54 min, quality 2-) 11 kPa (`lcdb_spin_strength`) |
| Yarkovsky sign test | JPL transverse non-gravitational terms of 611 asteroids (567 at 3 sigma), DAMIT pole solutions | all 14 drifts with poles have the sign the spin gives (11 inward on retrograde spins, 3 outward on prograde); five drifts exceed all absorbed sunlight at 500 kg/m^3 and albedo 0.5, four of them the published dark comets 2003 RM, 2005 UY6 and 2012 UR158 and the active 362P, and the fifth, 2016 TA56, on a Jupiter-family orbit (T_J 2.69, q 0.59) like the outer dark comets; at 2000 kg/m^3 and albedo 0.14, ten, adding 1998 SH2 (T_J 2.91) and 2006 VC (T_J 3.72, A2 at 3.7 sigma) (`yarkovsky_sign`); 2016 TA56 refitted in ASSIST gives A2 -3.54e-12 +- 0.17e-12 au/d^2 with site weights, -3.56 +- 0.19e-12 with the sqrt(N/4) same-night deweighting of JPL's fits and -3.45 +- 0.37e-12 (9 sigma) with the whole 2007 night as one position, the figure to quote; a radial term fitted alongside is A1 +3.7 +- 1.9e-10 (2 sigma) with A2 -3.32 +- 0.21e-12 beside it; the term rests on the one-night 2007 precovery (without it -2.2 +- 4.3e-12; a gravity-only orbit through the later apparitions, predicted there to 0.2 arcsec, misses the precovery by 3.45 arcsec, 3.0 of them across the apparent motion where no clock error reaches, both reports being re-measurements of the same CFHT frames, and misses the 2025 positions by 10.5 arcsec, 8 across), and NEOWISE W2 gives D 2.4 km (1.4-3.7) and albedo 0.017, like the dark comet 2005 UY6, the drift 15-39 times all absorbed sunlight at 1000 kg/m^3; the two orbits part by 4-7 arcsec in 2030 August-September, where one 0.2 arcsec position separates them at 4.7 sigma (one position a night) to 7.5 sigma (site weights) after both orbits' covariances are propagated; refitted with one later night left out at a time, A2 has a jackknife error of 0.53e-12 (6.5 sigma), resampled nights with the 2007 night held give -4.9 to -3.2e-12 (95 per cent of 200), clipping and error-floor variants keep it at 7.4-10.6 sigma; the twelve CFHT frames of 2007, re-measured against Gaia DR3, hold the 3 arcsec cross-track offset, both reports lying 0.10 arcsec rms across our track, and none of the twenty known asteroids within 0.5 deg (SkyBoT) moves within 5 arcsec/h and 10 deg of it; under a night-level covariance whose shared variance restricted maximum likelihood sets at tau 0.17 arcsec (0.11-0.23), A2 is -3.85 +- 0.30e-12 (13 sigma), and the twelve 2007 positions would have to share a further 1.2 arcsec to bring it under 3 sigma (0.68 for 5 sigma); every orbit fitted without 2007 puts the object on one line in those frames (0.93 arcsec west per 1e-12 of A2, A1 spreading it only along the line), and the median flux along it finds the measured source alone (0.96 of its flux at A2 -3.75e-12, at most 0.05 elsewhere) and nothing at the gravity-only position to 3.9 mag below it (3 sigma, against 954 control lines, none reaching half the detection's flux); the census of all sixteen frames finds 68 moving sources besides it over 0.86 deg^2 (21 of the 22 known ones on the frames), none within 5 arcsec/h and 10 deg of its motion and three within 10 and 20, recovers 109 of 115 injected copies within 0.5 mag of its brightness and links nothing with the frame times shuffled, so 8e-6 unrelated movers are expected within 30 arcsec, 0.5 arcsec/h and 1 deg of it; no other archival image before the discovery reaches it (DECam 2013 September at V 23.9 gives S/N 0.9 and 2.2, the two orbits 0.5 arcsec apart then); one 0.2 arcsec position in 2030 July would measure A2 to 0.39e-12 without the 2007 night; of the fourteen published dark comets, thirteen carry a transverse term and the screen flags six, the seven inner ones of 4-21 m lying at xi_typ 0.01-0.09 with their published accelerations in the radial and normal terms (`darkcomet_2016_ta56`); 1998 SH2 refitted the same way gives A2 -6.1e-13 +- 0.24e-13 au/d^2 (-6.4e-13 +- 0.54e-13, 12 sigma, with each night as one position) across its 1998, 2016 and 2025 apparitions, chi2/dof 0.67 against 0.90 without it, and NEOWISE W2 gives D 0.64 km and albedo 0.019 at eta 1.4 (0.39-0.93 km over eta 0.9-1.9), so the drift is 1.2 times all absorbed sunlight at 1000 kg/m^3 on a Jupiter-family orbit (T_J 2.91, q 0.79), a twentieth of 2016 TA56's by that measure; large-aperture imaging during its 2025 August close approach found a weak tail, so it is a comet (Farnocchia et al. 2026), which the screen picks out from its drift alone (`darkcomet_1998_sh2`); 2006 VC's A2 rests on its 2025-2026 apparition and the gravity-only orbit fits all four apparitions as well (chi2/dof 0.96 against 0.95), the two orbits parting by up to 25 arcsec in 2034 February (`darkcomet_2006_vc`) |
| Nightside heat on bare rocks | published phase curves of LHS 3844 b (Spitzer) and GJ 367 b (JWST MIRI) | nightside power below 1e19 and 4e18 W at two sigma; Kardashev-I powers are out of reach |
| Waste heat in ultra-diffuse galaxies | SMUDGes DR9, 7070 galaxies; AllWISE within 3 arcsec and Gaia DR3 within 2 arcsec through CDS XMatch | 7 centroid sources at 5 sigma in W3 or W4, 2 of them neither AGN-coloured nor Gaia stars (both at W1-W2 0.43-0.47), against 11 and 6 at positions 60 arcsec away (`smudges_waste_heat`) |
| Surface-brightness-fluctuation deficit | Cosmicflows-4: 414 galaxies with an SBF modulus and another method in the galaxy (191) or its group (223) | 5 too far by 0.3 mag at 4 sigma, the weak-fluctuation sign, against 2 too near: NGC 1023 against a group modulus of 2.3 Mpc, the dust lanes of M64 and the edge-on NGC 4565, and two Fornax galaxies 0.5 mag behind the cluster's group modulus (`cf4_sbf_deficit`) |
| Missing bolometric flux | 14959 Kepler giants: seismic radii (Yu et al. 2018) against Gaia luminosities (Berger et al. 2020) | deficits as common as excesses at every threshold; the extreme deficits are background giants oscillating in foreground dwarfs' apertures |
| Missing bolometric flux, eclipsing binaries | DEBCat (Southworth): 388 detached eclipsing binaries, 252 with both components' luminosities and Gaia DR3 parallaxes by CDS XMatch, 117 with components below 8000 K within 1 kpc at RUWE 1.4 or less | G predicted from the components' log L and log Teff with bolometric corrections at the Gaia distance, the extinction the larger of Gaia's A_G and 2.7 E(B-V) from the catalogue's B-V against the components' intrinsic colours: G_obs - G_pred median -0.04 mag, robust scatter 0.12; one system too faint by 0.3 mag at 3 sigma, KIC 2557430 (KOI-6277, +1.05 +- 0.19 mag, RUWE 0.81), whose published surfaces (1.88 and 1.23 Rsun at 7050 and 6050 K, Hoyman et al. 2020) outshine its Gaia distance 2.6 times while an earlier light-curve analysis (Kamil and Dal 2017) read it as a triple with a gamma Dor pulsator and two flaring components; Gaia resolves the visual double WDS J19074+3749AB into the eclipsing pair (G 11.44, 2.916 +- 0.012 mas, RUWE 0.81, radial velocity varying by 20 km/s) and a co-moving K star 2.4 arcsec away (G 13.30, 2.946 mas), inside Kepler's pixels, and gives the pair 6130 K and A_G 0.001, so the catalogue's B-V of 0.58 is its own colour and not the 0.38 of a 7050 K primary with reddening, and its FLAME luminosity with the K star's sums to 2.9 Lsun against the solution's 9.7: the published temperatures, and the extinction the test inferred from them, are too high, and the light is not missing; 12 too bright, third light and blends; BG Ind, IM Per and the other high-RUWE systems set aside (`debs_missing_flux`) |
| Transits faster than escape velocity | Kepler DR25 threshold-crossing events with Berger et al. (2020) hosts (29820; 6833 at S/N 15) and 7523 TOIs with host radii | a bound body crosses a star no faster than its surface escape speed, so a full transit lasts at least 2R sqrt((1+k)^2 - b^2)/v_esc, 37.5 min (R/Rsun)^1.5 (M/Msun)^-0.5 at b 0, whatever the eccentricity; Kepler events below 0.8 of the floor at their fitted geometry and within the host errors: 281, of which 253 sit on giants (background binaries and the giants' own variability), 26 on hot or multiply-flagged stars with 3 to 10 events each (pulsators), one is a catalogued shallow eclipsing binary, one a KOI with centroid flags, and the one left, KIC 7292626 (a 12 per cent, 50-minute dip at 204.8 d, S/N 465), is a single cadence flagged for cosmic rays with the other epochs flat; TOIs below 0.8 of the b = 0 floor: 242, of which 97 sit on giants, 69 have sub-day periods (contact binaries and pulsators), 34 are published false positives, and 42 planet candidates have no impact parameter in the TOI table; fitted in their TESS light curves, 20 last long enough for a bound orbit at any impact parameter (the TOI table's durations are short), 4 are V-shaped and 3 flat-bottomed with an impact parameter that keeps the crossing below the escape speed, 5 show no transit at the TOI ephemeris and 10 have no TESS light curve in the public stores, so none is a full transit faster than escape (`escape_transits`) |
| Transit-depth growth, Kepler to TESS | 102 KOI-TOI pairs matched within 6 arcsec and 0.2 per cent in period; Kepler long-cadence and TESS SPOC, TESS-SPOC and QLP light curves | 3 deeper in TESS at 5 sigma in the catalogues with the duration held and 2 shallower; measured the same way in both missions' light curves, none is deeper in TESS's uncorrected flux: Kepler-13 b and Kepler-718 b deepen only through the crowding correction (4249 and 11468 ppm uncorrected against Kepler's 4526 and 13828), Kepler-506 b reads 572 +- 53 ppm against 491 +- 4 rather than the TOI table's 771, Kepler-25 c agrees, and Kepler-546 b, shallower in the corrected flux as well, holds more light in TESS's aperture than the crowding model, the star giving 0.26-0.46 of it by its TESS magnitude, over which its depth is 4077 +- 424 ppm against 3584 +- 13 (`transit_depth_growth`) |
| Coronal X-rays without a dynamo | eRASS1 HamStar coronal counterparts (137896 with a distance and colour) with rotation periods from TESS (Fetherolf et al. 2023), Gaia DR3 and ZTF (Chen et al. 2020): 8287 at 3000-6000 K | L_X from the 0.2-2.3 keV flux and distance, L_bol from G and BP-RP, the turnover time from the colour's temperature (Cranmer and Saar 2011), the residual above the Wright et al. (2011) relation (saturated at 10^-3.13 below Ro 0.13, Ro^-2.5 beyond): scatter 0.82 dex at Ro below 1 with 0.24 per cent beyond 1.5 dex; only 26 stars reach Ro 1 (the period catalogues hold few slow rotators and Gaia's periods beyond 10 d are not trusted), and the one beyond 1.5 dex is a ZTF RS CVn binary at 1 kpc; late-F stars at 6000-6500 K sit 2-3 dex above the relation's extrapolation through their basal coronae and are left out of its domain (`dynamo_dead_xray`) |
| Circular polarisation at inactive stars | V-LoTSS (Callingham et al. 2023, 77 stars with Gaia counterparts) and the RACS circular-polarisation stars (Pritchard et al. 2021, 34) against eRASS1 and the rotation catalogues | 23 of the 31 in eRASS1's half of the sky are detected at L_X/L_bol 7.5e-5 to 3.6e-3, the rest are RS CVn, BY Dra and flare stars by name and type, 5 have catalogued periods, all short; none above 30 per cent polarisation at L_X/L_bol below 1e-5 with a period above 20 d (`dynamo_dead_polarised`) |
| X-ray output above the coronal ceiling | eRASS1 HamStar coronal counterparts, 137896 with a distance and colour | L_X/L_bol percentiles 50/90/99/99.9 at -3.42/-2.85/-2.30/-1.90 dex; 250 above 1e-2 and none above 0.1; of the 250, 153 sit off Gaia's main sequence, 38 carry a cataclysmic, young, emission-line or extragalactic type on the counterpart or on a SIMBAD object within 20 arcsec (HamStar's own SIMBAD columns miss both the entries SIMBAD names after Gaia and those it files at the X-ray position), and 59 are main-sequence M dwarfs of 3000-3550 K at 50-630 pc with counterpart probability 0.5 or more, whose flares reach 1e-2 within eRASS1's day-long scan average; the one K dwarf of the first pass, 1eRASS J082623.3-703142 at 7.6e-2, is the cataclysmic variable 1ES 0826-70.3 (PBC J0826.3-7033 of the Swift BAT catalogue, typed CV in the ART-XC catalogue, a pointed XMM target), which SIMBAD files 11 arcsec from its Gaia counterpart and which holds the same flux in eRASS1 and eRASS:3 (`coronal_ceiling`) |
| Straight limbs in occultation profiles | PDS small-bodies occultation bundle V4.0 (2024 March): 395 events of fit quality 3 or 4 with five or more positive chords from distinct sites, 376 measured once chords landing nowhere near the fitted position and ellipses off the nominal size are set aside, the table's unsigned western longitudes resolved by the catalogue's own fitted position | the longest run of consecutive limb points from different sites that a line fits within the timing errors, over the diameter: median 0.21, 90th percentile 0.67; 25 beyond the null of the fitted ellipse's points at the same angles and errors at p below 0.01, the longest on (3317) Paris 2020 (0.97 D over 6 sites), (134) Sophrosyne 1980 (0.86 over 5), (64) Angelina 2023 (0.82 over 7), (39) Laetitia 1998 (0.79 over 6) and (2) Pallas 1983 (0.70 over 6 of 120 chords), bodies whose shape models carry the flat facets an ellipse lacks, so a null from DAMIT shapes projected at each event's geometry is the step that remains (`occultation_limbs`) |
| Plate-like bodies | LCDB details V4.0: 47635 records with an amplitude and a phase angle, 31008 of quality 2 or 3 at phase angles up to 15 deg | amplitudes reduced to zero phase at 0.03 mag/deg: 5 records above 1.6 mag (0.02 per cent, against 0.11 per cent of the quality-1 records), one above 2.0 and none above 2.5, in five objects, every one a single TESS record of Pal et al. (2020) of a rotator of 9 to 627 h, three marked ambiguous; no body above the 4:1 ceiling at low phase (`plate_bodies`) |
| Shared clocks | ZTF periodic variables (Chen et al. 2020): 770043 of 781602 with periods off the day and sidereal-day aliases | pairs of stars more than 10 arcsec apart within a fractional period tolerance scale linearly with the tolerance (212473 at 1e-6, 631793 at 3e-6, 2077868 at 1e-5), as a smooth period distribution gives; of the 1e-5 pairs, 42112 agree in phase to 0.01 cycle at MJD 58700 against 41384 to 42020 with the phases shuffled eight times, in 3731 groups of three or more against 3675 to 3848; the largest groups (nine Miras at exactly 380 and 420 d) sit on periods the catalogue repeats exactly, its own grid, and the largest off the grid holds 7 against 8 shuffled (`ztf_shared_clocks`) |
| Stellar-synchronous orbits beyond the tidal radius | the cumulative KOI table's candidates and confirmed planets joined by KIC to the KOI rotation periods of McQuillan et al. (2013) and Mazeh et al. (2015): 1099 hosts, 541 planets at 10 d or more, where tides cannot synchronise the star | P_orb within 2 per cent of P_rot, 2 P_rot or P_rot/2: 25 against 23.4 +- 4.6 with the rotation periods shuffled among the hosts within 500 K bins (p 0.39); the four 1:1 matches consistent within their errors (KOI-757.01, 492.01, 3029.01 and 1910.01) fitted for the rotational phase at each transit in windows of three rotations with the transits masked: the phase scatters by 0.17-0.25 cycle over four years, as it does for eight rotators at like periods on the same epochs (0.13-0.28), the random walk of spots and not a lock (`synchronous_orbits`) |
| Aimed transits | cumulative KOI table: 2294 candidates and confirmed planets at S/N 20 (77 in the habitable zone); the DR25 injected planets' recovered fits (2091 at MES 20, impact parameters drawn uniformly) as the null | a structure placed to be seen from Earth sits at b below R*/a; the injections' fits put 7.4 per cent of a uniform population below b 0.05 and 37 per cent in 0.1-0.5, the KOI fits 20 and 25 per cent, the difference carried by fits with b at its lower bound and errors near 0.4 (21 of the 77 habitable-zone planets, every one with an error above 0.13), while the 153 planets with b measured to 0.1 hold 7 below 0.05 against 11.3 expected; no excess of central transits beyond what the fits' degeneracy puts there, and the test reaches only planets whose geometry the light curve constrains (`aimed_transits`) |
| Replicated bodies on unrelated orbits | LCDB summary table V4.0 (PDS) and the 2024 proper elements of the Nesvorny family bundle: 4315 numbered asteroids with quality-3 periods | pairs with periods agreeing to 2e-4, H to 0.1 mag and amplitude to 0.05 mag more than 300 m/s apart in the Zappala metric: 14 against 8.6 +- 2.8 with periods shuffled within half-magnitude bins; one group of three against 0.04 +- 0.18 (one in 25 shuffles): (3305) Ceadams, (5122) Mucha and (2019) van Albada at 2.7290-2.7294 h, H 12.3-12.4, amplitude 0.20-0.23, in three families, at the fast-rotator pile-up near the spin barrier; their Gaia DR3 reflectance spectra are all S-type, the commonest class, with red slopes reaching 1.21-1.26 at 770 nm and the 1 um band, so three ordinary stony bodies of like size at the spin barrier's pile-up share a period, as the shuffles give once in 25 (`replicated_bodies`) |
| Chromatic-only variables | Gaia DR3 vari_summary: 1073 variables brighter than G 16 with twenty or more transits whose G scatter is below 0.003 mag with BP and RP scatter above 0.02 each, against 172707 sources quiet in G (scatter below 0.01) | the ratio sqrt(s_BP^2 + s_RP^2)/s_G in half-magnitude bins of G puts 899 beyond the quiet sources' 5 sigma tail, the highest at 25 sigma with BP and RP scattering by 0.6-0.8 mag around a G constant to 0.002; the 60 highest read epoch by epoch (DataLink's unfiltered table, since the server refuses the valid rows alone for a source whose every transit carries a flag): 57 move BP and RP together at correlation above 0.9, a neighbour entering both windows on a few transits, 3 scatter in one band with the other quiet, and none moves BP against RP; the highest sit in crowded fields where the 3.5 by 2.1 arcsec windows take a neighbour (`chromatic_only_variables`) |
| Opaque lightweight eclipsers | Gaia DR3 vari_eclipsing_binary: 196041 eclipses deeper than 0.75 mag at periods under 30 d, 4803 with RVS velocities and 956 with ten or more RVS transits | the observed RVS semi-amplitude over the least a main-sequence eclipser of the depth's size demands: median 0.73, tenth percentile 0.33; 10 below 0.1 spanning five or more cycles, every one explained: 15 Eri, a naked-eye K giant whose 4.4 mag model depth is saturation; HD 112604, an A0 subgiant with an unphysical 98 per cent model depth; a twin binary and a 6-hour contact binary whose blended lines read low in the RVS; KOI-6903, where Kepler shows a 31 per cent eclipse at 38 d with a stellar secondary against Gaia's 1.8 mag at 1.4 d; and five stars whose light curves are flat at Gaia's period against model depths of 0.77-1.73 mag: two in ZTF to 0.05 mag, and TYC 4267-1042-1, TYC 7438-551-1 and BD+09 1746 in TESS to 0.1-0.3 mag in their clean sectors; so Gaia's derived depths and periods, not the velocities, are what fails, and the test needs light curves for its depths (`lightweight_eclipsers`) |
| Transiting bodies inside the fluid Roche limit | Gaia DR3 vari_short_timescale: 216720 sources faster than 8.6 cycles a day with gaia_source rows, 10906 on the main sequence with amplitudes above 0.02 mag, 10875 with epoch photometry; ZTF DR23 light curves of the candidates | a fluid body survives only at periods above 12.6 h times the inverse root of its density, so a box-shaped transit under 2.8 h at a main-sequence host needs 20 g/cm3 or a rigid structure; each band of the epoch photometry folded at the Gaia period, its double and half, a box of duty under 0.15 against a one-harmonic sinusoid, with the band's best sinusoid plus its own residuals resampled at the same epochs as the null (2000 draws, ten times that when fewer than ten reach the data): 1277 light curves box-like, the lead band's p-values uniform above 0.1 with a tail of non-sinusoidal variables (92 below 0.001 against 10.9), 12 box-like beyond the null at p below 0.001 with the other bands below 0.05, 11 of them with equal depths in BP and RP; in ZTF g and r the 10 with light curves hold no box from 0.45 to 2.2 Gaia periods, the best in each a single point below 3 sigma against Gaia's boxes of 0.06-0.97 mag at 10-15 per cent duty, so the boxes are Gaia's period or depth, and Gaia DR3 5713030673830580608 has no ZTF light curve (`roche_transits`) |
| Euclid Q1 sources bluer than the Rayleigh-Jeans limit | Euclid Q1 MER catalogue, 63 deg2: point sources at S/N above 10 in VIS, Y, J and H | 14 sources bluer than the Rayleigh-Jeans slope in I_E - H_E, 9 below -2.3, and none at 3 sigma with the NISP fluxes falling faster than nu^2, clean flags, unblended and not variable; the blue tail is flagged or blended sources (`euclid_bluefloor`) |
| Hot bodies too small to be stars | the Gaia Catalogue of Nearby Stars' sources within 100 pc bluer than BP-RP 0.6 at parallax_over_error above 10, their gaia_source and astrophysical_parameters rows by id: 5278 with black-body colour temperatures above 7000 K, 3812 of them on the white-dwarf sequence | the black-body radius from G, the parallax and the colour temperature (GSP-Phot fits white dwarfs with main-sequence libraries and cools them, so it is the second estimate, not the selection): median 0.016 Rsun; 33 below 0.003 Rsun and 22 of those with clean astrometry and single-source photometry, against 0.00 from the white-dwarf sequence pushed through its errors 200 times; all 22 are G 18-21 objects already in the Gaia white-dwarf catalogues, 4 of them in the IR-faint list of Bergeron et al. (2022), where collision-induced absorption strips the red light from a 3000 K helium photosphere and makes it read 9000-17000 K by colour, and none has an ultraviolet detection, which a body hot by colour would have; the floor is empty once that mimic is named (`hot_small_bodies`) |
| Non-thermal or recurrent lunar flashes | NELIOTA's flash lists read from the tables of Liakos et al. (2020) and (2024): 284 flashes of 2017-2023, 188 validated, 192 with R and I, positions to 0.5 deg | colour temperatures from R - I through the Planck ratio with Vega's colour as the zero point: median 2935 K, 5th-95th percentiles 2027-5020 K, none hotter than 8000 K or cooler than 1000 K at 3 sigma, none longer than 0.5 s (the longest 429 ms); pairs within 1.5 deg on the Moon 21 against 23.9 +- 4.9 with the longitudes permuted among the flashes (p 0.75), the closest a validated pair 0.10 deg apart on consecutive Perseid nights of 2018 August at (+26.7, +60.2) with temperatures of 4100 and 3000 K, where a tenth of a pair is expected that close (`neliota_flashes`) |
| Achromatic long-period modulation | ZTF periodic variables (Chen et al. 2020): BY Dra and RS CVn stars at 5-500 d with A_g of 0.15 mag or more and g brighter than 18, 1549 with catalogue A_r/A_g of 0.9 or more and 296 controls at 0.7-0.9; ZTF DR23 g and r light curves by object identifier, 1845 fitted at the catalogue period by a mean and two harmonics per band | the light-curve A_r/A_g of the controls has median 0.95 with robust scatter 0.25 where the catalogue amplitudes gave 0.83, so the catalogue ratio runs low; 9 candidates are grey at 3 sigma (ratio 0.97-1.15 with the bands in phase), eight of them RS CVn or BY Dra systems 2.1-4.1 mag above the main sequence by Gaia, where the companion that defines the class dilutes the spots' colour, and the ninth, ZTF J064125.61+093443.1 with W1-W2 of 0.46, a pre-main-sequence star in NGC 2264 (Gaia parallax 1.39 mas, 719 pc) occulted by its own disk; none left (`ztf_achromatic`) |
| TeV neutrinos moving with the planets | the IceCube ten-year point-source sample, 1134450 tracks over 10.3 years; Jupiter, Saturn, Mars and Venus from the built-in ephemeris on an hourly grid, events taken with the planet within 5 deg of the Sun set aside | the unbinned point-source likelihood in each planet's frame against 1000 time scrambles that fix the events and move the planet: Jupiter TS 0.9 (p 0.17), Saturn 0.6 (0.17), Mars 0.0 (0.42), Venus 0.3 (0.23), where the scrambles reach 9-13; 90 per cent E^-2 flux limits of 1.3-2.1e-12 per TeV cm2 s at 1 TeV, 1.5-2.4e-11 erg/cm2/s over 1 TeV-1 PeV, and luminosities below 7e9 W at Venus, 1e10 W at Mars, 2e11 W at Jupiter and 6e11 W at Saturn (`icecube_planets`) |
| Brick-wall spectral edges in GLEAM-X | GLEAM-X DR1 (VizieR VIII/110): 28682 sources above 20 sigma in the wide band, 27585 with sixteen or more of the twenty 7.68 MHz sub-bands from 72 to 231 MHz, observed in five 30 MHz settings | a curved power law against the same law times a step at each boundary within one setting, where the sub-bands are simultaneous: the chi-square gain's median 0.2, 99th percentile 7.9 and 99.9th 71 carry the sub-band flux-scale errors common to all sources; one source in the top 0.1 per cent with a step above 30 per cent, GLEAM-X J082817.6-221400 (1.23 Jy, +35 per cent after 115 MHz, its twenty neighbours flat there), which has a second 1.18 Jy source 69 arcsec away inside the low-frequency beam, so the sub-band fits merge and split the pair as the beam shrinks with frequency, the 76-99 MHz fluxes alternating by 40 per cent; none left (`gleamx_edges`) |
| Line-only X-ray sources in eROSITA DR1 | the eROSITA DR2 eRASS:3 main catalogue (VizieR J/A+A/712/A171): 1975540 sources, 63043 point sources with 80 or more counts in 0.2-0.5, 0.5-1, 1-2 and 2-5 keV | the fraction of the counts in each band with its errors: the maximum fraction has median 0.46, 90th percentile 0.62 and 99th 0.78 across the point sources; sources holding 85 per cent or more of their counts in one band at 3 sigma with every other band below 5 per cent number 13 in 0.2-0.5 keV, the supersoft class, 2 in 2-5 keV, the absorbed class, and none in 0.5-1 or 1-2 keV, where no continuum could put them; the spectral-fit version of the test on the released source spectra is the step that remains (`erosita_line_only`) |
| Dimming with mid-infrared brightening | the Hipparcos-to-Gaia dimming run and the NEOWISE W2 decade trends of the same stars: 671 with both | an industrial shroud dims the optical and brightens the mid-infrared together; the one-sided optical and W2 deviations, each scaled to its own run's robust spread, combined by Fisher's method, against the W2 trends re-paired among stars within 0.5 mag in W1 (2000 draws): the highest value, HIP 67858, is 24.4 sigma fainter in Gaia with W2 fading as well and arises by chance at its rank 99 per cent of the time, and the lowest chance at any of the twenty ranks is 0.04 (HIP 57115), one in twenty ranks; the top of the list is optical dimming alone (`dimming_ir_joint`) |
| The Wow! signal's cloud | HI4PI at the two fields of Arecibo Wow! II (19h25m02s and 19h27m55s, -26d57m +-20 arcmin), at the signal's -74 km/s LSR | no H I at the velocity in either field: 0.010 and 0.003 K against 0.019 K noise over the 10 arcmin average, N(HI) below 1.4e17 cm-2 for a one-channel line, while the fields' own emission peaks at +3 to +4 km/s with 26 K; the brightest pixel at the velocity inside each field's +-20 arcmin holds 0.11 K against a single-pixel noise of 0.040 K, and none of the 8800 pixels within 3 deg of either field reaches 5 sigma of its own noise there, while their mean spectrum carries the wing of the local emission falling smoothly through the velocity at 0.014 K, with no feature there; so no cloud filling HI4PI's 16 arcmin beam sits in either field at the velocity, and a compact one is diluted by the beam (`wow_hi4pi_cloud`) |
| Vanished numbered asteroids | JPL Small-Body Database: the 69 numbered asteroids brighter than H 17 with no observation since 2017, each orbit propagated to today and the bodies left within reach looked up in JPL Horizons | all 69 are trans-Neptunian objects (53) or Centaurs (16); 66 are fainter than V 21.5 at opposition now, 2004 YH32 and 2001 KD77 stand at V 21.5 tonight, the Centaur at declination -78, and Pluto's small-body orbit stops in 2016 because its ephemeris comes from the planetary solution; none is a body the surveys should see and do not (`sbdb_vanished_numbered`) |
| Negatively dispersed and pulsar-locked pulses | Breakthrough Listen 349 us products of 88 scans (44 ON, 44 OFF) of the nearest stars' cadences | broadband DM-peaked pulses at 7 sigma per scan, ON against OFF: DM < -1: 25 against 39; -1 to 1: 36 against 34; > 1: 9 against 12; the OFF scans carry every class as often, so the pulses are interference; folds at the Crab, Vela, B1937+21 and J0437-4715 periods as each star sees them: 26 of 176 folds below p 0.05 against 8.8 by chance, but the OFF scans of a control cadence fold as low (4 of 12) and one scan folds at two pulsars' periods at once, so the excess is the red noise of the zero-DM series, not a lock (`bl_pulses`); the HST photon-event lists await a re-download for the same fold, and the X-ray archives cannot serve it, since ACIS frames of 3.2 s and EPIC-pn imaging frames of 73 ms cannot resolve the periods, leaving only HRC and pn timing-mode observations, which the nearby stars lack |
| Beams between stars | the 2705 stars within 20 pc: pairs on opposite sides of the Earth within a 0.25 deg beam | the only sightlines on which traffic between two stars crosses Earth; 37 pairs within a 0.25 deg beam among 2705 stars, as many as random directions give (31 +- 6) (`beam_pairs_20pc`); the pairs' narrowband radio archives are not yet searched |
| Long occulters' companions | Gaia DR3 astrometry of VVV-WIT-08, VVV-WIT-07, Gaia17bpp, TYC 2505-672-1, ASASSN-21qj and J1407, with EE Cep as the control, against field stars matched in G and colour | none stands out: RUWE 1.04-1.10 with 26-70 per cent of the controls as high, and astrometric excess noise within the controls' spread except VVV-WIT-08's 0.42 mas at 16 sigma, in the top 12 per cent; EE Cep's known disk-bearing companion gives RUWE 1.28 and 0.16 mas, in the top 24-31 per cent, so Gaia DR3 cannot see the companions these eclipses need (`long_occulters_gaia`) |
| Interstellar arrivals along the ecliptic | 1I, 2I and 3I from JPL SBDB; 2e7 arrivals carrying the velocities of the 169740 Gaia DR3 stars within 100 pc, perihelia within 2 AU | 0.28 per cent within 5 deg of the ecliptic (isotropic 0.38, retrograde alone 0.14); passes as close as 3I/ATLAS's by Venus, Mars and Jupiter 1.5e-5 of all arrivals and 1.2e-3 of those along the ecliptic, 3.5e-6 together with the alignment; along the ecliptic and within 0.2 AU of one of the three 5.3e-4 (`iso_ecliptic_arrivals`) |
| Signals of interest traced through their sessions | Ma et al. (2023)'s eight signals of interest; every scan of their six Breakthrough Listen GBT sessions, 335 scans, in the 2.84 Hz product | MLc2-MLc8 lie on their own lines in their cadences' OFF scans at 4.8-11.5 sigma combined, 2-34 per cent of their ON level, and MLc3-MLc8 recur in 1-25 scans pointed at other stars; MLc8 is a carrier rising 1.72 kHz over four hours through four other stars' cadences, at S/N to 158 in OFF pointings against 20-40 in its own ON scans; MLc1, at 1188.54 MHz in the aeronautical radionavigation band, is in its ON scans alone, drifting at -1.51 and -0.85 Hz/s in the first two where a transmitter at rest at HIP 13402 would drift at -0.08 Hz/s (`bl_soi`) |
| Stars at rest with the Sun | Gaia DR3: the 169,740 stars within 100 pc with radial velocities and parallaxes at 10 sigma, 48,129 with their velocity relative to the Sun measured to 0.5 km/s | a companion keeping pace with the Solar System: 5 within 1 km/s against 1.01 from a velocity density flat near zero (Poisson p 0.004), the density in 1 km/s shells from 1 to 10 km/s at 0.86-1.39 of that flat value: CD-75 143 (0.29 km/s, 93 pc), UCAC2 1168584 (0.35 km/s, 93 pc), BD+68 1331 (G0, 0.71 km/s, 72 pc), the dMe star PG 0943+489 (0.82 km/s, 26 pc, RUWE 1.53) and Gaia DR3 5415736782809366144 (0.98 km/s, 84 pc); with RUWE below 1.4, 4 against 0.82 (p 0.0097) in 3 systems, CD-75 143 and UCAC2 1168584 lying 7.6 pc apart at 0.37 km/s as members of Crius 131 (Moranta et al. 2022), 40 stars at 113 pc moving at (-0.2, +0.5, -1.7) km/s relative to the Sun with a spread of 1.1-1.3 km/s, part of Theia 371 (Kounkel and Covey 2019); of 35,128 balls of the same density centred elsewhere in velocity space, 0.6 per cent hold as many stars and 4.3 per cent three or more systems; BD+68 1331 (HIP 112584) is a 0.3 Gyr star whose radial velocity of -0.3 +- 0.1 km/s Liu et al. (2015) measured when they rejected it as a sibling of the Sun; the sideways speeds of the 138,627 stars within 100 pc measured to 0.1 km/s, radial velocity or not, put 12, 37 and 193 below 0.25, 0.5 and 1 km/s against 11.4, 45.5 and 181.8 from the flat density, and one other star within 15 pc moves with the Crius 131 pair against 0.36 by area; an association moving with the Sun, as the young disc's do (`gaia_rest_stars`) |
| Stars on a straight line to the Sun | Gaia DR3: 75,785 stars within 100 pc with radial speeds above 20 km/s and sideways speeds measured to 0.5 km/s | an object aimed at the Solar System: 42 move sideways at under 1 km/s against 53.2 from a sideways-velocity density flat near zero; their least distances run from 30,237 au (Gaia DR3 510911618569239040 at 76 pc, receding, 2.77 Myr ago), the stellar encounters of the published lists (Bailer-Jones et al. 2022) (`gaia_headon_stars`) |
| Non-stellar spectra at stellar distances | Gaia DR3's discrete source classifier on the Gaia Catalogue of Nearby Stars beyond parallax 10 mas: 64 sources it calls quasar or galaxy at 0.9; SIMBAD | every one explained, some twice: 53 white dwarfs by SIMBAD or the colour-magnitude locus, 10 components of resolved multiples or stars with a catalogued neighbour within 10 arcsec whose light enters the BP and RP windows, 3 cataclysmic variables, 2 binaries and one source without photometry (`gaia_qsolike_nearby`) |
| Light that appeared since 2MASS | the Gaia Catalogue of Nearby Stars within 20 pc at G 5-13: 91 sources without a 2MASS best neighbour in Gaia DR3; the 2MASS point-source catalogue (II/246) by CDS XMatch | a source switched on since 1999: 88 lie in 2MASS within 5 arcsec plus 2.5 years of their proper motion of their position carried back to 2000, the cross-match's misses among fast stars (median 457 mas/yr); the other 3 are eps Ret B, eps Sco B and bet Aql B, secondaries in their primaries' glare (`gaia_no2mass_nearby`) |
| Objects of unknown nature within 10 pc | SIMBAD entries with parallaxes above 100 mas typed of unknown nature or not an object | one entry, omi02 Eri b, the retracted planet of 40 Eri, typed not an object (`simbad_unknown_nearby`) |
| Pulsars that hold their period | ATNF catalogue (VizieR B/psr): 1,843 isolated pulsars outside globular clusters and the Magellanic Clouds with a period derivative | a beacon kept at a constant period: 4 with a measured derivative zero or negative, J1829-1011 (-1.3 sigma), J1817-0743 (-0.3), J1144-6146 (-0.4) and J1852+0033 (none measured), none below zero at 3 sigma; J1024-0719, J1843-1448 and J1801-1417 turn negative only once corrected for the Galactic acceleration and the Shklovskii term at their DM distance (`atnf_spinup_pulsars`) |
| Pulsars on nearby stars | the 2,530 ATNF pulsars with positions against Gaia DR3 within 2 arcsec by CDS XMatch | a beacon placed at a star: 1,077 Gaia sources within 2 arcsec, 2 of them within 200 pc at 5 sigma, the helium white-dwarf companion of J0437-4715 (G 20.4, 7.1 mas) and a foreground star (6.6 mas) over J1701-3006E in the globular cluster M62 (`atnf_pulsars_on_stars`) |
| Planets on Earth's year | NASA Exoplanet Archive composite table: 86 planets with periods of 300-430 d | a period chosen to match ours: one within 0.2 per cent of the sidereal year, Kepler-1536 b at 364.758 d (0.14 per cent short), against 0.97 expected from the density of periods (`exoplanets_earth_year`) |
| Planetary systems in equal period steps | NASA Exoplanet Archive composite table: 535 consecutive triples in 356 systems of three or more planets | a spacing no resonance asks for: 3 triples step equally to 0.5 per cent, TOI-1136 c-d-e (1:2:3), HD 110067 d-e-f and Kepler-223 c-d-e (2:3:4), chains n : n+1 : n+2 that are arithmetic and resonant at once; 17 triples have equal period ratios (`exoplanets_period_steps`) |
| Asteroids on circles in the ecliptic | JPL Small-Body Database: 895,910 numbered asteroids | an orbit made rather than captured: none with eccentricity below 0.001 and inclination below 0.2 deg, against 0.01 from the 24 below that eccentricity and the 537 below that inclination taken as independent (`sbdb_circular_asteroids`) |
| Lithium in old cool dwarfs | GALAH DR4: 1,844 dwarfs below 5300 K (log g above 4.3) with a clean A(Li) and isochrone ages above 6 Gyr; their Gaia DR3 speeds; the red-arm spectra of the 135 above A(Li) 2.0 and of 135 lithium-poor stars of the same selection and S/N | an element such a star has burned: 135 above A(Li) 2.0, 26 of them at young-disc speeds (below 20 km/s) and 10 at thick-disc speeds (above 60 km/s); mass rules out an industrial origin, A(Li) 3.69 in a 0.04 M_sun envelope holding 1.9e21 kg of lithium, about 200 times the Earth's; the Li I 6708 line refitted in each spectrum at the instrument's width, at that width broadened by GALAH's vsini and at the star's own Ca I 6717.7 width, against the lithium-poor stars read at their partners' claimed widths (132 of 135 absent, 1 confirmed) and the same stars with lines of those widths injected (134 of 135 recovered, at 1.00 of the injected width): 95 lines confirmed, every one in a star with a sign of youth (vsini of 5 km/s or more in 92, H-alpha in emission, Ca II triplet activity or a young-disc speed) or of a companion, so their isochrone ages are wrong; 18 absent where GALAH gives 113-600 mA with a clean flag, among them the highest, Gaia DR3 3910691559800909568 (401 mA listed, 17 +- 28 mA measured, GALAH's own neural-network [Li/Fe] 0.21 +- 0.17); 1 much weaker; 21 at a median S/N of 6, too noisy to test; the one real line at a thick-disc speed, Gaia DR3 5489922653396735360, belongs to a close double whose images Gaia splits in 44 per cent of its transits (RUWE 6.6) and whose velocity reads 19.7 km/s in GALAH against 56.9 +- 16.4 km/s from Gaia's two transits, so its speed is not its own; none left (`galah_lithium_old_dwarfs`) |
| Planets on Earth's day | NASA Exoplanet Archive composite table: 170 planets with periods of 0.7-1.4 d | a period chosen to match Earth's turning: one between the sidereal day less 0.2 per cent and the solar day plus 0.2 per cent, TIC 18942729 b (0.998178 d, found by TESS from space, where no night aliases a period), against 1.64 expected (`exoplanets_earth_day`) |
| Planets on one clock | NASA Exoplanet Archive composite table: 330 planets with periods measured to 5e-7 | a period standardised across systems: no pair in different systems within 1e-6 against 0.04 from the pairs within 1e-4; the two pairs within 1e-5, Kepler-550 b with Kepler-435 b and Kepler-856 b with TOI-1135 b, differ by 11 and 19 times their combined errors (`exoplanets_shared_periods`) |
| Pulsars on one clock | ATNF catalogue (VizieR B/psr): 2,071 pulsars with frequencies measured to 1e-7 and first derivatives, carried to MJD 56000 | a beacon period shared between sites: 3 pairs more than 1 deg apart outside one globular cluster within 1e-6 against 1.23 from the pairs within 1e-4, each apart by 41 to 7,855 times the combined errors; periods the catalogue gives to two digits pile onto round values (4.1 and 3.6 ms) and are left out (`atnf_shared_clocks`) |
| Fast radio bursts at nearby stars | CHIME/FRB Catalog 1 (VizieR J/ApJS/257/59): 536 bursts; the 312 sources of the Gaia Catalogue of Nearby Stars within 10 pc | a burst sent from a neighbour: one 2-sigma ellipse, FRB 20190429A's, holds a nearby double (Gaia DR3 2154880616774131840 and 2154880616774131712) 0.30 deg from the burst, against 1.88 with the bursts moved 5-20 deg in right ascension (`chime_frb_nearby_stars`) |
| Asteroids brighter than a mirror | JPL Small-Body Database: 128 asteroids with geometric albedos above 0.8; AKARI (J/PASJ/63/1117), WISE fits with errors (J/ApJ/741/68) and taxonomy from the ATLAS phase curves (VII/288) | a polished or white made surface: 93 fall below the 0.6 of the brightest natural surfaces at 3 sigma in AKARI or WISE or carry a dark class their albedo contradicts (27413 Ambruster and 1999 CX85 are C-types listed at 0.86 and 0.99), 24 are fits pinned at 1.000 and 11 are enstatite, basaltic or X-type surfaces; 17 rest on one albedo with no class or second measurement, at the sizes (1-4 km) where Pravec et al. (2012) found catalogue absolute magnitudes too bright by 0.3-0.5 mag, enough to bring 0.9 to 0.6 (`sbdb_mirror_asteroids`) |
| Retrograde orbits inside Jupiter's | JPL Small-Body Database: bound orbits with i above 90 deg, a below 4.5 au and q beyond 1.3 au | bodies circling against the planets' flow, which collisions and the planets remove: one, 2022 OF60 (a 4.28 au, e 0.68, i 124 deg), on a 15-day arc of orbit quality 8 with a Tisserand parameter of 0.47, a Damocloid captured from the comets (`sbdb_retrograde_inner`) |
| Objects on Earth's own orbit | JPL Small-Body Database: 23 asteroids with a 0.95-1.05 au, e below 0.05 and i below 3 deg | something parked on our path round the Sun: 23 bodies of 2-34 m; radiation pressure measured at 3 sigma for 4 (2020 GE, 2006 RH120, 2021 GM1 and 2020 CD3), area-to-mass ratios of 1.7-5.2e-4 m2/kg, a tenth of a spent rocket stage's or less, each allowing rubble's density or more at albedo 0.5 (662-5,659 kg/m3); the other 19 have arcs too short to measure it, and identified rocket stages such as 2020 SO leave the asteroid catalogue (`sbdb_earth_orbit`) |
| Light Gaia's outlier map could not place | Gaia DR3 Outlier Analysis (astrophysical_parameters, oa_neuron_information): 99,119 sources within 100 pc at G below 17 with RUWE below 1.4 and single-source BP/RP excess | 154 of the 900 neurons carry no class and hold 11.1 per cent of all mapped sources, but only 3 of the nearby clean sources against 11,000 at that share: the white dwarf G 171-B10A, a double and the cataclysmic variable GD 552 (`gaia_oa_unlabelled`) |
| Bright nearby light no class claims | Gaia DR3 discrete source classifier: 116,448 sources within 100 pc at G below 15 with RUWE below 1.4 | one source with every class probability below 0.5, its BP/RP excess not a single source's (`gaia_noclass_nearby`) |
| Something at rest in the universe's frame | Gaia DR3: 295,762 stars with radial velocities at heliocentric speeds of 300-440 km/s, 24,211 with velocity errors below 10 km/s | a body at rest relative to the cosmic microwave background moves at 369.8 km/s toward Galactic (84.0, -48.3) deg as we see it: none within 10 km/s of that velocity, against 0.39 around 1000 random directions of the same speed (`gaia_cmb_rest`) |
| Stars accelerating along their own motion | Gaia DR3 nss_acceleration_astro: 334,107 solutions at 5 sigma after the perspective term | thrust gathers accelerations along the motion: 4.53 per cent lie within 8 deg of it and 4.54 per cent within 8 deg against it, against 4.44 per cent for a uniform angle, the same small excess at both ends, which no thrust gives (`gaia_thrust_alignment`) |
| Copy stars on opposite sides of the sky | Gaia DR3: 48,075 stars within 100 pc with velocities to 0.5 km/s | no pair more than 90 deg apart alike to 0.002 mag in G and BP-RP, 0.2 per cent in parallax and 0.5 km/s in velocity, and none with the velocities shuffled (`gaia_copy_stars`) |
| Our explained flags in Earth's transit zone | the coverage store: 166,903 Gaia DR3 stars, 15,894 of them vetted | 48 vetted stars within 0.27 deg of the ecliptic against 413 at the store's share (`store_flags_etz`) |
| Our flags toward the obvious meeting-point directions | the coverage store: 180,822 Gaia DR3 stars, 32,003 of them vetted | toward the Galactic centre 3,646 vetted stars against 6,772 from the whole store's share, toward the anticentre 1,743 against 2,268 and toward the poles 3,394 against 2,208, the footprints of the surveys that produced the vets, which avoid the plane; with each run's own coverage setting its share, 3,819 run targets against 3,832 toward the centre, 1,786 against 1,771 toward the anticentre and 3,464 against 3,465 toward the poles (`store_flags_directions`) |
| Planets inside their own Roche limit | NASA Exoplanet Archive composite table: 1,287 planets with mass and radius measured to a third | none inside the fluid Roche limit at 3 sigma; the nearest, WASP-12 b, 0.3 sigma outside it (`exoplanets_inside_roche`) |
| Copy planets in different systems | composite table: 25 planets with mass and radius to 3 per cent | no pair alike to 1 per cent in radius, mass and period (`exoplanets_copies`) |
| Daysides hotter than their stars allow | the Exoplanet Archive's emission-spectroscopy table: 103 brightness temperatures with host temperature and a/R* | one above the hottest dayside that zero albedo and no redistribution allow, GJ 436 b at 3.6 um (1120 +- 20 K against 875 K), the band where Stevenson et al. (2010) found methane missing on the tidally heated planet (`exoplanets_dayside_excess`) |
| Period ratios that spell constants | composite table: 1,591 adjacent planet pairs | none within 1e-4 of pi, e, the golden ratio, sqrt 2 or sqrt 3, against 0.93 for five random numbers (`exoplanets_constant_ratios`) |
| Systems packed tighter than Hill stability | composite table: 1,482 adjacent pairs with masses and semi-major axes | 29 below 2 sqrt 3 mutual Hill radii: microlensing pairs with projected separations, masses from mass-radius relations, pairs near 3:2, 4:3 and 2:1 resonance (HR 8799, 7 CMa, HD 5319, HD 200964), the circumbinary claims around the post-common-envelope binaries NN Ser and HU Aqr, and Kepler-132 b and c, which orbit different stars of a binary (`exoplanets_hill_packing`) |
| Two planets on one orbit | composite table: 1,067 systems of two or more planets | no pair within 1 per cent in period (`exoplanets_coorbital`) |
| Pulsars with square pulses | ATNF catalogue (VizieR B/psr): 1,050 pulsars with both widths | none with W10/W50 below 1.05; median 2.00 (`atnf_square_pulses`) |
| Pulsars with no electrons in front | ATNF: 2,457 pulsars with a dispersion measure | none below 1 pc cm^-3; the lowest, J0108-1431, at 2.38 (`atnf_no_dispersion`) |
| Pulsars spinning faster than a neutron star survives | ATNF: 2,527 pulsars with a period | none below 0.7 ms; the fastest, J1748-2446ad, at 1.396 ms (`atnf_breakup`) |
| Pulsars radiating more than their spin supplies | ATNF: 1,563 pulsars with 1.4 GHz luminosity and spin-down power | none above it even taken isotropic over 1 GHz (`atnf_overpowered`) |
| Pulsars of one globular cluster on one clock | ATNF: 72 cluster pulsars timed to 1e-7 in 21 clusters | no same-cluster pair within 1e-4 (`atnf_cluster_clocks`) |
| Binary pulsars on Earth's year | ATNF: 256 binary pulsars | none within 0.1 per cent of a year; the nearest, J1823-1115, at 357.8 d (`atnf_year_orbits`) |
| Burst dispersions on shared values | CHIME/FRB Catalog 1: 492 sources, one burst for each repeater | 107 pairs within 0.5 pc cm^-3 against 111 +- 12 from the smoothed distribution; counting every repeat burst gives 216 against 140, the repeaters' own bursts (`chime_dm_shells`) |
| Bursts arriving together from different directions | CHIME/FRB Catalog 1: 536 bursts over 341 days | none more than 10 deg apart within 1 s, against 0.01 (`chime_simultaneous`) |
| Copy bursts from different directions | CHIME/FRB Catalog 1: 227 non-repeating bursts with width, fluence, scattering and spectral index | none alike in all four (`chime_copy_bursts`) |
| Gamma-ray bursts from nearby stars | Swift (HEASARC swiftgrb): 711 bursts with XRT positions; 2,575 sources within 20 pc | no star inside an error circle, and none with the bursts moved 1-2 deg (`swift_grb_nearby_stars`) |
| Nearby stars LAMOST labelled unknown | LAMOST DR10 low-resolution general catalogue | no spectrum classed Unknown reaches r-band S/N 50; the class holds low-S/N spectra alone (`lamost_unknown_nearby`) |
| Bright nearby stars DESI fitted badly | DESI DR1: 12,624 stellar spectra with a fit warning and a Gaia identifier | one within 100 pc at G below 16, Gaia DR3 3836824650659924992 (G 15.3), its warning bit 2048 that of poor data (`desi_badfit_nearby`) |
| Zinc far above iron | GALAH DR4: 226,305 clean dwarfs at [Fe/H] -0.3 to +0.3 | 58 above [Zn/Fe] +0.8 where the sample scatters by 0.11, their S/N in the blue arm, where the zinc lines lie, a median of 13 (`galah_zinc_excess`) |
| Dwarfs that look mined | GALAH DR4: 215,038 clean dwarfs at [Fe/H] above -0.3 | none with [Si/Fe] and [Al/Fe] both below -0.4 (`galah_mined_dwarfs`) |
| Interstellar bands within 50 pc | GALAH DR4: 198 stars within 50 pc with a fitted 5780 A band | 27 above 5 sigma and 20 mA, 19 of them below 4500 K, where the star's own lines fill the band; 8 hotter ones at up to 2.1 A, more than any 50 pc sightline holds, are open; the band's median is 56 mA at 0.5-1 kpc against 20 within 50 pc (`galah_dib_within_50pc`) |
| Stars spinning faster than they hold together | GALAH DR4: 320,994 clean dwarfs with v sin i, mass and luminosity | none; the fastest at 0.075 of break-up (`galah_breakup_rotation`) |
| Flares firing together across the sky | Yang et al. (2023) TESS flare catalogue: 60,810 flares | 3,876 pairs more than 10 deg apart within a minute against 3,657 from the rate at 10-60 minutes; 607 of them crowd minutes holding several pairs, the busiest at two moments of 2018 November and December when flares registered on many stars at once, the spacecraft's events and not the stars' (`tess_flare_synchrony`) |
| Standardised flares | Yang et al. (2023): 1,352 stars with ten or more flares | none whose energies agree to 5 per cent; the tightest spreads by 36 per cent (`tess_standard_flares`) |
| Stars steadier than photon noise allows | Kepler DR25 stellar table: 198,670 stars with 6-hour CDPP | 97 below 0.8 of the shot noise their Kepler magnitude gives, the lowest at 0.27, each over the full four years and most of the lowest at 6000-8200 K, where pulsations shape the pipeline's noise filter; no star can be quieter than its photons, so the figure is the pipeline's (`kepler_steadier_than_photons`) |
| Copied planetary systems | composite table: 535 consecutive triples | 3 pairs of systems with both period ratios equal to 0.1 per cent against 0.44 shuffled, every one a chain of 3:2 and 4:3 resonances (TOI-178 with K2-138, HD 110067 with Kepler-223, Kepler-80 with K2-138), the steps that migration in a disc builds and the shuffle breaks (`exoplanets_copied_systems`) |
| Planets brighter than a mirror | the emission-spectroscopy table: 128 eclipse depths shortward of 1 um with geometry | no geometric albedo above 1 at 3 sigma (`exoplanets_mirror_albedo`) |
| Planets orbiting inside their star or hotter than it | composite table: 6,057 planets | none inside its star; two hotter than their star can hold, Oph 11 b and CFHTWIR-Oph 98 b, young companions glowing from their own contraction (`exoplanets_inside_star`) |
| Pulsars paired in simple ratios | ATNF: 1,999 pulsars timed to 1e-7 outside clusters, 2,655 pairs within 1 deg | none in a ratio p/q to 1e-6, against 0.03 (`atnf_simple_ratios`) |
| Bursts masquerading from pulsars | CHIME/FRB Catalog 1 and the ATNF catalogue | no burst within 1 deg and 5 per cent in dispersion of a pulsar (`chime_frb_pulsars`) |
| Well-studied neighbours of unknown nature | SIMBAD entries within 100 pc | none typed unknown or not an object with 20 or more references (`simbad_studied_unknowns`) |
| Stars leaving the Galaxy from next door | Gaia DR3: 146,385 stars within 100 pc with velocities to 5 km/s | none above the 550 km/s escape speed; the fastest at 479 km/s (`gaia_unbound_nearby`) |
| Nearby stars SDSS could not classify | SDSS DR17 SpecObj through SkyServer: 9,148 primary stellar spectra at S/N above 20 with a redshift warning or no subclass; Gaia DR3 by CDS XMatch | 64 within 100 pc, every one typed by SDSS: 35 white dwarfs or cataclysmic variables in SIMBAD, many given the nearest template of another class (L, T, carbon, O, B, F-K supergiant) for want of white-dwarf templates, and 29 K, M and F stars typed as they are, most of the K and F stars at G 9-11, where high-S/N spectra show more outlying pixels than the fit allows (`sdss_unclassified_nearby`) |
| X-rays from cold white dwarfs | Gentile Fusillo et al. (2021): 12,007 white dwarfs within 100 pc below 8000 K; eRASS1 main catalogue by CDS XMatch | 21 within three positional errors of an eRASS1 source against 6-23 (mean 12.4) with the white dwarfs moved 2 arcmin; 6 share the error circle with a companion at the white dwarf's parallax (four M dwarfs, a K dwarf and a second white dwarf), 11 with other Gaia stars, and 4 lie 1.8-2.9 errors off with no other star in the circle, at the chance rate (`erass1_cold_white_dwarfs`) |
| Dwarfs whose 12 um output changed between 1983 and 2010 | IRAS PSC (II/125) and AllWISE (II/328) by CDS XMatch at 7,556 Gaia DR3 stars within 100 pc at G below 8: 1,226 measured in both | W3 - IRAS median 0.44 mag, scatter 0.10; two parted by 1 mag, both fainter in W3 and both the B stars of doubles, HD 58038 B and 20 Gem B, whose partners 7 and 20 arcsec away lie inside IRAS's beam and outside W3's (`iras_wise_12um`) |
| Dwarfs larger than their light allows | JMMC Measured Stellar Diameters (II/345) by CDS XMatch with Gaia DR3 FLAME radii: 62 dwarfs within 100 pc | measured over predicted diameter median 0.975, scatter 0.057; none above 1.2 at 3 sigma (`jmdc_swollen_dwarfs`) |
| Stars dimmer in the infrared than their spectra allow | Gaia DR3 RVS temperatures with GSP-Spec flags of 0 or 1 and AllWISE W1 through Gaia's best neighbours: 16,360 stars within 100 pc | G - W1 scatters by 0.106 mag about its locus; 28 with a colour temperature 500 K above the spectroscopic at 5 sigma, every one with a BP-RP temperature within 90 K of its G - W1 temperature, so the optical colour agrees with the infrared and the RVS temperature reads 500-760 K low, 19 of them at RVS temperatures of 3,880-4,100 K (`gaia_infrared_deficit`) |
| Hipparcos stars Gaia cannot find | Hipparcos new reduction: 15,332 stars at Hp 7-11 without a Gaia DR3 best neighbour; Gaia DR3 by CDS XMatch at positions carried to 2016.0 | 15,328 have a Gaia source within 10 arcsec, the best-neighbour table's misses; of the other 4, three carry a Gaia DR3 identifier in SIMBAD, and HIP 116191 is GJ 897 BC, a pair Gaia holds as two sources of G 10.0 6.5 arcsec from SIMBAD's position, where Hipparcos's solution of the double (parallax 5 +- 35 mas) does not carry it (`hipparcos_gone`) |
| RR Lyrae on one clock | Gaia DR3 vari_rrlyrae: 60,123 stars with periods to 1e-5 | 7,430 pairs more than 1 deg apart within 1e-6 against 7,392 scaled from the pairs within 1e-4 (`gaia_rrlyrae_clock`) |
| Cepheids on one clock | Gaia DR3 vari_cepheid: 994 stars with periods to 1e-5 | 2 pairs within 1e-6 against 0.46, one pair in each Magellanic Cloud (`gaia_cepheid_clock`) |
| Eclipsing binaries on one clock | Gaia DR3 vari_eclipsing_binary: 27,900 binaries with periods to 1e-6 | 791 pairs more than 1 deg apart within 1e-6 against 788 scaled from the pairs within 1e-4 (`gaia_eclipser_clock`) |
| Binary orbits on one clock | Gaia DR3 nss_two_body_orbit: 1,435 orbits with periods to 1e-5 | 1 pair within 1e-6 against 0.5 (`gaia_orbit_clock`) |
| Systems built from identical planets | composite table: 8 systems of three or more planets with every mass and radius measured to 15 per cent | none whose masses and radii are both consistent with one value; TOI-125's radii agree (p 0.55) and its masses do not (p 4e-5) (`exoplanets_identical_systems`) |
| Something closer than Proxima Centauri | Gaia DR3: sources with parallaxes above 700 mas | one, Proxima itself at 768.1 mas; none beyond it (`gaia_closer_than_proxima`) |
| Something faster across the sky than Barnard's Star | Gaia DR3: every source with a proper motion above 9000 mas/yr | one, Barnard's Star itself at 10393 mas/yr (`gaia_faster_than_barnard`) |
| Stars standing still in the Galaxy | Gaia DR3: 146,385 stars within 100 pc with velocities to 5 km/s | 2 below 30 km/s about the Galactic centre against 2.9 from the 23 below 60 km/s scaled by the volume of speeds: BD+11 4725 (23 km/s) and the halo subdwarf G 226-48 (29 km/s, [M/H] -1.1), then G 167-12 and G 240-40 ([M/H] -1.4) at 30 km/s (`gaia_still_in_galaxy`) |
| Radial velocities the Galaxy cannot hold | Gaia DR3: radial velocities beyond +-700 km/s measured to 5 km/s over ten or more transits | 2, Gaia DR3 347866482390401280 (+863 km/s) and 5254851637274716288 (-811 km/s), faint RVS spectra at expected S/N 5 with 6 of 14 and 9 of 17 transits deblended from neighbours, and no APOGEE spectrum (`gaia_rv_beyond_escape`) |
| A lattice among the nearby stars | Gaia DR3: 14,815 systems within 50 pc brighter than absolute G 10, those closer than 0.1 pc merged | Clark-Evans ratio 0.942 against 1.000 +- 0.004 for uniform volumes, clustered rather than regular (`gaia_nearby_lattice`) |
| Bright stars no older catalogue holds | Gaia DR3: 1,064 sources brighter than G 6 without a Hipparcos-2 or Tycho-2 best neighbour | 1,046 named in SIMBAD (the brightest stars, whose Gaia solutions have three parameters or a binary's perturbation) and the other 18 within 2 arcsec of a Hipparcos star; none uncatalogued (`gaia_bright_uncatalogued`) |
| Galaxies with parallaxes | Gaia DR3: 139 sources the discrete source classifier calls galaxies above 0.9 with parallaxes above 10 mas at 10 sigma | 137 with solutions Gaia's statistics doubt (RUWE, a second image peak, image asymmetry or excess noise), median G 19.3 and 132 within 15 deg of the Galactic plane; the other 2 move at 29 and 48 mas/yr with BP/RP flux excesses of 3.6 and 9.5, one 4.8 arcsec from the binary CD-34 6718, the neighbours' light in the spectra the classifier reads (`gaia_galaxies_with_parallax`) |
| Quasars that move | Gaia DR3: 391,934 quasar candidates both classifiers call quasars at QSOC redshift above 1 | 2 moving above 10 mas/yr at 10 sigma, both with solutions Gaia's statistics doubt (`gaia_moving_quasars`) |
| Planets denser than iron | composite table: 317 transiting planets below 30 Earth masses with measured mass and radius to 20 per cent | none smaller than a pure-iron planet of their mass at 3 sigma; the nearest K2-229 b (2.2 sigma) and Kepler-107 c (on the iron line) (`exoplanets_denser_than_iron`) |
| Planets in exact resonance | composite table: 598 adjacent pairs with both periods measured to 1e-5 | 1 within 1e-4 of a small-integer ratio, Kepler-87 b and c at 5:3 (+2.4e-5), against 1.04 from the pairs 1e-3 to 1e-2 from the ratios (`exoplanets_exact_resonance`) |
| Copies of Earth | composite table: 1,699 planets of 0.5-2 Earth radii with insolation and host temperature | none within 10 per cent of Earth's radius and 20 per cent of its mass, both measured, at 0.75-1.25 of its insolation around a 5300-6100 K star; the nearest Kepler-1126 c and Kepler-452 b at 1.45 and 1.63 Earth radii, their masses estimated (`exoplanets_earth_copies`) |
| Copy pulsars | ATNF (VizieR B/psr): 1,765 pulsars with period, period derivative, dispersion measure and W50 | no pair more than 10 deg apart alike to 1e-3 in period and 5 per cent in the other three, and none with them shuffled among pulsars of like period (`atnf_copy_pulsars`) |
| Binary pulsars on Earth's day | ATNF: 256 binary pulsars | none within 0.1 per cent of the solar or sidereal day, against 0.08 from the 4 within 10 per cent of a day (`atnf_day_orbits`) |
| Pulsars beyond the magnetar limit | ATNF: 2,052 pulsars with a positive period derivative | none with a dipole field above 1e16 G; the strongest the magnetar SGR 1806-20 (J1808-2024) at 2.1e15 G (`atnf_beyond_magnetars`) |
| Pulsar pairs whose frequencies spell constants | ATNF: 1,999 pulsars timed to 1e-7 outside globular clusters | 8 pairs whose frequency ratio equals pi, e, the golden ratio, sqrt 2 or sqrt 3 to 1e-6, against 8.9 from the 891 within 1e-4 (`atnf_constant_ratios`) |
| Bursts from inside the Galaxy | CHIME/FRB Catalog 1: 492 sources, one burst for each repeater | none with dispersion below the Milky Way's in both NE2001 and YMW16; the smallest excess FRB 20181030A at 62-70 pc cm^-3 (`chime_inside_galaxy`) |
| Bursts from Earth's transit zone | CHIME/FRB Catalog 1: 492 sources | 1 within 0.264 deg of the ecliptic, FRB 20190224C, against 1.33 from random right ascensions at the sources' declinations (`chime_transit_zone`) |
| Burst dispersions on a ladder | CHIME/FRB Catalog 1: 492 sources | the strongest spacing 9.45 pc cm^-3 at Rayleigh power 9.1, reached or exceeded by 5.8 per cent of draws from the smoothed distribution (median 6.4) (`chime_dm_ladder`) |
| White dwarfs above the Chandrasekhar mass | Gentile Fusillo et al. (2021): 16,281 white dwarfs within 100 pc with hydrogen-model masses | none above 1.40 solar masses at 3 sigma in both models; the heaviest WDJ200417.75-821223.74 at 1.38 +- 0.11 (`wd_above_chandrasekhar`) |
| X-rays from cold brown dwarfs | Kirkpatrick et al. (2021) 20 pc census: 133 T and Y dwarfs with Spitzer astrometry, carried to 2020.0; eRASS1 (half the sky) by CDS XMatch | no eRASS1 source within 15 arcsec, and none with the dwarfs moved 2 arcmin (`erass1_cold_brown_dwarfs`) |
| Ultraviolet from cold brown dwarfs | the same 133 T and Y dwarfs carried to 2007.0; GALEX GUVcat AIS (II/335) by CDS XMatch | no GALEX source within 5 arcsec, against 0-3 (mean 1.6) with the dwarfs moved 2 arcmin (`galex_cold_brown_dwarfs`) |
| Radio from cold white dwarfs | Gentile Fusillo et al. (2021): 12,007 white dwarfs within 100 pc below 8000 K carried to 1995.0; NVSS (VIII/65) by CDS XMatch | 20 with an NVSS source within 15 arcsec against 26-35 (mean 30.4) with the white dwarfs moved 2 arcmin, the radio sky behind them (`nvss_cold_white_dwarfs`) |
| Ultraviolet from the coldest white dwarfs | Gentile Fusillo et al. (2021): 885 white dwarfs within 100 pc below 4500 K carried to 2007.0; GALEX GUVcat AIS by CDS XMatch | 16 with a GALEX source within 5 arcsec against 5-14 (mean 10.4) moved 2 arcmin; most at NUV 21-22.7, what a 4500 K photosphere at G 17-18 gives at GALEX's limit, and the two at NUV 18.2 and 18.7 4 arcsec away (`galex_coldest_white_dwarfs`) |
| Infrared at isolated millisecond pulsars | ATNF pulsars below 30 ms with no orbit, outside globular clusters, timed to 1 arcsec; AllWISE by CDS XMatch, Gaia DR3 and the Legacy Survey DR10 for the matches | 3 of 35 with an AllWISE source within 3 arcsec against 0-1 (mean 0.5) moved 2 arcmin: at J1024-0719 the Gaia star that shares the pulsar's proper motion, its wide companion; at B1937+21 a reddened field star 2.2 arcsec off a timing position good to a milliarcsecond; at J1551-0658 a galaxy the Legacy Survey resolves (`allwise_isolated_msps`) |
| Unique variables next door | GCVS stars of the unique type; Gaia DR3 by CDS XMatch; SIMBAD | 13 of 93 within 100 pc, every one of a natural kind: five L dwarfs whose clouds turn with them, four magnetic white dwarfs carrying spots round (GD 356 among them, with its emission lines), the AM CVn binary GP Com, the gamma Doradus pulsator V2118 Oph, the spotted binary AS Dra, and UU CrB, whose one event is the 1980 superflare Schaefer, King & Deliyannis (2000) list on an ordinary F8 dwarf (`gcvs_unique_near`) |
| Gamma rays from cold white dwarfs | Gentile Fusillo et al. (2021): 12007 white dwarfs within 100 pc below 8000 K; Fermi-LAT 4FGL-DR4 | 28 inside an unassociated 95 per cent ellipse against 22-54 (mean 36.4) moved 1 deg; 39 more inside ellipses the catalogue gives to blazars, radio galaxies, pulsars, supernova remnants and the binary V918 Sco (`fermi_cold_white_dwarfs`) |
| Hard X-rays from the nearest stars | Gaia Catalogue of Nearby Stars: 2575 objects within 20 pc; Swift-BAT 105-month and 150-month catalogues (14-195 keV) | 0 inside a BAT error circle against 0-6 (mean 2.5) moved 1 deg; none of BAT's 13 catalogued stars lies within 20 pc (`bat_nearest_stars`) |
| Warm stars in Earth's transit zone | Gaia Catalogue of Nearby Stars with its WISE photometry; SIMBAD | 7 warm of 911 stars in the zone against 12.3 expected from the 186 of 13800 stars 1-5 deg away (p 0.96); the seven are bright G and K dwarfs, a giant and a double star (`etz_warm_stars`) |
| Radio from Earth's transit zone | Gaia Catalogue of Nearby Stars north of -40 deg; VLASS epoch-1 components by CDS XMatch | 0 of 1502 zone stars with a 3 GHz source within 3 arcsec, against 0.74 from the 11 of 22386 stars 1-5 deg away and a mean of 0.5 with the zone moved 2 arcmin (`etz_vlass_stars`) |
| Light at 4.6 um alone | Gaia Catalogue of Nearby Stars with its WISE photometry: 49753 stars at BP-RP 0.5-2.5 with W1, W2 and W3 measured; AllWISE flags; SIMBAD | 7 stars five widths above the W1-W2 locus with W1-W3 on it, against 7 as far below; 4 carry AllWISE contamination or extended-source flags, and the 3 left, K and M dwarfs 0.1 mag above the locus, are as common as the deficits (`w2_only_excess`) |
| Glitches firing together | Jodrell Bank glitch catalogue (Basu et al. 2022): 285 glitches in 107 pulsars timed to 2 days or better | 13 pairs in different pulsars within their epoch uncertainties against a mean of 8.8 (95th percentile 14) with each pulsar's glitches moved 100-2000 days, as many or more in 0.11 of draws (`glitch_coincidences`) |
| X-rays from Earth's transit zone | Gaia Catalogue of Nearby Stars in the eRASS1 half of the sky; eRASS1 main catalogue by CDS XMatch; SIMBAD | 83 of 762 zone stars with an eRASS1 source within 15 arcsec against 80.2 expected from the 1151 of 10938 stars 1-5 deg away (p 0.39), and 1.2 with the zone moved 2 arcmin (`etz_erass1_stars`) |
| Ultraviolet from Earth's transit zone | Gaia Catalogue of Nearby Stars; GALEX GUVcat AIS by CDS XMatch; SIMBAD | 251 of 1502 zone stars with a GALEX source within 5 arcsec against 294.5 expected from the 4389 of 22386 stars 1-5 deg away (p 0.996), and 17.0 with the zone moved 2 arcmin (`etz_galex_stars`) |
| Nearby dwarfs APOGEE could not fit | SDSS DR17 APOGEE on SkyServer: 5294 dwarfs within 100 pc at S/N above 100 and 4000-6500 K; SIMBAD; Gaia DR3 | 130 STAR_BAD, every one explained: 101 binaries (double-lined, scattering velocities, or Gaia's RUWE and radial-velocity swing), 27 with a temperature or gravity outside the pipeline's calibrated range, 2 by their SIMBAD types (`apogee_star_bad_dwarfs`) |
| Stars dimmed grey on thin-disc orbits | Gaia Catalogue of Nearby Stars with GSP-Phot metallicities and 2MASS; SIMBAD; GALEX GUVcat AIS by CDS XMatch | 335 of 149417 stars more than 1.5 mag below the main sequence with clean photometry, 66 of them crossing the sky at under 50 km/s against 269 faster; of the 66, 35 metal-poor by GSP-Phot or a J-Ks bluer than the main sequence's, 12 carrying a white dwarf's light (a J-Ks redder than the main sequence's at the star's BP-RP, a D+dM type or an NUV within 5 mag of G), 4 of other SIMBAD types, and 15 M dwarfs at G 15-18 with neither a metallicity nor an ultraviolet detection, left for spectra (`grey_dimmed_disc_stars`) |
| Methanol masers away from the Galactic plane | Pestalozzi, Minier and Booth (2005): 519 masers at 6.7 GHz; SIMBAD | 14 more than 2 deg from the plane, every one at a star-forming region: NGC 281, L1206, Cepheus A, Mon R2, NGC 2024, S231 and eight IRAS or MSX sources with young stars, cores or H II regions beside them (`methanol_masers_off_plane`) |
| Compact radio sources that move like neighbours | Radio Fundamental Catalogue rfc_2026c: 23866 VLBI-compact sources; Gaia DR3 by CDS XMatch; SIMBAD | 16 with a Gaia parallax above 2 mas: 14 known radio stars (RS CVn and Algol binaries, the Be star HD 142184, the Orion Trapezium, young stars), a blazar candidate at G 20.2 whose 4.5 mas parallax is the faint-end tail of spurious solutions, and a star 0.2 arcsec in front of a background source (`rfc_nearby_compact`) |
| Dead stars with living companions | Gaia DR3 binary_masses: 208 astrometric binaries with an unseen companion above 1.4 solar masses, with Gaia BH1-3; AllWISE and eRASS1 by CDS XMatch; SIMBAD | 15 with W1-W3 above 0.3 against 0-3 (mean 0.8) moved 2 arcmin: 13 under AllWISE's halo, spike, persistence or extended-source flags in the Galactic plane, 1 eclipsing binary, and Gaia DR3 5331686334409329664 at b 0.5 deg with W1-W3 1.19 and no explanation in the catalogues; 4 eRASS1 sources within 15 arcsec against 0-1 moved: the Am binary HD 67518, the double star GALEX J145250.3-192225, and the A stars HD 23021 and HD 97080, whose X-rays want a late-type companion their dark 1.6 solar-mass companions cannot be; the three black holes match nothing (`gaia_dead_companions`) |
| Identical black holes merging | GWOSC event list, GWTC-1 to GWTC-5: 282 mergers with component masses | 161 of 282 equal within one combined error, the pile-up of the convention that the primary is the heavier; of the 10 events with the primary to 10 per cent, mass ratios run 0.84-0.96, and GW250114_082203 alone reaches one within an error below 0.05 (0.96 +- 0.05) (`gwtc_equal_masses`) |
| Przybylski's star re-measured | ESO archive: the six highest-S/N HARPS and four highest-S/N UVES spectra of HD 101065; NIST ASD | the promethium line set sits deeper than 2000 random line sets of the same size (p 0.002 HARPS, 0.004 UVES) and the actinides and technetium at chance (p 0.05-0.7); the depth at the promethium positions rests on lines of Nd II (4297.80), Fe II (4157.92), Th II (4381.86), Y II and Cr II that this star's rare-earth forest carries, and without them the four and two lines left sit at p 0.05 and 0.08 (`przybylski_actinides`) |
| The random transiter in TESS | TESS QLP light curve of HD 139139, sector 91: 7556 cadences over 24.7 d at 607 ppm a cadence | 0 dips against 8.0 at K2's rate (Poisson 3e-4), with 3-sigma depths of 429, 248 and 162 ppm for 1, 3 and 7 h dips, which reach the deeper half of K2's 200-1600 ppm; whatever crossed the star in 2017 did not in 2025 (`hd139139_tess`) |
| Microlensing of the neighbours | Gaia DR3 vari_microlensing (363 events), gaia_source and vari_classifier_result; SIMBAD | 14 events on sources with parallax above 1 mas at 3 sigma: 11 with a doubtful parallax (RUWE above 1.4, or under 5 sigma at G above 19 in the bulge fields), 1 a young star brightening, and 2 clean events on stars at 0.8-1 kpc (Gaia DR3 2214532279378994816, 1819571454860230400) whose blended fits leave the lens anywhere in front of the source at any small mass (`gaia_microlensing_near`) |
| TeV light at the nearest stars | 1LHAASO catalogue: 42 point-like sources without an association; Gaia Catalogue of Nearby Stars within 20 pc | 0 stars inside an unassociated source's error circle against 0-2 (mean 0.4) with the sources moved 2 deg, and 0 inside an associated one (`lhaaso_nearest_stars`) |
| Unbound stars from nowhere | Li et al. (2023): 52 hypervelocity candidates with Gaia astrometry, traced straight back for 300 Myr | 17 in or from the disc, 14 more likely bound than not in the catalogue's own potential, 14 with velocity errors above 150 km/s, and 7 at 490-590 km/s and 2-4 kpc above the plane whose straight paths pass 4-9 kpc from the Centre and 50 kpc from the Cloud, left for orbits in a Galactic potential (`hvs_origins`) |
| Stars that passed within a parsec of the Sun | Bailer-Jones (2022): 61 Gaia EDR3 stars with a median perihelion below 1 pc, 32 past and 29 to come; eRASS1, VLASS, GALEX and AllWISE by CDS XMatch; SIMBAD; Breakthrough Listen open data | 8 with eRASS1 sources, 8 with GALEX, 10 with W1-W3 above 0.3 and 0 with VLASS, against 0-1 of each with the stars moved: the coronae, chromospheres and photospheres of K and M dwarfs; Breakthrough Listen has observed 2 of the 61, HD 168442 and Ross 248, and the other 59 are listed for it (`close_encounter_stars`) |
| The solar siblings | SIMBAD; eRASS1, VLASS, GALEX and AllWISE by CDS XMatch; Breakthrough Listen open data | HD 162826 (F8 V, 33 pc) carries a photospheric W1-W3 and nothing else; HD 186302 (G3 V, 57 pc) a chromospheric GALEX NUV and a photospheric W1-W3; neither has a VLASS or eRASS1 source, and Breakthrough Listen has observed neither (`solar_siblings`) |
| Galaxies that suppress supernovae | HECATE: 1770 galaxies within 20 Mpc with star-formation rates; Asiago supernova catalogue, 644 supernovae of 1980-2015 matched to them by CDS XMatch | 2 galaxies short of their supernovae at p below 0.01, both luminous infrared galaxies with active nuclei whose dust hides their supernovae and whose nuclei inflate their rates: Messier 77 (6.4 expected, 0 seen) and NGC 7552 (4.8 expected, 0 seen) (`supernova_deficits`) |
| The 2004 SETI@home candidate SHGb02+14a | Breakthrough Listen open data: the GBT L-band cadence on GJ 83.1 (TZ Arietis) of 2016-06-18, the hydrogen coarse channel of its 3 ON and 9 other scans of the session, dedrifted over -40 to +40 Hz/s; the 2016-09 and 2017 cadences are S band and do not hold the line | 101 peaks on the ON scans and 45 off, 3 of them on TZ Arietis alone: 10-12 sigma at 1420.0173 MHz drifting -2.0 to -2.25 Hz/s on the first scan, beside the 1420.017 MHz line every pointing of the session shows at zero drift; nothing in the candidate's 8-37 Hz/s (`shgb02_14a`) |
| Bursts peaking at the electron's mass | Fermi GBM burst catalogue (HEASARC): 1437 bursts with a Band peak energy to 10 per cent, 1696 with a Comptonised one | 9 within 2 per cent of 511 keV against 8.1 from the smooth run of peak energies either side (p 0.42), and 12 against 12.6 for the Comptonised fits (`gbm_bursts_511kev`) |
| Gamma-ray bursts repeating at one position | Swift GRB catalogue (HEASARC): 711 bursts with XRT positions | 0 pairs within their position errors plus 5 arcsec against 0.0001 by chance (`swift_repeating_bursts`) |
| Twelve-micron light at cold brown dwarfs | Kirkpatrick et al. (2021): 133 T and Y dwarfs with Spitzer astrometry carried to 2010.5; AllWISE by CDS XMatch | 33 carry a W3 at S/N 3 within 5 arcsec against 1.4 with the dwarfs moved 2 arcmin, and against 27.5 from the share of field sources of the dwarfs' own W1 and W2 that the catalogue gives such a W3 (90 of 436, p 0.14): the catalogue measures W3 at every source it holds at W1 and W2, and one in five of the faint red ones comes out at S/N 3 (`allwise_w3_cold_brown_dwarfs`) |
| The Sun's co-movers against the Sun | the store's five stars within 1 km/s of the Sun; Gaia DR3 astrophysical parameters; SIMBAD | the two warm enough to compare, BD+68 1331 and CD-75 143, are 0.34 and 0.24 dex metal-poor and 1-2 Gyr younger than the Sun, so no sibling; the other three are cool dwarfs Gaia cannot place in metallicity; the co-motion stays a chance alignment, the lowest p of a store of several hundred tests being its expected extreme (`sun_comovers_composition`) |
| H-alpha emission at quiet Sun-like neighbours | Gaia DR3 ESP-ELS: 4 emission-line stars within 100 pc at BP-RP 0.5-1.5; eRASS1 by CDS XMatch; SIMBAD | AE Aquarii (a cataclysmic variable), CPD-68 1894 (a T Tauri star with an X-ray source), a binary at RUWE 56, and Gaia DR3 394161419479425152, 3.6 mag under the main sequence of its colour, a white dwarf's light on a red dwarf's (`gaia_halpha_quiet_dwarfs`) |
| Rhythm in the repeaters | CHIME/FRB Catalog 1 as tabulated by Hashimoto et al. (2022; J/MNRAS/511/1961): the 2 repeaters with five or more bursts, FRB 20180814A (10 bursts over 315 d) and FRB 20180916B (19 over 262 d); the table lists a burst's sub-bursts as rows of their own at one arrival time, counted once | a clock, whose intervals are integer multiples of one period, which magnetars are not: the share of intervals from the first burst on the best tick over 4000 periods from 10 min to 100 d, the multiples of half a sidereal day left out since a transit telescope sees a source at those alone; FRB 20180814A 44 per cent on 2.79 d against 41 from burst sets drawn on random days at the real bursts' sidereal phases (p 0.60), FRB 20180916B 44 per cent on 0.514 d against 31 (p 0.065), whose 16.35 d activity cycle (CHIME/FRB Collaboration 2020) spreads its bursts over a five-day window rather than placing them on a tick (`chime_repeater_rhythm`) |
| The triangular points of nearby binaries | Sixth Catalog of Orbits of Visual Binary Stars: 2686 orbits of grade 4 or better, each solved for 2016.0; Gaia DR3 by CDS XMatch and gaia_source cones | L4 and L5 of a stellar pair are unstable at any stellar mass ratio, so nothing natural stays there: 6 orbits within 100 pc hold their secondary where the orbit puts it at a separation of 1-20 arcsec (STF 1457, STF 1639 AB, BU 823 AB, I 658, STF 2596 and HU 1626, at 1.0-2.0 arcsec with periods of 156-2971 yr; the catalogue's wider grade-4 orbits lie beyond 100 pc); Gaia sources at L4 or L5 of the six: 0 against 0.00 at ten other angles of the same orbits, where at 1-2 arcsec from a bright primary Gaia's completeness for a faint neighbour, not the sky, sets the limit (`binary_triangular_points`) |
| Impulses on 3I/ATLAS's orbit | Minor Planet Center astrometry of 3I/ATLAS (C/2025 N1): 8431 positions from 345 sites, 2025 May 8 to 2026 April 14, 70 of them after the Jupiter passage of 2026 March 16; ASSIST with DE440 and sb441-n16 from JPL's solution; SOHO/SWAN's water production (Combi et al. 2026) and the nucleus masses of Thoss et al. (2026) | a velocity change that outgassing cannot give: on one set of 7633 positions gravity alone leaves chi-square 36362 and three outgassing accelerations scaling as r^-2 11983 (the normal term -6.97 +- 0.07e-9 au/d^2 against JPL's -6.85e-9), outgassing that changes at perihelion 468 less and seven month-long bins of outgassing 836 less, as a water production that peaked a week after perihelion and fell tenfold in 40 days requires; an impulse in the 20 days behind the Sun reads 1.2 m/s at Mars or at perihelion on constant outgassing (chi-square 453 and 407 less) and +0.5 +- 4.7 m/s radial on the binned outgassing (11 less, 3 sigma below 15 m/s), -4.6 +- 1.7 m/s over 100 resampled sets of the 270 observing nights and -4.3 to -4.5 +- 4-5 m/s with any one of the 30 busiest sites left out, where water alone supplies 0.5-2 m/s to a nucleus of 1e12 kg or more and the 1.6e11 kg of the CO2-only estimate allows 20 m/s; an impulse at the Jupiter passage reads -115 +- 71 m/s radial on constant outgassing and -50 +- 78 on the bins, -133 +- 255 over resampled nights, -185 +- 360 without R59, which holds most of the positions after it, and -520 +- 417 without R59 and C23, so those 70 positions see nothing under a few hundred m/s; an impulse every five days at 53 times from 2025 June 29 to 2026 March 16 on the binned outgassing worsens no fit and bounds the velocity change below 2.2-18.6 m/s (3 sigma) through 2026 February 14 and 21-220 m/s after, the largest gains in chi-square 42 on 2025 November 16 (-4.2 +- 1.4 m/s radial, +1.6 +- 0.7 transverse), 39 on 2026 January 5 (+0.6 +- 0.6 radial, +0.7 +- 0.2 transverse) and 31-32 in early December, changes the month-long bins cannot follow and the bursts of activity after perihelion give; Breakthrough Listen's 1-12 GHz observation of 2025 December 18 holds no transmitter above about 0.1 W (Jacobson-Bell et al. 2026) (`iso3i_impulses`) |
| Stars Gaia DR3 sees that DR2 did not | Gaia DR3: 190,985 sources within 100 pc at G below 17 with RUWE below 1.4, read in 192 source_id ranges; gaiadr3.dr2_neighbourhood; DR2 within 10 arcsec of each candidate | a star that began shining between the releases' data spans: 110 have no DR2 neighbourhood row, 6 of them in DR2 after all (2 within 5 arcsec and a magnitude, 4 with two-parameter or duplicated DR3 solutions), 10 with a second DR3 source within 2 arcsec, 90 lying 2-7 arcsec from a DR2 star 1-11 mag brighter, inside whose image DR2 catalogued no second source, and 4 moving at 585-4812 mas/yr, Lalande 21185 among them, which DR2 holds nowhere within 30 arcsec at any magnitude, the fastest movers its cross-match lost; none left (`gaia_dr3_appeared`) |
| Stars Gaia DR2 saw that DR3 cannot find | Gaia DR2: 241,075 sources within 100 pc at G below 17, read in 192 source_id ranges; gaiadr3.dr2_neighbourhood; DR3 within 10 arcsec of each candidate; SIMBAD | a star that stopped shining between the releases' data spans: 2 have no DR3 neighbourhood row, both companions of bright stars that DR3 holds as one source with the primary: iota Leo B (G 6.8, F5 V), 2.1 arcsec from the DR3 source of the F1 IV spectroscopic binary iota Leo, 2.9 mag brighter, and chi Eri B (G 9.7), 2.5 arcsec from the DR3 source of the G8 giant chi Eri, 6.2 mag brighter, its DR2 solution carrying an excess-noise significance of 163; none left (`gaia_dr2_vanished`) |
| Comets on Earth's years | JPL Small-Body Database: 1030 periodic comets with periods below 200 years, periods within 0.002 y of a whole number of years against the same window at half-years and against uniform fractional periods, each read for its condition code, arc and period uncertainty | 6 at whole years against 4.1 expected and 4 at half-years (Poisson p 0.23); 2 are lost comets with rounded periods and no uncertainty, the other 4 within chance |
| Orbits tangent to Earth's | JPL Small-Body Database: 2645 asteroids and comets with perihelia and 128 with aphelia within 0.01 au of 1 au, those within 0.0005 au of 1.0000 au against the band's density and the windows at 0.995 and 1.005 au, each read for its condition code, arc and uncertainty | perihelia 111 against 132 expected (p 0.97, the control windows 276), aphelia 4 against 6.4 (p 0.88, the controls 14); no excess at Earth's distance |
| Planets on perfect circles | NASA Exoplanet Archive composite table: 1014 planets with periods beyond 30 d and a measured eccentricity (635 more fixed or limits), those whose upper eccentricity lies below 0.002 | none; the lowest percentile of upper eccentricities sits at 0.018 |
| Asteroid spins on the clock | LCDB frequency-diameter table: 4172 secure rotation periods (U 3) quoted to three decimals between 2 and 48 h, those within 0.02 per cent of a whole number of hours against the half-hour windows and uniform fractions, the day's harmonics counted apart | 11 at whole hours against 12.8 expected and 12 at half-hours (Poisson p 0.73), 1 of them at a harmonic of the day |
| Planets on whole days | NASA Exoplanet Archive composite table: 1494 planets with periods of 1.5-400 d known to better than 0.00002 d, those within 0.00002 d of a whole number of days against the half-day windows and uniform fractions | none, against 0.06 expected; none at half-days |
| Light at 12 um alone | Gaia Catalogue of Nearby Stars with its WISE photometry: 3510 stars within 100 pc at BP-RP 0.5-2.5 with W1 8-14 and W1, W3 and W4 measured to 0.05, 0.1 and 0.2 mag, W1-W3 more than five widths and five errors above the single-star locus at their colour with W1-W4 within two widths of its own, against the stars as far below; each read in AllWISE for flags and faint W3, in Gaia for a second source in the W3 beam and for a W4 excess at three errors | 27 above against 2 below; 6 carry AllWISE flags, 3 have a W4 excess at three errors (dust), and 18 K and M dwarfs with W3 of 7.6-8.8 mag and a 12 um excess of 0.3-0.5 mag remain unexplained, their W4 excess of 0.1-0.5 mag at one to three errors too coarse to separate warm dust from a narrow emitter |
| Symmetric flares | Yang et al. (2023) TESS flare catalogue: 24232 of 60810 flares lasting 40 minutes or more, those whose rise from start to peak takes as long as the decay within 10 per cent of the duration, or longer, read by duration and by the star's flare count | 1034 symmetric and 4482 rising longer than decaying, a share that holds at every duration and on quiet and busy stars alike, so the catalogue's event boundaries set the shapes and no single flare's shape can be read from it |
| Pulsars ticking in whole hertz | ATNF pulsar catalogue: 2118 of 2527 pulsars with periods quoted to eight digits or more, spin frequencies within 0.00001 Hz of a whole hertz or periods within 0.00001 ms of a whole millisecond, against the half-integer windows and uniform fractions; periods rounded to fewer digits counted apart | none against 0.085 expected, none at half-integers; 54 periods quoted to two to four digits land on the millisecond grid by rounding alone |
| Pulsars on the hydrogen line's decimals | ATNF pulsar catalogue: 2118 pulsars with periods quoted to eight digits or more, spin frequencies within one part in 100,000 of 1420.405751 Hz scaled by a power of ten, against the windows shifted by half a decade and uniform logarithmic fractions | none against 0.018 expected, none at the half-decade shift |
| Stars that stepped a magnitude between Gaia releases | Gaia DR3 sources within 100 pc whose DR2 counterpart within 0.1 arcsec (gaiadr3.dr2_neighbourhood) carries a mean G differing by more than a magnitude, each read for its transit counts, variability flags, SIMBAD type, DR2 saturation above G 4 and the missing colour of a source in a bright neighbour's light | 40: 13 are the brightest stars, whose DR2 photometry is saturated, 23 are companions of bright stars whose DR2 window took in the primary's light, 2 are variables and 1 a blend; HD 207964 C, a companion with a colour and RUWE 1.39, remains unexplained |
| Lurkers at Earth's Lagrange points | JPL Small-Body Database: 165 asteroids within 0.01 au of Earth's semi-major axis with e below 0.3 and i below 30 deg, placed by their mean longitude at epoch relative to Earth's; the count within 20 deg of L4 and of L5 against the ring's other longitudes, each read for its arc and condition code | 9 at L4 and 8 at L5 against 18.3 expected per point from a uniform ring, whose longitudes in fact crowd within 30 deg of Earth (123 of 165) because such orbits are found when near Earth; 11 of the 17 rest on arcs of days |
| Watchers of Jupiter's transits | Gaia Catalogue of Nearby Stars: 292 stars within 100 pc and 0.051 deg of Jupiter's orbital plane, the band from which Jupiter is seen to cross the Sun, carried to 2007.0 and matched to GALEX GUVcat AIS within 5 arcsec, against the share of the 22303 stars 1-5 deg from the plane and the band moved 2 arcmin in eight directions; matches read in SIMBAD | 59 with an ultraviolet source against 57.6 from the share beside the zone (p 0.45), the moved bands holding 0-8; the zone's ultraviolet share is the sky's |
| Light at 2 um alone | Gaia Catalogue of Nearby Stars with its 2MASS and WISE photometry: 128161 stars within 100 pc at BP-RP 0.5-3.0 with J, Ks and W1 measured to 0.03, 0.03 and 0.05 mag, J-Ks more than five widths and five errors above the single-star locus at their colour with J-W1 within two widths of its own, against the stars as far below; each read in 2MASS for its quality, read and extended-source flags and in SIMBAD | 3 above against 9 below; 2 carry 2MASS quality below AAA and the third, an M dwarf with J-Ks 0.36 mag above the locus and J-W1 on it, lies within the chance rate of the mirror |
| Planets in step with their star's spin | NASA Exoplanet Archive composite table: 178 planets whose host carries a rotation period and whose orbital period is 1.5-20.5 times it, those at a whole multiple within 0.5 per cent against the half-integer windows and uniform fractions, each read for the source of the rotation period | 12 at whole multiples against 10.1 expected and 13 at half-integers (Poisson p 0.32) |
| Nearby light bluer than any star | Gaia Catalogue of Nearby Stars: sources within 100 pc with BP-RP below -0.65, bluer than the Rayleigh-Jeans tail of any photosphere gives in Gaia's bands, each read for its BP/RP flux excess, image-peak and RUWE flags, white-dwarf probability and SIMBAD type | 1, a G 17 source with a BP/RP flux excess of 26 over the single-star relation, a blend or a corrupted BP and no bluer star |
| Comets pushed toward the Sun | JPL Small-Body Database: 32 comets and 3 asteroids whose radial non-gravitational term A1 is negative, those negative at three sigma, each read for its arc and condition code, its transverse term A2 and the asymmetric outgassing parameter DT | 27 at three sigma: 1 on a short arc, 6 with a larger transverse term or a shifted outgassing law; 20 comets and the asteroid 4179 Toutatis keep a radial term toward the Sun of 2e-10 to 6e-7 au per day squared on arcs of 3-75 years, which the symmetric outgassing law returns for a nucleus venting mostly after perihelion, and they await refits with an asymmetric law |
| Galaxies warm without star formation | HECATE: 669 galaxies within 150 Mpc with GSWLC stellar masses and ultraviolet-optical star-formation rates and with WISE 22 um and IRAS far-infrared luminosities, the 38 quiescent ones (specific rate below 1e-11 per year) radiating more than a tenth of a solar luminosity per solar mass at 22 um within a factor of three of their far-infrared, against the quiescent population's own distribution; each read for HECATE's nuclear-activity flags and its inclination | 6, every one with an active nucleus; the quiescent galaxies' 22 um heat per mass runs 0.035 solar at the median and 0.55 at the 99th percentile |
| Stars that dimmed since Hipparcos | Hipparcos new reduction and Gaia DR3: 17285 Hipparcos stars within 100 pc with a Gaia best neighbour, G against Hp through the sample's running median of G - Hp in BP-RP, those fainter by 0.5 mag and those brighter by as much, each read for Hipparcos's scatter and variability, Gaia's variability flag and RUWE, SIMBAD's type, a pair's name or component letter and a Gaia neighbour within 10 arcsec | 297 fainter against 4 brighter: 274 are pairs whose joint light Hipparcos measured and Gaia resolves, most by 0.75 mag, 23 are variables and 4 rest on Hipparcos records without a scatter; none unexplained |
| Asteroids on polar orbits | JPL Small-Body Database: 51 bound orbits of asteroids and comets within 3 deg of 90 deg inclination, those within 0.5 deg of polar against a flat inclination density and the bands either side, each read for its arc and condition code | 9 against 8.5 expected (Poisson p 0.48): 8 long-period and Halley-type comets and one trans-Neptunian object |
| Stars enriched evenly in every heavy element | GALAH DR4: 46868 stars with clean measurements of all eleven neutron-capture elements Sr, Y, Zr, Mo, Ru, Ba, La, Ce, Nd, Sm and Eu, those with every [X/Fe] above +0.4 dex and a spread below 0.1 dex across the eleven, against the stars depleted as evenly and the sample's own spread | none of the 41 stars enriched above +0.4 dex carries a flat pattern, and none is depleted evenly; the sample's spread across the elements runs 0.12 dex at the median against errors of 0.09 |
| Transits longer than the star allows | NASA Exoplanet Archive composite table: 4328 transiting planets with a duration, period, semi-major axis and radii, those whose duration exceeds by a quarter the longest central transit a circular orbit allows at the catalogued geometry, each read for its duration error, the sources of its duration and stellar radius and its eccentricity | 188: 167 carry a stellar radius of the Kepler Input Catalogue era or a duration and a radius from different solutions, 8 have loose or missing duration errors, 7 are eccentric, 4 have eccentricities fixed without errors and WASP-132 b's duration stands off by itself; TOI-1295 b, at 1.38 times the maximum with e 0.02 in one solution, remains unexplained |
| Gamma rays peaked like a line | Fermi-LAT 4FGL (HEASARC): 2766 sources above 10 sigma with a log-parabola curvature, those with beta above 0.8 at a curvature significance above 4, a spectrum peaked within a factor of a few in energy, against the catalogue's curvatures (median 0.10, 99th percentile 0.64); each read for its class and analysis flags | 3, all of known classes: the pulsars J1827-1446 and J1057-5851 and the globular cluster Terzan 1, whose cutoff spectra the log parabola bends to fit |
| Nearby stars flickering by the minute | Gaia DR3 short-timescale variables within 100 pc: 909 stars, those whose characteristic frequency exceeds 48 cycles a day (the catalogue reaches 72), each read for its white-dwarf locus, its SIMBAD type, its image and RUWE flags and its colour, since a red dwarf the pipeline picks up flares and its variogram timescale is the flares' rise | 220: 35 white dwarfs and compact stars, 67 of other known types, 108 flaring red dwarfs; 10 remain, five G and K dwarfs and three A stars with 20-30 minute timescales and amplitudes of 0.01-0.09 mag |
| Infrared dimming next door | Gaia Catalogue of Nearby Stars within 20 pc with AllWISE W1 8-15: 1004 stars matched to AllWISE at 2010.5 and CatWISE2020 at 2015.0 within 3 arcsec, those whose profile W1 differs by more than 0.3 mag between the two means, against the stars that brightened as much; each read for Gaia's variability flag, RUWE and image flags, SIMBAD's type, the WISE flags, CatWISE's saturation brighter than 8.5 mag, the match separation and the proper motion, since a star moving a second a year is split between the epochs of CatWISE's coadds | 92 fainter in CatWISE against 2 brighter: 14 variables, 29 blends, 29 saturated or flagged, 16 matched to another source or split by their motion; 6 M6-L3 dwarfs moving 0.4-0.9 arcsec a year, fainter by 0.5-0.9 mag, remain unexplained and carry the fast movers' signature |
| Systems turned face-on to us | NASA Exoplanet Archive composite table: 302 non-transiting planets with a measured inclination, those within 5 deg of face-on from either pole against the 0.4 per cent of random orientations, each read for its inclination error and method | 1 against 1.15 expected (binomial p 0.68): HD 204313 e, an astrometric orbit at 4 deg from the pole |
| Masers at rest in the universe's frame | Pestalozzi et al. (2005) 6.7 GHz methanol masers: 519 peak velocities taken from the kinematic local standard of rest to the Sun and to the cosmic microwave background's frame, those within 2 km/s of rest there against the velocities' own density within 30 km/s of rest | 8 against 7.7 expected (Poisson p 0.50) |
| Waste heat in HI-dark galaxies | Leisman et al. (2017) ALFALFA HI sources with low-surface-brightness counterparts: 115 positions matched to AllWISE within 10 arcsec, a source at 5 sigma in W3 or W4 against the positions moved 2 arcmin in eight directions scaled by the warm share of the matches, each read for an AGN colour and a Gaia star | 1 against 0.5 expected (p 0.37), AGC 188768 with an AGN's W1-W2 colour |
| Missing bolometric flux, dwarfs | JMMC Measured Stellar Diameters Catalogue: 62 dwarfs within 100 pc with a limb-darkened diameter, a Gaia parallax, a GSP-Phot temperature and a FLAME luminosity, the luminosity each surface and temperature give against Gaia's, a deficit of 20 per cent at 3 sigma against the mirror excess | none short and none over; the ratio of Gaia's luminosity to the predicted runs 1.05 at the median with a scatter of 0.12 |
| Circles between the giant planets | JPL Small-Body Database: 169 bodies with semi-major axes of 5.5-30 au, perihelia beyond Jupiter and eccentricities below 0.3, those circular to 0.02 against the region's own eccentricities (median 0.19, 5th percentile 0.04), each read for its arc, condition code and a resonance with a planet | 3 Centaurs with e of 0.009-0.010, each on an arc of 2-29 days with condition code 9, where the eccentricity is unmeasured |
| Cerium without carbon in dwarfs | APOGEE DR17 unevolved metal-rich dwarfs of the CNO sample with unflagged carbon and cerium (25), those with [Ce/Fe] above +0.5 dex and [C/Fe] at or below zero, each read for a Gaia binary, its Teff edge and its rotation | 1 of 1 cerium-rich dwarf, 2M08332894+2247535 at [Ce/Fe] +0.77 and [C/Fe] -0.13, is a Gaia binary with RUWE 3.6 |
| Refuges at white dwarfs | NASA Exoplanet Archive composite table: the 6 planets at white dwarfs, each placed against the 1 au its host's giant phase reached, with its discovery method and the published account of its arrival | 3 sit inside the giant's reach: two 20-Jupiter-mass companions on 3- and 6-hour orbits drawn in through a common envelope, and WD 1856+534 b on a 1.4-day orbit, which its discovery paper brings in through its outer pair of stars; the other three orbit at 8-19000 au |
| Variables Gaia could not classify next door | Gaia DR3 vari_summary within 50 pc: 50 variables with a G range above 0.3 mag, the 23 the DR3 classifier left without a class, each read in SIMBAD, for its RUWE and image flags, for the white-dwarf locus and for the flare stars' colour | 23 unclassified: 1 compact star, 7 of known types, 5 blends and 10 red dwarfs whose range is one flaring transit; none unexplained |
| Asteroids in the ecliptic to the hundredth of a degree | JPL Small-Body Database: 107677 bound orbits within 2 deg of the ecliptic, those within 0.02 deg against the band's own density at 0.02-0.2 deg and a density rising as the inclination, each read for its arc and condition code | 12 against 10.8 expected (Poisson p 0.40): 11 main-belt asteroids on decade-long arcs and one near-Earth object on a one-day arc |
| White dwarfs varying outside the pulsation strips | Gaia DR3 vari_summary within 100 pc on the white-dwarf locus, matched to Gentile Fusillo et al. (2021): 132 catalogued white dwarfs flagged variable with a G range above 0.1 mag, those outside the pulsation strips with their margins (DA 10,000-13,500 K, DB 21,000-31,000 K, GW Vir above 70,000 K), each read in SIMBAD, including the magnetic types, for a companion's BP/RP flux excess and for RUWE | 103 sit in a strip or are cataclysmic, eclipsing, magnetic or otherwise known, 5 carry a companion's signature; 24 DA and DC white dwarfs of 3900-10000 K at G 16-19 with ranges of 0.1-0.4 mag over 20-60 transits remain unexplained, a residue for a period search in survey photometry |
| Binaries on perfect circles | Ninth Catalogue of Spectroscopic Binary Orbits: 1725 orbits with periods beyond 100 d and a measured eccentricity (fixed or errorless ones set aside), those with an upper eccentricity below 0.002, against the measured eccentricities themselves | none; the lowest percentile of upper eccentricities sits at 0.019 |
| Copy eclipsing binaries | Kepler eclipsing binary catalogue (Prsa et al. 2011): 1780 systems, pairs whose periods agree within the catalogue's quantum of 0.00001 d, against the periods' own density in a window ten times wider and the pairs within 2 arcmin; copies must also agree in temperature ratio and summed radii to 10 per cent | 24 pairs share a period to the catalogue's quantum, 1 of them one signal in two apertures and 23 apart on the sky against 14 expected (Poisson p 0.018); none of the 23 agrees in temperature ratio and radii, so none is a copy |
| Slow pulsars older than the universe | ATNF pulsar catalogue: 1803 pulsars slower than 0.1 s with a period derivative, those whose intrinsic derivative gives a characteristic age beyond 15 Gyr, each read for the derivative's error and its binary | none |
| Stars leaving the nearest clusters too fast | Hunt and Reffert (2023) open-cluster members with Gaia radial velocities: 1076 members of the 18 clusters within 200 pc whose twenty or more velocities cohere to a median of 3 km/s about the mean, each star's space velocity against its cluster's, those moving faster than 10 km/s, each read for RUWE and SIMBAD binarity, its membership probability and its colour, since Gaia's velocities of hot stars carry errors of tens of km/s | 12: 1 binary, 8 of membership probability below 0.8 and as likely field stars, 1 hot B star; a member of Alessi 84 at 42 km/s with probability 0.82 and HD 74117 in IC 2391 at 10 km/s with probability 0.80 remain unexplained |
| Transits deeper than the planet | NASA Exoplanet Archive composite table: 4455 transiting planets with a depth and a radius ratio, those whose depth exceeds 1.5 times the ratio squared, each read for the depth's error and the sources of depth and ratio | 82: 75 draw depth and ratio from different solutions, 5 carry loose or missing depth errors; TOI-5624 c, whose depth of 0.76 per cent stands ten times its ratio's in one solution, and TOI-4427 b at 1.6 times remain unexplained |
| Gamma rays with fast radio bursts | Fermi GBM burst catalogue against CHIME/FRB Catalog 1: 4398 gamma-ray bursts over 18.3 years and 536 radio bursts inside that span, pairs within 100 s whose positions overlap within the gamma-ray error circle plus a degree, against the pairs the two rates give by chance | 1 pair within 100 s (0.8 expected), FRB 20190217A eleven seconds after GRB 190217188 but 91 deg from its 9 deg error circle; none overlapping in position against 0.004 expected |
| Spinning stars without coronae | Gaia DR3 stars within 20 pc with rotation periods below 5 days (vari_rotation_modulation) in the eROSITA-DE half of the sky, carried to 2020.0 and matched to the eRASS1 main catalogue within 15 arcsec; a fast rotator without X-rays, read for its brightness and in SIMBAD | all 11 rotators carry an eRASS1 source; none is without a corona |
| Neutrinos with gamma-ray bursts | IceCube ten-year point-source events above 10 TeV (372661) against the 2355 Fermi GBM bursts of the same span: a neutrino within 100 s of a burst and inside the two error circles plus a degree, against the pairs the event rate and the circles' sky fraction give by chance | 543 neutrinos fall in the time windows against 542 expected, and 3 inside the circles against 3.1 (Poisson p 0.59), each 5-6 deg from a burst localised to 7-13 deg |
| Warm stars in the Hyades | Hunt and Reffert (2023) Hyades members above probability 0.5: 157 at BP-RP 0.5-2.5 with clean AllWISE W1 and W3, those with W1-W3 more than five widths and five errors above the cluster's own locus, their share against the field's 0.8 per cent from the same test within 100 pc; each read for AllWISE flags and in SIMBAD | 1 of 157 (0.6 per cent against the field's 0.8, binomial p 0.70): HZ 9, a white dwarf with an M-dwarf companion |
| Resonant pairs without timing variations | Holczer et al. (2016) Kepler transit timings and the DR25 KOI table: 46 pairs within 2 per cent of 2:1 or 3:2 among 2106 systems, 88 planets with timing measurements, each planet's timing scatter against the variation its neighbour's mass, estimated from the radius, demands (Lithwick et al. 2012), a quiet planet keeping time below a fifth of that with no detected variation | none of the 88 keeps time below a fifth of the expected variation |
| Light at 3.4 um alone | Gaia Catalogue of Nearby Stars with its 2MASS and WISE photometry: 60000 stars within 100 pc at BP-RP 0.5-2.5 with Ks, W1 and W2 measured to 0.03, 0.05 and 0.05 mag, Ks-W1 more than five widths and five errors above the single-star locus at their colour with Ks-W2 within two widths of its own, against the stars as far below; each read against AllWISE's plain profile W1, its flags, 2MASS's flags and SIMBAD | 299 above against 9 below, and every one is the catalogue's proper-motion-fitted W1 mis-fitting a fast mover: the excess vanishes with AllWISE's plain W1, or the star has moved out of the match, or a flag marks it; none unexplained |
| Dark companions on perfect circles | Gaia DR3 astrometric two-body orbits within 200 pc with periods beyond 200 d and a measured eccentricity: 8874 orbits, those with an upper eccentricity below 0.005, against the solutions' own eccentricities | none; the lowest percentile of upper eccentricities sits at 0.055 |
| Planets lapping their star's spin in whole steps | NASA Exoplanet Archive composite table: 441 planets whose host carries a rotation period 1.5-20.5 times their orbital period, those at a whole ratio within 0.5 per cent against the half-integer windows and uniform fractions, each read for the source of the rotation period | 20 at whole ratios against 26.5 expected and 25 at half-integers (Poisson p 0.92) |
| Radio from cold brown dwarfs | Kirkpatrick et al. (2021) 20 pc census: 133 T and Y dwarfs carried to 2019.0 and matched to the VLASS epoch-1 components within 5 arcsec, against the positions moved 2 arcmin in eight directions | none, against a mean of 0.1 at the moved positions |
| Methane in a star's light | Gaia Catalogue of Nearby Stars: 7 objects at BP-RP 0.5-3.0 fainter than W1 8 with clean W1 and W2 and W1-W2 above +0.8, the colour of a T dwarf's methane band; AllWISE, Gaia DR3 and SIMBAD | 2 saturated in WISE with the colour absent in AllWISE's plain magnitudes, 4 of known types (three T dwarfs and an emission-line star), 1 blended with a neighbour in the beam; none unexplained (`gcns_methane_colour`) |
| Neutrinos from Earth's transit zone | IceCube ten-year point-source events (HEASARC icecubepsc): 372661 above 10 TeV by ecliptic latitude, the count within 0.262 deg of the ecliptic against the twenty strips of that width on either side out to 5.5 deg, which share the zone's declinations | 1543 in the zone against 1542 +- 29 beside it (z +0.03); above 100 TeV 549 against 528 +- 24 (z +0.88, p 0.18); the zone's ten highest-energy events at the chance rate (`icecube_transit_zone`) |
| Gamma-ray bursts from Earth's transit zone | Swift GRB table (HEASARC swiftgrb): 872 bursts at arcminute positions; Fermi GBM bursts with an error radius below 1 deg: 910; the count within 0.262 deg of the ecliptic against the twenty strips of that width on either side out to 5.5 deg | Swift 4 in the zone against 3.9 +- 1.9 beside it, GBM 3 against 3.7 +- 1.8; the seven at the chance rate (`grb_transit_zone`) |
| Pulsars in Earth's transit zone | ATNF pulsar catalogue (VizieR B/psr): 2530 pulsars with positions, the count within 0.262 deg of the ecliptic against the twenty strips of that width on either side out to 5.5 deg, which the Galactic plane crosses as it crosses the zone | 8 in the zone against 13.3 +- 12.0 beside it, 2 millisecond pulsars against 3.9 +- 10.3; the eight at the chance rate (`atnf_transit_zone`) |
| Asteroids pushed harder than sunlight allows | JPL Small-Body Database: 611 asteroids with a transverse non-gravitational term, those at 3 sigma whose lower bound exceeds twice Bennu's term scaled to their diameter, the ceiling re-radiated sunlight sets | 9: the eight published dark comets 2012 UR158, 2016 TA56, 2003 RM, 2005 UY6, 2001 ME1, 1998 SH2, 1998 FR11 and 2006 RH120, and the active asteroid 2008 GO98; none unexplained (`sbdb_pushed_asteroids`) |
| Emission lines in asteroid reflectance | Gaia DR3 sso_reflectance_spectrum: 60518 asteroids with sixteen-band reflectance spectra, 20569 carrying an unflagged interior band above 1.5; interior bands more than 0.3 and five combined errors above the mean of their neighbours | 5 spikes, every one on a flagged band or beside one (19336, 8854, 6107, 17091, 150784); none unexplained (`gaia_sso_reflectance_spikes`) |
| Lines in transmission spectra | NASA Exoplanet Archive transmission-spectroscopy table (transitspec): 53 published spectra of five or more bins, 3618 bins; a bin four combined errors, four times the spectrum's bin-to-bin scatter and 2 per cent of the depth from the mean of its neighbours, in either sign | none; at three sigma KELT-9 b's H-beta line and four single bins of JWST series within 3.8 sigma (`exoplanet_transmission_lines`) |
| Open clusters orbiting backwards | Hunt and Reffert (2023) clusters (VizieR J/A+A/673/A114): 3170 with a parallax at 10 sigma and a radial velocity from three or more members to 10 km/s, Galactic rotation and vertical speeds from their mean motions | 20 retrograde, every one a globular cluster; 7 with vertical speeds above 150 km/s, six globular clusters and Pismis 26, which is the globular cluster Tonantzintla 2; none unexplained (`clusters_retrograde`) |
| Pulsars faster than a kick can throw | ATNF pulsar catalogue (VizieR B/psr): 257 pulsars with a proper motion and a distance, transverse speeds at the proper motion's 3 sigma lower bound | one above 2000 km/s, J2013+3845 at 2183 km/s on a 13 kpc dispersion-measure distance; none unexplained (`atnf_kick_speeds`) |
| Asteroids blacker than any surface | JPL Small-Body Database: 352 asteroids listed with a geometric albedo below 0.02, 15 of them with an AKARI albedo and error (J/PASJ/63/1117) | none below 0.02 at AKARI's 3 sigma upper bound; the database values rest on a diameter and an absolute magnitude fitted together (`sbdb_blackest_asteroids`) |
| Two neutrinos from one spot | IceCube ten-year point-source events (HEASARC icecubepsc): 192107 above 100 TeV, pairs within one hour and within the sum of their errors plus half a degree, against the same events with their times shuffled twenty times | 382 doublets against 362 +- 18 shuffled (Poisson p 0.16); at the chance rate (`icecube_doublets`) |
| Hyperbolic excess beyond planetary perturbation | JPL Small-Body Database: 5 asteroids and 520 comets with eccentricity above 1, the speed at infinity from the eccentricity's 3 sigma lower bound and the perihelion distance, above the 3.9 km/s that C/1980 E1's Jupiter encounter gave it | the three published interstellar objects alone, 3I/ATLAS at 58 km/s, 2I/Borisov at 32 and 1I/'Oumuamua at 26; of the eleven comets between 1.5 and 3.9 km/s, two carry recorded encounters (C/1980 E1 with Jupiter, C/2024 L5 with Saturn), the rest are fragments or rest on short arcs (`sbdb_hyperbolic_excess`) |
| Copy gamma-ray bursts | Fermi GBM burst catalogue (HEASARC fermigbrst): 3779 bursts with T90, T50, fluence and a Band peak energy; pairs more than 10 deg apart alike to 2 per cent in T90 and fluence and 5 per cent in T50 and peak energy, against the pairs found with T90 rescaled by six factors | 3 pairs against 3.0 rescaled; at the chance rate (`gbm_copy_bursts`) |
| Gamma-ray bursts arriving together from different directions | Fermi GBM burst catalogue (HEASARC fermigbrst): 4398 bursts over 18.3 years, pairs triggered within 10 s from directions farther apart than their error radii and 5 deg | none, against 0.34 for Poisson arrivals; no two bursts within 10 s at all (`gbm_bursts_together`) |
| Copy comets | JPL Small-Body Database: 4080 comets with orbital elements, pairs agreeing under the Southworth-Hawkins criterion to 0.05, read against shared parent designations, the sungrazing families inside 0.1 au, the published comet pairs and families, and the arcs | 62969 pairs: 2770 fragments of one comet, 60198 in the sungrazing families or the published pairs and families (Levy and Shoemaker-Holt, the Liller family, the 1844 great comet and C/2019 Y4, C/2002 A1 and A2, C/2002 Q2 and Q3, 169P and P/2003 T12, de Vico-Hind and Kohoutek, 332P and 412P), 1 resting on an arc under 30 d; none unexplained (`sbdb_copy_comets`) |
| Stars that jumped between 2MASS and Gaia | Gaia DR3 stars within 25 pc with a 2MASS counterpart: 4915, the Gaia position carried to the 2MASS night with the proper motion and that night's parallactic shift, against the 2MASS position | offsets of 0.10 arcsec median and 0.90 at the 99th percentile; 32 above 1 arcsec, 29 saturated, poor or flagged in 2MASS or Gaia and 3 blended with a second Gaia source in the 2MASS beam; none unexplained (`gaia_2mass_jumped`) |
| Lurkers at Jupiter's far Lagrange point | JPL Small-Body Database: 16412 bodies within 0.35 au of Jupiter's semi-major axis with e below 0.3, their mean longitudes at the element epoch against Jupiter's, the count within 20 deg of the L3 point opposite the planet | 4 at L3 against 9414 and 5374 in the L4 and L5 swarms: 2 on arcs of days, 2 Trojans librating widely (2015 OL106 at 162 deg and 2020 BZ43 at 199 deg); none unexplained (`sbdb_jupiter_l3`) |
| Waste heat at room temperature | Gaia Catalogue of Nearby Stars: 16037 stars at BP-RP 0.5-2.5 with clean Ks, W3 and W4, 175 with excess at both 12 and 22 um and 30 of them unflagged in AllWISE with a colour temperature from the excess flux ratio | 3 between 280 and 320 K against 1.5 in the bins beside (Poisson p 0.19); the excesses run from 100 to 320 K with none hotter; at the chance rate (`gcns_room_temperature_excess`) |
| Warm stars in Jupiter's transit zone | Gaia Catalogue of Nearby Stars with its WISE photometry: 175 stars with W1 and W3 or W4 within 0.051 deg of Jupiter's orbital plane, the band that sees Jupiter transit the Sun, against the 13736 stars 1-5 deg from the plane; SIMBAD | 3 warm (HD 13997, HD 112250 and a G 14.9 star with W3 and W4 excess) against 2.36 expected from the band's share (p 0.42); with the ultraviolet count of the zone's stars this closes the Jupiter-zone programme (`jupiter_zone_warm_stars`) |
| Two pulsars at one spot | ATNF pulsar catalogue (VizieR B/psr): 2358 pulsars outside globular clusters and the Magellanic Clouds, pairs within 2 arcmin, against the pairs the mirrored declinations give | 7 pairs against 7 mirrored: the double pulsar J0737-3039A and B bound to each other, the six others at different dispersion measures; none unexplained (`atnf_pulsars_one_spot`) |
| Glitches on a schedule | Jodrell Bank glitch table: 34 pulsars with five or more dated glitches, the scatter of their glitch intervals as a fraction of the mean against 4000 draws of exponential intervals | 4 regular, J1420-6048 (scatter 0.20 of the mean, p below 2.5e-4), J2021+3651, J1023-5746 and J1709-4429 (0.27-0.29), every one a young pulsar of large Vela-like glitches, which recur at the crust's critical lag; none unexplained (`jbo_glitch_schedules`) |
| Warm stars in the nearest clusters | Hunt and Reffert (2023): the 58 clusters and moving groups within 250 pc with 100 or more members, each member at BP-RP 0.5-2.5 matched to AllWISE, the share with W1-W3 five widths above the cluster's own locus against the field's 0.77 per cent, judged over the 58 | no cluster beyond chance over the 58; 23 warm stars, 13 flagged in AllWISE, 6 of known types; the highest shares in the clusters of 5-10 Myr (HSC 2986, OCSN 96, HSC 2907 at 5-6 per cent) and the Pleiades at 2.3 per cent; none unexplained (`clusters_warm_stars`) |
| Waste heat at the oldest Sun-like neighbours | GALAH DR4 (Data Central): 4248 dwarfs within 200 pc at 5300-6200 K with a clean fit, an isochrone age and clean AllWISE W1 and W3; the oldest tenth, 425 stars older than 12.4 Gyr, against the rest | none of the oldest 425 warm against 11 of the 3823 younger (Fisher p 1) (`galah_oldest_sunlike_warm`) |
| Planets on polar orbits | NASA Exoplanet Archive planetary systems table: 166 planets with a projected obliquity measured to 15 deg, the measurement of smallest error for each, the count within 15 deg of 90 against a uniform projected obliquity | 16 against 27.7 (binomial p 0.996), with 95 within 15 deg of alignment and 5 of anti-alignment; the sixteen at the chance rate (`exoplanet_polar_orbits`) |
| Neighbours Gaia's classifier calls galaxies | Gaia DR3: 372226 sources within 100 pc at parallax over error above 10, those whose discrete source classifier gives a galaxy or quasar probability above 0.5; Gaia's image flags, BP/RP excess and RUWE; SIMBAD | 335: 249 blends by the BP/RP excess or image peaks, 14 without a colour, bluer than any star or saturated, 4 of poor astrometry, 68 of known types; none unexplained (`gaia_dsc_galaxies_nearby`) |
| Stars that changed velocity between GALAH and Gaia | GALAH DR4 (Data Central): 396280 stars with a clean fit and both GALAH's and Gaia DR3's radial velocities to 2 km/s, those apart by more than 30 km/s; GALAH's second components, Gaia's orbits, amplitudes, variability flags, RUWE and image peaks, the two surveys' temperatures, Gaia's transit counts and a third epoch from RAVE DR6 or LAMOST DR5 | 48: 14 binaries, one of them by a third velocity from RAVE apart from GALAH's, one GALAH spectrum of a different star by its temperature, one Gaia velocity on two transits; 32 remain, single-lined binaries by their rate, which Gaia's variability statistics do not reach at their brightness and which RAVE and LAMOST have not observed (`galah_gaia_rv_jumps`) |
| Europium far above iron in dwarfs | GALAH DR4 (Data Central): 1337 dwarfs with a clean fit and a clean europium abundance to 0.2 dex at S/N above 40, those with [Eu/Fe] above 1.0 at the lower bound; metallicity, companions and the s-process elements as the natural routes | none (`galah_europium_dwarfs`) |
| Zirconium alone | GALAH DR4 (Data Central): 11597 dwarfs with a clean fit and clean zirconium, yttrium and barium to 0.15 dex at S/N above 40, those with [Zr/Fe] above 0.8 at the lower bound while [Y/Fe] and [Ba/Fe] stay below 0.3; companions by GALAH's second components and Gaia's flags, and the temperature range of trusted zirconium lines | 29: 6 with a companion, 23 cooler than 5000 K, where the weak zirconium lines blend with molecular bands; none unexplained (`galah_zirconium_alone`) |
| Lines in dayside spectra | NASA Exoplanet Archive emission-spectroscopy table (emissionspec): 25 published eclipse spectra of five or more bins, 2167 bins; a bin five combined errors, five times the spectrum's bin-to-bin scatter and a tenth of the depth from the mean of its neighbours, in either sign | 3: two bins of WASP-33 b's WFC3 spectrum, whose host is a delta Scuti pulsator, and one at the red edge of a NIRISS spectrum of WASP-18 b; none unexplained (`exoplanet_dayside_lines`) |
| Bodies aimed at Earth | JPL Small-Body Database: 147 near-Earth asteroids on arcs of a year or more with a minimum orbit intersection distance below 0.001 au (1764 on shorter arcs set aside), the count below 0.0001 au against the uniform run of the next nine bins | 19 against 14.2 (Poisson p 0.13); at the chance rate (`sbdb_aimed_at_earth`) |
| Bodies parked in the Kirkwood gaps | JPL Small-Body Database: numbered asteroids within 0.03 au of the 3:1, 5:2 and 2:1 resonances with e below 0.1 on arcs of twenty years or more, the count within 0.002 au of each resonance centre against the density 0.01-0.03 au either side | the gaps are empty as they should be: 1 against 296 expected at the 3:1, 13 against 669 at the 5:2, 1 against 60 at the 2:1; the fifteen in the centres at the chance rate (`sbdb_kirkwood_parked`) |
| Masers in Earth's transit zone | Pestalozzi et al. (2005) 6.7 GHz methanol masers (VizieR J/A+A/432/737): 519 masers, the count within 0.262 deg of the ecliptic against the twenty strips of that width on either side out to 5.5 deg | 2 in the zone against 2.4 +- 2.6 beside it; at the chance rate (`methanol_masers_transit_zone`) |
| Circles beyond Neptune | JPL Small-Body Database: 4941 trans-Neptunian objects beyond 40 au with an eccentricity uncertainty, those whose eccentricity at its 3 sigma upper bound lies below 0.005, against the Rayleigh rise of the belt's eccentricities near zero | 4 (Praamzius, 2010 PK66, 2003 YN179 and 2010 NF146, all on arcs of twelve years or more) against 7.5 expected from the 746 below 0.05; at the chance rate (`sbdb_tno_circles`) |
| Gamma-ray sources that moved between catalogues | Fermi-LAT 3FGL (HEASARC fermi3fgl) and 4FGL-DR4 (fermilpsc): 1717 associations shared by both, the separation of the two positions against the sum in quadrature of the 95 per cent axes | 2 apart by more than twice the combined axes: the extended source W 41 and PSR J1112-6103 in the Galactic plane, where confusion moves a faint source's centroid; none unexplained (`fermi_3fgl_4fgl_moved`) |
| Bursts from the nearest galaxies | CHIME/FRB Catalog 1: 492 sources against the 46 large galaxies within 10 Mpc north of -11 deg, a burst inside a galaxy's optical radius plus the half-degree localisation, against the bursts' density within 10 deg of each galaxy | none against 1.76 expected (`chime_nearest_galaxies`) |
| Gamma-ray bursts from the nearest galaxies | Swift GRB table (HEASARC swiftgrb) and Fermi GBM bursts with errors below 1 deg: 1782 bursts against the 50 large galaxies within 10 Mpc, a burst inside a galaxy's radius plus its own error, against the bursts' density within 10 deg of each galaxy | 1 against 1.86 expected: GRB 231115A in M82, the published magnetar giant flare; none unexplained (`grb_nearest_galaxies`) |
| Bodies at the Sun's focus | JPL Small-Body Database: 16 bodies with perihelia beyond 60 au, the count beyond 100 au, from where the Sun's lens brings other stars' light to a focus | none beyond 100 au; the farthest perihelia are 2012 VP113 at 80.6 au and Sedna at 76.2 (`sbdb_sun_focus`) |
| Stars that changed colour since Hipparcos | Hipparcos new reduction and Gaia DR3: 77746 stars with a B-V measured to 0.03 mag and a BP-RP, those five robust widths, five times the carried B-V error and 0.2 mag off the run of BP-RP with B-V; Hipparcos scatter, RUWE, Gaia's excess, SIMBAD's types and spectral classes | 1527 off the run: 386 saturated or with BP/RP excess, 538 variable, 135 binaries, 26 whose spectral class sides with Gaia against the Hipparcos B-V; 442 remain, stars whose Hipparcos B-V, compiled from ground photometry, is the only old colour and cannot be checked against a second (`hipparcos_gaia_colour_change`) |
| Eclipsing binaries on whole days | Kepler eclipsing binary catalogue (Prsa et al. 2011, VizieR J/AJ/141/83): 1242 systems with periods between 0.5 and 50 d measured from space, those within 0.0002 d of a whole number of days against the periods' own density and the half-day windows | none against 0.5 expected; 2 at half-days (`kepler_eb_whole_days`) |
| Retrograde co-orbitals of the giant planets | JPL Small-Body Database: bodies within 5 per cent of Jupiter's, Saturn's, Uranus's or Neptune's semi-major axis with inclination above 90 deg and eccentricity below 0.5 | 3, all at Jupiter: the published co-orbital (514107) Ka'epaoka'awela, 2007 VW266 published in the neighbouring 13/-14 resonance, and 2016 YB13, which fifty clones of its orbit hold in the resonance for thousands of years each way, a transient member; none unexplained (`sbdb_retrograde_coorbitals`) |
| Radio sources that switched off | NVSS (VizieR VIII/65): 37223 compact sources above 100 mJy north of -40 deg and more than 10 deg from the Galactic plane, those without a VLASS epoch-1 quick-look component (J/ApJS/255/30) within 20 arcsec; SIMBAD, the artefact zones of sources above 5 Jy, RACS-low of 2019-2020 and the component list's own holes | 281 missing: 132 of known types, 12 beside sources above 5 Jy, 113 still shining in RACS-low or in holes of the component list; 24 remain, north of RACS-low's reach or unmatched in it, with VLASS components around them (`nvss_vlass_switchoffs`) |
| Bodies pushed out of their orbital planes | JPL Small-Body Database: 113 comets and 10 asteroids with normal and radial non-gravitational terms, those whose normal term at 3 sigma exceeds half the radial; the ratio's distribution has a median of 0.19 and a 90th percentile of 0.86 | 28: 21 comets, whose polar jets push across the plane, 5 on arcs under 1000 d; the two near-Earth asteroids 2016 GW221 and 2013 XY20, whose normal terms rest on 209 and 72 observations, remain unexplained (`sbdb_out_of_plane`) |
| Gamma rays harder than any shock | Fermi-LAT 4FGL-DR4 (HEASARC fermilpsc): 2766 sources above 10 sigma with a power-law index, those with an index below 1.3 at its upper error | none (`fermi_hard_spectra`) |
| Stars whose distance changed since Hipparcos | Hipparcos new reduction and Gaia DR3: 98004 stars with both parallaxes, the differences in combined sigmas scaled by the sample's scatter of 1.24, those apart by 5 scaled sigma and 2 mas; the match's brightness, RUWE, Gaia's flags, Hipparcos's goodness of fit, SIMBAD and the Gaussian tail | 43: 3 matched to a Gaia source two magnitudes too faint, 27 binaries, 12 saturated or with poor solutions, 1 within the Gaussian tail (p 0.055); none unexplained (`hipparcos_gaia_parallax_change`) |
| Lithium above the meteoritic | GALAH DR4 (Data Central): 124623 dwarfs with a clean fit and a clean lithium abundance to 0.15 dex at S/N above 40, those with A(Li) above 4.3 at the lower bound, a dex above the meteoritic and beyond what engulfing a giant planet adds; the stars between 3.6 and 4.3 counted as within engulfment's reach | 1 above 4.3, a 6600 K star where the line blends; 11 between 3.6 and 4.3; none unexplained (`galah_lithium_meteoritic`) |
| Gamma-ray flares from the nearest stars | Fermi All-sky Variability Analysis second catalogue (HEASARC fermi2favs): 518 flaring sources with error radii, against the 2551 Gaia Catalogue of Nearby Stars objects within 20 pc, with the stars moved 2 deg in eight directions as the null | 7 stars inside error circles against 9.4 moved (Poisson p 0.83), five of the circles carrying their own blazar or nova counterpart; at the chance rate (`fava_nearest_stars`) |
| Surfaces bluer than any asteroid class | Gaia DR3 sso_reflectance_spectrum: 60515 asteroids with six or more unflagged bands from 450 to 850 nm, the slope of each by least squares, those below -15 per cent per 100 nm at 3 sigma; the slopes' 0.1st percentile sits at -3.1 | none (`gaia_sso_blue_surfaces`) |
| Stars whose infrared changed since 2MASS | Gaia Catalogue of Nearby Stars: 142514 stars brighter than G 15 with 2MASS Ks to 0.03 mag, the G-Ks of each against the run of G-Ks with BP-RP, those five widths and 0.3 mag off; Gaia's neighbours within the 2MASS beam, image peaks, variability flag and RUWE; SIMBAD | 4847 off the run: 4732 with a Gaia neighbour within 2 mag inside the 2MASS beam, 27 white dwarfs, 6 young stars, 3 subdwarfs, 19 variable, 26 binaries; 34 remain, mostly red dwarfs with Ks brighter than their Gaia colour gives by 0.3-0.7 mag and no resolved neighbour (`gcns_2mass_gaia_ir_change`) |
| Rotation periods on whole days in TESS | Fetherolf et al. (2023) TESS rotation periods (VizieR J/ApJS/266/22): 1416 stars with one period between 0.5 and 13 d measured to 0.005 d, those within 0.005 d of a whole number of days against the periods' density and the half-day windows | none against 14.2 expected, the catalogue holding no period at a whole day; 107 at half-days, a pile-up of the catalogue's own (`tess_rotation_whole_days`) |
| Carbon stars on the main sequence next door | Gaia DR3 gold sample of carbon stars joined to gaia_source: 99 within 1 kpc at parallax over error above 5, those whose absolute G places them on the main sequence, fainter than 4 | 2, both with RUWE above 10, their parallaxes dragged by a companion; none unexplained (`gaia_carbon_dwarfs`) |
| Eclipsing twins to a part in a thousand | Kepler eclipsing binary catalogue (Prsa et al. 2011, VizieR J/AJ/141/83): 1642 systems with a fitted temperature ratio, 307 within 0.05 of one, those within 0.001 against the ratios' density and the fits pegged at exactly 1.000 | 6 free of the boundary against 6.1 expected, none pegged; at the chance rate (`kepler_eb_twins`) |
| Stars WISE could not see | Gaia Catalogue of Nearby Stars: 156334 stars brighter than G 15, 11207 without a WISE counterpart in the catalogue's own match, each carried to 2010.5 and sought in AllWISE within 3 arcsec; WISE's saturation, Gaia's neighbours in the beam, the halos and glare of brighter stars out to ten arcminutes, image peaks, RUWE, SIMBAD, unWISE's deeper coadds and the Galactic plane | 1658 unmatched: 384 saturated, 1003 blended with a Gaia neighbour in the beam, 164 in a brighter star's halo or glare, 15 of poor astrometry, 82 listed by unWISE and so dropped by AllWISE's own extraction, 10 in the plane's confusion; none unexplained (`gcns_wise_missing`) |
| Launch provenance of light bodies | JPL Small-Body Database: 22 asteroids and 279 comets with a radial non-gravitational term, those at 3 sigma whose term needs an area-to-mass ratio above 0.1 m^2/kg from sunlight alone; the database's bodies of our launching, the dark comets, comets' outgassing and the arcs | 71: 70 comets, whose outgassing supplies the push, and 'Oumuamua at 1.2 m^2/kg, whose published outgassing models do the same; none of our launching carries a term in the database (`sbdb_light_bodies`) |
| VASCO transients and the geosynchronous belt | the Villarroel et al. (2020) POSS-I transient candidates (VizieR J/AJ/159/8): 127 positions spanning declinations -5.7 to 82.9 deg | in the band from -6.1 to -4.6 deg, where the geosynchronous belt stands seen from Palomar, 1 against 3.03 from the band's share of that sky (binomial p 0.95); nothing crowds the belt (`vasco_geosynchronous_belt`) |
| Our flags toward the solar apex | the coverage store: 180,822 Gaia DR3 stars, 32,003 of them vetted, within 30 deg of the solar apex (l 56.2, b +22.8 deg) and of the antapex | 2,671 vetted stars toward the apex against 1,875 from the whole store's share and 2,154 toward the antapex against 1,810, the whole of it the footprints of the runs that vet every target; with each run's own coverage setting its share, 2,723 run targets against 2,720 (p 0.31) and 2,185 against 2,181 (p 0.29) (`store_flags_apex`) |
| Warm dust in globular clusters | the Harris (2010) Galactic globular clusters with a half-light radius (VizieR VII/202): 141 clusters; the AllWISE sources with W1-W3 above 1 mag at W3 signal-to-noise 10 within the half-light radius against the annulus from three to five half-light radii | no cluster holds more warm sources inside its half-light radius than its surroundings give, beyond chance over the 141 (`allwise_globular_warm_dust`) |
| Single hot subdwarfs in the thin disc | the known hot subdwarfs of Culpan et al. (2022) (VizieR J/A+A/662/A40) with a Gaia parallax at 5 sigma, a proper motion and an SDSS or LAMOST radial velocity: 1,034 sdB, sdOB and sdO stars, 485 of them without a companion in their class, Gaia's RUWE, non-single-star flag or colour | 129 singles within 50 km/s of the local standard of rest, a thin-disc share of 0.27 against the binaries' 0.25, so single hot subdwarfs sit on thin-disc orbits as often as the binaries do; every one an evolved star the disc's mergers supply (`hot_subdwarfs_single_thin_disc`) |
| Sky clustering of our residues | the coverage store: 180,822 Gaia DR3 stars in 158 runs, 32,003 of them vetted; vetted pairs within 1, 3 and 10 deg as a share of all pairs against 50 draws in which each run marks as many of its own targets at random | 1.759 pairs per 10,000 within 1 deg against 1.752 +- 0.002, an excess of 0.4 per cent; 13.067 against 13.058 within 3 deg (p 0.16) and 111.606 against 111.671 within 10 deg (p 0.84); within each run the vetted pairs match the draws (55,957 against 55,843), so the small excess at 1 deg lies between runs and is not explained (`store_residue_clustering`) |
| Binary pulsars decaying at the wrong rate | the ATNF catalogue's field binary pulsars with a measured orbital decay and the companion's mass: 13, the total mass from the periastron advance or from sin i and the mass function; general relativity's decay, the Shklovskii term and the Galactic acceleration, with the masses and a 20 per cent distance error carried by Monte Carlo | the double pulsar J0737-3039A matches relativity to 0.2 sigma; one remainder beyond 3 sigma, the redback J2339-0533 at 3.5 sigma, whose orbital period wanders with its companion's shape (`atnf_orbital_decay_remainder`) |
| The axis of the universe | SIMBAD's objects of unknown nature and its unclassified radio, X-ray and gamma-ray sources within 2 deg of the CMB dipole's apex and antapex, against 34 patches at each one's Galactic latitude | apex 1 unknown, 102 radio, 18 X-ray and 2 gamma-ray sources against control medians of 1, 133, 35.5 and 0, the gamma-ray count matched or beaten by 12 per cent of the controls; antapex 0, 47, 28 and 0 against 0.5, 79, 31 and 0; nothing marks the axis (`simbad_cmb_dipole_axis`) |
| The Lagrange points of the Galactic bar | the bar's L4 and L5 at corotation (6.5 kpc, bar angle 27 deg), at l 27.5 and 312.1 deg; the 171 unassociated Fermi-LAT 4FGL-DR4 sources within 3 deg of the plane that are neither confused nor flagged as soft Galactic unassociated, counted within 2 deg against 27 windows along the inner plane | L4 2 against the plane's mean 1.26 (p 0.36); L5 7 (p 0.0003), the densest window of the inner plane, on the Crux-Centaurus arm's tangent at l 310 deg and around the Kookaburra and Rabbit pulsar wind nebulae; the bar's parameters allow L5 anywhere in l 302 to 321 deg, so the point cannot be told from the tangent (`fermi_bar_lagrange_points`) |
| Two messengers at once | IceCat-1 (VizieR J/ApJS/269/25): the 65 IceCube alert tracks that arrived during TESS sectors 1-30, MJD 58325-59141; the Yang et al. (2023) TESS flares (VizieR J/A+A/669/A15): 480 flaring stars inside the tracks' 90 per cent regions with 1,722 flares | no flare within an hour of its neutrino against 0.125 from 1,999 shifts of the alert times by up to 100 days, and none within 100 pc against 0.062 (`icecat_tess_flare_coincidence`) |
| Dyson spheres built for our eyes | Gaia Catalogue of Nearby Stars: 8,688 Sun-like stars within 100 pc at BP-RP 0.65-1.0 with clean Ks, W3 and W4, 26 with excess at both 12 and 22 um and 6 of them unflagged with a colour temperature | 2 between 280 and 320 K against 1.0 in the bins beside (Poisson p 0.26), at 285 and 320 K; the excesses run from 100 to 320 K, at the chance rate (`gcns_room_temperature_sunlike`) |
| Cosmic-ray doublets, northern sky | Telescope Array's 72 events above 57 EeV of 2008-2013 (VizieR J/ApJ/790/L21) | no two events within 2 deg; within 4 deg 5 pairs, none within 10 days against 0.06 from 5,000 shuffles of the arrival times, and no triplet (`ta_doublets`) |
| Centrifugal habitats, survey periods | Lo et al. (2020) faint main-belt asteroids (VizieR J/AJ/159/25): the 122 with secure periods and diameters, 0.19-2.7 km, among them 22 super-fast rotators | no kilometre body under 10 minutes or needing 100 kPa; 4 bodies of 0.3 km or more spin past the 2.33 h gravity limit, needing 1.0-5.8 kPa, the fastest 510525 (1.75 km, 36.6 min), all within the strength of a coherent or cohesive body (`lo2020_spin_strength`) |
| Debris-disk voids | the Cotten and Song (2016) WISE excess stars (VizieR J/ApJS/225/15) matched to the 101,867 Gaia DR3 stars within 150 pc at G below 11 and BP-RP below 1.5, 860 of them excess stars; every 20 pc sphere about a parent star against its colour-binned excess rate | the deepest deficit, 0 excess stars against 3.9 about Gaia DR3 1613739235969713280 at 86 pc (Poisson 0.02), is matched or passed by 93 per cent of 200 shuffles of the labels within colour bins; at 15 pc the deepest is 2 against 3.0; no region of stripped belts (`cotten_song_debris_voids`) |
| Spectra no stellar model fits | GALAH DR4: 1,379 dwarfs within 100 pc at red-arm S/N above 100; the worst 0.5 per cent of the spectral fit's chi-square over the median of its 250 K temperature bin | 7 spectra at 5 to 42 times their bin's median, 6 of them binaries with a second velocity component or a Gaia RUWE above 1.4 and one star with H-alpha filled in; none unexplained (`galah_worst_fits_nearby`) |
| Gaia XP spectra the models fit worst | Gaia DR3: 118,030 stars within 100 pc with parallaxes at 10 sigma and a GSP-Phot fit; each log-posterior against its bin of 0.1 mag in BP-RP and 1 mag in G fitted with the same model library, the worst 0.1 per cent | 118 worst fits: 22 with a companion, 6 with emission lines, 2 blended and 69 at an extinction no star within 100 pc carries; 19 mid-M dwarfs fitted with MARCS remain, the far end of a tail of 149 beyond 5 widths among 34,969 such stars; PHOENIX fits of M dwarfs run far worse than MARCS fits and pile at [M/H] -0.8, so the bins are kept apart by library (`gaia_xp_worst_fits_nearby`) |
| Herded stars, GALAH and ages | GALAH DR4 dwarfs within 100 pc with isochrone ages, GALAH radial velocities and Gaia DR3 astrometry: 2,895 with 3D velocity errors under 0.5 km/s and one velocity component | 482 pairs within 10 pc moving together within 1 km/s against 2.2 from velocity shuffles; of the 34 pairs both hotter than 5,600 K, where ages carry information, the age gaps run to a median of 1.6 Gyr and a largest of 4.9 Gyr, and none exceeds 5 Gyr (`galah_herded_ages`) |
| Fireballs from outside the Solar System | the CNEOS fireball database through the JPL fireball API: 360 fireballs with a location and a pre-entry velocity vector, taken from Earth-fixed axes to barycentric axes with Earth's gravity removed and Earth's velocity added | 8 arrive faster than the Sun's escape speed at Earth's distance; redrawn with CNEOS's errors against ground-based networks (Peña-Asensio et al. 2025), the five before 2018 or at the threshold are bound in 2 to 48 per cent of the draws, among them IM1 (2014-01-08, 60.6 km/s heliocentric, bound in 2 per cent) and IM2 (2017-03-09, 21 per cent); three since 2018 are bound in none of 20,000, 2021-05-06 (43.7 km/s), 2022-07-28 (47.4 km/s, CNEOS-22) and 2026-04-01 (51.8 km/s), and are not explained (`cneos_hyperbolic_fireballs`) |
| The temperate rocky-planet hosts in every band | NASA Exoplanet Archive composite table: the hosts within 100 pc of planets below 1.8 Earth radii (or 10 Earth masses) at 0.2-2 times Earth's insolation, against the other planet hosts within 100 pc weighted to the same temperatures and distances; eRASS1, GALEX AIS, VLASS and RACS-low by CDS XMatch inside each footprint, the radius widened by each star's motion over the survey's span | X-rays 6 of 11 against 4.7 (p 0.31); radio none of 24 in VLASS and none of 17 in RACS-low against 0.5 and 0.4; ultraviolet 5 of 29 against 11.7, a deficit (lower tail 0.007) from AIS fields that missed 13 of the 29 and from the quiet M dwarfs that radial-velocity searches choose; no band raises its detections at these hosts (`exoplanet_hz_hosts_bands`) |
| Retrograde co-orbitals of the inner planets | JPL Small-Body Database: asteroids and comets within 5 per cent of the semi-major axis of Mercury, Venus, Earth or Mars with inclinations above 90 deg and eccentricities below 0.5 | none at any of the four (`sbdb_retrograde_coorbitals_inner`) |
| Clusters missing their brightest stars | Hunt and Reffert (2023) open clusters at 100-1000 pc younger than 400 Myr with A_V below 1.5 and 300 or more members: 88 with 20 or more members at absolute G 4-6.5; their members at absolute G 0.5-2.5, late-B to F stars still on the main sequence, against the bright-to-faint ratio fitted in log age (0.32 at log age 7.5, 0.34 at 8.5) | no cluster short of bright stars beyond the 88 trials; the deepest, NGC 2301 with 29 against 48.7 (p 0.0016, corrected 0.14), Roslund 5 and NGC 1039, lie at the chance level (`hunt_reffert_missing_bright`) |
| Hostless flat-spectrum radio sources | CRATES (VizieR J/ApJS/171/61): 4,396 point-like flat-spectrum sources with 8.4 GHz interferometric positions more than 30 deg from the Galactic plane and declination above -30 deg, against AllWISE, Pan-STARRS1, CatWISE2020, unWISE, SIMBAD, the Legacy Surveys DR10 and VLASS | 132 with no AllWISE, Pan-STARRS1, CatWISE2020 or unWISE counterpart: 27 classed as active galaxies by SIMBAD, 56 compact knots or hotspots more than 3 arcsec from their NVSS centroid, 11 with a Legacy DR10 galaxy or quasar at r 21-24.6, 15 at positions where VLASS sees nothing within 30 arcsec though it recovers 78 of 79 CRATES sources, and one beside HD 81417; 22 remain, each a VLASS source at its position with nothing in the Legacy Surveys within 2 arcsec, alike to the infrared-faint radio sources thought to be radio-loud nuclei at high redshift and not explained one by one (`crates_hostless_flat_spectrum`) |
| A model-free outlier search over the nearest stars | Gaia DR3: the 1,000 sources with the largest parallaxes at 10 sigma (beyond 67.7 mas); 2MASS and AllWISE through Gaia's best neighbours, GALEX AIS and eRASS1 by CDS XMatch at their epochs; each archive's colours or flux ratio against the 50 stars nearest in BP-RP, the ultracool dwarfs fainter than absolute G 15 against each other by G-RP | 196 stars odd in at least one archive by 5 robust widths and 3 in three or more, all astrometric binaries, two of them the components of one pair at 4.3 pc; none unexplained (`nearest_stars_multi_archive_outliers`) |
| Time clustering of our residues | the coverage store's unexplained candidate events with dates, a candidate being a row with a p-value below 0.01 or a cosmic-ray multiplet, since most dated rows record the epochs searched: 5 runs, 2,408 distinct days, from the Auger doublets and triplets of four data sets and the occultation limbs beyond their null | 6 days on which candidates of different instruments fall within a day of each other, all between the Auger 750 m array and the occultation limbs, against 6.0 +- 2.0 when each run's days are shifted by up to a year (p 0.62) (`store_residue_time_clustering`) |
| Deliveries from stellar encounters | the three interstellar objects from the Small-Body Database, their incoming velocities at infinity (26.3, 32.3 and 57.9 km/s from the published radiants), against the Gaia DR3 stars within 100 pc with radial velocities, both carried back on straight lines for 10 Myr | stars that passed within 1 pc of an object's path at under 10 km/s: one for 'Oumuamua, Gaia DR3 6476662183875784064, 0.39 pc and 7.9 km/s 6.9 Myr ago, against 0.11 for the same speed in random directions (p 0.11); none for Borisov against 0.08 and none for 3I/ATLAS against 0.01; at the chance rate (`interstellar_object_home_stars`) |
| Fireballs seen twice | the CNEOS fireballs since 2017 July 23 inside the GOES lightning mappers' view, 79, against NASA's GLM bolide database (11,611 bolides), within 60 s and 300 km; the two-satellite sightings triangulated frame by frame into trails | 68 of 79 matched; both fast fireballs in view were seen, 2026-04-01 by GOES-19 and 2022-07-28 by GOES-16 and GOES-17; the mappers' triangulated trail speeds run at 0.66-1.65 of the CNEOS speeds on 16 slower fireballs (median 1.14) and at 0.61 for 2022-07-28 (18.4 km/s), too scattered to test its 21 per cent excess (`cneos_glm_bolides`) |
| Radio spectra of the hostless flat-spectrum sources | the 22 compact CRATES sources the hostless test left without an infrared or optical counterpart, and 200 hosted CRATES point sources treated alike: TGSS, GLEAM, RACS-low, NVSS and VLASS by CDS XMatch, the CRATES fluxes and the VLBI bands of the Radio Fundamental Catalogue | 17 of 22 are VLBI-compact, the hosted sources' rate (0.77); their spectra are 8 peaked, 8 flat and 6 steep against the hosted sources' 43, 124 and 28 of 200, flat less often (Fisher p 0.019) and peaked more often (p 0.10); none varied by a factor 2 between NVSS and VLASS; compact young radio galaxies rather than beamed quasars, whose hosts lie below the Legacy Surveys' depth (`crates_hostless_seds`) |
| What sets the worst-fitted nearby M dwarfs apart | the 19 MARCS-fitted mid-M dwarfs among the Gaia XP worst fits with no companion, emission, blend or extinction behind them, against 3,000 stars of their colour and magnitude within 100 pc with ordinary fits | all 19 lie below the main sequence at fixed BP-RP and at fixed G-RP alike (1.5 robust widths against 0.0, p 5e-10; 0.36-1.0 mag, and 2.3 mag for one), with parallaxes three times as precise as their peers' (signal-to-noise 1,283 against 366, p 2e-10), at higher Galactic latitude (64 against 25 deg, p 2e-5), faster on the sky (45 against 31 km/s, p 0.08), redder in BP-G at fixed G-RP (p 0.012), with no excess radial-velocity scatter or GALEX detection (`gaia_xp_misfit_traits`) |
| What a pile of unassociated gamma-ray sources is | the 4FGL-DR4 sources associated with pulsars, blazars and remnants or nebulae (3,946) train a random forest on power-law index, curvature and its significance, peak energy and variability; the clean unassociated sources within 2 deg of l 312.07, b 0 against those elsewhere within 5 deg of the plane; eRASS1 by CDS XMatch | 5 of the window's 7 classifiable: none pulsar-like against 25 per cent elsewhere, four uncurved and steady (variability indices 8-20) and the extended FGES J1409.1-6121 classed with remnants and nebulae; eRASS1 counterparts 1 of 7 against 4 of 135; extended emission around the Kookaburra and Rabbit nebulae rather than a pile of young pulsars (`fermi_unassociated_pile_classes`) |
| Fireballs the meteor cameras caught | the 360 CNEOS fireballs with velocity vectors against the Global Meteor Network's trajectory summaries for 2018-2026, a camera trajectory beginning within 10 s and 300 km of the fireball's peak | none of the 360, the eight faster than the Sun's escape speed among them, has a camera trajectory; the network's cameras and the satellites' fireballs, mostly over the oceans, do not overlap (`cneos_gmn_trajectories`) |
| Hosts of the hostless radio sources in the near infrared | the 22 hostless compact CRATES sources against VHS DR5, VIKING DR2 and UKIDSS LAS DR9 within 2 arcsec, coverage from any source within 1 arcmin, and the K-z relation of radio galaxies (Willott et al. 2003) | none has a near-infrared counterpart; the 15 the surveys cover are fainter than K 18.1-18.2, which on the K-z relation puts their hosts beyond redshift 1.5, and 7 lie outside the surveys (`crates_hostless_nir`) |
| Spectral classes of the worst-fitted nearby M dwarfs | the 19 MARCS misfits of the trait test looked up in LAMOST DR5 and SDSS DR17 within 3 arcsec of their positions at those surveys' epochs | 4 have spectra, typed M2 and M3 by LAMOST's pipeline and M2V by SDSS's, neither of which carries a metallicity class; the subdwarf verdicts rest on the luminosity and J-Ks tests (`gaia_xp_misfit_spectra`) |
| Gamma-ray points inside TeV glows | the 7 clean unassociated 4FGL-DR4 sources within 2 deg of l 312.07, b 0 against the H.E.S.S. Galactic Plane Survey's components (VizieR J/A+A/612/A1), inside when within twice a component's Gaussian width, against the 106 clean unassociated sources elsewhere in the survey's footprint | 1 of the 7, 4FGL J1417.7-6057, lies inside HESS J1418-609, against 17 of 106 elsewhere (Fisher p 0.71); the other 6 lie outside every TeV source, most 0.5-1.6 deg above the plane, so the TeV glows of the Kookaburra complex do not hold the pile (`fermi_unassociated_in_tev_glows`) |
| Subdwarf indices of the worst-fitted nearby M dwarfs | the 19 MARCS misfits' LAMOST DR5 and SDSS DR17 spectra, put in air at rest and measured in the CaH2, CaH3 and TiO5 bands, and the zeta of Lepine et al. (2013); APOGEE DR17 holds none of the 19 | 4 measured: Gaia DR3 2470131113219840128, the one 2.3 mag below the main sequence, is a subdwarf (zeta 0.56); the other three, 0.5-0.8 mag below, are dwarfs of ordinary metallicity (zeta 1.01-1.12), so the faintness of most is not the subdwarfs' (`gaia_xp_misfit_subdwarf_indices`) |
| Gas under a pile of gamma-ray points | the 7 clean unassociated 4FGL-DR4 sources within 2 deg of l 312.07, b 0; the Schlegel, Finkbeiner and Davis dust column at each from the IRSA dust service against 26 points at the same latitude 3-15 deg along the plane | the sources' dust ranks a median 0.69 among their controls (p 0.038 against uniform ranks), the two in the plane at 0.92 and 0.88; they sit on more gas than their latitudes' share, as gamma rays from cosmic rays in unmodelled gas would (`fermi_pile_dust`) |
| Methane and carbon dioxide without carbon monoxide | the NASA Exoplanet Archive's JWST transmission spectra of the 13 planets below 3.5 Earth radii with equilibrium temperature below 450 K or insolation below three Earths' (K2-18 b, L 98-59 d, LHS 1140 b and c, LP 791-18 c, LTT 3780 c, TOI-270 d, TOI-776 c, TRAPPIST-1 b-f), one reference per planet and instrument and each visit once, fitted together with templates of ten gases from their cross-sections at the planet's temperature | TOI-270 d holds CH4 (6.7 sigma) and CO2 (3.7) without CO, the disequilibrium pair, which the published metal-rich mini-Neptune envelope makes without life; dimethyl sulfide's template fits K2-18 b at 3.4 sigma with its methane at 0.4, the band the template overlaps, where the median over the atlas's 44 spectra of the planet reads 0.5, L 98-59 d at 3.6 sigma, a world of volcanic sulfur gases, and TRAPPIST-1 e at 4.5 sigma, whose spectrum its star's spots dominate (`jwst_temperate_disequilibrium`) |
| Flux in discrete levels, Kepler | Kepler DR25 long-cadence PDCSAP light curves of 199,624 stars, every quarter, read in memory from the STScI mirror | 132,275 steps within one cadence between 7.4-hour medians at 7 sigma, of which 2,767 are shared by three or more stars of the CCD channel and 6,438 by twenty or more stars of the focal plane; 18,465 stars keep steps of their own (8,108 up, 19,044 down) and 54 hold three or more levels each revisited in a quarter: 34 eclipsing binaries of the Kepler catalogue, 10 giants, whose oscillations and granulation step the window medians, the dwarf novae V447 Lyr and V1504 Cyg, the delta Scuti star TYC 3142-717-1 and the transits of Kepler-678 b; 6 dwarfs remain unexplained, Kepler-1645, TYC 3132-601-1, the A star TYC 3125-2793-1, KIC 7679979, KIC 11824498 and KIC 12783196, with steps of 0.1-9 per cent at irregular intervals (`kepler_levels`) |
| PSF-shaped flashes in pixel data | Kepler DR25 long-cadence target pixel files of the 3,611 KOI hosts with a candidate or confirmed planet, 48,779 quarters, their COSMIC_RAYS column | cadences where three or more optimal-aperture pixels were corrected together: 100,836 against 1,303 from the pixels' own rates, the cosmic rays' tracks; 2,135 shaped like the star's image (correlation 0.9 or more and 0.2 above the image shifted by one pixel) against 6,463 shaped like a shifted image, the most like of four shifts; the PSF-shaped events run at 3.7 times a quarter of the shifted-image rate on M dwarfs, 2.7 on K dwarfs, 1.1 on G dwarfs and 0.8 on F stars, the cool and young stars' flares, led by Kepler-1627, LSPM J1852+4740 and BY Draconis-type hosts; of the 860 stars with PSF-shaped events their channel does not share, 313 are flaring (cooler than 5300 K, three or more events, or light in the next cadence) and 547 carry one or two, the chance rate of cosmic rays shaped like the star's image, whose amplitudes the shifted-image class reaches as often (`kepler_psf_flashes`) |
| Atmospheres of the Rocky Worlds planets | the JWST MIRI 15 um eclipses the Rocky Worlds DDT has released on MAST: GJ 3929 b (four eclipses, the team's joint fit), TOI-771 b (three) and LHS 1140 b (one), with the stars' measured 15 um fluxes; TEPCat's radii, temperatures and separations and the Encyclopaedia of Exoplanetary Systems' distances | each dayside brightness temperature against the hottest a bare dark rock can be: GJ 3929 b 0.99 (0.91-1.07), TOI-771 b 1.03 (0.94-1.14) and LHS 1140 b 1.07 (0.96-1.17), each a bare rock's dayside with no heat carried away; on its one eclipse the habitable-zone LHS 1140 b lies 2.5 sigma above the 0.8 a heat-carrying atmosphere would give; LTT 1445 A b and c and TOI-198 b are still to be released (`rocky_worlds_15um`) |
| Gases of every planet with a published spectrum | 1037 transmission and emission spectra of 153 planets from the NASA Exoplanet Archive (649), Zenodo (279), VizieR (80) and MAST's Exo.MAST (29), identical ones kept once; templates from Exo-Transmit's cross-sections at each planet's temperature, HITRAN's N2O lines and NIST's dimethyl sulfide spectrum; Earth's transit spectrum from ACE-FTS (Macdonald and Cowan 2019) as the control | Earth's own spectrum reads CO2 at 22 sigma, O3 17.5, H2O 11.8, CH4 3.9 and N2O 3.9 and raises the methane-and-CO2 and N2O flags, and it reads dimethyl sulfide at 3.0 sigma, which it does not hold, from methane's 3.3 um band; of the 153 planets five raise a flag and none is left unexplained: dimethyl sulfide in the hot giants HAT-P-18 b (4.3 sigma), HAT-P-30 b (3.2) and TOI-5205 b (5.0) and in the hydrogen-enveloped L 98-59 d (3.7), and CH4 (5.0) with CO2 (3.3) without CO in the hot Jupiter HD 209458 b; K2-18 b's 44 spectra put dimethyl sulfide at a median 0.5 sigma, none of the 35 that cover it at 3 sigma; an Earth twin laid on TRAPPIST-1 e's JWST spectra shows CO2 at 0.7 sigma and CH4 at 0.1 sigma in the median one, so that about 17 such spectra would show its CO2 and about 1000 its methane (`spectra_atlas_gases`) |
| Computation at the cosmic floor | the SPT-SZ multiband catalogue (Everett et al. 2020): 4845 sources at 95, 150 and 220 GHz over 2500 square degrees, each source's two spectral indices against the track of a 2.8-10 K body seen against the microwave background | 9 sources on the track, rising from 95 to 150 GHz and below dust's index from 150 to 220 GHz, against 9.5 from each source's natural spectrum drawn through its errors; seven have radio, infrared or X-ray counterparts or are extended, two of them stars on the survey's own list, and the two clean ones, SPT-S J050800-6450.8 and J232128-5833.3, are detected at 150 GHz alone; a 4 K body is recovered at 20 mJy three times in four, so no computing shell radiating 1e-4 of the Sun's output lies within about 100 pc in the field (`spt_cold_computing`) |
| Ghost spectra | rest-frame stacks of 313 stars from the ESO laser-line runs (HARPS 97, ESPRESSO 87, FEROS 80, UVES 49), 4100-5600 A, each with a twin correlating at 0.9: each star's lines taken out by its twins and what remains correlated with its own lines at every shift from 1,000 to 60,000 km/s either way | 9 stars carry a copy of their own lines at 7 widths or more, every one at a shift other stars' strongest peaks share (+44,552 km/s in three UVES stacks, +46,180 in four, +59,424 in two, +57,552 in six HARPS stacks), the meeting of strong lines with the ends of the blue arm and of the range rather than a body; zeta2 Reticuli's peak is one of the UVES three; a copy of 0.3 per cent depth scores a median 4.5 widths, so no reflector returning about half a per cent of its star's light moves through these systems at 1,000-60,000 km/s (`eso_ghost_spectra`) |
| Flare echoes | GJ 1243 (KIC 9726699) in Kepler's one-minute photometry, 841 flares at 10 noise widths in 11 quarters; Proxima Centauri, AU Mic, YZ CMi, EV Lac, AD Leo, GJ 1243, Wolf 359 and UV Ceti in TESS's twenty-second and two-minute photometry, 39-259 flares each; the 8 stars within 30 pc brighter than Tmag 15 whose twenty-second light curves hold 30 flares; each flare's five-minute impulse correlated with the light curve 3-180 minutes after it and before it for the null, every other peak at 5 widths masked | no echo: GJ 1243 in Kepler reads 2.8 widths after its flares against 7.3 before, Proxima 5.8 at 156 min against 6.8; EV Lac's excess 10 and 22 minutes after its flares, 7.3 widths with secondary peaks unmasked, falls to 2.9 once they are, the second bursts of complex flares; of the nearby stars EQ Peg A (BD+19 5116 A) reads 2.5 per cent of its flares at 155 min and 7.5 widths, which one flare left out cuts to 1.0 per cent and the sector's first half does not show, and BB Scl's 40-minute excess rests on one of its eclipse edges; an echo of 0.3 per cent laid 30 min after GJ 1243's flares returns at 5.2 widths, under the 7.4 the null reaches, so the limit is about half a per cent of GJ 1243's flares and 0.6 per cent of Proxima's from a reflector 0.2-11 au away (`kepler_flare_echoes_9726699`, `tess_flare_echoes`, `tess20_nearby_flare_echoes`) |
| Optical frequency combs | rest-frame stacks of 313 stars from the ESO laser-line runs (HARPS 97, ESPRESSO 87, FEROS 80, UVES 49), 4100-5600 A: each star's residual after its twins laid on a grid uniform in frequency and its Fourier power read at every line spacing from 20 GHz to 1 THz against its own running median | 4 stars reach 30 times their level, all at spacings other stars share (20.5 GHz in HARPS and ESPRESSO stacks, 97.8 GHz in HARPS), the spectrographs' own; a star's strongest peak has a median of 13.7 and a 99th percentile of 36, and a comb of 0.2 per cent depth at 50 GHz laid into the stacks reaches a median 53, passing 30 in 216 of the 313 (`eso_optical_combs`) |
| Minute tones at the nearest stars | the 1806 TESS twenty-second light curves of stars within 30 pc read by the discrete-level search, hour-long variations and flares removed, Fourier amplitude at every period of 1-60 minutes against its running median, the tone's centroid amplitude, VSX and SIMBAD | 28 tones at 6 times the local amplitude, none left: 8 at frequencies other stars share, the spacecraft's; 8 moving the centroid as a neighbour's would; 10 on stars that pulsate at minutes, among them the ZZ Ceti white dwarfs DN Dra (109 s), MY Aps (193 s), PY Vul (216 s) and WD J174349.28-390825.95 (399, 491 and 568 s, a ZZ Ceti of Guidry et al. 2021); the 54-minute tone of the M3.5 dwarf BPM 45048 is the third harmonic of its 2.69-hour spot signal (5.38-hour rotation, 12 per cent peak to peak), and HD 9770's 57-minute tone the twelfth harmonic of BB Scl's 0.4765-day eclipses (`tess20_minute_tones`) |
| Chirps at the nearest stars | the 1756 TESS twenty-second light curves of stars within 30 pc at Tmag 15 or brighter, cut into six-hour and hour-and-a-half windows, each frequency levelled over time, and summed along every straight track drifting 1-60 cycles a day per day at periods of 1-60 minutes, as radio searches de-Doppler a carrier | 35 tracks below p 1e-12, none left: 28 matched by the same light curve's windows shuffled; 4 carried by other stars of their sector along the same track; psi1 Dra B's sweep of +59 c/d per day at 1008 c/d lies in its centroid (log p -279 against -28 in its light), pointing jitter; HD 146946's at 208 c/d drifting -33 joins the family of 210-225 c/d tracks drifting -20 to -40 that other stars of sector 67 carry in their flux and not their centroid; chi Ceti's slow track at 56 c/d vanishes once the band starts at 32 c/d, the leakage of its gamma Doradus pulsations (622 ppm at 2.54 c/d); a chirp of 0.05 per cent at 300 c/d drifting 20 c/d per day is found on its track in 14 of 20 light curves (`tess20_chirps`) |
| Atmospheres of the rocky planets of red dwarfs | ESO Phase 3 (HARPS, ESPRESSO, NIRPS, CRIRES, UVES), the CADC (CFHT SPIRou) and KOA (Keck NIRSPEC): 1,611 spectra in or beside the transits of 42 of the 114 planets below 1.8 Earth radii of stars cooler than 4000 K within 50 pc, 13 planets with four or more spectra on each side of a transit, each night's out-of-transit median as the star; the 229 HARPS spectra of the Moon through the Venus transit of 2012 June 6 as the control | 27 planet-instrument-line tests and no planetary absorption: 3 sigma limits on He I 10830 in the planet's frame (the core mean, the reversed trail's residual folded in) of 0.12 per cent at GJ 486 b from 86 SPIRou in-transit spectra, below the 0.2 published from two of its transits, 0.16 and 0.30 at HD 260655 b and c, 0.50 and 0.57 at L 98-59 d and c, 0.75 at TOI-270 b, 2.1 at LP 791-18 d and 15.7 at TRAPPIST-1 b, the first helium limits for all but GJ 486 b and TRAPPIST-1 b; the M dwarfs' H alpha and Na D cores move by 1-13 per cent with the sky's sodium and the stars' flares, every excursion matched by the reversed trail; the Moon through the Venus transit shows a -2.9 per cent core residual in both lines from the night's airmass, matched by the reversed trail as well; a 0.5 per cent line injected in the planet's frame returns 0.12-0.20 in the core mean, 0.4 of a 4 km/s line's depth (`rocky_dwarfs_shoreline`) |
| Planet-frame compositions of the giant planets | ESO Phase 3 and the CADC: the 48 HARPS and ESPRESSO transit sets of four or more in-transit spectra among the 945 giant planets brighter than V 11 (588 of their 800 hosts hold archived spectra), 2,463 in-transit spectra of 45 planets with the same nights' spectra beside them, and the SPIRou sets of WASP-76 b and HD 209458 b and the NIRPS sets of WASP-76 b and WASP-121 b; Kurucz's gfall lines for Fe I, Fe II, Ti I, V I, Cr I, Na I, Ca I, Mg I and K I, petitRADTRANS cross-sections for CO and water; SIMBAD's velocity where the archive lacks one | 47 planet-instrument sets searched and one species found: vanadium in WASP-121 b at 6.2 sigma on the orbit against a sham of 2.8 (Ben-Yami et al. 2020 found it at 4.5 from the same spectra), chromium there at 2.5 and in WASP-76 b at 3.1 under the threshold; a species resting on one line (Ca I, Mg I) or two (Na I, K I) is left to the line tests, since a deep stellar line's transit distortion sums along every trail; the shadow fit is bounded, kept to the optical atomic templates and given to the sham rows as well, since laid into the in-transit rows alone it sums to tens of sigma at rest; water in WASP-76 b at 4.7 sigma on the orbit from its 87 archived SPIRou in-transit spectra after three SysRem passes, the sham at 1.9 and the map's peak at K_p 50, so held under the rule (Hood et al. 2024 found it in one of those transits), CO there at 3.4; water in HD 209458 b's 13 SPIRou spectra at 3.9 with the map's peak off the orbit; HD 209458 b empty in the optical as published; sodium in WASP-69 b, a published detection, at 1.0 sigma in the cross-correlation, its two D lines left to the line tests; every other orbital value below 6 sigma or matched by the sham, the K dwarf HD 189733's own iron pattern reaching 5.4 against a sham of 6.4 and WASP-101 b's Fe II 5.7 with the map's peak at K_p 30, which the rule refuses; WASP-189 b, an A star rotating at 93 km/s, beyond the shadow model and flagged; the NIRPS sets of WASP-76 b and WASP-121 b, whose telluric residuals drive the sham maps to -12 and -90 sigma, marked not measured; a 0.5 per cent iron line injected into WASP-76 b adds 0.8 sigma; reflected starlight, the star's own spectrum as the template with the pattern and five principal components taken out of the rows and the gain measured by a 100 ppm copy laid into the same spectra: none from 51 Peg b at 43 ppm (3 sigma) from 300 HARPS and ESPRESSO spectra, the probe returned at 0.90, which places the contrast of 6e-5 claimed by Martins et al. 2015 at 4.2 sigma in the map, and tau Boo b's 299 campaign spectra near superior conjunction, where the components take 0.79 of the probe, at 546 ppm (`giants_planet_frame`) |
| Companions of single-lined binaries along their known orbits | ESO Phase 3: the 37 EBLM binaries with Gaia DR3 single-lined orbits and archived HARPS series of 20 or more spectra above S/N 10, periods below 100 d covered three or more times, up to 300 spectra each spread over the span, and TOI-1338's 260 ESPRESSO spectra; Gaia DR3 non-single-star orbits and SB9 for the catalogue orbits; an M1 V template from GJ 367's archived HARPS spectra and a G0 V velocity template from J0310-31's own | seven companions at 5 sigma or more against the stricter null: TOI-1338's at 19.3 (ESPRESSO), J0310-31's at 19.0, J2101-45's at 15.0, HD 4875's (J0050-18) at 13.9, J0649-27's at 6.7, J0825-67's at 6.4 and J1141-37's at 5.2; with the companion's systemic offset free, K2 of 77.27, 88.12 and 75.29 km/s for the three with published values (77.16 +- 0.48, 88.27 +- 0.46 and 75.13 +- 0.16), masses within 0.5 per cent of the published dynamical ones and the companions' lines +1.05 to +1.25 km/s from the primary's systemic velocity, which held at zero moves K2 by up to 0.55 km/s; J2101-45 at K2 65.41 km/s with minimum masses of 1.431 and 0.556 Msun, and J0649-27, J0825-67 and J1141-37 at 119.40, 78.18 and 114.68 km/s, none with a published semi-amplitude; TOI-1338's 73 HARPS spectra at 2.8 sigma and J1928-38's 74 at 0.3 at their published K2; J0415-16 and J0057-21 at 4.5 and 4.4; J0543-57 and J2126-28 too thin to search (`binaries_eblm_known_orbits`) |

## Queued

| Approach | Data | Note |
|---|---|---|
| Narrowband signals at high drift rates | Breakthrough Listen GBT mid-resolution products (2.86 kHz, 1.07 s): the 1118 ABACAD cadences of 882 targets with those products in the open data | tracks from -300 to +300 Hz/s with drift changing by up to +-0.3 Hz/s^2 within the scan, a hit at 10 sigma in all three ON scans along one track with the OFF scans below 5 sigma |
| Sources shining in one filter only | Pan-STARRS1 DR1 mean objects (VizieR II/349) | objects detected five or more times in one filter and never in the other four, brighter than g or r 19, i 18.5, z 18 or y 17, beyond what any stellar colour leaves undetected in the neighbouring filters; the per-filter detection counts carry no index, so each filter's selection reads all 1.9 billion rows |
| SPHEREx cold objects too large for degeneracy | SPHEREx QR2 spectral images (forced photometry at the ultracool dwarfs with parallaxes of the UltracoolSheet and Kirkpatrick 2021); WISE W3 and W4 | below 1500 K degeneracy allows 0.8-1.3 Jupiter radii, so a radiator of 1e22-1e23 W at 500-1500 K measures above 3 Jupiter radii once the band depths fix the temperature and the integrated flux the luminosity; Sonora Elf Owl and ATMO2020 fits with (R/d)^2 free, flagged above 2.5 Jupiter radii at 3 sigma, the field T dwarfs setting the null at 1.0 +- 0.15; binaries (at most 1.41), disks and variability between passes set aside |
| CHIME/FRB Catalog 2 replicated burst structure | Catalog 2 fitburst components of about 5000 sub-bursts; the waterfalls where needed; the tables sit on CANFAR storage behind a login, so the download waits on an account | a standardised engineered pulse recurs with the same relative component timings, amplitudes and widths from unrelated positions, while natural bursts and successive bursts of one repeater differ; the vector of normalised component times and amplitude ratios for bursts with three or more components, nearest-neighbour distances between sources more than 1 deg apart against shuffled parameters, any cross-source pair closer than the closest within-repeater pair |
| Hertz-scale coherent optical modulation in JWST guide stars | MAST fine-guidance products at 64 ms cadence for thousands of Gaia-selected guide stars, extracted with spelunker | no photosphere varies coherently at 0.05-8 Hz; Lomb-Scargle on the high-passed per-visit flux against the power distribution of the other guide stars of the month, the frequency absent from other stars and from the centroids; a 200-visit pilot first |
| Grey veiling of old stars in DESI DR1 | DESI DR1 stellar spectra (4 million) with the Milky Way Survey parameters, Gaia parallaxes, XP and kinematics | a featureless continuum added to an old, inactive star's light shallows every line by one factor, which metallicity does not; equivalent widths across Balmer, Ca II, Mg b and Fe I fitted as template times (1 - v) plus v times a continuum, the null the bulk's v at matched S/N and temperature; fibre contamination, sky residuals, white-dwarf companions (a black-body veil matching the parallax) and young accretors set aside |
| Recurrent hostless point sources in Rubin DP1 | Rubin DP1's DiaSource, DiaObject, Object, ForcedSource and SSObject tables | a PSF-shaped source on two or more nights at one position with nothing in the deep coadd, which no natural variable under 3 mag of amplitude gives; the null from rematching the detections at positions offset by 30 arcsec; asteroids, variables with coadd flux, dwarf novae and flares set aside |
| Hot featureless excess at old stars in SPHEREx | SPHEREx QR2 spectral images with forced photometry at the Gaia positions of FGK dwarfs within 300 pc, Gaia XP for the photosphere, 2MASS and AllWISE, Gaia kinematics and activity for age | a 600-2000 K black-body excess above 1e-3 of an old main-sequence star's light, read from twenty channels between 3.5 and 5 um, with no water, CO, methane or CO2 band between 1 and 5 um and without the blue slope of sub-micron dust; the band indices at zero against the 5 sigma tail of the whole sample's excess distribution; YSOs, Be stars, AGB stars, debris discs and brown-dwarf companions set aside by their lines and bands |
| SPHEREx at every star | SPHEREx QR2 spectral images: forced photometry at the 1701 unsaturated stars within 25 pc (`infrared volume`) | 402 of the 1701 measured; the spectra of the rest, then the line and excess tests over all of them; pulsars and habitable-zone hosts next |
| ALMA cubes, larger units | 21 observing units over 1.5 GB of products, and early cycles | early cycles hold visibilities only |
| Other radio morphologies | Breakthrough Listen | spread spectrum, chirps, wideband pulses |
| Microlensing anomalies | OGLE, MOA, KMTNet | ring and shell lenses |
| Polluted white dwarfs | DESI DR1, 455 white dwarfs within 100 pc | Huang et al. 2026 tested 697 published abundance sets against a processed-metal template: 8 above Bayes factor 10, none claimed |
| Silhouettes on the Sun | SDO/HMI continuum | |
| STEREO and SOHO artifacts | heliospheric imagers | |
| Guest stars | historical transient records | |
| Outgassing against radiation pressure | MPC astrometry of light bodies | needs accelerations at 10 sigma |
| Industrial gases on Mars | ExoMars TGO occultations | |
| Dust impacts, Apollo seismometers, lunar imagery | PDS, LRO | |
| Low-frequency all-sky archives | OVRO-LWA and similar | |
| Isolated tracklets | Minor Planet Center Isolated Tracklet File | glints from flat reflectors: brighter than diffuse reflection allows at the tracklet's parallactic distance, no phase reddening, recurring at the same Sun-object-Earth geometry |
| Particle, gravitational-wave and ionospheric archives | GWOSC, INTEGRAL, SuperDARN | |
| Template library of human artifacts | labelled human signals in archives | |
| Single-channel sources in coronagraph cubes | SPHERE/IFS and GPI archives, about 1000 nearby stars | a point fixed on the sky in one spectral channel, which every reduction discards; null from the opposite parallactic angle and shuffled channels |
| Flashes in up-the-ramp jumps | JWST and HST infrared ramps of TRAPPIST-1, LHS 1140, GJ 1214 and other transit targets | a PSF-shaped jump in one group at the star, against sharp cosmic rays and snowballs |
| PSF-shaped cosmic rays | HST CR-split pairs, DQ arrays at nearby stars | a flag over the star's core in one member of a pair |
| Frequency parallax | Breakthrough Listen hit tables, recurring hits classed as interference | barycentric residuals on the annual parallax ellipse place a transmitter at 1e3-1e5 AU |
| Zero-drift carriers on the target | Breakthrough Listen hit tables with the drift floor removed | ON-only in three cadences on different days, chance (1/2)^6 per cadence |
| Planetary rotation in the frequency | GJ 169's 24 GBT files, the long Kepler-field tracks, pulses from transiting-planet hosts | a barycentric sinusoid at a period other than 23.934 h; folds made coherent with the planet's light-travel delay |
| Radar leakage at transiting hosts | Breakthrough Listen Kepler and TESS campaigns | the rate of single-scan, drifting, ON-only hits at transiting hosts against non-transiting controls |
| Beams between stars, radio archives | narrowband radio archives at the members of the 37 pairs in `beam_pairs_20pc` | a line at one member's frame whose drift matches a beam aimed at the other |
| Planet-frame lines, optical | HARPS, ESPRESSO and HIRES series of about 100 transiting planets | an unresolved line on K_p sin 2 pi phi, gone in secondary eclipse; null from negative and unphysical K_p |
| Lasers in line cores, ultraviolet and Mg II | COS and STIS spectra at Mg II h and k | the optical cores are searched; the ultraviolet ones next |
| Sub-photospheric absorption | the laser-line spectra | unresolved absorption at the star's velocity, narrower than its thermal and rotational width, not interstellar, diffuse-band or telluric |
| Lines in sky fibres, DESI and integral-field cubes | DESI DR1 sky fibres; the blank sky of MaNGA and SAMI cubes | the same test; single lines tested for [OII] doublet width and Lyalpha asymmetry |
| Narrow lines in Gaia XP spectra | 219 million mean XP spectra | against a data-driven model at the same colour, magnitude and parallax; lines of 2 per cent of the flux in 10 nm |
| Polarised narrow lines | PolarBase (ESPaDOnS, NARVAL) and HARPSpol Stokes V, Q and U | an unresolved feature in V, Q or U with nothing in I; null from the N profile |
| Eclipses by dark companions | the 279 Gaia DR3 orbits of the dark-companion search | ASAS-SN, ZTF and TESS at the predicted conjunctions bound each companion's radius |
| Coherent dust streams, spacecraft detectors | Ulysses, Galileo, Cassini CDA and New Horizons SDC at PDS | one mass at one velocity vector off the interstellar inflow |
| Determinism | TESS 20 s light curves within 30 pc; TESS two-minute star-sectors of the Gaia nearby stars within 100 pc, nearest first; Kepler long cadence of the KOI hosts | the compressed length of the residual's quantile symbols, its nonlinear prediction error and its time asymmetry against 99 IAAFT surrogates once the trend, three periodic signals and flares are removed, at the native cadence and binned eightfold; more compressible or predictable by 5 sigma, deterministic but not periodic |
| Low-DM pulse trains in pulsar surveys | Parkes PMPS and HTRU-S, GBNCC, LOTAAS | DM 0.05-2, the 5-120 pc range pulsar pipelines discard as interference; delay exponent 2 and confinement to one or two beams |
| PSF-shaped flashes in TESS pixel data | TESS 20 s and 2 min target pixel files of the stars within 100 pc | the Kepler search (`kepler_psf_flashes`) carried to TESS: a one-cadence brightening with the star's pixel response and no decay, against the image shifted by one pixel and the cool stars' flare rate |
| Senders behind nearby stars | Gaia DR3 pairs with a farther star within arcminutes of a nearer one; Breakthrough Listen cadences whose beam holds both | a beam from the farther star to the nearer continues to Earth; hits re-tested in the farther star's frame at the retarded positions |
| Sky-locked Doppler tracks among interference | Breakthrough Listen hit tables, lines seen in every pointing | a sidelobe beacon's frequency follows Earth's rotation and orbit for one sky position; fitted position repeating on other days |
| Shared rest frequencies across stars | Breakthrough Listen hit tables with Gaia velocities | ON-only hits of different stars at one barycentric frequency within the velocity errors; null from permuted epochs |
| Images of flagged channels | LoTSS, MeerKAT, ASKAP WALLABY and GASKAP, VLA spectral-line visibilities | a narrowband point source in channels the flaggers removed; fringe-rate test against near-field interference |
| Sub-thermal millimetre lines | ALMA spectral windows with channels of 15 kHz or less toward stars within 150 pc | a line narrower than 30 m/s, below any molecular gas, after per-integration barycentric correction |
| Narrowband radio stars | VLASS single-epoch 16-plane cubes, RACS, LoTSS at stars within 100 pc | a co-moving source confined to one 128 MHz spectral window |
| Decade W2-W1 trends at scale | unTimely epochal unWISE photometry joined to Gaia | a rising W2-W1 colour with flat W1 and optical, against neighbours of the same magnitude |
| HI point sources at 0.18 km/s | GALFA-HI DR2, EBHIS and GASS cubes | single-channel, beam-shaped 21 cm emission at a fixed LSR velocity in every pass |
| Asteroid glints in survey photometry | ZTF and ATLAS photometry of numbered asteroids (Fink), single-frame transients | a one-frame excess of 1.5 mag over the phase and rotation curve, back on the curve in the next frame |
| Meteor alloy spectra and thrust | AMOS, Ondrejov and CAMS-S spectra; Global Meteor Network and FRIPON trajectories | Al, Ti, Li or steel ratios at 20 km/s or more; acceleration or curvature beyond drag, gravity and Coriolis |
| Radar point targets on the Moon and Venus | Arecibo-GBT and LRO Mini-RF lunar maps, Chandrayaan-2 DFSAR, Magellan FMAP | single-cell, omnidirectional returns of trihedral or plate cross-section, calibrated on the landers |
| Lines below the cutoff, further receivers | Cassini RPWS, Juno Waves, Voyager PRA and PWS, Parker Solar Probe RFS, Solar Orbiter RPW | the Wind and STEREO search carried to the outer Solar System and the inner heliosphere, with direction finding |
| Fast radio movers | VLASS epochs 1-3, RACS, LoTSS DR2, FIRST and NVSS component catalogues | compact sources on straight constant-speed tracks across three epochs above 6 arcsec/yr with no Gaia, 2MASS or WISE counterpart (a bow shock ahead of a craft at 0.01-0.1 c); null from relinking with epochs shuffled in position |
| Moving high-energy point sources | Fermi-LAT yearly slices and 4FGL unassociated sources; eROSITA DR1, the XMM slew survey and RASS | detections linked into linear tracks, with a pion-bump spectral test near 70 MeV for annihilation drives; null from slices shuffled in time |
| Nightside light, Kepler and JWST | Kepler phase curves of ultra-short-period rocky planets, CHEOPS and JWST short-wavelength phase curves | the TESS nightside search carried to Kepler's precision and JWST's band: eclipse depth minus phase amplitude above the thermal floor of under 0.1 ppm |
| Fluorinated gases, further planets | public MIRI LRS transits of rocky and sub-Neptune planets with NIRSpec companions | CF4, SF6, NF3 and CFC bands retrieved against the companion bands of CH4, NH3 and O3; K2-18 b is searched |
| Energy budgets of airless rocks | JWST MIRI eclipses and phase curves of bare rocky planets (Rocky Worlds DDT, Hot Rocks) | Bond albedo above 0.6 or a night side above 250 K without an atmosphere's CO2 band or phase offset |
| Exobelt pedestals beyond 30 days | the Kepler planets below 2 Earth radii beyond 30 d, TESS | a symmetric pedestal at 5-10 planetary radii by Delta BIC against injections; the shoulder test is searched |
| Deuterium depletion below the burning limit | JWST NIRSpec G395 spectra of cold companions with dynamical masses | CH3D/CH4 giving D/H below 5e-6 under 12 Jupiter masses; the brown dwarfs above 13 are the control |
| Monodisperse swarms | Spitzer IRS spectra of 571 debris disks (CASSIS), ISO SWS, JWST MIRI MRS | Mie interference ripples periodic in wavenumber, 100-500 cm-1, against IRS standard stars' fringes |
| Dark microlenses with mid-infrared counterparts | OGLE, MOA and KMTNet lenses with measured masses and no lens light, AllWISE, GLIMPSE, MIPSGAL | a 200-600 K blackbody at the lens position with nothing in the near infrared; control positions in the same fields |
| Information content of pulsar single pulses | Parkes, FAST and LOFAR search-mode archives of bright pulsars | block entropy and compression of pulse-energy sequences against hidden Markov and drift-preserving surrogates |
| Flux in discrete levels, TESS two-minute | SPOC two-minute light curves of the Gaia nearby stars within 100 pc, 362,656 star-sectors nearest first | the 20 s test carried to the two-minute targets: 7-sigma steps between half-hour medians, transitions within a few cadences, levels revisited |
| Grey dimming over a century | DASCH DR7 plates with Gaia, ASAS-SN and ZTF | differential slopes below -2 per cent per century in both plate halves, grey in colour, continuing to the present |
| Buried masses in lunar gravity | GRAIL GRGM1200B with LOLA topography and the magnetic maps; MRO gravity of Mars | point-mass Bouguer anomalies at 2-10 km depth uncorrelated with topography, basins or magnetisation |
| Fissiogenic nuclides in deep time | published 236U/238U and 129I/127I in ores, formation waters and sediments; ice cores | an excess over in-situ spontaneous fission in the host rock |
| Thrusted cluster escapees | Gaia DR3 6D, GALAH DR4, APOGEE DR17, Hunt and Reffert (2023) clusters | stars with a cluster's abundance fingerprint whose ballistic traceback never enters the cluster's tidal radius; null from chemical doppelgangers on the far side of the Galaxy |
| Shkadov open side | Gaia DR3 colour-magnitude diagrams of old clusters with spectroscopic temperatures and RV constancy | single stars between the twin sequence and the isochrone, too hot for any mass ratio |
| Star lifting in eclipsing binaries | DEBCat, TESS eclipsing binaries with RV orbits, Gaia DR3 double-lined solutions | the lower-mass component fitting an isochrone over 0.5 dex older than its companion, without mass transfer; the reversed sign measures model error |
| Resolved Kardashev-III fronts | Legacy Surveys, unWISE, GALEX and integral-field kinematics of 5000 galaxies within 50 Mpc | an m=1 or m=2 asymmetry in W4/r beyond the asymmetry in Halpha, FUV and optical colour, with W4/W3 near 1 |
| Nova ellipsoids, wider photometry | ZTF, ASAS-SN and TESS FFI light curves of the shells' stars without 2-minute data; Schaefer's nova distances for fainter eruptions | the same test on the stars the 2-minute sample misses; one star crossed by more than one eruption's shell is the discriminator |
| Earth-transit-zone stars at opposition, later pointings | TESS ecliptic sectors after 92 as they are released, FFIs for stars without 2-minute data | the sectors 42-46, 70-72 and 91-92 test carried to more windows |
| Rimless pits in the lunar highlands | LOLA and SLDEM2015 DEMs, LROC WAC, Robbins crater database | full-depth, flat-floored depressions without rims, ejecta or rays, 200 km from maria |
| Constant heat in the lunar night | Diviner level 3 and 4 night-time temperatures, rock abundance, LOLA slopes | a constant residual through the night against the decaying excess of rocks; the ALSEP generators as controls |
| Station-kept planetary systems | NASA Exoplanet Archive multi-planet systems, TTV posteriors, isochrone ages | posteriors unstable within 1 per cent of the age in over 99 per cent of draws (SPOCK, REBOUND), against injected stable systems |
| Mirror planets | Kepler and TESS eclipse catalogues (Esteves, Angerhausen, Wong), CHEOPS | a minimum geometric albedo above 1.5 at 3 sigma after bounding thermal emission; the Exoplanet Archive's eclipse depths shortward of 1 um are searched (`exoplanets_mirror_albedo`) |
| Planet-locked Doppler drifts | Breakthrough Listen hit tables of the TOI campaigns (Traas 2021, Franz 2022, Barrett 2025) with Exoplanet Archive ephemerides | hits at the drift a transiting planet's acceleration predicts at each scan, against the off-source scans |
| Self-luminous asteroids, raw photometry | ATLAS and ZTF photometry of the 221 edge-pinned curves, with rotation removed | a linear phase slope below 0.0179 mag/deg once the light curve is fitted |
| Co-occurrence of anomaly lists | Hephaistos II, Schmidt's dipper analogues, ZTF dippers, BL signals of interest, laser candidates, VASCO | stars on two or more lists against the hypergeometric expectation, and 3D clustering against parent-matched draws |
| Dippers' kinematic ages | Gaia DR3 and LAMOST velocities of the ZTF and TESS dippers, Schmidt's lists, KIC 8462852 | the fraction of dippers with field-star vertical velocities, against the young dust-bearing population |
| Przybylski's star half-lives | ESO UVES, HARPS, FEROS and ESPRESSO spectra of HD 101065 since 2000 | equivalent widths of Pm, Es and Ac lines against Nd II and Pr II over two decades: decay, constancy or replenishment |
| HD 139139's dip shapes | TESS 2 min and 20 s light curves, Gaia DR3 for the companion | the K2 dip rate and the ingress fraction of each dip against grazing chords and dilution; sector 91 holds no dips (`hd139139_tess`), so the test waits on a sector that does |
| Switch-offs at 150 MHz | LoTSS-DR3 mosaics against TGSS ADR1 positions, GLEAM-X and LoLSS spectra, VLASS and NVSS | compact sources above 100 mJy in 2010-2012 and below 0.5 mJy in 2014-2024 by forced photometry, against the switch-on rate measured the same way; de Ruiter et al. 2021 found none at catalogue level over half the area |
| Hot radiators without molecular bands, Euclid | Euclid Q1 NISP grism spectra and MER photometry of the ultracool-dwarf pool, with proper motions from DES, HSC and VISTA | a 500-2000 K point source with proper motion whose 1.4 um water index is zero at 5 sigma, where every brown dwarf shows the band at 20-50 per cent |
| Beacons recurring across years in Breakthrough Listen | the Breakthrough Listen hit tables and 3 Hz products of the stars observed in two or more years between 2016 and 2020 | a narrow tone at one frequency in the star's own frame on two epochs years apart, absent from the OFF scans at both; the chance of interference absent from the OFF scans twice is bounded by the ON-OFF geometry |
| Deep temporary fades in ZTF | ZTF DR23 light curves of the Gaia Catalogue of Nearby Stars within 100 pc | a star that dropped by a magnitude for weeks with g - r unchanged and returned, an occultation by something large and grey; dust clumps redden, eclipses repeat, and young stars dip on their own |
| The ten nearest systems in every method | the coverage store's rows on Proxima Centauri, Barnard's Star, Wolf 359, Lalande 21185, Sirius, Luyten's Star and the rest of the nearest systems | each method that never touched one of them run on it, past the catalogue cuts in declination, brightness and binarity that skipped them |
| Photospheres with edges in SPHEREx | the SPHEREx spectra of the stars within 25 pc (`infrared volume`) | a step or cutoff between 0.75 and 5 um that no black body with absorption makes; unresolved companions and the water bands of M dwarfs set aside |
| The hydrogen line in every Breakthrough Listen cadence | the 3 Hz products of the L-band cadences of 406 stars within 50 pc (dwarfs in Earth's transit zone, hosts of temperate planets, dwarfs within 13.8 pc, Sun-like F5-K5 dwarfs within 50 pc and other dwarfs within 30 pc): the coarse channels where the H I and OH lines arrive from a sender at rest in the CMB, Galactic, barycentric or stellar frame, 100 km/s either side | dedrifted tracks to +-20 Hz/s with a track's spread across channels summed, 7 sigma within the windows, a hit in every ON scan along one track and absent from the OFFs; the Painter et al. (2025) candidates within the windows as the check |
| Industrial gases on temperate rocky planets | JWST transmission spectra of TRAPPIST-1 e and LHS 1140 b | the K2-18 b band fits repeated on the CF4, SF6 and CFC bands |
| Night sides hotter than day sides | the Spitzer and JWST phase-curve compilations | a nightside temperature above the dayside's, which winds that shift the hot spot never produce |
| Technetium in polluted white dwarfs | SDSS and DESI DR1 white-dwarf spectra with metal lines | Tc I at 4238, 4262 and 4297 A, which decays in a few million years and so marks recent production rather than an asteroid's debris |
| White dwarfs polluted by refined metal | the published abundances of polluted white dwarfs | Ni/Fe and Cr/Fe ratios that no chondrite, core or crust gives and a steel does; core material carries its own Fe-Ni ratio |
| Supernova echoes from 1054, 1006 and Cassiopeia A | TESS 2-minute light curves of the stars on the three ellipsoids | the nova test carried to the brightest events in recorded history, whose reply ellipsoids cross stars within 500 light years |
| Breakthrough Listen's Galactic Centre data in the Centre's frame | the GBT 4-8 GHz Galactic Centre survey | the frame-predicted line tracks at the one meeting point in position as well as frequency |
| The protactinium residue on other spectrographs | ESPRESSO, UVES and HARPS-N spectra of the three HARPS stars below p 0.01 at the Pa II line | the same line score on an independent instrument |
| The grey-dimmed M dwarfs' spectra | LAMOST, SDSS and DESI spectra of the 15 stars 1.5 mag under the main sequence at disc speeds with no metallicity (`grey_dimmed_disc_stars`) | a subdwarf's hydride bands, or their absence |
| Blazar flares synchronised across the sky | the Fermi-LAT light-curve repository | simultaneous flares of unrelated blazars beyond a time-shuffled null; the repository's API did not answer |
| Switched clocks in eclipsing binaries | Kepler eclipse-timing variations | a square wave in eclipse timing, where a third body makes a sinusoid and mass transfer a parabola; the published timings are not tabulated as one catalogue |
| Exocomets without a reservoir | the comet-like asymmetric transits of TESS and Kepler; AllWISE excess and Gaia youth | a tailed body at a star with no belt to come from; belts too faint to see are the limit |
| Voyager's interstellar lines | Voyager 1 plasma-wave spectra beyond the heliopause (PDS) | a line that holds its frequency while the plasma density and its hum change; the spacecraft's own interference set aside |
| Fast X-ray transients at nearby stars | Einstein Probe transients since 2024 | against the Gaia Catalogue of Nearby Stars within 100 pc, with the shifted null; flares by the star's type |
| White-dwarf transits of constant depth | ZTF light curves of transiting white dwarfs | a shallow, long transit that repeats exactly at a white dwarf, which debris never does and a planet does at a planet's depth |
| Nulling with low entropy | public single-pulse records of nulling pulsars | a null sequence structured beyond a random process, the known quasi-periodic nullers aside |
| Interstellar absorbers that do not move with the gas | ultraviolet and optical absorption lines toward nearby stars | a velocity outside the Local Interstellar Cloud's flow, held by something that is not gas; unmapped small clouds set aside |
| Under our own radar fences | GLEAM-X at 212-220 MHz and the Breakthrough Listen files on the stars within 32 light years in the declinations the Space Fence swept at 217 MHz and BMEWS lit at 425 MHz | a reply at the carrier's own frequency from a star that has had it for decades |
| Trojan swarms of hot Jupiters | TESS light curves of the hot Jupiters | the light curve folded 60 deg ahead of and behind the planet's phase, where no natural trojan of a hot Jupiter is known |
| The positronium and fine-structure lines | the ALMA archive's cubes at nearby stars | the positronium hyperfine line at 203.389 GHz and hydrogen's line times the fine-structure constant at 194.65 GHz, with the narrow-line code |
| Eclipses as public clocks | TESS 2-minute light curves of the nearest eclipsing binaries | flashes at phase zero against every other phase |
| The hidden point | STEREO HI-1 images of Sun-Earth L3 over six years | the one place in the Solar System Earth never sees; a kilometre-sized body is the limit |
| Nucleosynthesis lines from a point | INTEGRAL/SPI public data | a point source of aluminium-26 at 1.809 MeV or of 511 keV at a star within 20 pc, against the Galaxy's diffuse glow in both |
| Industrial molecules in the clouds | the unidentified lines of the Sgr B2 and TMC-1 line surveys | against the rotational spectra of CFC-11 and CFC-12, which need laboratory line lists first |
| The shape of the noise | TESS residuals of the nearest stars against matched distant ones | the kurtosis of the residuals, a population test for pulses below any threshold |
| The one list | the coverage store | every star's results across every test combined into one likelihood ratio against the natural model, a ranked follow-up list of the ten strangest |
| Asteroid non-gravitational accelerations | Gaia DR4 | December 2026 |
| DESI second epoch | DESI DR2 | not yet public |
| Umbra flashes and GEO lurkers | Global Meteor Network, GEO lists | GEO lists not public |
| Pulsar-survey rejects, SETI@home candidates, DSN recordings, maser monitoring, Auger triggers, CTBTO detections | | not public |
| Companions read out of their stars' spectra | the ESO archive's best-observed stars: 471 series of a hundred or more HARPS, ESPRESSO, NIRPS, UVES or CRIRES spectra spanning a year or more, up to 300 spectra a star spread over its span; an M dwarf's HARPS spectrum from the archive (GJ 367) as the companion template in the optical | each spectrum on a grid uniform in velocity in the primary's own frame, so the primary's lines cancel whatever its reflex motion, its running median and the series' median divided out, whitened; the template's inverse-variance cross-correlation with every spectrum, the primary's own pattern taken out of each row at its own strength and five principal components of the rows after it; the trail summed along every orbit of a grid in period (at a periodogram's resolution from half the span, two cycles at least, down to half a day), phase and amplitude from 30 km/s, readings within 25 km/s of the primary left out and periods the sampling keeps at one phase set aside; the summit against the summits of the same grid with the epochs shuffled; a tenth-per-cent M dwarf injected into tau Ceti's 300 HARPS spectra on a 7.3-day orbit at 40 km/s is recovered at its period and amplitude at 7.0 sigma, the blind search of the same spectra at -0.7 |

## Findings

Results about natural objects, instruments and catalogues that the searches produced, each with the run that found it.

| Finding | Run | Status |
|---|---|---|
| (883607) 2016 TA56, a candidate dark comet on a Jupiter-family orbit: a transverse non-gravitational acceleration A2 of -3.45e-12 +- 0.37e-12 au/d^2 (9 sigma with the 2007 night as one position) on a body of 2.4 km and albedo 0.017, 15-39 times all absorbed sunlight at 1000 kg/m^3; the two orbits part by 4-7 arcsec in 2030 August-September | `darkcomet_2016_ta56` | papers/dark_comet |
| 2016 YB13, a transient retrograde co-orbital of Jupiter not in the literature: inclination 140 deg, eccentricity 0.41, semi-major axis 5.46 au on a 642-day arc with a formal eccentricity error of 2e-6; the nominal orbit and fifty clones of its covariance integrated with the four giant planets (hybrid integrator, step 0.05 yr) hold Jupiter's semi-major axis without an approach inside 0.5 au for 7 kyr each way from the nominal orbit, for a median of 3 kyr forward (10th to 90th percentile 1-27 kyr) and 13 kyr backward (6-31 kyr) over the clones, with 2 of 50 still held at -100 kyr and none at +100 kyr, while the control (514107) Ka'epaoka'awela holds for the whole 100 kyr each way and never comes within 0.7 au; a Jupiter-crosser of that eccentricity outside the resonance meets the planet within a few kyr; the resonant angle was not established under the conventions tried | `sbdb_retrograde_coorbitals` | a transient member of the resonance on a 10 kyr timescale, which the published cases of such capture explain; a dynamics note would need the angle and the capture history |
| PSR J1420-6048's glitch schedule has lapsed: the eight glitches of the Jodrell Bank table from MJD 51600 to 58555 come at intervals of 994 +- 196 days, a scatter random intervals give once in four thousand draws, and the published intervals of two to three years agree; the schedule put the ninth glitch at MJD 59549 +- 196, and the table, complete to MJD 60980, lists none, a gap of 2425 days, nearly twice the longest before it | `jbo_glitch_schedules` | the vet stands as a young pulsar of Vela's kind; the next glitch, when it comes, dates the lapse |
| Ma et al. (2023)'s eight Breakthrough Listen signals of interest: MLc2-MLc8 lie on their own lines in their cadences' OFF scans and MLc3-MLc8 in other stars' pointings; MLc8 is one terrestrial carrier rising 1.72 kHz over four hours through four other stars' cadences; the published table's drift signs run opposite to df/dt and its MJD column holds GUPPI scan labels | `bl_soi` | papers/ml_signals |
| HD 31435's 5.48 per cent polarisation (Moneti et al. 1984) belongs to another star: the star's photometry, astrometry, spectrum and infrared allow no polariser, and the field behind the cloud gives the measured angle | `intrinsic_polarisation` | papers/hd31435 |
| KIC 2557430 (KOI-6277): the published surface temperatures run too hot; Gaia resolves WDS J19074+3749AB into the eclipsing pair at 6130 K and a co-moving K star whose luminosities sum to the light observed | `debs_missing_flux` | papers/kic2557430 |
| Wind/WAVES RAD1 measured only 32 to 38 of its 256 channels in nearly every minute of every year, and the archive interpolates the rest | `wind_rad1_2020` | papers/subcutoff_radio |
| 154 emission-line galaxies at z 0.016-1.069 identified in SDSS sky fibres by two or more lines, 122 of them with a Legacy Surveys source of median r 23.1; the line at 4732.6 A on 54 plate-nights in the SDSS-RM field is Lyman alpha at z 2.893 | `sdss_sky_fibres_shared2` | papers/sky_fibres |
| Five DESI DR1 white dwarfs with unblended infrared excess 1.6-3.3 mag above the photosphere in W1 and black-body temperatures of 900-1500 K, the excess of unresolved brown-dwarf companions | `desi_wd_dust_pollution` | candidates |
| Gaia DR3 eclipsing-binary depths and periods that fail: TYC 4267-1042-1, TYC 7438-551-1 and BD+09 1746 are flat in TESS to 0.1-0.3 mag against model depths of 0.77-1.73 mag, two more stars flat in ZTF, and 15 Eri's 4.4 mag model depth is saturation | `lightweight_eclipsers` | catalogue corrections |
| Gaia DR3 short-timescale box transits on ten main-sequence stars are absent from ZTF g and r at 0.45-2.2 times the Gaia period: Gaia's periods or depths | `roche_transits` | catalogue corrections |
| NVSS gives polarised flux at or above the total for 23 sources in Fornax A's lobes and fields of the Galactic plane, where the field's diffuse polarisation enters | `nvss_polarisation_ceiling` | catalogue artefact |
| GLEAM-X J082817.6-221400's 35 per cent spectral step: a 1.18 Jy source 69 arcsec away inside the low-frequency beam, the sub-band fits merging and splitting the pair | `gleamx_edges` | catalogue artefact |
| Kepler catalogue durations short of the light curves: KOI-4371.01 (8.6 h against 11.1), KOI-6343.01, KOI-5227.01, KOI-2086.04, KOI-7954.01 and KOI-719.03; KOI-3436.01's transit times scatter by 735 min and its fold at the catalogue ephemeris brightens | `exobelts_kepler_long` | catalogue corrections |
| GJ 725 A: an isolated 100 ms near-ultraviolet brightening, 7 photons against 0.2 expected, fixed to the star in rebuilt detector coordinates, in the star's only GALEX photon list | `galex_nuv_pulses` | open |
| HD 101805 (F8V, 34 pc, 3.9 Gyr): 223 ppm of linear polarisation at 9 deg, rising from 172 ppm in R to 314 in B, where neighbours within 35 pc read 12-45 ppm | `polarised_reflectors` | open; Gemini/GHOST spectra from 2027 July |
| The stars within 100 pc at rest with the Sun: two members of Crius 131 (Moranta et al. 2022), an association moving at 1.8 km/s relative to the Sun, the 0.3 Gyr star BD+68 1331, PG 0943+489 (RUWE 1.53) and a K dwarf at 0.98 km/s; counted as systems, 4.3 per cent of balls of the same density elsewhere in velocity space hold as many | `gaia_rest_stars` | explained |
| Gaia DR2 holds no source for Lalande 21185 and three other stars within 100 pc at G below 17 moving faster than 585 mas/yr, nor for 90 stars 2-7 arcsec from a star 1-11 mag brighter, all of which DR3 catalogues; DR3 in turn holds iota Leo B (G 6.8, 2.1 arcsec from iota Leo) and chi Eri B (G 9.7, 2.5 arcsec from chi Eri) as no source of their own, both catalogued by DR2 | `gaia_dr3_appeared`, `gaia_dr2_vanished` | catalogue property |
| GALAH DR4 lithium of cool dwarfs: 18 of the 135 dwarfs below 5300 K listed with a clean A(Li) above 2.0 and isochrone ages above 6 Gyr show no Li I 6708 line in their own spectra where the catalogue gives 113-600 mA, a line the refit recovers in 134 of 135 injections at the same S/N; the highest, Gaia DR3 3910691559800909568, listed at A(Li) 3.69 (401 mA), measures 17 +- 28 mA; the 95 real lines belong to young stars and binaries whose isochrone ages are wrong | `galah_lithium_old_dwarfs` | catalogue corrections |
| HERMES camera I records round spots of 1.5-1.7 million electrons, the charge 5.3-6.2 MeV releases in silicon (the energies of alpha particles), about 4 px across like light through the spectrograph; in an observation of one exposure GALAH DR4 passes one into a spectrum as an emission line 21 times the continuum (Gaia DR3 609133088216624000, 7790.24 A rest, 2017 January 2, fibre 47), the spot 2.2 px from the fibre's trace, where the arc lines fall within 0.6 px | `laser_galah` | instrument artefact |
| CNEOS fireballs since 2018 faster than the Sun lets anything bound move: 2026-04-01 02:13:14 UTC over the South Atlantic (41.9 S, 54.7 W, 90.5 km), 69.2 km/s at entry and 51.8 km/s heliocentric against the 42.1 km/s escape speed; 2022-07-28 01:36:07 UTC (CNEOS-22 of Cloete and Loeb 2026), 47.4 against 41.8 km/s; 2021-05-06 05:54:26 UTC, 43.7 against 41.9 km/s; none bound in 20,000 draws within the post-2018 errors Peña-Asensio et al. (2025) measured against ground-based networks; the 2026 event is not in the published candidate lists, and CNEOS-25 (2025-02-12), listed as hyperbolic by Cloete and Loeb, is bound at 37.4 km/s from the database's present entry; the GOES lightning mappers saw both that fell in their view, 2026-04-01 from GOES-19 0.7 s and 144 km from the CNEOS fix for 1.1 s, and 2022-07-28 from GOES-16 and GOES-17, whose triangulated trail runs at 18.4 km/s from 42 to 33 km, 0.61 of the CNEOS speed, where the mappers' trail speeds on 16 slower fireballs run at 0.66-1.65 of CNEOS's; no Global Meteor Network camera recorded any of the 360 CNEOS fireballs | `cneos_hyperbolic_fireballs`, `cneos_glm_bolides`, `cneos_gmn_trajectories` | the sightings fix both events' times and places; the mappers' trail speeds scatter too widely to test a 21 per cent excess and no camera network saw them, so an infrasound or seismometer record would settle a speed |
| 22 compact radio sources of 65-890 mJy at 4.8 GHz, more than 30 deg from the Galactic plane, with nothing in AllWISE, CatWISE2020, unWISE, Pan-STARRS1 or the Legacy Surveys DR10 within 2-3 arcsec of positions VLASS confirms, so above 5,000 in radio-to-infrared flux ratio, beyond the infrared-faint radio sources; 17 are VLBI-compact, and their spectra are peaked or steep more often and flat less often than hosted sources' (8 of 22 flat against 124 of 200), the signature of young compact radio galaxies rather than beamed quasars; none shows in VHS, VIKING or UKIDSS, the 15 those cover fainter than K 18.1, beyond redshift 1.5 on the K-z relation of radio galaxies | `crates_hostless_flat_spectrum`, `crates_hostless_seds`, `crates_hostless_nir` | a sample of candidate young radio galaxies beyond redshift 1.5; K-band imaging deeper than 20 or a radio redshift from HI or OH absorption would place them |
| Nearby M dwarfs too faint for their colour: 18 mid-M dwarfs at 30-53 pc, G 13-16, lie 0.36-1.0 mag below the main sequence at fixed G-RP, with parallaxes measured to 0.1 per cent, concentrated at high Galactic latitude (median 64 deg against 25) and moving faster than their peers (median 45 km/s, two at 119 and 132), with no companion, activity or ultraviolet sign; the three with spectra show the CaH and TiO bands of ordinary metallicity (zeta 1.01-1.12), while the one further 2.3 mag below is a subdwarf (zeta 0.56); Gaia's GSP-Phot fits them worst of all nearby M dwarfs | `gaia_xp_worst_fits_nearby`, `gaia_xp_misfit_traits`, `gaia_xp_misfit_spectra`, `gaia_xp_misfit_subdwarf_indices` | open: mildly metal-poor old disc stars above the subdwarf threshold would sit this low, which a metallicity from new spectra of the other 15 would test; at ordinary metallicity, 30-60 per cent too little light for their colour has no explanation in hand |
| The densest pile of clean unassociated Fermi-LAT sources in the inner plane, 7 within 2 deg of l 312.1 deg (the Galactic bar's L5 line of sight and the Crux-Centaurus tangent) against a mean of 1.3, sits around the Kookaburra and Rabbit nebulae: a random forest trained on 3,946 associated sources classes none of its 5 measurable members as a pulsar, against a quarter of the plane's other unassociated sources; four are steady uncurved power laws and the fifth is the extended FGES J1409.1-6121; only 1 of the 7 lies inside a H.E.S.S. source, HESS J1418-609, the plane's own rate, and the rest sit outside every TeV glow, most 0.5-1.6 deg above the plane; they sit on more dust than their latitudes' share (median rank 0.69, p 0.038) | `fermi_bar_lagrange_points`, `fermi_unassociated_pile_classes`, `fermi_unassociated_in_tev_glows`, `fermi_pile_dust` | not pulsars and not inside the TeV-bright nebulae; unexplained, and a dedicated LAT fit of the region with the gas maps would say whether they are emission the diffuse model misses |

## Confirmation

| Candidate | Next step |
|---|---|
| Infrared excess | JWST MIRI spectrum, then interferometry |
| Radio point source | VLBI, Breakthrough Listen at Hz resolution, a second site |
| Line below the ionospheric cutoff | STEREO/WAVES direction finding at the line's epochs |
| Optical trend or transient | present-day photometry; SPHEREx for where the light went |
| Chemistry | high-resolution spectroscopy of isotopes |
| Polarised star | one modern polarimetric measurement at 0.1 per cent, then the angle against the field's |
| Solar-system object | radar, then a flyby |

`python -I seti.py store card <target>` gives one target's results across every method.