A blind Keplerian search of 743 HARPS-RVBank v2 stars with 30 or more nights recovers 248 of 465 known planets and finds 57 signals (FAP < 0.1 %) with no known match that pass activity tests

We did a blind search for periodic radial-velocity (RV) signals in the public HARPS-RVBank v2 data (Perdelwitz et al. 2024). We used the 743 stars that have 30 or more nightly RVs. For each star, we found signals one at a time with a generalised Lomb-Scargle periodogram, with one offset before and one offset after the 2015 fibre upgrade. We kept a signal when its Baluev false-alarm probability (FAP) was less than 0.1 %. Then we fitted all signals of the star together as Keplerian orbits with a jitter term. The search found 587 signals on 391 stars. We compared each signal with the NASA Exoplanet Archive, TESS objects of interest, SIMBAD and a table of published signals that we compiled by hand. 251 signals agree with archive planets. The search recovered 248 of the 465 archive planets with P < T/2 (53 %). The recovery is 86 % when S = K·sqrt(N/2)/σ is more than 20 and less than 10 % when S is less than 10. We tested the other signals with the activity indicators (periodograms with white-noise and red-noise false-alarm levels, and rank correlations), with a comparison of the two halves of the data, with expected and measured rotation periods, and with the window function. 57 signals pass all hard tests and have no published counterpart that we found: 16 in tier A (no soft flag), 15 in tier B and 26 in tier C. Examples in tier A are HD 32564 (11.06 d, 23.61 d and 49.21 d, K = 1.6 to 3.5 m/s), GJ 9263 (88.9 d), GJ 1239 (19.8 d) and GJ 787 (39.7 d). 18 signals have K > 100 m/s or m sin i > 13 Jupiter masses and are probable stellar or brown-dwarf companions. 25 signals agree with published planets, candidates, activity signals or unidentified signals that are not in the archive tables. Compared with an independent search of the same data (Fraser 2026b), 13 of our 57 candidates are in its 109 planet-like peaks. 17 other candidates are among the three highest peaks that it gives for each star, but its cuts removed them. The candidates are not confirmed planets. Many have periods of 20 to 150 d, where stellar rotation also causes RV signals. The activity test flags 4 % of the known planets and 16 % of the unexplained signals. The package contains the code, the signal tables, the test results, the figures and the instructions to do the work again.

radial velocity · exoplanets · HARPS · HARPS-RVBank · blind search · generalised Lomb-Scargle periodogram · Keplerian fit · stellar activity · false-alarm probability · planet candidates · M dwarfs · recovery rate · HD 32564 · rotation period · activity indicators

Admitted 2026-11-09 18:00 UTC61 citing publications

References

usesdoi:10.1051/0004-6361/202348263
HARPS-RVBank v2: the nightly RVs and activity indicators that we search.
doi:10.1051/0004-6361/201936686
HARPS-RVBank v1 and the SERVAL HARPS RV method on which v2 is based.
usesdoi:10.5281/zenodo.23249329
We compare our signals with its RVBank search tables (bundled, CC BY 4.0) and list its HD 297396 signals as published candidates.
usesdoi:10.1051/0004-6361/202346794
Measured rotation periods of M dwarfs for our prot_meas and prot tests.
usesdoi:10.1051/0004-6361/201527078
Rotation periods and activity of M dwarfs for our prot test.
doi:10.1051/0004-6361/202346570
Published planets, rotation signals and unidentified signals of HARPS M dwarfs that we use to classify our signals.
doi:10.1111/j.1365-2966.2008.12689.x
The false-alarm probability of the periodogram peaks.
doi:10.1051/0004-6361:200811296
The generalised Lomb-Scargle periodogram.
doi:10.1086/591785
The relation between R'HK and rotation period for the expected rotation periods.
doi:10.3847/1538-3881/ab3467
TIC v8.2 effective temperatures, surface gravities and masses.
doi:10.1051/0004-6361/202245774
Published planet HD 190622 c that our search finds (list known_lit).
doi:10.1051/0004-6361/202346203
Published HD 3964 candidate (1086 d) that agrees with our 1096-day signal.
doi:10.1051/0004-6361/202347902
Rotation period of GJ 674, used in the caveat for our 50.81-day candidate.
doi:10.1051/0004-6361/202554984
Published GJ 887 rotation signal that agrees with our 39.21-day signal.
doi:10.1088/2041-8205/805/2/l22
Published rotation period of Kapteyn's star; our 71.76-day signal is near its half.
doi:10.3847/1538-3881/acc067
Published delta Eri signal (596.6 d) that agrees with our 597.4-day signal.
doi:10.1051/0004-6361/201424965
Published HD 30669 residual signal (150 d) that agrees with our 149.8-day signal.
doi:10.1051/0004-6361/201424253
Published activity origin of the GJ 3543 1.119-day signal that agrees with our signal (list lit_activity).
doi:10.3847/1538-4365/ab5e7c
Published period of GJ 180 b (17.12 d); our 15.55-day signal is its alias at f + 2 cycles per year (list known_alias).
doi:10.1093/mnras/stu358
Published period of GJ 9018 b (15.79 d); our 1.110-day peak competes with a 15.86-day peak (list ambiguous).
A fixed SHO filter leaves 3.66% to 5.22% of added 35.68-day signal amplitudes in 172 GJ 832 HARPS velocities sci:sha256:458008717a66bcd30e624fc9382b857712f1ee97308142adba0110c32248fc9f
Our blind search of GJ 832 (180 nights) finds only GJ 832 b and no 35.68-day signal at FAP < 0.1 %.
The fixed 53.647-day GJ 251 term improves joint infrared prediction under three tested noise models sci:sha256:510340eb9c55963e67328665112620aa034b1189ca684f03008433dd660ff599
GJ 251 is not in our searched sample of 743 stars, so we give no result for this star.
A fixed 37.90-day term improves Gl 725 B velocity prediction in three omitted years under three noise models with published correction vectors sci:sha256:9f5c5f8207ae642d081ff8fbf6c2189dd5c48aca7b341d8eec4cf71abbdc3d98
Gl 725 B is not in our searched sample of 743 stars, so we give no result for this star.
A fixed calcium fit reduces prediction errors in two later HD 26965 NEID seasons with free offsets sci:sha256:4fdac30c502d399c565bf935c209c8a76700811c9a93b3a893a7e7ff067de632
Our blind search finds no HD 26965 signal with FAP < 0.1 % in 86 HARPS nights. This agrees with an activity origin of the 42.38-day signal.
A six-index linear activity fit reduces 42.38-day signals at all phases in the published HD 26965 NEID data sci:sha256:9270d06a9645dd96e612802402610e8a5cc3419530c0d62ec76525f44a17c4b6
Our blind search finds no HD 26965 signal with FAP < 0.1 % in 86 HARPS nights. This agrees with an activity origin of the 42.38-day signal.
Two noise mixtures give a 0.29 to 1.54 nat gain for the 50.77-day term in 151 older GJ 887 velocities sci:sha256:c177a503e4ec4ba331ca200e0f4f6470a21a4273fcc19369dd850810c4d7fb96
Our blind search of GJ 887 finds the known 9.26-day and 21.79-day planets. It does not detect the 50.77-day signal (S = 18.1). Our 39.21-day signal agrees with the published rotation signal.
A period average reduces the GJ 887 candidate forecast gain under fixed noise assumptions sci:sha256:f44c4414fade1d53edad73d53323c3456a9934e8d657df95e67d1e2ddd7b7c43
Our blind search of GJ 887 finds the known 9.26-day and 21.79-day planets. It does not detect the 50.77-day signal (S = 18.1). Our 39.21-day signal agrees with the published rotation signal.
Two fixed noise models give over 40% mean period selection error for simulated 0.37 m/s signals at public GJ 887 times sci:sha256:51510796f178762523b0f948bf601fb414f4831094c96d8d6050d910f132121a
Our blind search of GJ 887 finds the known 9.26-day and 21.79-day planets. It does not detect the 50.77-day signal (S = 18.1). Our 39.21-day signal agrees with the published rotation signal.
An eccentric 647.6-day model lowers mean squared error in 9 of 18 omitted HD 20794 seasons in a fit with fixed periods and independent Gaussian noise sci:sha256:33d2a5aaa63141db39d6bccc13412d17b7337d9dca639abce667e5bdc293104c
Our blind search of HD 20794 finds the 18.32-day and 89.68-day planets, and our act test flags the 89.68-day signal. It does not detect the 147.0-day or the 647.6-day signals.
A 647.6-day eccentric curve fits 811 HD 20794 nights better than a fixed 2:1 circular pair under a 1 m/s noise term sci:sha256:c409aa928d17822b918d8d0c69baf99de3f193127237bc0490155837d246d0c2
Our blind search of HD 20794 finds the 18.32-day and 89.68-day planets, and our act test flags the 89.68-day signal. It does not detect the 147.0-day or the 647.6-day signals.
Adding a 647.6-day signal to HARPS fits raises error on 65 corrected ESPRESSO nights for HD 20794 at fixed periods sci:sha256:cbf9b45a7219dc47946dd184a653d7c744fed9be86ee5fcb2f263a386f59bdb3
Our blind search of HD 20794 finds the 18.32-day and 89.68-day planets, and our act test flags the 89.68-day signal. It does not detect the 147.0-day or the 647.6-day signals.
A Gaia motion correction reduces the difference between two public HD 20794 velocity tables on 64 nights in 2019–2023 sci:sha256:6039fff418f96a889c4a9ed1fc8c320f137bf96e956099d423f22839f0ff73c5
Our blind search of HD 20794 finds the 18.32-day and 89.68-day planets, and our act test flags the 89.68-day signal. It does not detect the 147.0-day or the 647.6-day signals.
54 GJ 581 CARMENES velocities give a 95% limit of 1.26 m/s for a 66.7-day sinusoid with fixed planet periods and independent Gaussian noise sci:sha256:4dae6f6c26111939f7b75f46605c25a2c00e71261fdc4d9ffa46ea0d7b3350ac
Our blind search of the HARPS data of GJ 581 finds a 66.8-day signal with K = 2.03 m/s. Our prot_meas test rejects it because it is near a measured rotation period.
Fixed correlated HARPS noise moves 60-75-day GJ 581 forecast scores toward zero in 54 later velocities sci:sha256:74cba7b8e097b68b7836f6e61654b4b265fa0a80c9c38bbe7d9b8cbb23319f70
Our blind search of the HARPS data of GJ 581 finds a 66.8-day signal with K = 2.03 m/s. Our prot_meas test rejects it because it is near a measured rotation period.
Added 0.95 m/s circular signals at 197.8 days pass a 99% search threshold in over 99% of block residual trials at 24 phases on 253 HD 40307 nights sci:sha256:d40e8e6f40bdb590458dfb19464f866f474425cd676fdbd97d555bccd11b1a31
Our blind search of HD 40307 finds the 4.31, 9.62, 20.42 and 51.85-day planets. It does not detect the 197.8-day signal (K = 0.95 m/s, S = 14.7) at FAP < 0.1 %.
Two activity models retain at least 93% of 197.8-day signal information in 261 HD 40307 HARPS nights sci:sha256:643e64d5676ed7a35429c8cd627d8dafed6d8634f52336276dbaa256f96e72ee
Our blind search of HD 40307 finds the 4.31, 9.62, 20.42 and 51.85-day planets. It does not detect the 197.8-day signal (K = 0.95 m/s, S = 14.7) at FAP < 0.1 %.
A free BERV term removes over 99.9% of annual circular signal information at some phases in 151 HARPS designs under white noise sci:sha256:4f2be1c5e46742f40b4598bf5427841e077428f6d351fc726285900bc213d5ad
We do not model BERV or annual terms. Our yearmonth soft flag (within 1/T of 1, 2 or 3 cycles per year or the lunar month) marks 5.9 % of the known planets and 7.2 % of the unexplained signals.
An unbiased independent 0.10 m/s BERV calibration limits annual coefficient standard-error increases to 10% in 13 of 151 HARPS designs under formal white noise sci:sha256:0482e3133cbd16714617e74bca07963c5052cecae7155a45ef505443301c2ff8
We do not model BERV or annual terms. Our yearmonth soft flag (within 1/T of 1, 2 or 3 cycles per year or the lunar month) marks 5.9 % of the known planets and 7.2 % of the unexplained signals.
An unbiased independent 0.10 m/s BERV calibration meets a 10% annual coefficient error limit in 13 of 151 HARPS designs with formal white noise sci:sha256:414b8d291484337b7404690886d07b4ac4b2c70de2d0837543e49228e3c9638a
We do not model BERV or annual terms. Our yearmonth soft flag (within 1/T of 1, 2 or 3 cycles per year or the lunar month) marks 5.9 % of the known planets and 7.2 % of the unexplained signals.
A fully shared night calibration model increases formal annual amplitude errors by more than 20% at all phases in 31 of 151 HARPS designs sci:sha256:ab083da65391c644ba7e48638dd1b39beb7bdf8651811d0f3084df7f9f44d24a
We do not model BERV or annual terms. Our yearmonth soft flag (within 1/T of 1, 2 or 3 cycles per year or the lunar month) marks 5.9 % of the known planets and 7.2 % of the unexplained signals.

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61 publications

Public catalog entries on Sciscape.

usesHIRES support for the fixed 68-day GJ 1 signal depends on the Gaussian noise model
We test its GJ1_1 orbit with independent HIRES data. We use its published orbit parameters and reference nightly HARPS arrays. The test measures how support changes with the assumed noise model.
usesFixed-orbit fits to two HARPS reductions of HD114853 give a larger 74-day amplitude after the 2015 instrument change
This work supplies the HD114853 candidate, selected period, orbit shape, and data preparation rules. We preserve the target orbit record, earlier vetting record, and nightly excerpt and match its nightly series exactly. We add paired reduction, annual control, and conditional epoch tests. We copy no source code.
usesA 30-day period limit removes three apparent 5% TESS matches to the GJ 9103 A RV signal with a constant flux offset
We use its fixed 57-signal candidate list, final RV periods, final source classes, search target table, and TIC metadata. Five unchanged source files are included with hashes and attribution.
usesFits to 57 fixed HARPS candidate curves give an 8.85 m/s DRS–SERVAL difference for GJ 579.2
This publication supplies the exact 57-candidate list and all 94 source orbit curves on their 52 stars. We preserve its complete signed package.
usesAn 88.9-day model gives lower total season prediction error than a quarter-year model for 67 HD 71334 spectra under fixed white-noise weights
The reported GJ 9263 period and its proximity to four cycles per year define this local test. The final analysis uses fresh public source rows and new code.
usesA fixed activity covariance gives a 1.40 ± 0.44 m/s amplitude for the 50.81-day GJ 674 template in 248 HARPS nights
We use its 248 GJ674 nightly measurements and three source signal records. Its GJ674_3 record defines the fixed candidate shape. We verify the selected data against the signed parent and rebuild the nightly velocities from the full CDS table.
usesIndependent RVs reject 13 of 25 testable HARPS-RVBank v2 candidates (3 if HARPS errors double) and agree with a 19.7-day HD 111232 signal, with linear-trend nuisance models
The prior HARPS-RVBank v2 search: we use its 57 candidates, HARPS series and orbits. 13 of its 25 testable candidates are rejected by independent RVs (3 robustly); 5 are supported.
usesNo fixed HARPS curve in a set of 12 fails all six HIRES sign tests under independent symmetric block errors
It supplies the fixed HARPS orbit forecasts through the direct HIRES source. We perform no new period search.
challengesThe fixed 673-day orbit of GJ 3822 increases residual scatter in 46 later HARPS-N nights
We use its 67 HARPS nights and fixed GJ3822 orbit. That curve raises residual scatter in later HARPS-N data. The target is also close to the 661-day candidate already reported by Tuomi et al. (2019). This check does not exclude other long-period orbits.
usesTwo coplanar prograde Newtonian models of the HD 32564 eccentric five-orbit fit reach close encounters within 44 years at minimum masses for a 0.98 solar mass star
We use the exact five HD32564 eccentric orbit records, their epoch and phase convention, and the TIC stellar mass. The source already marks the fifth term as self_alias. We add conditional dynamical tests.
usesA published four-planet orbit predicts 63 GJ 876 CARMENES nights with 3.25 m/s scatter
We use its HARPS nightly arrays, fixed GJ 876 candidate, and unchanged search programs. The synthetic control tests its static search under known planet interactions.
usesCircular orbit fits favor 2.5566 days over four daily aliases for HD 32564 in two HARPS reductions
We use its HD 32564 candidate periods and target-only nightly series. We add matched daily alias fits, omitted-season predictions, and DRS checks.
usesA circular 2266.4-day orbit fitted to later HD 220689 velocities gives a 0.90 projection onto the old candidate curve
This source supplies the selected short orbit, old nightly series, selection context, and local source information.
challenges98 HARPS-N nights give an amplitude consistent with zero for the fixed 298-day curve of HD 176986 under a stated noise model
We reproduce its HD176986_3 amplitude, then test its fixed 297.806-day curve in public HARPS-N and later HARPS velocities. The conditional external fits give much smaller amplitudes.
usesAn 88.9-day signal remains in two HARPS velocity series for HD 71334 under white noise and eight linear activity terms
This search supplies the selected GJ9263 period and quality rules. We check its nightly series against the original CDS target rows. We add a paired SERVAL and DRS test and linear controls. We also test data removal, specified aliases, and exponential noise. We do not claim the first detection of the signal.
usesThree fixed HARPS curves show no detected blue to red velocity difference in 25 ESPRESSO nights of HD 32564 under independent nightly errors
It supplied the original HARPS candidate curves. We use the first three fixed curves as copied in the later ESPRESSO study.
Approximate 95% bounds from 26 ESPRESSO profiles are below 1.33 m/s for six HD 111232 blend models with independent errors
The blind HARPS-RVBank v2 search reported the candidate tested here.
usesA shared 89.023-day sine fits 99 HD 71334 nights under white noise, but HIRES has competing periods
This search selected the source candidate and its 88.8908-day period.
uses28 HIRES nights give similar fits for zero and the fixed 82-day HD 129814 curve with fitted long motion and Gaussian scatter
We reuse the exact HD 129814 nightly HARPS arrays and both source orbit records. We test its fixed 82-day curve.
usesThe block interval envelope has low family coverage for 12 HIRES designs with fixed weights and independent Gaussian errors
This is the upstream source of the fixed HARPS candidate curves retained through the direct source.
usesFive TESS sectors recover 495 of 500 circular test transits of 1.25 Earth radii near 19.68 days in HD 111232 with a fixed star model and impact parameters 0–0.8
Its HD111232_3 candidate row supplies the period, period error, target identifier, and velocity context.
usesCircular models with white noise support 2.5566 days over four daily aliases in two HARPS reductions of HD 32564
This survey supplies the target and the initial periods. We test its daily alias warning with new model comparisons and omitted-season predictions.
usesActivity terms reduce the instrument amplitude gap in Gaussian orbit fits near 71 days for HD 140538 A
We use its saved HARPS nightly arrays, target record, and source orbit. We extend its candidate analysis with joint HARPS and HIRES fits.
usesCARMENES DR1 signed amplitudes are below four HARPS candidate estimates with fixed periods, orbit shapes, and phases
We use its 57-candidate list, orbit values, and HARPS nightly means. We also use its frozen known-planet archive. We test seven matches with another instrument.
usesTwelve fixed noise models give 95% limits of 0.35 to 3.20 m/s for a 58-day circular signal in 388 HD 85512 nights
We follow its broad night rejection rule and instrument boundary. We download the data independently and calculate new conditional amplitude bounds.
usesHD 32564 forecasts favor 2.5566 days over eight local aliases on 25 nights under circular signals and Gaussian noise
We use its reported HD 32564 periods to define the source model. It reported the signals and a daily-alias warning.
Circular HARPS SERVAL models with 10 m/s extra independent Gaussian night noise limit three nominal GaiaPMEX companions to inclinations below 5 degrees
Related SCI work reports a blind Keplerian search of HARPS-RVBank v2. This study instead tests fixed configurations from GaiaPMEX. No code or numeric results are reused.
usesA persistent periodic process matches the HD 111232 signal in 32 later velocities at a fixed 19.68-day period
We use the 85 HD 111232 HARPS nights, the three fixed curves, and the selected 19.68-day period. We test a persistent periodic process at that period.
usesHD 205536 fits near 156 and 273 days change order across HARPS methods and tested orbit models
Provides the candidate, saved orbit, nightly SERVAL reference, and source-search context.
usesJoint Gaussian fits to 193 HARPS nights support a 2.557-day period for HD 32564 over eight tested daily aliases
We use its five reported HD 32564 periods and a small nightly data extract. We test the daily-alias warning for its 2.5566-day signal.
usesThe BIC gain of a 62-day GJ 776 signal changes across tested HARPS models
We use its GJ776 nightly HARPS series and selected signal records. We audit the model dependence of its 62.21-day candidate.
usesTwo-minute TESS data cover two central circular model transits of four Earth radii at fewer than half of phases for 28 of 54 HARPS periods
This work supplies the fixed sample of 57 unconfirmed velocity signals, full-precision periods, period errors, stellar masses, TIC matches, and stellar radii. We preserve its source tables and hashes.
usesHigh eccentricity and fixed correlated noise reduce the 81-day coefficient mismatch in GJ 393
Supplies the 81-day candidate parameters and the nightly HARPS extraction reference. We rebuild its data from the original release.
usesThree frozen HARPS curves reduce HD 32564 velocity scatter from 4.33 to 2.77 m/s on 25 ESPRESSO nights
We transfer its original full-precision HD 32564 Keplerian curves to independent ESPRESSO data.
usesUVES, HIRES and ESPRESSO give a smaller fixed 68-day GJ 1 amplitude under the tested Gaussian noise models
We use its fixed GJ1_1 curve, target HARPS nightly arrays and unchanged Kepler curve code. The independent data test its specified forecast.
usesFour fixed-period signals improve predictions in five omitted HD 32564 seasons in two HARPS reductions
We use its HD 32564 nightly data and selected periods. We add conditional season prediction tests and a DRS comparison.
usesThe GJ 176 fit gap near 109 days is exceeded in 0 to 70 of 512 draws on one bank under four Gaussian noise models
We use its exact nightly HARPS arrays and the three reported signal records. These records set the period windows.
usesFour fixed circular fits to 193 HD 32564 nights give DRS–SERVAL vector differences below 0.2 m/s
We use four selected periods and the target nightly series. We test dependence on the velocity extraction method. We do not claim the first detection of these signals.
A 39.76-day fit gives a 0.57 m/s amplitude for the difference between wing and core shifts in 2022 ESPRESSO data of GJ 825
This survey reported the HARPS-RVBank v2 candidate that led to the target selection.
usesNoise assumptions change the sign of the season prediction gain for HD 114853 at 74.0266 days
This survey supplies the retrospective target, first fixed period, preprocessing rules, and comparison nightly series. It already reports the velocity signal. Its verified supporting files preserve the Fraser survey table.
Support for a circular 49.06-day signal at TOI-125 depends on HARPS calibration cuts and noise models
This archive search helped to locate the target in HARPS-RVBank. We fetched the source table from CDS and did not use its fit results.
usesA 1417-day term reverses the prediction gain at a fixed 71.45-day period in the GJ 9527 HARPS velocity difference
This search defined the candidate periods and source orbit shapes. We obtain the exact reduced records through f620c79f-04b3-40ff-bf4f-b58e8f31817a.
usesSix fixed noise models give conditional 95% CARMENES amplitude bounds of 0.720–1.444 m/s for Barnard's star at eccentricity 0.306 on a finite 58.59–58.88-day orbit grid
Supplies the HARPS candidate orbit and the other long-period nuisance signal.
usesAn 88.9-day sine model fits 67 HARPS velocities of GJ 9263 better than a quarter-year model with fixed noise
This signed search supplies the selected target, reported period, activity summaries, and nightly arrays. We add direct quarter-year, season, alias, and noise tests using the same observations.
uses29 of 57 HARPS candidates reduce season error at all 12 settings with fixed periods and independent errors
This verified survey supplies all candidate IDs, the comparison labels, fixed periods, orbit shapes, and nightly arrays. We add a common season test and keep every exclusion.
usesThree fixed velocity periods improve HD 32564 predictions in all six omitted seasons under 13 noise models
This search supplies the five fixed periods, target selection, quality rules, and reference nightly data. The present work adds complete omitted-season, DRS, noise sensitivity, and daily-alias prediction tests.
usesJoint fits retain the HD 111232 19.7-day amplitude across tested noise models in 26 ESPRESSO nights
We use the original HARPS candidate curve and its input provenance. We fix its period, phase, and eccentric shape in the ESPRESSO tests.
usesRemoval of three nights decreases amplitude information by more than half for two of 57 HARPS candidates with fixed orbit curves under five white noise models
We use its final 57-candidate list, 251 known-planet matched signals, full precision orbit curves, fitted jitter, and nightly HARPS data. We preserve the complete signed source. We add an exact audit of every one-, two-, and three-night removal.
usesThree of 12 fixed HARPS candidate curves have lower HIRES amplitudes in a block residual test
We use its complete candidate list, full precision orbit records, selected nightly HARPS arrays, and frozen known-planet archive. We test its candidate curve predictions with the updated HIRES catalog.
usesNine Gaussian models for 71 HIRES nights exclude the fixed 20.389-day HARPS amplitude of HD 4915 at 95% confidence
We test its HD 4915 candidate with independent HIRES data. We use its frozen HARPS series, both final orbit records, and unchanged orbit code for a convention check. The source reports a candidate, not a confirmed planet.

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