A free BERV term removes over 99.9% of annual circular signal information at some phases in 151 HARPS designs under white noise
We test how a free residual term for barycentric Earth radial velocity (BERV) changes information about circular planet signals. We use public HARPS-RVBank version 02 times, BERV values, flags, and formal errors. Fixed rules select 151 archive target names with at least 100 nights over at least five years. No measured stellar radial velocity enters the calculation. Under independent noise, we compare amplitude information with and without the BERV term, after fitting era offsets and a linear time slope. At 365.25 days, every target has a phase that retains less than 0.1% of its information. The median fraction of uniform physical phases that retain less than 10% is 32.5%. The median connected interval of periods with a smallest ratio below 0.1 is 19 days on a 200 to 600 day grid. Equal night weights give 31.5% and 18 days. One common BERV coefficient leaves one signal direction unchanged. Direct least squares fits and signal injections verify the calculations. The annual instrumental effect is known from prior work. This contribution provides a defined archive benchmark, exact phase fractions, and reusable code. It does not report a planet or measure a detection rate. The package preserves the exact source fields, provenance, plan, scores, figures, and offline repeat instructions.
HARPS · radial velocity · barycentric Earth radial velocity · annual signals · Fisher information · nuisance regression · public astronomical data · reproducible research
References
4- usesdoi:10.1051/0004-6361/202348263
We use the public HARPS-RVBank version 02 source described by this database update. The package identifies the exact author website snapshot with a SHA256 hash.
- usesdoi:10.1051/0004-6361/201936686
This paper describes the earlier HARPS-RVBank methods and nightly zero point corrections. It supplies context for the formal errors and instrument eras.
- doi:10.1088/0004-637X/808/2/171
This paper establishes the annual HARPS detector effect and the risk of fitting away an annual planet signal. We measure conditional information loss for a defined archive design sample.
- usesdoi:10.1051/0004-6361/201833795
Figure 1 gives 1 June 2015, JD 2457174, as the HARPS fibre change date. We use that boundary for era intercepts.
Cited by
11 publicationsPublic catalog entries on Sciscape.
- usesAn 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
We reuse its exact source extract, target selection, and comparison table. We extend its free-BERV design test to finite independent calibration and bias.
- 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 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 free cadence phase fit keeps 18.5 to 37.1 percent of alias timing information in ten Kepler designs with independent errors
This earlier study used weighted information ratios to test a free nuisance term in HARPS schedules. We apply the same established projection principle to Kepler cadence phase. No data or code from that study are used.
- usesA free scale on each released correction curve keeps at least 67% of annual circular signal information in 105 CARMENES series under the stated diagonal weights
We apply its established interpretation of phase information bounds and a free BERV coefficient to CARMENES dates. The main new dataset concerns the observed correction shape. We wrote new code.
- usesAn 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
We reuse its exact source extract, target selection, and comparison table. We extend its free-BERV design test to finite independent calibration and bias.
- Earlier linear Earth velocity fits reduce later squared loss by at least 10% in 11 of 74 selected HARPS difference series before the adopted 2015 boundary, with free year means
This work gives context on design overlap between Earth velocity terms and annual planet terms.
- usesAll 152 selected HARPS series give under 10% of ideal amplitude information for some 365.25-day orbits at eccentricity 0.8 under independent noise
We use the quadratic-form angle fraction from this related circular HARPS design study. We apply it to eccentric signals and a uniform phase reference. We wrote new code.
- usesWith fixed independent noise, annual curves leave 8.7 to 27.7 percent of 389.7 day signal information in 143 GJ 1151 velocities
This design study separates information loss from evidence for an annual instrument error. We use that distinction for the GJ 1151 velocity fits.
- usesA fully shared night calibration model increases formal annual amplitude errors by more than 20% at all phases in 31 of 151 HARPS designs
Uses its observation cuts and instrument boundary for a comparable sample of 151 HARPS target names. This study tests calibration covariance rather than a fitted BERV term.
- usesAdded 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
We use its general projection concept for a different nuisance term and target. We wrote new code and add measured velocities and residual-noise trials.
- A fixed annual term reduces omitted-year squared error by at least 10% in 9 of 77 selected HARPS velocity differences
This verified SCI study measures annual signal information loss in HARPS designs with a free Earth-velocity term. We add measured paired-velocity prediction results.