![]() None of these approaches yields an unassailable characterization of the eta Aql A-B system. Ascribing photocenter motion to the photometric variation of the Cepheid, eta Aql A, yields a plausible separation that is consistent with a long period and explains the lack of RV variation. Using the astrometric noise or parallax mismatch with EDR3, we estimate possible periods and mass for eta Aql B. In an effort to further characterize eta Aql B, we hypothesize that eta Aql residuals larger than those of the associated reference stars or a parallax inconsistent with EDR3 and the Benedict 2007 Leavitt Law indicate unmodeled orbital motion. Translations in context of 'METODE KECEPATAN RADIAL YANG DIGUNAKAN' in indonesian-english. As modeling confirmation, we reanalyze zeta Gem in parallel, deriving values for its parallax and proper motion consistent with Gaia EDR3, and consistent with the Benedict 2007 Leavitt Law. Models the motion of an extrasolar planet and its star around their common center of mass, and the effect this motion has. ![]() Reanalysis of Hubble Space Telescope Fine Guidance Sensor astrometry now includes reference star parallax and proper motion priors from Gaia EDR3. RV residuals provide no evidence of orbital motion, suggesting either nearly face-on orientation or a very long period. With these we establish the RV variation due to Cepheid pulsation, using a model with 12 Fourier coefficients, while solving for velocity offsets required to bring the RV data sets into coincidence. To determine the orbit of eta Aql B, we analyze a significant number of radial velocity (RV) measurements from eight sources. ![]() The classical Cepheid eta Aql was not included in past Leavitt Law work because of a presumed complicating orbit due to a known B9.8V companion.
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