Three new exoplanet systems from the Dispersed Matter Planet Project

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ID: 324939
2026
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Abstract
Abstract We present a radial velocity analysis of three bright, low-activity stars identified by the Dispersed Matter Planet Project (DMPP). We use a Bayesian framework to compare purely Keplerian models with models incorporating stellar activity via a quasi-periodic Gaussian Process (GP). DMPP-7 (HD 118006) is a slightly evolved star that harbours a single 0.72 Saturn-mass giant (mp sin i =69 M⊕) with an orbital period of P = 4.93 d. A longer 21 d – 22 d period cannot be conclusively confirmed as a stellar rotation signature rather than a purely Keplerian signal. For HD 67200, which exhibits Ca ii H&K variability, a model with only a GP is strongly favoured over a purely dynamical model. The GP model shows moderate evidence for a single Keplerian with P = 2.67 d. For HD 2134, a 21 d – 32 d rotation period signal is associated with tentative FWHM variability. A model with a GP is not conclusively favoured, but all models considered show moderate evidence for an additional single Keplerian with P = 2.78 d. Despite our target selection favouring near edge-on orbital geometries, we find no evidence for transits in TESS photometry. DMPP-7 b lies at the transition between the high-radius population and the Neptunian ridge and savannah regions. Further observations are required to establish whether the coherent short-period HD 67200 and HD 2134 signals are stellar or dynamical in origin. If planetary, the signals correspond to minimum masses of mp sin i =2.07 M⊕ and mp sin i =2.86 M⊕.
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Authors J. R. Barnes, C. A. Haswell, Zachary O. B. Ross, E Rutherford, Matthew R. Standing, Adam T Stevenson, D Staab, L Fossati, J S Jenkins, D. R. Alves
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1486
URL
https://doi.org/10.1093/mnras/stag1486
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