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Detection and Astrometry of the Ba–Bb Subsystem in α Piscium: First Dual-field Interferometry at the CHARA Array

  • Authors: Narsireddy Anugu, Robert Klement, John D. Monnier, Douglas R. Gies, Gail H. Schaefer, Stefan Kraus, Sebastián Carrazco-Gaxiola, Akshat S. Chaturvedi, Mayra Gutierrez, Becky Flores, Jeremy Jones, Colin Kane, Rainer Köhler, Karolina Kubiak, Olli W. Majoinen, Nicholas J. Scott, Kayvon Sharifi

Narsireddy Anugu et al 2026 The Astronomical Journal 171 .

  • Provider: AAS Journals

Caption: Figure 6.

Dispersion-corrected δOPDmeas plotted against the projected baseline component B for the MJD = 60918 A–B sequence. B is computed from the (u, v) coordinates via B = (uΔα + vΔδ)/∣θ∣, where Δα and Δδ are the east and north components of θ = rA − rB. Each color denotes a baseline (W2 reference), and the black line is the best-fitting linear relation. For a fixed separation vector, δOPD scales linearly with B (the component of the projected baseline along the A–B separation; using ∣B∣ would not yield a linear relation), so the alignment of the multibaseline points provides a direct consistency check on the OPD sign conventions and time matching. The residual scatter about the fit reflects the ∼0.37 μm effective OPD noise used in the bootstrap uncertainty estimate.

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