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Stellar Multiplicity of M Dwarfs with Short-period Giant Planets, and the Characterization of TOI-5628Ab

  • Authors: Tianjun Gan, Alexandrine L'Heureux, Charles Cadieux, Shude Mao, Enric Pallé, Sharon X. Wang, Keivan G. Stassun, Steve B. Howell, Benjamin V. Rackham, Steffani M. Grondin, Khalid Barkaoui, Luc Arnold, Étienne Artigau, Artem Burdanov, Adam J. Burgasser, Douglas A. Caldwell, David R. Ciardi, Karen A. Collins, Neil J. Cook, René Doyon, Georgina Dransfield, Akihiko Fukui, Michaël Gillon, Emmanuel Jehin, Felipe Murgas, Norio Narita, Federico R. Noguer, Howard M. Relles, Avi Shporer, Molly N. Simon, Abderahmane Soubkiou, Christopher A. Theissen, Mathilde Timmermans, Amaury H. M. J. Triaud, Robert T. Zellem, S. Zúñiga-Fernández, Celso P. Machado, Ian R. Mason, Michele T. Mazzucato, Jingyuan Zhao

Tianjun Gan et al 2026 The Astrophysical Journal Letters 1006 .

  • Provider: AAS Journals

Caption: Figure B1.

SED of TOI-5628A (Top left) and the associated WD TOI-5628B (Top right). Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the passband. Blue dots are the model fluxes from the best-fit PHOENIX (left) and D. Koester 2010 (right) atmosphere models (black). Bottom left: The stitched blue (3700–5400 Å) and red (5900–9000 Å) Shane/Kast spectrum of TOI-5628B, normalized to an arbitrary continuum level. The raw spectrum is shown in gray, whereas a Gaussian-smoothed spectrum (σ = 1 Å) is plotted in black. Clear Balmer absorption features are marked with dashed vertical lines. Bottom right: normalized Balmer line profiles plotted as a function of Δλ from line center. Each line is vertically offset for clarity. These spectral features confirm the DA WD nature of TOI-5628B.

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