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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 3.

Comparison of the stellar multiplicity of M dwarfs with hot Jupiters and field M stars at projected separations between 100 and 10,000 au. The multiplicity of the planet sample, P(Comp∣HJ) = 34.2% ± 9.5%, is indicated as a vertical red line with the shaded region marking the 1σ uncertainty. The multiplicity of field M dwarfs, P(Comp) = 5.3% ± 3.7%, is shown as a histogram based on the search for 1000 sets of randomly selected field M stars with properties matched to those of the planet sample.

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