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Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS

  • Authors: Noah Vowell, Joseph E. Rodriguez, David W. Latham, Samuel N. Quinn, Jack Schulte, Jason D. Eastman, Allyson Bieryla, Khalid Barkaoui, David R. Ciardi, Karen A. Collins, Eric Girardin, Guillaume Hébrard, Elisabeth Heldridge, Marziye Jafariyazani, Brooke Kotten, Luigi Mancini, Felipe Murgas, Norio Narita, D. J. Radford, Howard M. Relles, Avi Shporer, Melinda Soares-Furtado, Ivan A. Strakhov, Carl Ziegler, Isabelle Boisse, César Briceño, Michael L. Calkins, Catherine A. Clark, Kevin I. Collins, Jerome de Leon, Gilbert A. Esquerdo, Sergio B. Fajardo-Acosta, Thierry Forveille, Akihiko Fukui, Cristilyn N. Watkins, Ruixuan He, Neda Heidari, Keith Horne, Jon M. Jenkins, Andrew W. Mann, Luca Naponiello, Enric Palle, Richard P. Schwarz, S. Seager, John Southworth, Gregor Srdoc, Jonathan J. Swift, Joshua N. Winn

Noah Vowell et al 2025 The Astronomical Journal 170 .

  • Provider: AAS Journals

Caption: Figure 2.

TESS, follow-up, and archival observations of TOI-2844 compared to the the EXOFASTv2 results. Upper left: unbinned TESS and follow-up ground-based transits, phase-folded and shown in comparison to the best-fit EXOFASTv2 model with an arbitrary normalized flux offset. Multiple TESS sectors in the same cadence are stacked on top of each other. Bottom left: the SED of the target star compared to the best-fit EXOFASTv2 model. Residuals are shown on a linear scale, using the same units as the primary y-axis. Upper right: RV observations vs. time, including any significant long-term trend. The residuals are shown in the subpanel below in the same units. Middle right: RV observations phase-folded using the best-fit ephemeris from the EXOFASTv2 global fit. The phase is shifted so that the transit occurs at phase + offset = 0. The residuals are shown in the subpanel below in the same units. Bottom right: the evolutionary track and current evolutionary stage of the primary star according to the best-fit MIST model. The blue line indicates the best-fit MIST track, while the gray shaded contours show the 1σ and 2σ constraints on the star’s current Teff and ﹩\mathrm{log}g﹩ from the MIST isochrone alone. The green contours represent the 1σ and 2σ constraints on the star’s Teff and ﹩\mathrm{log}g﹩ from the EXOFASTv2 global fit, combining constraints from observations of the star and planet. The red cross indicates the median and 68% confidence interval.

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