%N 1
%V 530
%A Beth A Henderson
%A Sarah L Casewell
%A Michael R Goad
%A Jack S Acton
%A Maximilian N Guenther
%A Louise D Nielsen
%A Matthew R Burleigh
%A Claudia Belardi
%A Rosanna H Tilbrook
%A Oliver Turner
%A Steve B Howell
%A Catherine A Clark
%A Colin Littlefield
%A Khalid Barkaoui
%A Douglas R Alves
%A David R Anderson
%A Daniel Bayliss
%A Francois Bouchy
%A Edward M Bryant
%A George Dransfield
%A Elsa Ducrot
%A Philipp Eigmueller
%A Samuel Gill
%A Edward Gillen
%A Michael Gillon
%A Faith Hawthorn
%A Matthew J Hooton
%A James AG Jackman
%A Emmanuel Jehin
%A James S Jenkins
%A Alicia Kendall
%A Monika Lendl
%A James Mccormac
%A Maximiliano Moyano
%A Peter Pihlmann Pedersen
%A Francisco J Pozuelos
%A Gavin Ramsay
%A Ramotholo R Sefako
%A Mathilde Timmermans
%A Amaury HMJ Triaud
%A Stephane Udry
%A Jose Vines
%A Christopher A Watson
%A Richard G West
%A Peter J Wheatley
%A Sebastian Zuniga-Fernandez
%T NGTS-28Ab: a short period transiting brown dwarf
%D 2024
%P 318-339
%L discovery10191948
%J Monthly Notices of the Royal Astronomical Society
%K (stars:) brown dwarfs
%I OXFORD UNIV PRESS
%O © 2024 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.
This is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.
%X We report the disco v ery of a brown dwarf orbiting a M1 host star. We first identified the brown dwarf within the Next Generation Transit Surv e y data, with supporting observations found in TESS sectors 11 and 38. We confirmed the disco v ery with follow- up photometry from the South African Astronomical Observatory, SPECULOOS-S, and TRAPPIST-S, and radial velocity measurements from HARPS, which allowed us to characterize the system. We find an orbital period of ∼1.25 d, a mass of 69 . 0 + 5 . 3 -4 . 8 M J , close to the hydrogen burning limit, and a radius of 0.95 ±0.05 R J . We determine the age to be > 0.5 Gyr, using model isochrones, which is found to be in agreement with spectral energy distribution fitting within errors. NGTS-28Ab is one of the shortest period systems found within the brown dwarf desert, as well as one of the highest mass brown dwarfs that transits an M dwarf. This makes NGTS-28Ab another important disco v ery within this scarcely populated region.