The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs
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Published:2021-02-23
Issue:1
Volume:253
Page:7
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ISSN:0067-0049
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Container-title:The Astrophysical Journal Supplement Series
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language:
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Short-container-title:ApJS
Author:
Kirkpatrick J. DavyORCID, Gelino Christopher R., Faherty Jacqueline K.ORCID, Meisner Aaron M.ORCID, Caselden DanORCID, Schneider Adam C.ORCID, Marocco FedericoORCID, Cayago Alfred J., Smart R. L.ORCID, Eisenhardt Peter R., Kuchner Marc J.ORCID, Wright Edward L.ORCID, Cushing Michael C.ORCID, Allers Katelyn N.ORCID, Bardalez Gagliuffi Daniella C.ORCID, Burgasser Adam J.ORCID, Gagné JonathanORCID, Logsdon Sarah E.ORCID, Martin Emily C.ORCID, Ingalls James G.ORCID, Lowrance Patrick J.ORCID, Abrahams Ellianna S.ORCID, Aganze Christian, Gerasimov Roman, Gonzales Eileen C.ORCID, Hsu Chih-ChunORCID, Kamraj NikitaORCID, Kiman RocioORCID, Rees Jon, Theissen ChristopherORCID, Ammar Kareem, Andersen Nikolaj StevnbakORCID, Beaulieu Paul, Colin GuillaumeORCID, Elachi Charles A., Goodman Samuel J.ORCID, Gramaize LéopoldORCID, Hamlet Leslie K.ORCID, Hong Justin, Jonkeren Alexander, Khalil Mohammed, Martin David W., Pendrill William, Pumphrey BenjaminORCID, Rothermich AustinORCID, Sainio ArttuORCID, Stenner Andres, Tanner Christopher, Thévenot MelinaORCID, Voloshin Nikita V., Walla Jim, Wędracki Zbigniew
Abstract
Abstract
We present final Spitzer trigonometric parallaxes for 361 L, T, and Y dwarfs. We combine these with prior studies to build a list of 525 known L, T, and Y dwarfs within 20 pc of the Sun, 38 of which are presented here for the first time. Using published photometry and spectroscopy as well as our own follow-up, we present an array of color–magnitude and color–color diagrams to further characterize census members, and we provide polynomial fits to the bulk trends. Using these characterizations, we assign each object a T
eff value and judge sample completeness over bins of T
eff and spectral type. Except for types ≥T8 and T
eff < 600 K, our census is statistically complete to the 20 pc limit. We compare our measured space densities to simulated density distributions and find that the best fit is a power law (
) with α = 0.6 ± 0.1. We find that the evolutionary models of Saumon & Marley correctly predict the observed magnitude of the space density spike seen at 1200 K < T
eff < 1350 K, believed to be caused by an increase in the cooling timescale across the L/T transition. Defining the low-mass terminus using this sample requires a more statistically robust and complete sample of dwarfs ≥Y0.5 and with T
eff < 400 K. We conclude that such frigid objects must exist in substantial numbers, despite the fact that few have so far been identified, and we discuss possible reasons why they have largely eluded detection.
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
108 articles.
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