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The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs

  • Authors: J. Davy Kirkpatrick, Christopher R. Gelino, Jacqueline K. Faherty, Aaron M. Meisner, Dan Caselden, Adam C. Schneider, Federico Marocco, Alfred J. Cayago, R. L. Smart, Peter R. Eisenhardt, Marc J. Kuchner, Edward L. Wright, Michael C. Cushing, Katelyn N. Allers, Daniella C. Bardalez Gagliuffi, Adam J. Burgasser, Jonathan Gagné, Sarah E. Logsdon, Emily C. Martin, James G. Ingalls, Patrick J. Lowrance, Ellianna S. Abrahams, Christian Aganze, Roman Gerasimov, Eileen C. Gonzales, Chih-Chun Hsu, Nikita Kamraj, Rocio Kiman, Jon Rees, Christopher Theissen, Kareem Ammar, Nikolaj Stevnbak Andersen, Paul Beaulieu, Guillaume Colin, Charles A. Elachi, Samuel J. Goodman, Léopold Gramaize, Leslie K. Hamlet, Justin Hong, Alexander Jonkeren, Mohammed Khalil, David W. Martin, William Pendrill, Benjamin Pumphrey, Austin Rothermich, Arttu Sainio, Andres Stenner, Christopher Tanner, Melina Thévenot, Nikita V. Voloshin, Jim Walla, and Zbigniew Wędracki

2021 The Astrophysical Journal Supplement Series 253 7.

  • Provider: AAS Journals

Caption: Figure 23.

Average ﹩V/{V}_{\max }﹩ value in 0.5 pc intervals for fourteen 150-K bins encompassing our 20 pc L, T, and Y dwarf census. Blue dots represent our empirical sample. Red labels mark the number of objects in the computation at each 0.5 pc interval. Black dashed line shows the ﹩\langle V/{V}_{\max }\rangle =0.5﹩ level indicating a complete sample. Gray error bars show the approximate 1σ range around ﹩\langle V/{V}_{\max }\rangle ﹩ = 0.5 that a complete sample of the size indicated by the red number would exhibit, given random statistics. Brown error bars, offset by +0.05 pc from the gray error bars for clarity, show the 1σ variation around 0.5 obtained by 10,000 Monte Carlo simulations having the number of objects and completeness limit listed in Table 15.

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