Figure 1. Astrometric fits to the 361 objects in the Spitzer parallax program from The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs

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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 1. Astrometric fits to the 361 objects in the Spitzer parallax program

The complete figure set (361 images) is available in the online journal.

Example of a target whose astrometric fit uses only Spitzer data. (Upper left) A square patch of sky showing the measured astrometry and its uncertainty at each epoch (black points with error bars) plotted in R.A. vs. decl.. Blue curve shows the best fit. Red lines connect each observation to its corresponding time point along the best-fit curve. (Upper right) A square patch of sky centered at the mean equatorial position of the target. Green curve is the parallactic fit, which is just the blue curve in the previous panel with the proper motion vector removed. Again, red lines connect the time of the observation with its prediction. In the background is the ecliptic coordinate grid, with lines of constant β shown in solid pale purple and lines of constant λ shown in dashed pale purple. Grid lines are shown at 0 farcs 1 spacing. (Lower left) The change in R.A. and decl. as a function of time with the proper motion component removed. The parallactic fit is again shown in green. (Lower right) The R.A. and decl. residuals from the fit as a function of time.

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