VizieR Online Data Catalog: A full-sky census of brown dwarfs within 20pc (Kirkpatrick+, 2021)

In Kirkpatrick+ (2019, J/ApJS/240/19), we used the Infrared Array Camera (IRAC) to measure preliminary trigonometric parallaxes a selection of objects having spectral types of T6 and later. These results were based on data from Spitzer programs 70062, 80109, 90007, 11059, and the first year's data from 13012 (all with Kirkpatrick as PI). This left a gap in the L and T dwarf sequence between T6 and the latest type for which Gaia has complete coverage (~L5). The aim of Spitzer program 14000 (Kirkpatrick, PI) was to astrometrically monitor those objects in the gap that lacked published parallaxes of high quality but were believed to fall within 23pc. An extension to provide additional data points for these objects at the end of the Spitzer mission was further approved as program 14326 (Kirkpatrick, PI). See Section 3 and Table 2 for the full list of Spitzer program IDs (spanning 2004 Nov 01 to 2019 May 30).

For sources not covered or detected by large-area photometric surveys, we obtained follow-up photometry using the 2MASS camera on the 1.5m Kuiper Telescope on Mount Bigelow, Arizona; the NOAO Extremely Wide Field Infrared Imager (NEWFIRM) at the 4m Victor M. Blanco Telescope on Cerro Tololo, Chile; FLAMINGOS-2 on the 8.1m Gemini-South Telescope on Cerro Pachon, Chile; the Persson's Auxiliary Nasmyth Infrared Camera (PANIC) at the 6.5m Magellan Baade Telescope at Las Campanas Observatory, Chile; the 1.3m Peters Automated Infrared Imaging Telescope (PAIRITEL) on Mount Hopkins, Arizona; the Wide-field Infrared Camera (WIRC) at the 5m Hale Telescope at Palomar Mountain, California; and the Ohio State Infrared Imager/Spectrometer (OSIRIS) at the 4.1m Southern Astrophysical Research Telescope (SOAR) located at Cerro Pachon, Chile. Data acquisition and reduction from these instruments are described in Kirkpatrick+ (2011, J/ApJS/197/19), except those for FLAMINGOS-2, which are described in Meisner+ (2020, J/ApJ/889/74). See Section 5.1.1 and Table A1.

We have obtained near-infrared spectra of some of the objects believed to lie within the 20pc volume that lacked spectral types in the literature. These are listed in Table 9. A single object, WISEJ2126+2530, was observed on 2019 July 22 (UT) using the Double Spectrograph (DBSP) at the Hale 5m telescope on Palomar Mountain, California. Two objects were observed on 2019 November 13 (UT) using the Near-Infrared High Throughput Spectrograph (NIHTS) at the 4.3m Lowell Discovery Telescope (LDT) at Happy Jack, Arizona. Four objects were observed over the nights of 2018 September 1, October 27, and November 17, and 2019 October 28 and December 19 (UT) using the Near-Infrared Echellette Spectrometer (NIRES) at the W. M. Keck II telescope on Maunakea, Hawaii. Eight objects were observed over the nights of 2018 April 1-3 and 2019 June 19 (UT) using the Astronomy Research with the Cornell Infra Red Imaging Spectrograph (ARCoIRIS) at the Victor Blanco 4m telescope at the Cerro Tololo Inter-American Observatory (CTIO), Chile. Ten objects were observed over the nights of 2018 June 16, November 25, and 2019 January 22/23 and March 16 (UT) using SpeX at the NASA Infrared Telescope Facility (IRTF) on Maunakea, Hawaii. Twenty-five objects were observed over the nights of 2016 August 9; 2017 December 3 and 6; 2018 January 2, February 2, September 23, and December 1; 2019 December 11/12; and 2020 February 13/14 (UT) using the Folded-port Infrared Echellette (FIRE) at the 6.5m Walter Baade (Magellan I) telescope at Las Campanas Observatory, Chile. See Section 5.2.

(15 data files).