the latter programs, which had many epochs of ch2 data, the PRF-fit photometry
from each individual epoch was used; the reported magnitude is that resulting
from the weighted mean flux. We also searched for ancillary data in the
Spitzer Heritage Archive to further supplement our ch1 and ch2 measurements.
Those ancillary data sets are listed in Table 8. We have reduced those data
using the same mosaic portion of our astrometric pipeline, and report the
resulting PRF-fit magnitudes in Table 17. In these reductions, we used the PRF
suite applicable to the phase of the mission, either cryogenic or warm, during
which the data were taken. For targets in campaigns using IRAC’s "sweet spot"
(Ingalls et al. 2012), we took only a portion of the resulting AORs since
there is an enormous amount of data available; specfically, we selected a set
of nine consecutive AORs toward the beginning of the campaign, another nine
toward the middle, and another nine toward the end, and used those to build
the mosaic needed for our pipeline.

Table 8: Ancillary Spitzer Photometry

Object | AOR | Bands | Program | PI
---|---|---|---|---
(1) | (2) | (3) | (4) | (5)
2MASS 0045+1634 | 67432448 | 1 | 14019ss | Vos
$\cdots$ | 67433472 | 2 | $\cdots$ | $\cdots$
WISE 0047+6803 | 58386688 | 1 | 12112ss | Allers
2MASS 0103+1935 | 43345408 | 1 | 80179ss | Metchev
$\cdots$ | 45626112 | 2 | $\cdots$ | $\cdots$
SDSS 0107+0041 | 10374912 | 1,2 | 3136* | Cruz
SIMP 0136+0933 | 21967360 | 1,2 | 40076* | Mainzer
2MASS 0144-0716 | 10375424 | 1,2 | 3136* | Cruz
2MASS 0251-0352 | 10376448 | 1,2 | 3136* | Cruz
WISE 0323+5625 | 32888832 | 1 | 61070 | Whitney
$\cdots$ | 32902912 | 2 | $\cdots$ | $\cdots$
2MASS 0326-2102 | 25362944 | 1,2 | 50059* | Burgasser
2MASS 0340-6724 | 53291776 | 1 | 11174ss | Metchev
$\cdots$ | 53291520 | 2 | $\cdots$ | $\cdots$
2MASS 0355+1133 | 25363712 | 1,2 | 50059* | Burgasser
WISE 0401+2849 | 61990912 | 1 | 13006 | Trilling
2MASS 0407+1514 | 12619008 | 1,2 | 35* | Fazio
2MASS 0421-6306 | 43338496 | 1 | 80179ss | Metchev
$\cdots$ | 45384960 | 2 | $\cdots$ | $\cdots$
2MASS 0439-2353 | 10377472 | 1,2 | 3136* | Cruz
2MASS 0443-3202 | 25363456 | 1,2 | 50059* | Burgasser
2MASS 0445-3048 | 10377728 | 1,2 | 3136* | Cruz
WISE 0457-0207 | 53278464 | 1 | 11174ss | Metchev
$\cdots$ | 53277952 | 2 | $\cdots$ | $\cdots$
PSO 0506+5236 | 67439360 | 1 | 14128ss | Faherty
2MASS 0512-2949 | 53291008 | 1 | 11174ss | Metchev
$\cdots$ | 53290752 | 2 | $\cdots$ | $\cdots$
2MASS 0523-1403 | 10377984 | 1,2 | 3136* | Cruz
WISE 0607+2429 | 50990336 | 1 | 10167ss | Gizis
$\cdots$ | 50990080 | 2 | $\cdots$ | $\cdots$
2MASS 0624-4521 | 10378240 | 1,2 | 3136* | Cruz
2MASS 0641-4322 | 50921984 | 1,2 | 10098 | Stern
2MASS 0700+3157 | 10378496 | 1,2 | 3136* | Cruz
WISE 0715-1145 | 39058944 | 1 | 61071 | Whitney
$\cdots$ | 39075584 | 2 | $\cdots$ | $\cdots$
2MASS 0755-3259 | 38996736 | 1 | 61071 | Whitney
$\cdots$ | 39031808 | 2 | $\cdots$ | $\cdots$
SDSS 0809+4434 | 67435776 | 1,2 | 14128ss | Faherty
SDSS 0830+4828 | 10379008 | 1,2 | 3136* | Cruz
SDSS 0858+3256 | 21984768 | 1,2 | 40198* | Fazio
SDSS 0909+6525 | 21985280 | 1,2 | 40198* | Fazio
WISE 0920+4538 | 19064832 | 1,2 | 30854* | Uchiyama
SIPS 0921-2104 | 10380288 | 1,2 | 3136* | Cruz
2MASS 0949-1545 | 21985792 | 1,2 | 40198* | Fazio
2MASS 1022+5825 | 10380800 | 1,2 | 3136* | Cruz
SDSS 1043+1213 | 43336448 | 1 | 80179ss | Metchev
$\cdots$ | 45622784 | 2 | $\cdots$ | $\cdots$
SDSS 1045-0149 | 10381056 | 1,2 | 3136* | Cruz
SDSS 1048+0111 | 10381312 | 1,2 | 3136* | Cruz
WISE 1049-5319 | 48640512 | 1,2 | 90095 | Luhman
2MASS 1051+5613 | 10381568 | 1,2 | 3136* | Cruz
2MASS 1122-3512 | 43331072 | 1 | 80179ss | Metchev
$\cdots$ | 45621504 | 2 | $\cdots$ | $\cdots$
2MASS 1126-5003 | 21981952 | 1,2 | 40198* | Fazio
2MASS 1213-0432 | 10382336 | 1,2 | 3136* | Cruz
SDSS 1214+6316 | 13778688 | 1,2 | 244* | Metchev
SDSS 1219+3128 | 53295104 | 1 | 11174ss | Metchev
$\cdots$ | 53294848 | 2 | $\cdots$ | $\cdots$
Gl 499C | 53289984 | 1 | 11174ss | Metchev
$\cdots$ | 53289472 | 2 | $\cdots$ | $\cdots$
2MASS 1315-2649 | 15033856 | 1,2 | 20716* | Gizis
2MASS 1324+6358 | 13777920 | 1,2 | 244* | Metchev
DENIS 1425-3650 | 10383104 | 1,2 | 3136* | Cruz
2MASS 1448+1031 | 10383360 | 1,2 | 3136* | Cruz
Gaia 1713-3952 | 45999616 | 1 | 80253 | Whitney
$\cdots$ | 45986304 | 2 | $\cdots$ | $\cdots$
VVV 1726-2738 | 21306368 | 1,2 | 30570* | Benjamin
2MASS 1731+2721 | 10384128 | 1,2 | 3136* | Cruz
WISE 1741-4642 | 67446272 | 1 | 14128ss | Faherty
2MASS 1750-0016 | 53283840 | 1 | 11174ss | Metchev
$\cdots$ | 53283072 | 2 | $\cdots$ | $\cdots$
SDSS 1750+4222 | 21986048 | 1,2 | 40198* | Fazio
2MASS 1753-6559 | 10384384 | 1,2 | 3136* | Cruz
2MASS 1807+5015 | 10384640 | 1,2 | 3136* | Cruz
WISE 1809-0448 | 54359040 | 1 | 11174ss | Metchev
$\cdots$ | 54358784 | 2 | $\cdots$ | $\cdots$
2MASS 1821+1414 | 43343616 | 1 | 80179ss | Metchev
$\cdots$ | 45625344 | 2 | $\cdots$ | $\cdots$
2MASS 1828-4849 | 12618496 | 1,2 | 35* | Fazio
Gaia 1831-0732 | 12109824 | 1 | 146* | Churchwell
$\cdots$ | 12105984 | 2 | $\cdots$ | $\cdots$
WISE 1906+4011 | 47929088 | 1 | 90152ss | Gizis
$\cdots$ | 47929344 | 2 | $\cdots$ | $\cdots$
Gaia 1955+3215 | 39262208 | 1,2 | 61072 | Whitney
2MASS 2002-0521 | 67453440 | 1 | 14128ss | Faherty
WISE 2030+0749 | 53278208 | 1 | 11174ss | Metchev
$\cdots$ | 53277440 | 2 | $\cdots$ | $\cdots$
DENIS 2057-0252 | 10385408 | 1,2 | 3136* | Cruz
PSO 2117-2940 | 67446784 | 1 | 14128ss | Faherty
2MASS 2139+0220 | 10385664 | 1,2 | 3136* | Cruz
2MASS 2148+4003 | 22144256 | 1,2 | 284* | Cruz
2MASS 2151-2441 | 25364736 | 1,2 | 50059* | Burgasser
2MASS 2152+0937 | 10385920 | 1,2 | 3136* | Cruz
2MASS 2209-2711 | 35348480 | 1,2 | 61009 | Freedman
DENIS 2252-1730 | 42482944 | 1,2 | 80183 | Dupuy
2MASS 2331-4718 | 12619264 | 1,2 | 35* | Fazio

Note. — Program numbers followed by an asterisk were part of the Spitzer
cryogenic mission and those with a suffix of "ss" used the IRAC "sweet spot".

###  5.2 Spectroscopy

We have obtained near-infrared spectra of some of the objects believed to lie
within the 20-pc volume that lacked spectral types in the literature. These
are listed in Table 9. Details on the observing runs and data reduction
methods are given in the subsections below.

Table 9: Spectroscopic Follow-up

Object | Instrument | Obs. Date (UT) | Spec. TypeaaAll are near-infrared spectral types except for that of WISE 2126+2530, which is an optical type.
---|---|---|---
(1) | (2) | (3) | (4)
CWISE 0027$-$0121 | Magellan/FIRE | 2018 Dec 01 | T9
CWISE 0041$-$4019 | Magellan/FIRE | 2018 Sep 23 | T8 pec
CWISE 0115$-$4616 | Magellan/FIRE | 2018 Dec 01 | T6
CWISE 0119$-$4937 | Magellan/FIRE | 2018 Dec 01 | T7
CWISE 0119$-$4502 | Magellan/FIRE | 2018 Dec 01 | T8
CWISE 0310$-$5733 | Magellan/FIRE | 2020 Feb 14 | T5
Gaia 0412$-$0734 | Keck/NIRES | 2018 Sep 01 | L2 pec (composite?)
$\cdots$ | $\cdots$ | 2018 Nov 17 | $\cdots$
CWISE 0424+0002 | Magellan/FIRE | 2019 Dec 12 | T9:
CWISE 0433+1009 | Keck/NIRES | 2019 Dec 19 | T8
CWISE 0514+2004 | IRTF/SpeX | 2018 Nov 25 | T0.5
CWISE 0540$-$1802 | CTIO/ARCoIRIS | 2018 Apr 01 | T5
CWISE 0601+1419 | IRTF/SpeX | 2018 Nov 25 | T2.5
CWISE 0602$-$4035 | Magellan/FIRE | 2017 Dec 03 | T5.5
CWISE 0613+4808 | LDT/NIHTS | 2019 Nov 13 | T5
CWISE 0620$-$3006 | Magellan/FIRE | 2017 Dec 06 | T2.5
Gaia 0623+2631 | IRTF/SpeX | 2019 Mar 16 | L3 pec (composite?)
CWISE 0627$-$3730 | Magellan/FIRE | 2017 Dec 03 | T6.5
CWISE 0630$-$6002 | Magellan/FIRE | 2019 Dec 11 | T7
Gaia 0640$-$2352 | Keck/NIRES | 2018 Oct 27 | L5
CWISE 0647$-$1600 | Magellan/FIRE | 2017 Dec 03 | T6
Gaia 0734$-$4330 | Magellan/FIRE | 2020 Feb 13 | L7 blue
CWISE 0749$-$6827 | Magellan/FIRE | 2017 Dec 03 | T8 (pec?)
CWISE 0804$-$0000 | CTIO/ARCoIRIS | 2018 Apr 03 | T4
CWISE 0845$-$3305 | Magellan/FIRE | 2020 Feb 13 | T7
WISE 0902+6708 | IRTF/SpeX | 2019 Jan 22 | L7 pec (low-g)
WISE 0911+2146 | Magellan/FIRE | 2020 Feb 13 | T9
CWISE 0917$-$6344 | Magellan/FIRE | 2020 Feb 14 | L7
CWISE 0953$-$0943 | IRTF/SpeX | 2019 Jan 23 | T5.5
CWISE 1130$-$1158 | CTIO/ARCoIRIS | 2018 Apr 02 | sdT5?
CWISE 1137$-$5320 | Magellan/FIRE | 2018 Feb 02 | T7
CWISE 1141$-$2110 | Magellan/FIRE | 2019 Dec 11 | T9:
CWISE 1152$-$3741 | CTIO/ARCoIRIS | 2018 Apr 02 | T7
Gaia 1159$-$3634 | IRTF/SpeX | 2019 Mar 16 | M9.5
CWISE 1205$-$1802 | CTIO/ARCoIRIS | 2018 Apr 02 | T8
CWISE 1315$-$4936 | Magellan/FIRE | 2018 Jan 02 | T3
Gaia 1331$-$6513 | CTIO/ARCoIRIS | 2019 Jun 19 | M9
WISE 1333$-$1607 | Magellan/FIRE | 2018 Feb 02 | T9
CWISE 1630$-$0643 | Magellan/FIRE | 2020 Feb 13 | T5
Gaia 1648$-$2913 | IRTF/SpeX | 2019 Mar 16 | L5 pec (composite?)
CWISE 1650+5652 | IRTF/SpeX | 2018 Jun 16 | T0
CWISE 1726$-$4844 | Magellan/FIRE | 2020 Feb 13 | T2.5
Gaia 1807$-$0625 | IRTF/SpeX | 2019 Mar 16 | M9 pec (composite?)
CWISE 1832$-$5409 | CTIO/ARCoIRIS | 2018 Apr 02 | T7
Gaia 1836+0315 | IRTF/SpeX | 2019 Mar 16 | L6 v. red
CWISE 2001$-$4136 | Magellan/FIRE | 2016 Aug 09 | T5
CWISE 2012+7017 | LDT/NIHTS | 2019 Nov 13 | T4.5
CWISE 2058$-$5134 | CTIO/ARCoIRIS | 2019 Jun 19 | T0
WISE 2126+2530 | Palomar/DBSP | 2019 Jul 22 | M8
CWISE 2138$-$3138 | Keck/NIRES | 2019 Oct 28 | T8
CWISE 2344$-$4755 | Magellan/FIRE | 2018 Dec 01 | T5.5

####  5.2.1 Palomar/DBSP

A single object, WISE 2126+2530, was observed on 2019 Jul 22 (UT) using the
Double Spectrograph (DBSP; Oke & Gunn 1982) at the Hale 5m telescope on
Palomar Mountain, California. The D55 dichroic was used to split the light
near 5500 Å (0.55 $\mu$m). The blue arm utilized the 600 line mm-1 grating
blazed at 4000 Å (0.40 $\mu$m), while the red arm utilized the 316 line mm-1
grating blazed at 7500 Å (0.75 $\mu$m), producing continuous coverage from
3400 to 10250 Å (0.340 to 1.025 $\mu$m) at a resolving power of $\sim$1500\. A
600s exposure was acquired through partly cloudy conditions. Standard
reduction procedures, as outlined in section 3.1.1 of Kirkpatrick et al.
(2016) were employed.

####  5.2.2 LDT/NIHTS

Two objects were observed on 2019 Nov 13 (UT) using the Near-Infrared High
Throughput Spectrograph (NIHTS; Gustafsson et al. 2019) at the 4.3-meter
Lowell Discovery Telescope (LDT) at Happy Jack, Arizona. The 1$\farcs$34-wide
slit was used providing an average resolving power of 62 over the 0.9–2.5
$\mu$m wavelength range. A series of ten 120s exposures was obtained of both
WISE 0613$+$4808 and WISE 2012$+$7017 at two different positions along the
10$\arcsec$-long slit. Flats and xenon arcs exposures were taken at the
beginning of the night and the A0 V stars, HD 45105 and HD 207646,
respectively, were obtained for telluric correction purposes. The data were
reduced using the Spextool data reduction package (Cushing et al. 2004), and
telluric correction and flux calibration were achieved following the technique
described in Vacca et al. (2003).

####  5.2.3 Keck/NIRES

Four objects were observed over the nights of 2018 Sep 01, Oct 27, and Nov 17,
and 2019 Oct 28 and Dec 19 (UT) using the Near-Infrared Echellette
Spectrometer (NIRES; see, e.g., Wilson et al. 2004) at the W.M. Keck II
telescope on Maunakea, Hawaii. Setup and reductions were identical to those
described in Meisner et al. (2020b) and covered a spectral range of 0.94-2.45
$\mu$m at a resolving power of $\sim$2700\. Note that the spectra for Gaia
0412$-$0734 were combined across nights.

####  5.2.4 CTIO/ARCoIRIS

Eight objects were observed over the nights of 2018 Apr 01-03 and 2019 Jun 19
(UT) using the Astronomy Research using the Cornell Infra Red Imaging
Spectrograph (ARCoIRIS) at the Victor Blanco 4m telescope at the Cerro Tololo
Inter-American Observatory (CTIO), Chile. Instrument setup and data reductions
are identical to those detailed in Greco et al. (2019) and covered a spectral
range of 0.8-2.4 $\mu$m at a resolving power of $\sim$3500.

####  5.2.5 IRTF/SpeX

Ten objects were observed over the nights of 2018 Jun 16, Nov 25, and 2019 Jan
22/23 and Mar 16 (UT) using SpeX (Rayner et al. 2003) at the NASA Infrared
Telescope Facility (IRTF) on Maunakea, Hawaii. SpeX was used in prism mode
with a 0$\farcs$8-wide slit to achieve a resolving power of R = 100-500 over
the range 0.8-2.5$\mu$m. All data were reduced using Spextool (Cushing et al.
2004). A0 stars were used for the telluric correction and flux calibration
steps following the technique described in Vacca et al. (2003).

####  5.2.6 Magellan/FIRE

Twenty-five objects were observed over the nights of 2016 Aug 09; 2017 Dec 03
and Dec 06; 2018 Jan 02, Feb 02, Sep 23, and Dec 01; 2019 Dec 11/12; and 2020
Feb 13/14 (UT) using the Folded-port Infrared Echellette (FIRE; Simcoe et al.
2008, 2010) at the 6.5m Walter Baade (Magellan I) telescope at Las Campanas
Observatory, Chile. Observations were done in high-throughput prism mode with
the 0$\farcs$6 slit, which gives a resolving power of R$\approx$450 covering
0.8-2.45 $\mu$m. Reductions followed the steps described in Meisner et al.
(2020b).

###  5.3 Spectral Classification

The spectra were classified as follows. For the single optical spectrum of
WISE 2126+2530 in Figure 7, we overplotted spectral standards from Kirkpatrick
et al. (1997), which are based on the optical classification system of
Kirkpatrick et al. (1991) and looked for the best match over the entirety of
the spectral range. For near-infrared spectra in Figures 8 and 9, we also
performed a best by-eye fit, but using the near-infrared standards established
by Kirkpatrick et al. (2010) for the L dwarfs, Burgasser et al. (2006) for
early-T through late-T, and Cushing et al. (2011) for late-T through early-Y.
In total, we classify four objects as M dwarfs, eight as L dwarfs, and 38 as T
dwarfs.

Figure 7: Spectrum of WISE 2126+2530 (black) compared to the spectrum of the
M8 standard van Biesbroeck 10 (red) from Kirkpatrick et al. (2010). The flux
of both objects is normalized to one at 8250 Å, a high-S/N portion of the
spectrum free from telluric absorption.  Figure 8: Spectra of M- and L-type
dwarfs compared to the spectrum of the standard nearest in type. These near-
infrared standards are taken from Kirkpatrick et al. (2010). The flux of all
objects is normalized to one at 1.28 $\mu$m and offset by integral increments
to ease comparison. Spectra of the target objects are in black and those of
the standards in other colors. Our spectral classification of each target
object is also shown in black and that of the nearest standard in other
colors. Smoothing has been applied for some of the noisier target spectra.
Figure 9: Spectra of WISE-selected objects compared to the spectrum of the
standard nearest in type. These near-infrared standards are taken from
Burgasser et al. (2006) and Cushing et al. (2011). See the caption to Figure 8
for other details.

##  6 Building the 20-pc Census

###  6.1 Objects to consider

The newly reduced Spitzer astrometry, along with published literature values,
now enables a refinement of the 20-pc census. If an object has a trigonometric
parallax measurement with an uncertainty $\leq$12.5%, we take that parallax at
face value and retain the object if $\varpi_{obs}\geq 50$ mas. In this group
there are a few objects that are worthy of special mention:

  * •

CWISE 0536$-$3055: Based on the data available to Meisner et al. (2020a),
those authors were unable to confirm the motion of this candidate. Using the
Spitzer ch1 and ch2 magnitudes and color, our type and distance estimates
suggest a [T9.5]181818We use brackets to denote estimates for spectral types
not yet measured. dwarf at $\sim$17.4 pc. Our Spitzer astrometry from Table 5
gives a total proper motion of 37.4$\pm$13.7 mas yr-1, which is different from
zero only at the 2.7$\sigma$ level. More telling, however, is the high-quality
absolute parallax, which is 78.1$\pm$3.8 mas (only 5% uncertainty; Table 5)
based on Spitzer astrometric sampling with good coverage over the parallactic
ellipse (Figure Set 1). CWISE 0536$-$3055 is therefore confirmed to be nearby
and to fall within 20 pc of the Sun. This object represents a rare case in
which the six-month parallactic motion (156.2 mas) is far (8.4$\times$) larger
than the six-month proper motion (18.7 mas). Obtaining a radial velocity of
this object would inform us whether CWISE 0536$-$3055 is coming toward our
Solar System or away, and how that translates into a closest approach
distance.

  * •

WISE 0546$-$0959: As with CWISE 0536$-$3055 above, this T5 dwarf has an
exceptionally small proper motion of 11.8$\pm$3.5 mas yr-1 according to Best
et al. (2020) or 10.3$\pm$2.5 mas yr-1 according to our Spitzer astrometry,
despite its large parallax of 50.4$\pm$3.6 (Best et al. 2020) or 57.5$\pm$3.9
mas (our Spitzer measurement). In this case, the six-month parallactic motion
is $\sim$20$\times$ larger than the six-month proper motion.

  * •

CWISE 1411$-$4811: Despite a robust Spitzer parallax value of 58.2$\pm$4.7
mas, this object has no measured spectral type. Its values of W1$-$W2 =
2.28$\pm$0.04 mag and Mch2 = 13.10$\pm$0.18 mag (Table 17) suggest a type of
[T6.5].

  * •

WISE 1600$-$4543: This object has no measured spectral type, despite a robust
parallax measurement of 74.7951$\pm$0.9190 mas from Gaia DR2. Using data in
Table 17, we find that this source has MW2 = 11.74$\pm$0.06 mag, which
suggests [L9]. The color of $J_{2MASS}-$W2 = 2.62$\pm$0.04 mag suggests a type
between mid-L and early-T.

  * •

CWISE 1926$-$3429: Despite a robust Spitzer parallax value of 51.6$\pm$3.9
mas, this object has no measured spectral type. Values of ch1$-$ch2 =
0.98$\pm$0.03 mag and Mch2 = 12.67$\pm$0.17 mag (Table 17) suggest a type of
[T5.5].

In addition to objects with well measured parallaxes, there is another set of
potential 20-pc members with poorer or non-existent parallax measurements that
need additional scrutiny. The objects are listed in Table 10 and are (a)
pulled from Table 1 or Tables 6-7, (b) are objects originally included in
Spitzer program 14224 but dropped because of time restrictions, or (c) are
previously published objects rediscovered by the CatWISE or Backyard Worlds
teams for which initial estimates indicated distances within 23 pc of the Sun.
We use a combination of photometric and spectrophotometric distance estimates
to determine whether each object should be included in the 20-pc census.
Namely, we use data from 20-pc census members with robust parallax
measurements (uncertainties $\leq 12.5\%$) to construct three independent
relations of MJ vs. $J-$W2 (valid for $J-$W2 $\geq$ 4.0 mag, or for 2.0 $\leq
J-$W2 $<$ 4 mag if W1$-$W2 $\geq$ 2.2 mag), MH vs. near-infrared spectral type
(valid for all L, T, and Y spectral types), and Mch2 vs. ch1$-$ch2 (valid for
ch1$-$ch2 $\geq$ 0.4 mag). Using data provided in Table 17, we use the
apparent magnitudes and colors of each object in Table 10 to estimate a
distance from each relation, and then average the results to provide a final
distance estimate. For some objects, there is not sufficient observational
data for any of these relations – or the object has colors outside the range
for which the relations are valid – so instead we use a MW2 vs. W1$-$W2
relation (valid for W1$-$W2 $\geq$ 0.5 mag), also constructed from 20-pc
members with robust parallax measurements, to provide a distance estimate.

Table 10: Other Objects Considered for the 20-pc Census

Object | Spec. | Spec. | Our | Pub. | Pub. | dest | dest | dest | dest | Final | Include | Remarks
---|---|---|---|---|---|---|---|---|---|---|---|---
name | type | type | $\varpi_{abs}$ | $\varpi_{abs}$ | $\varpi_{abs}$ |  $J$,W2 |  $H$,type | ch1,ch2 | W1,W2 | dest | in 20-pc |
|  | ref. | (mas) | (mas) | ref. | (pc) | (pc) | (pc) | (pc) | (pc) | census? |
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (13) | (12)
CWISE 0027$-$0121 | T9 | T | 54.2$\pm$7.9 |  $\cdots$ | - | 16.00 |  $\cdots$ | 17.47 |  $\cdots$ | 16.73 | yes |
2MASS 0034$-$0706 | L4.3 | D |  $\cdots$ | 55.8$\pm$12.3 | r |  $\cdots$ | 32.03 |  $\cdots$ |  $\cdots$ | 32.03 | no |
CWISE 0043$-$3822 | [T8.5] | T | 38.1$\pm$15.7 |  $\cdots$ | - |  $\cdots$ |  $\cdots$ | 19.24 |  $\cdots$ | 19.24 | yes |
WISE 0048+2508 | [T8.5] | m |  $\cdots$ |  $\cdots$ | - | 12.48 |  $\cdots$ | 14.54 |  $\cdots$ | 13.51 | yes |
2MASS 0051$-$1544 | L5 | B | 34.0$\pm$6.6 | 29.1$\pm$1.4 | G |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$ | 34.36 | no |
2MASS 0103+1935 | L6(o) | K | 35.9$\pm$5.7 | 46.9$\pm$7.6 | F |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$ | 21.32 | no | see text
CWISE 0115$-$4616 | T6 | T |  $\cdots$ |  $\cdots$ | - | 21.04 | 31.31 | 19.97 |  $\cdots$ | 24.11 | no |
CWISE 0119$-$4937 | T7 | T |  $\cdots$ |  $\cdots$ | - | 18.11 | 39.29 | 20.47 |  $\cdots$ | 25.96 | no |
CWISE 0119$-$4502 | T8 | T |  $\cdots$ |  $\cdots$ | - | 20.50 | 11.51 | 18.75 |  $\cdots$ | 16.92 | yes |
WISE 0132$-$5818 | [T9] | m | 27.2$\pm$7.3 |  $\cdots$ | - | 22.40 |  $\cdots$ | 21.67 |  $\cdots$ | 22.04 | no |
WISE 0135+1715 | T6 | k | 65.3$\pm$10.0 | 46.7$\pm$3.5 | W |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$ | 21.41 | no |
WISE 0138$-$0322 | T3 | J | 38.5$\pm$6.4 | 43.9$\pm$2.9 | W |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$ | 22.78 | no |

Note. — (This table is available in its entirety in a machine-readable form in
the online journal. A portion is shown here for guidance regarding its form
and content.)

Note. — Reference code for infrared spectral type. Values in brackets are
estimates, and the types for 2MASS 0103+1935 and 2MASS 0639$-$7418 are based
on optical spectra: (B) Burgasser et al. 2010, (b) Burgasser, et al. 2010b,
(C) Cruz, et al. 2007, (D) Bardalez Gagliuffi, et al. 2014, (F) Faherty et al.
2016, (G) Mace et al. 2013, (g) Greco et al. 2019, (i) Kirkpatrick et al.
2016, (J) Kirkpatrick et al. 2011, (j) Kirkpatrick et al. 2010, (K)
Kirkpatrick et al. 2000, (k) Kirkpatrick et al. 2012, (M) Meisner et al.
2020a, (m) Meisner et al. 2020b, (R) Reylé et al. 2014, (S) Schneider et al.
2017, (T) this paper, (U) Burningham et al. 2013, (u) Burningham et al. 2010,
(W) Best et al. 2015.

Note. — Reference code for published parallax: (c) Theissen et al. 2020, (F)
Faherty et al. 2012, (G) Gaia Collaboration et al. 2018, (g) Gaia
Collaboration et al. 2018 parallax for the primary is cited, (r) Smart et al.
2018, (W) Best et al. 2020.

We also provide spectral types in Table 10. For objects without measured
spectral types, we provide type estimates by using the final distance estimate
in the table combined with the object’s ch2 magnitude to provide an estimate
of $M_{ch2}$. We then take data from 20-pc census members having robust
parallax measurement (uncertainties $\leq 12.5\%$) to construct a relation of
spectral type vs. $M_{ch2}$ (valid over the entire range needed, 10.5
$<M_{ch2}<$ 16.0 mag), and use this to predict the type. (A value of $M_{W2}$
is used as a proxy for $M_{ch2}$ when no ch2 magnitude is available.) These
estimated types are enclosed within brackets in the table.

Several objects requiring special consideration are noted by "see text" under
the Remarks column in Table 10. Those objects are discussed below:

  * •

2MASS 0103+1935: This optical L6 dwarf (Kirkpatrick et al. 2000) has two
independent parallax measurements, both low quality, of 35.9$\pm$5.7 mas
(Table 6) and 46.9$\pm$7.6 mas (Faherty et al. 2012). Given that both measures
suggest a parallax below 50 mas, we consider this object to fall outside of 20
pc.

  * •

CWISE 0212+0531: This object was announced in Meisner et al. (2020a), although
those authors were not able to confirm the object’s motion. Based on the
Spitzer ch1 and ch2 magnitudes and color, our spectral type and distance
estimates suggest [$\geq$Y1] at $<$13.3 pc. Our Spitzer astrometry from Table
7 gives a total proper motion of 82.6$\pm$52.7 mas yr-1, which is different
from zero at only the 1.6$\sigma$ level. The resulting parallax is
24.7$\pm$16.3 mas, with one parallax factor being represented by only a single
Spitzer data point (Figure Set 1). Because both the motion and parallax are
insignificantly different from zero, and because the measured parallax is much
smaller than the expected value, we consider this to be a background object.

  * •

CWISE 0423$-$4019: Our Spitzer photometry suggests a [T9] dwarf at $\sim$16.5
pc. Our Spitzer parallax measurement of $-$11.7$\pm$6.9 mas and total proper
motion of 3.8$\pm$3.3 mas yr-1, however, show that this is a background object
and not a nearby brown dwarf.

  * •

CWISE 0424+0002: This object was announced in Meisner et al. (2020a), although
those authors were not able to confirm the object’s motion. Our Spitzer
astrometry from Table 7 gives a total proper motion of 208.7$\pm$35.0 mas
yr-1, which is different from zero at the 6.0$\sigma$ level. The resulting
parallax is 37.4$\pm$11.7 mas, representing a 31% uncertainty, and there is
only a single Spitzer data point at one of the maximum parallax factors
(Figure Set 1). Our spectrum from Figure 8 confirms that it is nearby. Because
the motion is confirmed but the trigonometric parallax is not yet credible, we
use our (spectro)photometric distance estimates to place this object within 20
pc.

  * •

CWISE 0442$-$3855: Our Spitzer photometry suggests a [T8.5] dwarf at
$\sim$16.8 pc. Our Spitzer parallax measurement of $-$12.4$\pm$4.9 mas and
total proper motion of 3.6$\pm$2.6 mas yr-1, however, show that this is a
background object and not a nearby brown dwarf.

  * •

CWISE 0617+1945: Using the colors of this object in Table 17, we are unable to
provide a distance estimate using any of our four preferred absolute magnitude
relations. Using the MKO-based $JHK$ magnitudes from Table 17, the color-color
plots presented in section 7.4 suggest that this is a late-L dwarf, which
would indicate MH = 13.8 mag and a distance of $\sim$7.5 pc. As further
discussed in section 7.3, the object appears to have a co-moving companion to
its north-east, which is faint enough that it does not strongly affect the
distance estimate. We consider this pair to fall within 20 pc.

  * •

ULAS 0745+2332: This object, discovered by Burningham et al. (2013), lies in
very close proximity to a background star that complicated our Spitzer
astrometric measurements, leading to a false, negative parallax (Table 7).
This object is not detected in any of the various WISE catalogs consulted for
Table 17. The discovery paper lists a T8.5 spectral type and estimated
distance of $<$19.4 pc, so we include this object in the 20-pc census.

  * •

WISE 0830+2837: This candidate Y dwarf from Bardalez Gagliuffi et al. (2020)
is sufficiently red in its Spitzer colors to be a possible bridge source in
Teff between spectroscopically verified early-Y dwarfs and WISE 0855$-$0714\.
Given its estimated distance of $\sim$8.2 pc and our low-quality parallax of
90.6$\pm$13.7 mas, we consider this object to be well within 20 pc.

  * •

CWISE 1008+2031: This object was announced in Meisner et al. (2020a), although
those authors were not able to confirm the object’s motion. Our Spitzer
astrometry from Table 7 gives a total proper motion of 215.3$\pm$51.5 mas
yr-1, which is different from zero at the 4.2$\sigma$ level. The resulting
parallax is 37.1$\pm$15.1 mas, representing a 41% uncertainty, with the
Spitzer astrometric sampling providing only a single point at one of the
maximum parallax factors (Figure Set 1). Because the motion of this object
confirms it as being nearby and our photometric distance estimates place it
within 20 pc, we include it in the 20-pc census.

  * •

WISE 1040+4503: This object was announced in Meisner et al. (2020a), although
those authors were not able to confirm the object’s motion. Our Spitzer
astrometry from Table 7 gives a total proper motion of 91.7$\pm$32.3 mas yr-1,
which is different from zero at the 2.8$\sigma$ level. The resulting parallax
is 18.8$\pm$9.8 mas, representing a 52% uncertainty, with the Spitzer
astrometric sampling providing only a single point at one of the maximum
parallax factors (Figure Set 1). Given that the photometric distance estimate
is outside of 20 pc and that a distance within 20 pc is not suggested by the
available astrometry, we exclude this object from the 20-pc census. It may, in
fact, be a background object.

  * •

CWISE 1047+5457: Meisner et al. (2020a) estimated that this is a [Y0] dwarf at
$\sim$21.7 pc. Our low-quality parallax value of 75.2$\pm$12.8 suggests that
it is closer. One of the maximum parallax factors is sampled with only one
Spitzer data point (Figure Set 1), but this together with the other data
samples strongly suggest a parallax $>$50 mas. We consider this object to lie
within 20 pc, although higher quality astrometry is clearly needed.

  * •

CFBDS 1118$-$0640: This object, which is a common proper motion companion to
the mid-M dwarf 2MASS J11180698$-$0640078, was included in our Spitzer
parallax program through a mistake. Its spectral type of T2 was paired up
incorrectly with the WISE magnitudes of the primary, resulting in a
photometric distance of $<$20 pc. The Gaia DR parallax of the primary is
9.90$\pm$0.15 mas, and our Spitzer parallax of the companion T dwarf is
1.4$\pm$5.2 mas. This object is therefore excluded from the 20-pc census.

  * •

CWISE 1130$-$1158: This object has wildly discrepant distance estimates, with
those using colors predicting a value within 20 pc and the one using spectral
type indicating a value well outside 20 pc. Our spectroscopic follow-up from
section 5.2 suggests that this object has a peculiar spectrum, particularly a
depressed $K$-band spectrum similar to that seen in other T-type subdwarfs
(e.g., Pinfield et al. 2014a). We therefore classify this object as an sdT5?.
Given its possible subdwarf status, neither the color-based nor type-based
relations may be accurate. For now, we consider this object to fall outside 20
pc, but additional astrometry is needed.

  * •

2MASS 1158+0435: This is an optical and near-infrared sdL7 (Kirkpatrick et al.
2010) placed on the parallax program because distance estimates for L
subdwarfs are not yet well established. Our Spitzer parallax value of
39.2$\pm$6.2 mas is based on a well-sampled parallactic ellipse (Figure Set
1), so we consider this object to lie outside of 20 pc.

  * •

ULAS 1319+1209: Burningham et al. (2010) classify this object as T5 pec based
on a T5 fit in the $J$ band and a T3 fit in the $H$ band. In preparing our
list of target objects for the Spitzer parallax program, we mistook this
object to be the bright proper motion star immediately to its north, which has
an AllWISE value of W2 = 12.56$\pm$0.03 mag. This led to an incorrect distance
estimate of $\sim$9 pc. Our Spitzer parallax (7.8$\pm$6.5 mas) was measured
for this brighter star, Gaia DR2 3739496602924096000, not of the T
dwarf191919Because our measurements are not of a brown dwarf or even of an
object within 20 pc, we have excluded this source from Table 17..
Investigating this further, we find that the Gaia star, which is not listed in
SIMBAD, has a Gaia DR2 parallax of 9.22$\pm$0.11 mas and motions of $\mu_{RA}$
= $-$135.2$\pm$0.2 mas yr-1 and $\mu_{Dec}$ = 3.8$\pm$0.2 mas yr-1. The motion
measured by Burningham et al. (2013) for the T dwarf is $\mu_{RA}$ =
$-$120.9$\pm$16.0 mas yr-1 and $\mu_{Dec}$ = $-$22.9$\pm$14.6 mas yr-1 which
is consistent within the uncertainties to those of the Gaia star. Murray et
al. (2011) estimate the distance of ULAS 1319+1209 to be 75$\pm$12 pc and note
that it might be a halo T dwarf, although Liu et al. (2011) contend that thick
disk membership is more likely. Burningham et al. (2013) estimate that the T
dwarf falls between 58.6 and 99.1 pc if it is a single object, and could be as
distant as 140.0 pc if a binary. These higher values are consistent with the
distance to the Gaia object at 108.5 pc. The Gaia star has teff_val = 3974K,
which would correspond to a late-K dwarf, whose metallicity should be easily
measurable. We believe that this may be a new benchmark system and a
particularly valuable one since the T dwarf shows peculiarities that may or
may not be linked to a lower metallicity.

  * •

Gaia 1331$-$6513: This is another object, like CWISE 0536$-$3055 discussed
above, that has a very low motion value given its proximity to the Sun
($\sim$16.0 pc). The total motion from Gaia DR2 is 21.2$\pm$0.3 mas yr-1,
meaning that the parallactic motion over six months is twelve times larger
than the proper motion. A measurement of the radial velocity would inform us
whether this object is coming toward the Sun or away from it and the timescale
for closest approach to the Solar System.

  * •

WISE 1355$-$8258: This object was announced in Schneider et al. (2016), and
Kirkpatrick et al. (2016) noted its unusual near-infrared spectrum, which they
tentatively interpreted to be an sdL5. Bardalez Gagliuffi et al. (2018)
attempted to explain the spectrum as that of an unresolved binary but were
unable to find a binary fit that provided a convincing explanation. They
noted, however, a possible kinematic association with the AB Doradus Moving
Group, despite finding no spectroscopic evidence of low-gravity. Their best
guess for the distance is 27-33 pc. Using WISE astrometry, Theissen et al.
(2020) measure a fragile parallax of 60$\pm$19 mas (32% error). Using a
combination of 2MASS and WISE astrometry, E. L. Wright (priv. comm.) finds a
still fragile parallax of 73$\pm$16 mas (22% error). For now, we consider this
object to lie outside of 20 pc but encourage future astrometric monitoring in
an effort to better understanding this intriguing object.

  * •

CWISE 1446$-$2317: Marocco et al. (2020) show that the Spitzer colors of this
object place it among the coldest Y dwarfs currently known. Our Spitzer
parallax measurements of 95.6$\pm$13.9 mas, though somewhat fragile based on
its poorly sampled parallactic ellipse (Figure Set 1), nonetheless strongly
suggests proximity to the Sun. We include this object within the 20 pc census.

  * •

CWISE 1458+1734: This object is from Meisner et al. (2020a), who suggest a
spectral type of [T8] and distance of $\sim$21.6 pc. Our Spitzer parallax
measurement of 1.3$\pm$7.2 mas (Table 7) is based on a fit to a well-sampled
parallactic ellipse. The proper motion of this source is measured at high
significance, 503.6$\pm$26.1 mas yr-1 (Table 7), so the lack of a measurable
parallax is puzzling. We have compared the UHS $J$-band image from 2013 May to
our own $J$-band image taken from Palomar/WIRC in 2020 Jul (Figure 10) and
confirm a motion along nearly the same position angle indicated by our
astrometric fit in Figure Set 1. We note, however that the position angle of
the motion vector is almost perfectly aligned with the major axis of the
parallactic ellipse, meaning that an incorrect motion magnitude could easily
erase the parallactic signature. We have performed a test of this hypothesis
by determining what value of the total motion is needed to create a
parallactic signature matching the distance estimate in Table 10 while also
assuming that the motion direction measured by our Spitzer+unWISE astrometry
is correct. We get the correct result if the total proper motion is reduced
from 504 mas yr-1 to $\sim$300 mas yr-1. This hypothesis is supported by the
fact that CWISE 1458+1734 is moving between – and is bracketed by – two
background objects that themselves fall along nearly the same position angle
as the proper motion, and it is thus conceivable the unWISE astrometry of the
T dwarf is pulled southeastward at early epochs by blending from the southeast
source and northwestward at later epochs by blending from the northwest
source, thereby inflating the true motion value. Crude measurements of the
astrometry from the images in Figure 10 give a proper motion of $\sim$305 mas
yr-1, confirming our hypothesis. Nevertheless, the photometric distance of
this source places it just outside 20 pc, so it is not included in our 20-pc
census.

Figure 10: Images at $J$-band for CWISE 1458+1734. (Top) The 2013 May image
from UHS. (Bottom) Our 2020 Jul image from Palomar/WIRC. These images are
1$\times$0.5 arcmin with north up and east to the left. Arrows mark the
location of CWISE1458+1734 and illustrate its motion over the 7.2-yr baseline.

  * •

WISE 1534$-$1043: This object is from Meisner et al. (2020a), who note that
its placement on the $J-$ch2 vs. ch1$-$ch2 color plot suggest it is a mid- to
late-T subdwarf. As such, deriving a photometric distance estimate from
relations that assume solar metallicity is useless. Too few late-T subdwarfs
are known to enable a better distance estimate, particularly since we do not
know if the object’s metallicity is similar to or more extreme than known T
subdwarfs, so our Spitzer  trigonometric distance measurement of 47.8$\pm$14.3
mas (Table 7) is the best current indicator, despite the large relative
uncertainty of 30%. The object’s high proper motion, 2772.7$\pm$57.3 mas yr-1,
also points to an old, kinematically heated object. (At 20 pc, this would
correspond to a tangential velocity of 263 km s-1.) The $<$50mas parallax
suggests that we exclude this object from the 20-pc census as we await
additional astrometric measurements.

  * •

WISE 1619+1347: This object was announced in Meisner et al. (2020b), although
those authors were not able to confirm the object’s motion. Our Spitzer
astrometry from Table 7 gives a total proper motion of 29.1$\pm$16.6 mas yr-1,
which is different from zero at only the 1.8$\sigma$ level. The resulting,
negative parallax of $-$9.1$\pm$4.3 mas, is based on Spitzer astrometric data
that sample the parallactic ellipse well (Figure Set 1). We therefore consider
this to be a background object.

  * •

CWISE 1827+5645: This object was re-discovered by high school student Justin
Hong as part of the Summer Research Connection at Caltech in the summer of
2020. The object was first discovered during the original WISE mission and
chosen for Spitzer follow-up in program 70062, where it was measured to have a
ch1$-$ch2 color indicative of a late-T dwarf. Subsequent Palomar/WIRC $J$-band
imaging indicated a magnitude of $\sim$19.0 mag, ruling out the possibility of
its being a late-T dwarf. The object was rediscovered again by the Backyard
Worlds team but was paired up with a $J$ = 19.33$\pm$0.17 mag UHS object – the
same object seen in the Palomar imaging – and believed to be a more distant
early-T dwarf based on its implied $J-$W2 color. This $J$-band source is,
however, an interloper in the field and not the brown dwarf candidate itself.
(The same background object also contaminates the proper motion measure from
CatWISE2020.) The Spitzer photometry from 2012 is clean; this color, together
with clear evidence of motion through the epochal coverage of WISE and NEOWISE
images, indicates a [T9.5] dwarf just outside of the 20-pc census.

  * •

CWISE 2058$-$5134: We are unable to provide a distance estimate to this object
using any of our four preferred absolute magnitude relations. Our
spectroscopic follow-up (Table 9) shows that this is a T0 dwarf, which would
indicate MJMKO = 14.5 mag using plots illustrated in the following section.
This suggests a distance of $\sim$33.9 pc. We consider this object to fall
outside of 20 pc.

###  6.2 The Resulting Census and Final Checks

Our final, full-sky census of L, T, and Y dwarfs within 20 pc of the Sun is
presented in Table 11. This includes not only solivagant dwarfs within that
distance but also all known L, T, and Y dwarf companions to earlier type stars
within 20 pc. For objects confirmed or believed to be double or triple
systems, each component that is an L, T, or Y dwarf is listed. The table lists
each object’s discovery name, discovery reference, and optical and near-
infrared spectral types (with reference), if measured. The table also lists
the absolute parallax from Table 17 and the total proper motion, along with a
reference for the astrometry. For cases in which either a spectral type or
parallax is estimated, the estimated value is shown in brackets. (For the
$T_{\rm eff}$ values listed in the penultimate column, the reader is referred
to section 8.1.) The last column of the table is reserved for special notes.
If a note of "[]" is listed, then that object’s listed parallax should be
ignored in favor of the spectrophotometric estimate shown in brackets. If a
note of "yng" or "sd" is listed, that object is discussed further in section
7.

Table 11: The Full-sky 20-pc Census of L, T, and Y Dwarfs (Known as of 2020
Oct)

Discovery | Disc. | Optical | Type | Infrared | Type |  $\varpi_{abs}$bbValues in brackets are estimates only. | $\mu_{tot}$ | Astrom. | $T_{\rm eff}$ | Special
---|---|---|---|---|---|---|---|---|---|---
Designation | Ref. | Sp. TypebbValues in brackets are estimates only. | Ref. | Sp. TypebbValues in brackets are estimates only. | Ref. | (mas) | (mas yr-1) | Ref. | (K) | NoteddA "yng" entry indicates that the spectrum of this object suggests low gravity and youth. An "sd" entry indicates that the spectrum of this object suggests low metallicity and hence, old age. A value in brackets indicates that the value of the parallax in the $\varpi_{abs}$ column is uncertain and that our distance estimate from Table 10 suggests the bracketed value be considered as the parallax instead.
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11)
SDSS J000013.54+255418.6 | 57 | T5 | 214 | T4.5 | 61 | 70.8$\pm$1.9 | 128.1$\pm$1.3 | 67 | 1227$\pm$95 |
GJ 1001B (000434$-$404405) | 101 |  $\cdots$ |  $\cdots$ | L5 | 102 | 82.0946$\pm$0.3768 | 1641.6$\pm$0.6 | 168 | 1613$\pm$134 |
GJ 1001C (000434$-$404405) | 116 |  $\cdots$ |  $\cdots$ | L5 | 102 | 82.0946$\pm$0.3768 | 1641.6$\pm$0.6 | 168 | 1613$\pm$134 |
WISE J000517.48+373720.5 | 8 |  $\cdots$ |  $\cdots$ | T9 | 8 | 126.9$\pm$2.1 | 1033.6$\pm$1.4 | 0 | 555$\pm$88 |
2MASS J00145575$-$4844171 | 103 | L2.5 pec | 103 | L2.5$\pm$1 | 104 | 50.1064$\pm$0.3898 | 915.1$\pm$0.5 | 168 | 1887$\pm$88 |
WISE J001505.87$-$461517.6 | 2 |  $\cdots$ |  $\cdots$ | T8 | 2 | 75.2$\pm$2.4 | 802.5$\pm$1.5 | 0 | 656$\pm$88 |
2MASSW J0015447+351603 | 105 | L2 | 105 | L1.0 | 106 | 58.6085$\pm$0.3664 | 262.9$\pm$0.5 | 168 | 1898$\pm$88 |
CWISE J002727.44$-$012101.7 | 0 |  $\cdots$ |  $\cdots$ | T9 | 0 | 54.2$\pm$7.9 | 452.9$\pm$3.3 | 0 | 566$\pm$79 | [59.8]
WISE J003110.04+574936.3 | 20 |  $\cdots$ |  $\cdots$ | L8 | 20 | 71.0$\pm$3.2 | 522.1$\pm$2.2 | 0 | 1460$\pm$88 |
WISE J003231.09$-$494651.4 | 2 |  $\cdots$ |  $\cdots$ | T8.5 | 2 | 60.8$\pm$2.5 | 937.2$\pm$1.6 | 0 | 609$\pm$88 |
ULAS J003402.77$-$005206.7 | 27 |  $\cdots$ |  $\cdots$ | T8.5 | 10 | 68.7$\pm$1.4 | 359.2$\pm$0.8 | 67 | 619$\pm$88 |
2MASS J00345157+0523050 | 3 |  $\cdots$ |  $\cdots$ | T6.5 | 61 | 118.8$\pm$2.7 | 696.8$\pm$2.0 | 0 | 899$\pm$82 |
2MASSW J0036159+182110 | 107 | L3.5 | 107 | L4 | 124 | 114.4167$\pm$0.2088 | 910.0$\pm$0.4 | 168 | 1869$\pm$64 |
WISE J003829.05+275852.1 | 8 |  $\cdots$ |  $\cdots$ | T9 | 8 | 88.2$\pm$2.0 | 93.2$\pm$1.4 | 0 | 545$\pm$88 |
Gl 27B (003921+211501) | 28 |  $\cdots$ |  $\cdots$ | T8 | 61 | 89.7891$\pm$0.0581 | 591.8$\pm$0.1 | 168aaThis object is excluded for our 20-pc L, T, and Y dwarf census because its type is earlier than L0. | 793$\pm$35 |
WISE J004024.88+090054.8 | 8 |  $\cdots$ |  $\cdots$ | T7 | 8 | 69.8$\pm$1.5 | 74.5$\pm$2.2 | 1 | 850$\pm$88 |
CWISE J004143.77$-$401929.9 | 0 |  $\cdots$ |  $\cdots$ | T8 pec | 0 | 76.7$\pm$9.6 | 1532.9$\pm$2.1 | 0 | 686$\pm$79 |
CWISE J004311.24$-$382225.0 | 0 |  $\cdots$ |  $\cdots$ | [T8.5] | 0 | [52.0] | 392.5$\pm$4.0 | 0 | 624$\pm$79 |
2MASSW J0045214+163445 | 109 | L2$\beta$ | 110 | L2$\gamma$ | 118,175 | 65.0151$\pm$0.2274 | 362.1$\pm$0.5 | 168 | 2059$\pm$45 | yng
WISE J004542.56+361139.1 | 8 |  $\cdots$ |  $\cdots$ | T5 | 8 | 57.0$\pm$3.7 | 185.7$\pm$2.2 | 0 | 1021$\pm$88 |
WISEP J004701.06+680352.1 | 182 | L7($\gamma$?) | 175 | L6-8$\gamma$ | 175 | 82.3$\pm$1.8 | 432.0$\pm$1.8 | 198 | 1230$\pm$27 | yng
WISEU J004851.21+250814.9 | 233 |  $\cdots$ |  $\cdots$ | [T8.5] | 233 | [74.0] | 1231.0$\pm$17.8 | 0 | 624$\pm$79 |
WISEPC J004928.48+044100.1 | 4 |  $\cdots$ |  $\cdots$ | L9 | 4 | 62.6$\pm$2.9 | 388.3$\pm$4.1 | 237 | 1256$\pm$88 |
WISE J004945.61+215120.0 | 8 |  $\cdots$ |  $\cdots$ | T8.5 | 8 | 140.4$\pm$2.1 | 482.4$\pm$1.4 | 0 | 640$\pm$88 |
2MASS J00501994$-$3322402 | 29 |  $\cdots$ |  $\cdots$ | T7 | 61 | 94.6$\pm$2.4 | 1485.1$\pm$2.1 | 67 | 836$\pm$71 |
CFBDS J005910.90$-$011401.3 | 30 |  $\cdots$ |  $\cdots$ | T8.5 | 10 | 103.2$\pm$2.1 | 885.8$\pm$1.1 | 67 | 566$\pm$88 |
CWISEP J010527.69-783419.3 | 232 |  $\cdots$ |  $\cdots$ | [T9] | 232 | 87.2$\pm$4.4 | 331.5$\pm$12.3 | 0 | 566$\pm$79 |
SDSSp J010752.33+004156.1 | 122 | L8 | 136 | L6 | 124 | 64.13$\pm$4.51 | 634.5$\pm$7.1 | 68 | 1385$\pm$89 |
WISE J011154.36$-$505343.2 | 184 |  $\cdots$ |  $\cdots$ | T1.5 | 184 | 57.3$\pm$4.7 | 498.6$\pm$1.8 | 0 | 1239$\pm$88 |
CWISE J011952.82$-$450231.2 | 0 |  $\cdots$ |  $\cdots$ | T8 | 0 | [59.1] | 160.2$\pm$31.3 | 0 | 686$\pm$79 |
2MASS J01282664-5545343 | 111 | L2 | 112 | L1 | 111 | 54.0168$\pm$0.2345 | 258.7$\pm$0.8 | 168 | 1955$\pm$88 |
CFBDS J013302.27+023128.4 | 5 |  $\cdots$ |  $\cdots$ | T8.5 | 5 | 53.1$\pm$2.6 | 617.0$\pm$1.8 | 0 | 661$\pm$88 |
SIMP J013656.57+093347.3 | 186 | T2 | 214 | T2 | 124 | 162.13$\pm$0.57 | 1237.9$\pm$0.2 | 172 | 1051$\pm$198 | yng
CWISE J014308.73$-$703359.1 | 0 |  $\cdots$ |  $\cdots$ | [T7.5] | 0 | [51.3] | 271.7$\pm$32.0 | 0 | 751$\pm$79 |
2MASS J01443536-0716142 | 113 | L5 | 113 | L4.5 | 124 | 79.0319$\pm$0.6240 | 431.6$\pm$1.3 | 168 | 1628$\pm$88 |
WISE J014656.66+423410.0A | 2 |  $\cdots$ |  $\cdots$ | T9 | 2 | 51.7$\pm$2.0 | 452.8$\pm$1.3 | 0 | 566$\pm$79 |
WISE J014656.66+423410.0B | 206 |  $\cdots$ |  $\cdots$ | Y0 | 2 | 51.7$\pm$2.0 | 452.8$\pm$1.3 | 0 | 460$\pm$79 |
WISEPC J014807.25$-$720258.7 | 4 |  $\cdots$ |  $\cdots$ | T9.5 | 4 | 91.7$\pm$3.4 | 1269.3$\pm$4.1 | 21,1 | 526$\pm$88 |
CWISE J014837.51$-$104805.6 | 0 |  $\cdots$ |  $\cdots$ | [T8.5] | 0 | [66.8] | 252.9$\pm$11.4 | 0 | 624$\pm$79 |
CWISE J015349.89+613746.3 | 0 |  $\cdots$ |  $\cdots$ | [T0] | 0 | [52.4] | 203.6$\pm$9.2 | 0 | 1254$\pm$79 |
DENIS-P J0205.4$-$1159A | 138 |  $\cdots$ |  $\cdots$ | [L5] | 202 | 53.67$\pm$1.12 | 432.3$\pm$0.2 | 172 | 1613$\pm$134 |
DENIS-P J0205.4$-$1159B | 203 |  $\cdots$ |  $\cdots$ | [L8] | 202 | 53.67$\pm$1.12 | 432.3$\pm$0.2 | 172 | 1335$\pm$134 |
DENIS-P J0205.4$-$1159[C] | 202 |  $\cdots$ |  $\cdots$ | [T0] | 202 | 53.67$\pm$1.12 | 432.3$\pm$0.2 | 172 | 1254$\pm$79 |
WISEPA J020625.26+264023.6 | 4 |  $\cdots$ |  $\cdots$ | L9 pec (red) | 4 | 52.1$\pm$1.4 | 444.7$\pm$3.1 | 198 | 1281$\pm$88 |
2MASS J02132062+3648506C | 80 |  $\cdots$ |  $\cdots$ | T3 | 80 | 70.0180$\pm$0.2041 | 92.1$\pm$0.6 | 168aaThe astrometry listed is for the primary star in the system. | 1175$\pm$88 |
2MASSI J0213288+444445 | 115 | L1.5 | 115 |  $\cdots$ |  $\cdots$ | 51.6812$\pm$0.3832 | 154.8$\pm$0.7 | 168 | 2056$\pm$88 |
WISEPC J022322.39$-$293258.1 | 4 |  $\cdots$ |  $\cdots$ | T7.5 | 4 | 80.7$\pm$2.6 | 946.1$\pm$1.9 | 1 | 706$\pm$88 |
WISEPA J022623.98$-$021142.8A | 4 |  $\cdots$ |  $\cdots$ | [T8] | 1 | 51.1$\pm$2.3 | 522.6$\pm$2.3 | 237 | 686$\pm$79 |
WISEPA J022623.98$-$021142.8B | 1 |  $\cdots$ |  $\cdots$ | [T9.5] | 1 | 51.1$\pm$2.3 | 522.6$\pm$2.3 | 237 | 511$\pm$79 |
CWISEP J023842.60-133210.7 | 232 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 232 | 85.8$\pm$21.4 | 771.00$\pm$73.32 | 0 | 367$\pm$79 | [55.6]
WISE J024124.73$-$365328.0 | 2 |  $\cdots$ |  $\cdots$ | T7 | 2 | 53.1$\pm$2.5 | 281.3$\pm$1.5 | 0 | 868$\pm$88 |
2MASSI J0243137$-$245329 | 32 | T5.5 | 214 | T6 | 61 | 93.62$\pm$3.63 | 354.8$\pm$4.1 | 68 | 972$\pm$83 |
WISE J024714.52+372523.5 | 8 |  $\cdots$ |  $\cdots$ | T8 | 8 | 64.8$\pm$2.0 | 92.6$\pm$1.8 | 237 | 656$\pm$88 |
2MASSI J0251148-035245 | 115 | L3 | 115 | L1 | 109 | 90.62$\pm$3.02 | 2149.7$\pm$0.9 | 169 | 1786$\pm$88 |
WISEPA J025409.45+022359.1 | 4,33 |  $\cdots$ |  $\cdots$ | T8 | 4 | 146.1$\pm$1.5 | 2572.2$\pm$0.1 | 1 | 621$\pm$73 |
DENIS-P J0255$-$4700 (025503$-$470051) | 81 | L8 | 103 | L9 | 61 | 205.3266$\pm$0.2545 | 1153.4$\pm$0.6 | 168 | 1290$\pm$78 |
2MASS J02572581$-$3105523 | 103 | L8 | 103 | L6 | 124 | 102.3651$\pm$0.6073 | 712.5$\pm$1.1 | 168 | 1311$\pm$88 |
WISEA J030237.53$-$581740.3 | 6 |  $\cdots$ |  $\cdots$ | Y0: | 6 | 59.9$\pm$3.3 | 87.8$\pm$5.0 | 0 | 460$\pm$79 |
WISE J030449.03$-$270508.3 | 7 |  $\cdots$ |  $\cdots$ | Y0 pec | 7 | 73.1$\pm$2.6 | 509.8$\pm$3.2 | 0 | 465$\pm$88 |
WISEA J030919.70$-$501614.2A | 6 |  $\cdots$ |  $\cdots$ | T7 | 236 | 62.2$\pm$2.8 | 566.8$\pm$1.9 | 0 | 819$\pm$79 |
WISEA J030919.70$-$501614.2[B] | 1 |  $\cdots$ |  $\cdots$ | [T7] | 6 | 62.2$\pm$2.8 | 566.8$\pm$1.9 | 0 | 819$\pm$79 |
2MASS J03101401$-$2756452 | 194 | L5: | 194 | L6.5 | 106 | [50.2] | 132.8$\pm$3.6 | 0 | 1465$\pm$134 |
WISEPA J031325.96+780744.2 | 4 |  $\cdots$ |  $\cdots$ | T8.5 | 4 | 135.6$\pm$2.8 | 91.4$\pm$1.4 | 0 | 570$\pm$88 |
2MASS J03140344+1603056 | 117 | L0 | 117 | M9.4 | 106 | 73.4296$\pm$0.2757 | 248.6$\pm$0.5 | 168 | 2129$\pm$88 |
WISE J031624.35+430709.1 | 8 |  $\cdots$ |  $\cdots$ | T8 | 8 | 74.7$\pm$2.1 | 439.0$\pm$1.3 | 0 | 520$\pm$88 |
2MASS J03185403$-$3421292 | 103 | L7 | 103 | L6.5 | 124 | 74.1$\pm$4.6 | 398.1$\pm$3.0 | 0 | 1344$\pm$107 |
CWISEP J032109.59+693204.5 | 232 |  $\cdots$ |  $\cdots$ | [Y0.5] | 232 | 68.5$\pm$4.0 | 993.5$\pm$13.9 | 0 | 412$\pm$79 |
WISE J032301.86+562558.0 | 184 |  $\cdots$ |  $\cdots$ | L7 | 194 | 51.9$\pm$3.0 | 434.3$\pm$2.7 | 0 | 1493$\pm$88 |
WISEA J032309.12$-$590751.0 | 1 |  $\cdots$ |  $\cdots$ | T7 | 236 | 72.1$\pm$2.9 | 735.6$\pm$2.1 | 0 | 819$\pm$79 |
WISEPC J032337.53$-$602554.9 | 4 |  $\cdots$ |  $\cdots$ | T8.5 | 4 | 71.7$\pm$2.3 | 543.0$\pm$1.4 | 0 | 617$\pm$88 |
WISE J032517.69$-$385454.1 | 8 |  $\cdots$ |  $\cdots$ | T9 | 8 | 60.2$\pm$3.5 | 308.4$\pm$2.1 | 0 | 556$\pm$88 |
WISE J032547.72+083118.2 | 8 |  $\cdots$ |  $\cdots$ | T7 | 8 | 76.3$\pm$2.8 | 135.0$\pm$2.0 | 0 | 885$\pm$88 |
PSO J052.7214$-$03.8409 (033053$-$035027) | 181 |  $\cdots$ |  $\cdots$ | L9: | 181 | 59.2$\pm$3.3 | 147.2$\pm$3.7 | 0 | 1197$\pm$88 |
WISE J033515.01+431045.1 | 8 |  $\cdots$ |  $\cdots$ | T9 | 8 | 84.8$\pm$1.7 | 1142.3$\pm$0.9 | 0 | 495$\pm$88 |
WISE J033605.05$-$014350.4 | 8 |  $\cdots$ |  $\cdots$ | Y0 | 22 | 99.8$\pm$2.1 | 1241.8$\pm$1.3 | 0 | 460$\pm$79 |
2MASS J03400942$-$6724051 | 120 |  $\cdots$ |  $\cdots$ | L7:: | 120 | 107.1165$\pm$0.6174 | 598.0$\pm$2.3 | 168 | 1267$\pm$88 |
2MASS J03480772$-$6022270 | 34 |  $\cdots$ |  $\cdots$ | T7 | 61 | 120.1$\pm$1.8 | 817.8$\pm$0.9 | 1 | 823$\pm$88 |
WISE J035000.32$-$565830.2 | 2 |  $\cdots$ |  $\cdots$ | Y1 | 2 | 176.4$\pm$2.3 | 612.1$\pm$1.5 | 0 | 388$\pm$88 |
2MASS J03552337+1133437 | 117 | L5$\gamma$ | 110 | L3-L6$\gamma$ | 175 | 109.6451$\pm$0.7368 | 668.4$\pm$1.8 | 168 | 1478$\pm$58 | yng
UGPS J03553200+4743588 | 83 |  $\cdots$ |  $\cdots$ | [T6] | 83 | 66.4$\pm$3.2 | 538.5$\pm$8.1 | 0 | 864$\pm$88 |
WISE J035934.06$-$540154.6 | 2 |  $\cdots$ |  $\cdots$ | Y0 | 2 | 73.6$\pm$2.0 | 770.7$\pm$1.1 | 0 | 436$\pm$88 |
WISE J040137.21+284951.7 | 119 | L3 | 119 | L2.5 | 119 | 80.2894$\pm$0.2615 | 480.9$\pm$0.6 | 168 | 1816$\pm$88 |
CWISEP J040235.55-265145.4 | 232 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 232 | 116.4$\pm$20.5 | 934.0$\pm$34.5 | 0 | 367$\pm$79 | [82.5]
WISE J040418.01+412735.6 | 119 | L2 | 119 | L3 pec (red) | 15 | 61.7516$\pm$0.4163 | 396.1$\pm$1.2 | 168 | 1780$\pm$88 |
2MASS J04070885+1514565 | 3 |  $\cdots$ |  $\cdots$ | T5.5 | 124 | 56.74$\pm$2.07 | 237.7$\pm$0.7 | 200 | 1027$\pm$88 |
WISEPA J041022.71+150248.5 | 10 |  $\cdots$ |  $\cdots$ | Y0 | 10 | 151.3$\pm$2.0 | 2418.3$\pm$1.1 | 0 | 451$\pm$88 |
CWISE J041102.41+471422.6 | 0 |  $\cdots$ |  $\cdots$ | [T7] | 0 | [61.0] | 463.1$\pm$35.8 | 0 | 819$\pm$79 |
Gaia J041246.85$-$073416.8ffThe Gaia DR2 identifications for these sources are given in Table 17 and are: Gaia J041246.85$-$073416.8 = Gaia DR2 3195979005694112768, Gaia J171340.47$-$395211.8 = Gaia DR2 5972124644679705728, Gaia J183118.29$-$073227.6 = Gaia DR2 4159791176135290752, Gaia J183610.72+031524.6 = Gaia DR2 4283084190940885888, Gaia J195557.27+321518.2 = Gaia DR2 2034222547248988032. | 229 | [L1:] | 229 | L2 pec | 0 | 59.6888$\pm$0.3365 | 592.3$\pm$0.5 | 168 | 1963$\pm$134 |
WISE J041358.14$-$475039.3 | 8 |  $\cdots$ |  $\cdots$ | T9 | 8 | 50.7$\pm$3.3 | 329.5$\pm$3.4 | 0 | 540$\pm$88 |
2MASS J04134574+3709087 | 133 | [L1] | 220 |  $\cdots$ |  $\cdots$ | 51.6559$\pm$0.3322 | 684.5$\pm$0.9 | 168 | 1965$\pm$88 |
2MASSI J0415195$-$093506 | 32 | T8 | 197 | T8 | 61 | 175.2$\pm$1.7 | 2278.2$\pm$1.2 | 67 | 677$\pm$56 |
WISEA J041743.13+241506.3 | 238 |  $\cdots$ |  $\cdots$ | T6 | 236 | [84.0] | 470.5$\pm$16.0 | 0 | 965$\pm$79 |
2MASS J04210718$-$6306022 | 120 | L5$\beta$ | 110 | L5$\gamma$ | 275 | 50.0$\pm$3.3 | 265.0$\pm$2.9 | 0 | 1388$\pm$197 | yng
SDSSp J042348.57$-$041403.5A | 122 |  $\cdots$ |  $\cdots$ | L6.5: | 67 | 67.8584$\pm$1.5052 | 354.2$\pm$2.3 | 168 | 1465$\pm$134 |
SDSSp J042348.57$-$041403.5B | 208 |  $\cdots$ |  $\cdots$ | T2 | 67 | 67.8584$\pm$1.5052 | 354.2$\pm$2.3 | 168 | 1218$\pm$79 |
CWISE 042455.69+000221.5 | 232 |  $\cdots$ |  $\cdots$ | T9: | 0 | [53.2] | 208.7$\pm$35.0 | 0 | 566$\pm$79 |
2MASS J04250679$-$4255085 | 158 |  $\cdots$ |  $\cdots$ | L8 | 158 | [59.7] | 156.1$\pm$7.2 | 0 | 1335$\pm$134 |
WISE J043052.92+463331.6 | 8 |  $\cdots$ |  $\cdots$ | T8 | 8 | 96.1$\pm$2.9 | 961.4$\pm$2.6 | 0 | 516$\pm$88 |
2MASSI J0439010$-$235308 | 115 | L6.5 | 115 | L6 | 124 | 80.7917$\pm$0.5139 | 190.7$\pm$1.1 | 168 | 1290$\pm$82 |
2MASSI J0445538$-$304820 | 115 | L2 | 115 |  $\cdots$ |  $\cdots$ | 61.9685$\pm$0.1843 | 449.7$\pm$0.5 | 168 | 1809$\pm$90 |
WISEPA J044853.29$-$193548.5 | 4 |  $\cdots$ |  $\cdots$ | T5 pec | 4 | 57.6$\pm$3.0 | 1179.5$\pm$1.3 | 0 | 950$\pm$88 | sd
WISE J045746.08$-$020719.2 | 35 |  $\cdots$ |  $\cdots$ | T2 | 35 | 82.0$\pm$2.9 | 140.4$\pm$3.7 | 237 | 1259$\pm$88 |
WISEPA J045853.89+643452.9A | 11 |  $\cdots$ |  $\cdots$ | T8.5 | 10 | 106.7$\pm$2.8 | 358.0$\pm$1.4 | 0 | 624$\pm$79 |
WISEPA J045853.89+643452.9B | 56 |  $\cdots$ |  $\cdots$ | T9.5 | 10 | 106.7$\pm$2.8 | 358.0$\pm$1.4 | 0 | 511$\pm$79 |
WISEPA J050003.05$-$122343.2 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 84.6$\pm$2.2 | 724.8$\pm$2.5 | 237 | 614$\pm$88 |
2MASS J05002100+0330501 | 117 | L4 | 117 | L4.1 | 106 | 76.2093$\pm$0.3565 | 351.8$\pm$0.7 | 168 | 1793$\pm$72 |
WISEU J050305.68-564834.0 | 233 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 233 | 98.3$\pm$3.9 | 812.1$\pm$13.7 | 0 | 367$\pm$79 |
PSO J076.7092+52.6087 (050650+523631) | 181 |  $\cdots$ |  $\cdots$ | T4.5 | 181 | 61.3$\pm$3.1 | 208.3$\pm$5.7 | 0 | 1135$\pm$88 |
WISE J050854.88+331920.8 | 16 | L2 | 149 |  $\cdots$ |  $\cdots$ | 52.9819$\pm$0.6076 | 654.1$\pm$1.4 | 168 | 1850$\pm$88 |
2MASS J05103524$-$4208146 | 24 |  $\cdots$ |  $\cdots$ | T5 | 24 | 53.8$\pm$2.4 | 592.1$\pm$1.5 | 200 | 1006$\pm$88 |
WISEPA J051317.28+060814.7 | 4 |  $\cdots$ |  $\cdots$ | T6.5 | 4 | 70.8$\pm$1.5 | 433.0$\pm$1.0 | 1 | 916$\pm$88 |
CWISE J051427.35+200447.7 | 0 |  $\cdots$ |  $\cdots$ | T0.5 | 0 | [54.1] | 103.8$\pm$10.0 | 0 | 1245$\pm$79 |
WISE J052126.29+102528.4 | 35 |  $\cdots$ |  $\cdots$ | T7.5 | 35 | 150.2$\pm$3.0 | 492.1$\pm$3.5 | 0 | 727$\pm$88 |
UGPS J052127.27+364048.6 | 46 |  $\cdots$ |  $\cdots$ | T8.5 | 46 | 122.2$\pm$1.6 | 1614.6$\pm$1.3 | 1 | 616$\pm$88 |
2MASSI J0523382-140302 | 115 | L2.5 | 115 | L5 | 109 | 78.3632$\pm$0.1855 | 193.4$\pm$0.4 | 168 | 1939$\pm$68 |
WISE J053516.80$-$750024.9 | 2 |  $\cdots$ |  $\cdots$ |  $\geq$Y1: | 2 | 68.7$\pm$2.0 | 122.4$\pm$1.1 | 0 | 410$\pm$88 |
CWISEP J053644.82-305539.3 | 232 |  $\cdots$ |  $\cdots$ | [T9.5] | 0 | 78.1$\pm$3.8 | 37.4$\pm$13.7 | 0 | 511$\pm$79 |
SDSSp J053951.99-005902.0 | 121 | L5 | 121 | L5 | 122 | 78.5318$\pm$0.5707 | 359.9$\pm$1.1 | 168 | 1659$\pm$74 |
CWISE J054025.89$-$180240.3 | 0 |  $\cdots$ |  $\cdots$ | T5 | 0 | 59.2$\pm$4.0 | 94.6$\pm$3.8 | 237 | 982$\pm$88 |
WISE J054047.00+483232.4 | 8 |  $\cdots$ |  $\cdots$ | T8.5 | 8 | 69.4$\pm$2.1 | 678.8$\pm$1.3 | 0 | 606$\pm$88 |
WISEPA J054231.26$-$162829.1 | 4 |  $\cdots$ |  $\cdots$ | T6.5 | 4 | 61.3$\pm$2.6 | 371.0$\pm$3.5 | 237 | 895$\pm$88 |
WISE J054601.19$-$095947.5 | 8 |  $\cdots$ |  $\cdots$ | T5 | 8 | 50.4$\pm$3.6 | 11.7$\pm$3.5 | 237 | 1105$\pm$88 |
2MASS J05591914$-$1404488 | 51 | T5 | 197 | T4.5 | 124 | 97.28$\pm$0.59 | 661.5$\pm$0.2 | 172 | 1301$\pm$75 |
CWISE J060149.45+141955.2 | 0 |  $\cdots$ |  $\cdots$ | T2.5 | 0 | [54.3] | 234.6$\pm$10.1 | 0 | 1209$\pm$79 |
2MASS J06020638+4043588 | 24 |  $\cdots$ |  $\cdots$ | T4.5 | 24 | 76.4$\pm$3.1 | 324.0$\pm$2.1 | 0 | 985$\pm$88 |
LSR J0602+3910 (060230+391058) | 123 | L1 | 123 | L1$\beta$ | 175 | 85.6140$\pm$0.1663 | 530.0$\pm$0.4 | 168 | 1857$\pm$133 | yng
WISEP J060738.65+242953.4 | 119 | L8 | 119 | L9 | 20 | 136.9449$\pm$0.6553 | 572.7$\pm$1.4 | 168 | 1271$\pm$88 |
Gl 229B (061034$-$215200) | 36 |  $\cdots$ |  $\cdots$ | T7pec | 61 | 173.6955$\pm$0.0457 | 731.8$\pm$0.2 | 168aaThe astrometry listed is for the primary star in the system. | 927$\pm$77 |
WISEPA J061407.49+391236.4A | 4 |  $\cdots$ |  $\cdots$ | [T6] | 1 | 53.7$\pm$1.7 | 529.3$\pm$1.2 | 1 | 965$\pm$79 |
WISEPA J061407.49+391236.4B | 1 |  $\cdots$ |  $\cdots$ | [T8] | 1 | 53.7$\pm$1.7 | 529.3$\pm$1.2 | 1 | 686$\pm$79 |
WISE J061437.73+095135.0 | 8 |  $\cdots$ |  $\cdots$ | T7 | 8 | 64.9$\pm$2.0 | 416.4$\pm$1.1 | 0 | 833$\pm$88 |
WISEA J061557.21+152626.1 | 22 |  $\cdots$ |  $\cdots$ | T8.5 | 22 | 52.8$\pm$3.1 | 532.9$\pm$3.6 | 0 | 624$\pm$88 |
CWISE J061741.79+194512.8A | 0 |  $\cdots$ |  $\cdots$ | [L6.5] | 0 | [133.0] | 119.8$\pm$5.5 | 0 | 1465$\pm$134 |
CWISE J061741.79+194512.8B | 0 |  $\cdots$ |  $\cdots$ | [T8:] | 0 | [133.0] | 119.8$\pm$5.5 | 0 | 686$\pm$79 |
CWISE J062050.79$-$300620.8 | 0 |  $\cdots$ |  $\cdots$ | T2.5 | 0 | [54.6] | 147.7$\pm$12.3 | 0 | 1209$\pm$79 |
WISEPA J062309.94$-$045624.6 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 86.5$\pm$1.7 | 921.9$\pm$2.4 | 237 | 688$\pm$88 |
2MASS J06244595-4521548 | 117 | L5 | 117 | L5 | 124 | 81.6233$\pm$0.4986 | 378.4$\pm$1.5 | 168 | 1501$\pm$85 |
WISEPA J062720.07$-$111428.8 | 4 |  $\cdots$ |  $\cdots$ | T6 | 4 | 74.8$\pm$3.6 | 338.1$\pm$1.6 | 1 | 1023$\pm$88 |
CWISEP J063428.10+504925.9 | 232 |  $\cdots$ |  $\cdots$ | [Y0] | 232 | 62.0$\pm$4.2 | 1192.4$\pm$19.2 | 0 | 460$\pm$79 |
2MASS J06411840-4322329 | 112 | L1.5 | 112 | L2.4: | 106 | 51.2819$\pm$0.1930 | 666.6$\pm$0.5 | 168 | 1927$\pm$120 |
WISE J064205.58+410155.5 | 8 |  $\cdots$ |  $\cdots$ | extr. red | 8 | 62.6$\pm$3.1 | 383.1$\pm$1.7 | 0 | 1185$\pm$88 |
WISE J064336.71$-$022315.4 | 228 |  $\cdots$ |  $\cdots$ | L8 | 228 | 71.9172$\pm$1.3761 | 223.0$\pm$3.4 | 168 | 1286$\pm$88 |
WISEA J064503.72+524054.1 | 233 |  $\cdots$ |  $\cdots$ | [T8.5] | 233 | 53.5$\pm$4.2 | 982.1$\pm$16.3 | 0 | 624$\pm$79 |
WISEA J064528.39$-$030247.9 | 6 |  $\cdots$ |  $\cdots$ | T6 | 6 | 54.1$\pm$3.0 | 322.2$\pm$2.2 | 0 | 817$\pm$88 |
2MASS J06453153$-$6646120 | 133 | sdL8 | 133 | sdL8 | 133 | 53.8$\pm$2.9 | 1582.3$\pm$2.6 | 0 | 1369$\pm$88 | sd
HD 46588B (064627+793504) | 84 |  $\cdots$ |  $\cdots$ | L9: | 84 | 54.9292$\pm$0.1076 | 612.0$\pm$0.3 | 168aaThe astrometry listed is for the primary star in the system. | 1257$\pm$88 |
WISE J064723.23$-$623235.5 | 12 |  $\cdots$ |  $\cdots$ | Y1 | 12 | 99.5$\pm$1.7 | 393.9$\pm$0.9 | 0 | 393$\pm$88 |
WISEA J064750.85$-$154616.4 | 85 |  $\cdots$ |  $\cdots$ | L9.5 | 85 | 62.7$\pm$3.3 | 178.4$\pm$3.0 | 0 | 1391$\pm$88 |
PSO J103.0927+41.4601 (065222+412736) | 86 |  $\cdots$ |  $\cdots$ | T0 | 86 | 57.6$\pm$3.3 | 41.0$\pm$3.2 | 0 | 1395$\pm$88 |
2MASSI J0652307+471034 | 115 | L4.5 | 115 | L6.5 | 124 | 110.31$\pm$0.29 | 181.7$\pm$0.1 | 172 | 1597$\pm$88 |
WISEPA J065609.60+420531.0 | 4 | T2 | 214 | T3 | 4 | 63.0$\pm$4.1 | 356.7$\pm$5.5 | 237 | 1235$\pm$88 |
2MASS J07003664+3157266A | 125 | L3 | 117 | L3: | 102 | 88.2790$\pm$0.3479 | 559.9$\pm$0.7 | 168 | 1838$\pm$134 |
2MASS J07003664+3157266B | 117 | L6.5 | 117 | L6.5: | 102 | 88.2790$\pm$0.3479 | 559.9$\pm$0.7 | 168 | 1465$\pm$134 |
2MASS J07003664+3157266[C] | 180 | L6.5:: | 180 |  $\cdots$ |  $\cdots$ | 88.2790$\pm$0.3479 | 559.9$\pm$0.7 | 168 | 1465$\pm$134 |
WISE J070159.79+632129.2 | 8 |  $\cdots$ |  $\cdots$ | T3 | 8 | 52.6$\pm$3.0 | 263.0$\pm$1.4 | 0 | 1281$\pm$88 |
WISEA J071301.86$-$585445.2 | 6 |  $\cdots$ |  $\cdots$ | T9 | 6 | 82.1$\pm$3.0 | 372.3$\pm$2.5 | 0 | 521$\pm$88 |
WISE J071322.55$-$291751.9 | 2 |  $\cdots$ |  $\cdots$ | Y0 | 2 | 109.3$\pm$2.1 | 542.0$\pm$1.3 | 0 | 464$\pm$88 |
WISEA J071552.38-114532.9 | 126 |  $\cdots$ |  $\cdots$ | L4 pec (blue) | 126 | 55.5855$\pm$0.3446 | 803.3$\pm$0.8 | 168 | 1154$\pm$88 |
WISE 072003.20$-$084651.2B | 238 |  $\cdots$ |  $\cdots$ | [T5.5] | 239 | 147.1$\pm$1.2 | 125.3$\pm$4.6 | 240 | 1183$\pm$88 |
UGPS J072227.51$-$054031.2 | 37 | T9 | 4 | T9 | 10 | 242.8$\pm$2.4 | 970.3$\pm$2.1 | 40 | 569$\pm$45 |
WISE J072312.44+340313.5 | 8 |  $\cdots$ |  $\cdots$ | T9: | 8 | 60.8$\pm$2.1 | 348.1$\pm$1.2 | 0 | 631$\pm$88 |
2MASSI J0727182+171001 | 32 | T8 | 197 | T7 | 61 | 112.5$\pm$0.9 | 1296.2$\pm$0.9 | 67 | 845$\pm$71 |
2MASS J07290002$-$3954043 | 24 |  $\cdots$ |  $\cdots$ | T8 pec | 24 | 126.3$\pm$8.3 | 1738.3$\pm$7.6 | 66 | 752$\pm$69 | sd
WISE J073444.02$-$715744.0 | 2 |  $\cdots$ |  $\cdots$ | Y0 | 2 | 74.5$\pm$1.7 | 569.0$\pm$0.9 | 0 | 462$\pm$88 |
SDSS J074149.15+235127.5 | 57 |  $\cdots$ |  $\cdots$ | T5.5 | 124 | 73.2$\pm$3.4 | 343.8$\pm$2.2 | 0 | 909$\pm$88 |
SDSS J074201.41+205520.5 | 57 |  $\cdots$ |  $\cdots$ | T5 | 124 | 63.5$\pm$3.1 | 400.3$\pm$1.1 | 0 | 958$\pm$102 |
WISEPA J074457.15+562821.8 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 65.3$\pm$2.0 | 781.7$\pm$1.1 | 0 | 726$\pm$88 |
ULAS J074502.79+233240.3 | 19 |  $\cdots$ |  $\cdots$ | T8.5 | 19 | [$\geq$51.5] |  $\cdots$ | - | 624$\pm$79 |
2MASSI J0746425+200032A | 107 | L0 | 128 |  $\cdots$ |  $\cdots$ | 81.9$\pm$0.3 | 378.5$\pm$0.3 | 170 | 2237$\pm$134 |
2MASSI J0746425+200032B | 127 | L1.5 | 128 |  $\cdots$ |  $\cdots$ | 81.9$\pm$0.3 | 378.5$\pm$0.3 | 170 | 2029$\pm$134 |
WISEPA J075003.84+272544.8 | 4 |  $\cdots$ |  $\cdots$ | T8.5 | 4 | 68.4$\pm$3.4 | 783.2$\pm$2.7 | 1 | 583$\pm$88 |
WISEPA J075108.79$-$763449.6 | 4 |  $\cdots$ |  $\cdots$ | T9 | 4 | 97.9$\pm$6.7 | 216.7$\pm$5.3 | 1 | 492$\pm$88 |
DENIS-P J0751164-253043 | 129 | L1.5 | 129 | L1.1 | 106 | 56.5689$\pm$0.1555 | 891.0$\pm$0.3 | 168 | 2083$\pm$64 |
WISE J075430.95+790957.8 | 8 |  $\cdots$ |  $\cdots$ | extr. red | 8 | 51.1$\pm$1.2 | 437.3$\pm$3.0 | 198 | 1248$\pm$88 |
2MASSI J0755480+221218 | 32 | T6 | 197 | T5 | 124 | 67.4$\pm$3.2 | 257.1$\pm$1.4 | 0 | 1001$\pm$88 |
HIP 38939B (075804$-$253735) | 88 |  $\cdots$ |  $\cdots$ | T4.5 | 88 | 54.1012$\pm$0.0386 | 437.8$\pm$0.1 | 168aaThe astrometry listed is for the primary star in the system. | 1095$\pm$88 |
SDSS J075840.33+324723.4 | 57 | T3 | 214 | T2.5 | 124 | 101.3$\pm$3.3 | 400.9$\pm$1.5 | 0 | 1169$\pm$88 |
WISEPC J075946.98$-$490454.0 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 90.7$\pm$2.1 | 447.1$\pm$1.1 | 0 | 666$\pm$88 |
CWISE J080556.14+515330.4 | 0 |  $\cdots$ |  $\cdots$ | [T7.5] | 0 | [64.2] | 578.0$\pm$28.3 | 0 | 751$\pm$79 |
WISEA J080622.22-082046.5 | 233 |  $\cdots$ |  $\cdots$ | [T8] | 233 | 82.2$\pm$9.0 | 1331.1$\pm$36.3 | 0 | 819$\pm$79 |
WISE J080700.23+413026.8 | 20 |  $\cdots$ |  $\cdots$ | L8 pec | 20 | 50.7$\pm$3.3 | 346.6$\pm$1.8 | 0 | 1383$\pm$88 |
WD 0806$-$661B (080714$-$661848) | 65 |  $\cdots$ |  $\cdots$ | [Y1] | 1 | 51.9342$\pm$0.0195 | 442.8$\pm$0.1 | 168aaThe astrometry listed is for the primary star in the system. | 377$\pm$88 |
WISE J081117.81$-$805141.3 | 8 |  $\cdots$ |  $\cdots$ | T9.5: | 8 | 99.1$\pm$7.7 | 293.4$\pm$6.9 | 21,1 | 479$\pm$88 |
DENIS J081730.0$-$615520 | 38 |  $\cdots$ |  $\cdots$ | T6 | 38 | 191.5301$\pm$0.6037 | 1110.7$\pm$1.7 | 168 | 1004$\pm$91 |
WISEPA J081958.05$-$033529.0 | 4 | T4 | 214 | T4 | 4 | 71.4$\pm$2.2 | 250.5$\pm$1.0 | 200 | 1225$\pm$88 |
WISE J082000.48$-$662211.9 | 184 |  $\cdots$ |  $\cdots$ | L9.5 | 184 | 56.1$\pm$3.4 | 355.9$\pm$2.9 | 0 | 1206$\pm$88 |
WISE J082507.35+280548.5 | 9 |  $\cdots$ |  $\cdots$ | Y0.5 | 9 | 152.6$\pm$2.0 | 245.1$\pm$1.3 | 0 | 376$\pm$88 |
2MASSI J0825196+211552 | 105 | L7.5 | 105 | L7 | 124 | 93.19$\pm$0.59 | 581.1$\pm$0.2 | 172 | 1341$\pm$73 |
WISEA J082640.45$-$164031.8 | 15 |  $\cdots$ |  $\cdots$ | L9 | 15 | 67.8$\pm$3.5 | 985.8$\pm$3.8 | 0 | 1263$\pm$88 |
SSSPM J0829-1309 (082834-130919) | 130 | L2 | 130 |  $\cdots$ |  $\cdots$ | 85.5438$\pm$0.1720 | 582.2$\pm$0.3 | 168 | 1983$\pm$88 |
SDSSp J083008.12+482847.4 | 122 | L8 | 103 | L9.5$\pm$1 | 124 | 76.42$\pm$3.43 | 1267.0$\pm$6.5 | 68 | 1258$\pm$97 |
WISEA J083011.95+283716.0 | 234 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 234 | 90.6$\pm$13.7 | 2054.1$\pm$57.1 | 0 | 367$\pm$79 | [121.4]
WISE J083337.83+005214.2 | 13 |  $\cdots$ |  $\cdots$ | (sd)T9 | 13 | 79.7$\pm$3.1 | 1777.3$\pm$2.9 | 0 | 472$\pm$88 | sd
2MASSI J0835425$-$081923 | 115 | L5 | 115 | L5 | 124 | 138.6098$\pm$0.2781 | 615.3$\pm$0.6 | 168 | 1754$\pm$112 |
CWISE J084506.51$-$330532.7 | 0 |  $\cdots$ |  $\cdots$ | T7 | 0 | [57.3] | 1061.8$\pm$35.1 | 0 | 819$\pm$79 |
2MASSI J0847287-153237 | 115 | L2 | 115 |  $\cdots$ |  $\cdots$ | 56.9235$\pm$0.3167 | 239.8$\pm$0.8 | 168 | 1794$\pm$81 |
WISE J085510.83$-$071442.5 | 14,16 |  $\cdots$ |  $\cdots$ | [Y4] | 1 | 439.0$\pm$2.4 | 8151.6$\pm$1.8 | 0 | 250$\pm$50 |
WISEPA J085716.25+560407.6 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 85.3$\pm$2.1 | 754.9$\pm$1.3 | 0 | 671$\pm$88 |
SDSSp J085758.45+570851.4 | 122 | L8 | 103 | L8 | 175 | 71.2343$\pm$1.0255 | 565.5$\pm$2.3 | 168 | 1455$\pm$88 |
ULAS J085910.69+101017.1 | 64 |  $\cdots$ |  $\cdots$ | T7 | 64 | 50.3$\pm$1.7 | 712.7$\pm$1.6 | 1 | 709$\pm$88 |
2MASSI J0859254$-$194926 | 115 | L7: | 120 | L8 | 20 | 71.22$\pm$3.54 | 337.5$\pm$1.0 | 199 | 1374$\pm$100 |
CWISEP J085908.26+152527.1 | 232 |  $\cdots$ |  $\cdots$ | [T8] | 232 | [53.2] | 271.9$\pm$61.1 | 0 | 686$\pm$79 |
CWISEP J085938.95+534908.7 | 232 |  $\cdots$ |  $\cdots$ | [Y0] | 232 | [53.8] | 392.4$\pm$52.3 | 0 | 460$\pm$79 |
ULAS J090116.23$-$030635.0 | 39 |  $\cdots$ |  $\cdots$ | T7.5 | 39 | 62.6$\pm$2.6 | 264.0$\pm$3.6 | 70 | 638$\pm$88 |
2MASSI J0908380+503208 | 115 | L5 | 115 | L6 | 124 | 95.8202$\pm$0.6983 | 628.6$\pm$2.2 | 168 | 1360$\pm$88 |
SDSS J090900.73+652527.2 | 53 |  $\cdots$ |  $\cdots$ | T1.5 | 124 | 63.9$\pm$3.9 | 253.0$\pm$1.8 | 0 | 1146$\pm$88 |
CWISE J091105.02+214645.1 | 0 |  $\cdots$ |  $\cdots$ | T9 | 0 | [72.8] | 667.0$\pm$2.5 | 0 | 566$\pm$79 |
2MASS J09153413+0422045A | 117 | L6: | 209 |  $\cdots$ |  $\cdots$ | 54.8460$\pm$1.0970 | 112.9$\pm$2.8 | 168 | 1512$\pm$134 |
2MASS J09153413+0422045B | 117 | L7:: | 209 |  $\cdots$ |  $\cdots$ | 54.8460$\pm$1.0970 | 112.9$\pm$2.8 | 168 | 1420$\pm$134 |
CWISE J091735.38$-$634451.2 | 0 |  $\cdots$ |  $\cdots$ | L7 | 0 | [62.2] | 110.0$\pm$8.8 | 0 | 1420$\pm$134 |
WISE J092055.40+453856.3 | 89 |  $\cdots$ |  $\cdots$ | L9 | 8 | 79.4$\pm$3.9 | 856.6$\pm$4.8 | 237 | 1288$\pm$88 |
SIPS J0921$-$2104 (092114$-$210444) | 117,131 | L2 | 117 | L4: (blue) | 132,133 | 79.3128$\pm$0.2253 | 944.2$\pm$0.5 | 168 | 1930$\pm$88 |
CWISE J092503.20$-$472013.8 | 0 |  $\cdots$ |  $\cdots$ | [Y0] | 0 | [93.3] | 808.0$\pm$57.2 | 0 | 460$\pm$79 |
2MASSI J0937347+293142 | 32 | T7 | 197 | T6pec | 61 | 162.84$\pm$3.88 | 1622.0$\pm$7.1 | 68 | 881$\pm$74 | sd
CWISEP J093852.89+063440.6 | 232 |  $\cdots$ |  $\cdots$ | [Y0] | 232 | 67.9$\pm$13.8 | 792.9$\pm$50.6 | 0 | 460$\pm$79 | [53.2]
2MASS J09393548$-$2448279A | 29 |  $\cdots$ |  $\cdots$ | [T8] | 61 | 187.3$\pm$4.6 | 1191.7$\pm$3.4 | 71 | 686$\pm$79 | sd
2MASS J09393548$-$2448279[B] | 29 |  $\cdots$ |  $\cdots$ | [T8] | 61 | 187.3$\pm$4.6 | 1191.7$\pm$3.4 | 71 | 686$\pm$79 |
CWISEP J094005.50+523359.2 | 232 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 232 | 66.4$\pm$12.2 | 491.2$\pm$51.9 | 0 | 367$\pm$79 | [75.0]
WISE J094305.98+360723.5 | 18 |  $\cdots$ |  $\cdots$ | T9.5 | 18 | 97.1$\pm$2.9 | 836.3$\pm$1.8 | 0 | 468$\pm$88 |
LHS 6176B (095047+011734) | 40,41 |  $\cdots$ |  $\cdots$ | T8 | 19,8 | 57.9$\pm$2.3 | 434.1$\pm$1.3 | 1 | 664$\pm$88 | sd
PSO J149.0341$-$14.7857 (095608$-$144708) | 181 |  $\cdots$ |  $\cdots$ | L9 | 181 | 65.4$\pm$3.4 | 167.4$\pm$6.4 | 237 | 1169$\pm$88 |
LHS 5166B (100439$-$333518) | 135 | L4 | 135 |  $\cdots$ |  $\cdots$ | 53.4639$\pm$0.0860 | 488.8$\pm$0.2 | 168aaThe astrometry listed is for the primary star in the system. | 1753$\pm$88 |
2MASS J10073369$-$4555147 | 24 |  $\cdots$ |  $\cdots$ | T5.5 | 24 | 72.64$\pm$2.80 | 736.9$\pm$1.2 | 200 | 1017$\pm$94 |
CWISEP J100854.84+203136.6 | 232 |  $\cdots$ |  $\cdots$ | [T9.5] | 0 | 37.1$\pm$15.1 | 215.3$\pm$51.5 | 0 | 511$\pm$79 | [53.9]
2MASSI J1010148$-$040649 | 115 | L6 | 115 | L5 | 124 | 57.7$\pm$3.6 | 320.0$\pm$3.6 | 0 | 1416$\pm$123 |
ULAS J101243.54+102101.7 | 26 |  $\cdots$ |  $\cdots$ | T5.5 | 19 | 59.7$\pm$1.8 | 680.2$\pm$2.7 | 237 | 799$\pm$88 |
DENIS J1013$-$7842 | 225 | L3 | 225 |  $\cdots$ |  $\cdots$ | 71.1390$\pm$0.2987 | 264.1$\pm$0.9 | 168 | 1799$\pm$88 |
WISEPC J101808.05$-$244557.7 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 83.0$\pm$2.8 | 822.5$\pm$1.5 | 0 | 627$\pm$88 |
2MASS J10224821+5825453 | 112 | L1$\beta$ | 110 | L1$\beta$ | 175 | 54.3331$\pm$0.3143 | 1095.7$\pm$0.5 | 168 | 1823$\pm$136 | yng
WISE J102557.72+030755.7 | 8 |  $\cdots$ |  $\cdots$ | T8.5 | 8 | 83.6$\pm$2.3 | 1211.5$\pm$1.4 | 0 | 594$\pm$88 |
2MASSI J1029216+162652 | 105 | L2.5 | 105 | L2.8 | 106 | 52.3361$\pm$0.7414 | 508.9$\pm$1.3 | 168 | 1834$\pm$88 |
ULAS J102940.52+093514.6 | 19 |  $\cdots$ |  $\cdots$ | T8 | 20 | 68.6$\pm$1.7 | 442.9$\pm$2.7 | 237 | 709$\pm$88 |
CWISEP J103453.14+161228.0 | 232 |  $\cdots$ |  $\cdots$ | [T7.5] | 232 | [52.1] | 242.3$\pm$52.2 | 0 | 751$\pm$79 |
2MASSW J1036530$-$344138 | 135 | L6 | 135 | L6.5 | 124 | 68.0213$\pm$1.7241 | 456.9$\pm$4.3 | 168 | 1368$\pm$131 |
WISEPC J104245.23$-$384238.3 | 4 |  $\cdots$ |  $\cdots$ | T8.5 | 4 | 65.4$\pm$3.4 | 93.7$\pm$6.2 | 21,1 | 570$\pm$88 |
2MASS J10430758+2225236 | 120 | L8 | 120 | L9 | 62 | 52.4$\pm$2.9 | 132.2$\pm$4.6 | 237 | 1377$\pm$88 |
SDSS J104335.08+121314.1 | 53 |  $\cdots$ |  $\cdots$ | L9 | 133 | 59.9$\pm$3.1 | 254.3$\pm$4.7 | 237 | 1252$\pm$88 |
SDSS J104523.98-014957.7 | 136 | L1 | 136 | L1 | 112 | 58.6576$\pm$0.2384 | 507.8$\pm$0.5 | 168 | 2091$\pm$88 |
2MASSI J1047538+212423 | 43 | T7 | 197 | T6.5 | 61 | 94.73$\pm$3.81 | 1728.4$\pm$7.7 | 68 | 880$\pm$76 |
CWISEP J104756.81+545741.6 | 232 |  $\cdots$ |  $\cdots$ | [Y0] | 232 | 75.2$\pm$12.8 | 452.7$\pm$54.6 | 0 | 460$\pm$79 |
SDSS J104842.84+011158.5 | 136 | L1 | 136 | L4 | 137 | 66.4589$\pm$0.2143 | 497.2$\pm$0.5 | 168 | 2078$\pm$88 |
WISE J104915.57$-$531906.1A | 90 | L8: | 211 | L7.5 | 210 | 501.557$\pm$0.082 | 2790.4$\pm$0.2 | 179 | 1334$\pm$58 |
WISE J104915.57$-$531906.1B | 90 | T1.5:: | 211 | T0.5: | 210 | 501.557$\pm$0.082 | 2790.4$\pm$0.2 | 179 | 1261$\pm$55 |
2MASS J10511900+5613086 | 117 | L2 | 117 | L0.8 | 106 | 63.9956$\pm$0.1886 | 389.0$\pm$0.4 | 168 | 2006$\pm$88 |
WISE J105130.01$-$213859.7 | 8 |  $\cdots$ |  $\cdots$ | T8.5 | 22 | 64.0$\pm$2.3 | 202.2$\pm$1.4 | 0 | 575$\pm$88 |
WISE J105257.95$-$194250.2 | 20 |  $\cdots$ |  $\cdots$ | T7.5 | 20 | 67.8$\pm$2.2 | 447.5$\pm$3.0 | 0 | 785$\pm$88 |
CWISE J105512.11+544328.3 | 0 |  $\cdots$ |  $\cdots$ | [sdT8] | 0 | 145.0$\pm$14.7 | 1534.9$\pm$2.9 | 0 | 686$\pm$79 |
WISEA J105553.62$-$165216.5 | 6 |  $\cdots$ |  $\cdots$ | T9.5 | 22 | 71.7$\pm$2.3 | 1084.1$\pm$1.4 | 0 | 511$\pm$79 |
DENIS-P J1058.7-1548 | 138 | L3 | 139 | L3 | 124 | 54.6468$\pm$0.5213 | 259.9$\pm$1.1 | 168 | 1809$\pm$68 |
CWISE J110201.76+350334.7 | 0 |  $\cdots$ |  $\cdots$ | [T9] | 233 | [59.3] | 170.4$\pm$57.1 | 0 | 566$\pm$79 |
2MASSI J1104012+195921 | 140 | L4.5 | 140 | L5.5 | 124 | 55.9160$\pm$0.4448 | 133.8$\pm$1.2 | 168 | 1722$\pm$88 |
2MASSW J1108307+683017 | 142 | L1$\gamma$ | 175 | L1$\gamma$ | 175 | 61.3537$\pm$0.1985 | 309.4$\pm$0.5 | 168 | 1951$\pm$197 | yng
SDSSp J111010.01+011613.1 | 122 |  $\cdots$ |  $\cdots$ | T5.5 | 61 | 52.1$\pm$1.2 | 355.0$\pm$0.7 | 67 | 926$\pm$18 | yng
WISE J111239.24$-$385700.7 | 6 |  $\cdots$ |  $\cdots$ | T9 | 6 | 102.6$\pm$3.7 | 951.4$\pm$2.2 | 0 | 461$\pm$88 |
2MASS J11145133$-$2618235 | 29 | T8 | 214 | T7.5 | 61 | 179.2$\pm$1.4 | 3043.2$\pm$1.1 | 67 | 669$\pm$55 |
WISE J111838.70+312537.9 | 2,44 |  $\cdots$ |  $\cdots$ | T8.5 | 44 | 114.4867$\pm$0.4316 | 696.2$\pm$1.1 | 168aaThe astrometry listed is for the primary star in the system. | 559$\pm$88 |
CWISE J112106.36$-$623221.5 | 0 |  $\cdots$ |  $\cdots$ | [Y0] | 0 | [96.8] | 669.0$\pm$69.8 | 0 | 460$\pm$79 |
LHS 2397aB (112149$-$131308) | 93 |  $\cdots$ |  $\cdots$ | [L7.5] | 180 | 69.4903$\pm$0.1760 | 474.5$\pm$0.4 | 168aaThe astrometry listed is for the primary star in the system. | 1282$\pm$88 |
2MASS J11220826$-$3512363 | 29 |  $\cdots$ |  $\cdots$ | T2 | 124 | 74.8605$\pm$1.5536 | 296.1$\pm$3.6 | 168 | 1269$\pm$88 |
WISEPC J112254.73+255021.5 | 4 |  $\cdots$ |  $\cdots$ | T6 | 4 | 66.3$\pm$2.3 | 1028.6$\pm$1.2 | 1 | 855$\pm$88 |
WISE J112438.12$-$042149.7 | 8 |  $\cdots$ |  $\cdots$ | T7 | 8 | 59.4$\pm$2.9 | 572.9$\pm$1.8 | 0 | 819$\pm$79 |
2MASS J11263991-5003550 | 143 | L4.5 | 132 | L6.5$\pm$2 pec | 132,133 | 61.6319$\pm$0.3273 | 1651.9$\pm$0.6 | 168 | 1718$\pm$88 |
SIMP J11322058$-$3809562 | 94 |  $\cdots$ |  $\cdots$ | L8: pec | 94 | 59.0$\pm$3.5 | 236.1$\pm$3.4 | 0 | 1284$\pm$88 |
CWISE J113833.47+721207.8 | 0 |  $\cdots$ |  $\cdots$ | [T7.5] | 0 | 40.7$\pm$7.1 | 517.7$\pm$1.8 | 0 | 751$\pm$79 | [54.6]
CWISE J114120.42$-$211024.5 | 0 |  $\cdots$ |  $\cdots$ | T9: | 0 | [57.9] | 1007.5$\pm$21.9 | 0 | 566$\pm$79 |
WISEA J114156.67$-$332635.5 | 21 |  $\cdots$ |  $\cdots$ | Y0 | 6 | 104.0$\pm$2.9 | 914.1$\pm$2.6 | 0 | 460$\pm$79 |
WISEP J115013.88+630240.7 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 121.4$\pm$2.7 | 676.6$\pm$1.4 | 0 | 686$\pm$79 |
ULAS J115239.94+113407.6 | 19 |  $\cdots$ |  $\cdots$ | T8.5 | 19 | 56.7$\pm$2.7 | 489.5$\pm$2.3 | 0 | 643$\pm$88 |
2MASSW J1155395-372735 | 135 | L2 | 135 | L2.3 | 106 | 84.5693$\pm$0.1867 | 792.1$\pm$0.3 | 168 | 1793$\pm$80 |
SDSSp J120358.19+001550.3 | 121 | L3 | 121 | L5 | 106 | 67.2362$\pm$0.5553 | 1250.0$\pm$1.4 | 168 | 1712$\pm$88 |
CWISE J120502.74$-$180215.5 | 0 |  $\cdots$ |  $\cdots$ | T8 | 0 | [52.3] | 164.3$\pm$3.6 | 0 | 686$\pm$79 |
WISE J120604.38+840110.6 | 9 |  $\cdots$ |  $\cdots$ | Y0 | 9 | 84.7$\pm$2.1 | 634.6$\pm$1.3 | 0 | 454$\pm$88 |
2MASSI J1213033-043243 | 115 | L5 | 115 | L4.2 | 106 | 59.4765$\pm$1.0156 | 369.7$\pm$2.6 | 168 | 1617$\pm$88 |
SDSS J121440.95+631643.4 | 53 |  $\cdots$ |  $\cdots$ | T4 | 124 | 55.8$\pm$4.6 | 132.9$\pm$2.3 | 0 | 1085$\pm$88 |
2MASSI J1217110$-$031113 | 43 | T7 | 197 | T7.5 | 61 | 91.7$\pm$2.2 | 1057.1$\pm$1.7 | 76,1 | 885$\pm$75 |
WISEPC J121756.91+162640.2A | 4 |  $\cdots$ |  $\cdots$ | T9 | 212 | 107.4$\pm$3.5 | 1460.1$\pm$2.2 | 0 | 566$\pm$79 |
WISEPC J121756.91+162640.2B | 4 |  $\cdots$ |  $\cdots$ | Y0 | 212 | 107.4$\pm$3.5 | 1460.1$\pm$2.2 | 0 | 460$\pm$79 |
SDSS J121951.45+312849.4 | 53 |  $\cdots$ |  $\cdots$ | L9.5 | 124 | 52.0$\pm$3.8 | 254.1$\pm$4.1 | 237 | 1332$\pm$88 |
2MASS J12212770+0257198 | 117 | L0 | 117 | L0.5 | 114 | 53.9501$\pm$0.2528 | 151.7$\pm$0.6 | 168 | 2149$\pm$88 |
WISE J122152.28$-$313600.8 | 8 |  $\cdots$ |  $\cdots$ | T6.5 | 8 | 76.8$\pm$2.2 | 715.2$\pm$1.5 | 0 | 898$\pm$88 |
2MASS J12255432$-$2739466A | 43 |  $\cdots$ |  $\cdots$ | T5.5 | 67 | 76.0$\pm$2.5 | 736.8$\pm$2.9 | 76,1 | 1044$\pm$79 |
2MASS J12255432$-$2739466B | 67 |  $\cdots$ |  $\cdots$ | T8 | 67 | 76.0$\pm$2.5 | 736.8$\pm$2.9 | 76,1 | 686$\pm$79 |
2MASS J12314753+0847331 | 3 | T6 | 214 | T5.5 | 61 | 70.2$\pm$3.6 | 1573.1$\pm$4.3 | 237 | 1047$\pm$88 |
2MASS J12373919+6526148 | 43 | T7 | 197 | T6.5 | 61 | 96.07$\pm$4.78 | 1131.4$\pm$8.9 | 68 | 851$\pm$74 |
CWISEP J124138.41-820051.9 | 232 |  $\cdots$ |  $\cdots$ | [T8.5] | 232 | 69.1$\pm$3.8 | 280.8$\pm$11.5 | 0 | 624$\pm$79 |
WISE J124309.61+844547.8 | 20 |  $\cdots$ |  $\cdots$ | T9 | 20 | 54.5$\pm$3.1 | 746.7$\pm$2.6 | 0 | 601$\pm$88 |
WISE J124629.65$-$313934.2 | 95 |  $\cdots$ |  $\cdots$ | T1 | 8 | 86.3432$\pm$1.6050 | 560.0$\pm$3.8 | 168 | 1234$\pm$88 |
WISE J125015.56+262846.9 | 8 |  $\cdots$ |  $\cdots$ | T6.5 | 8 | 57.5$\pm$3.7 | 738.4$\pm$4.2 | 237 | 889$\pm$88 |
DENIS-P J1253108-570924 | 129 | L0.5 | 129 |  $\cdots$ |  $\cdots$ | 60.0190$\pm$0.2612 | 1622.4$\pm$0.4 | 168 | 1963$\pm$88 |
SDSSp J125453.90$-$012247.4 | 96 | T2 | 197 | T2 | 124 | 78.34$\pm$1.07 | 489.4$\pm$0.2 | 172 | 1219$\pm$94 |
WISE J125715.90+400854.2 | 8 |  $\cdots$ |  $\cdots$ | T7 | 8 | 57.0$\pm$1.8 | 339.4$\pm$2.2 | 237 | 857$\pm$88 |
WISEA J125721.01+715349.3 | 233 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 233 | [60.2] | 932.1$\pm$19.1 | 0 | 367$\pm$79 |
VHS J125804.89$-$441232.4 | 23 |  $\cdots$ |  $\cdots$ | T6 | 23 | 67.0$\pm$2.9 | 203.6$\pm$2.6 | 0 | 965$\pm$79 |
Gl 494C (130041+122114) | 45 |  $\cdots$ |  $\cdots$ | T8 | 10 | 86.8570$\pm$0.1515 | 633.2$\pm$0.5 | 168aaThe astrometry listed is for the primary star in the system. | 721$\pm$94 |
2MASSW J1300425+191235 | 142 | L1 | 142 | L3 (blue) | 132,133 | 71.6755$\pm$0.2012 | 1488.5$\pm$0.4 | 168 | 2044$\pm$88 |
WISE J130141.62$-$030212.9 | 8 |  $\cdots$ |  $\cdots$ | T8.5 | 8 | 54.5$\pm$4.5 | 377.0$\pm$3.8 | 0 | 679$\pm$88 |
ULAS J130217.21+130851.2 | 31 |  $\cdots$ |  $\cdots$ | T8 | 10 | 65.0$\pm$5.0 | 445.0$\pm$9.2 | 77 | 640$\pm$88 |
Kelu-1A (130540-254105) | 144 | L3 | 146 | L1.5-L3 | 145 | 53.8492$\pm$0.7107 | 314.1$\pm$1.4 | 168 | 1931$\pm$134 |
Kelu-1B (130540-254105) | 145 | L3 | 146 | L3-L4.5 | 145 | 53.8492$\pm$0.7107 | 314.1$\pm$1.4 | 168 | 1750$\pm$134 |
Gl 499C (130541+204639) | 115 | L5 | 147 | L6.5 | 106 | 50.9035$\pm$0.0435 | 109.8$\pm$0.1 | 168aaThe astrometry listed is for the primary star in the system. | 1603$\pm$ |
WISEPC J131106.24+012252.4 | 4 |  $\cdots$ |  $\cdots$ | T9: | 4 | 68.8$\pm$2.7 | 860.0$\pm$1.3 | 1 | 554$\pm$88 |
ULAS J131508.42+082627.4 | 64 |  $\cdots$ |  $\cdots$ | T7.5 | 64 | 50.5$\pm$5.7 | 118.9$\pm$3.3 | 1 | 590$\pm$88 |
2MASSI J1315309$-$264951A | 98 | L5.5 | 103 | L5 | 213 | 53.8729$\pm$1.1265 | 746.5$\pm$2.4 | 168 | 1613$\pm$134 |
2MASSI J1315309$-$264951B | 213 |  $\cdots$ |  $\cdots$ | T7 | 213 | 53.8729$\pm$1.1265 | 746.5$\pm$2.4 | 168 | 819$\pm$79 |
CWISE J131548.23$-$493645.4 | 0 |  $\cdots$ |  $\cdots$ | T3 | 0 | [59.0] | 181.2$\pm$9.9 | 0 | 1199$\pm$79 |
WISE J131833.98$-$175826.5 | 8 |  $\cdots$ |  $\cdots$ | T8 | 22 | 63.5$\pm$2.2 | 526.0$\pm$1.4 | 0 | 719$\pm$88 |
WISEPC J132004.16+603426.2 | 4 |  $\cdots$ |  $\cdots$ | T6.5 | 4 | 60.6$\pm$2.5 | 561.3$\pm$1.4 | 1 | 901$\pm$88 |
WISEPA J132233.66$-$234017.1 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 77.5$\pm$4.2 | 524.1$\pm$1.9 | 1 | 808$\pm$88 |
2MASS J13243559+6358284 | 24,188 |  $\cdots$ |  $\cdots$ | T2: pec | 24 | 99.7$\pm$5.6 | 371.5$\pm$3.0 | 0 | 1051$\pm$197 | yng
2MASSW J1326201$-$272937 | 135 | L5 | 135 | L6.6: | 106 | 54.7$\pm$5.9 | 365.7$\pm$7.4 | 237 | 1349$\pm$88 |
WISEA J133300.03$-$160754.4 | 1 |  $\cdots$ |  $\cdots$ | T9 | 0 | 52.8$\pm$3.5 | 354.5$\pm$2.5 | 0 | 689$\pm$88 |
ULAS J133553.45+113005.2 | 42 |  $\cdots$ |  $\cdots$ | T8.5 | 10 | 99.9$\pm$1.6 | 278.2$\pm$1.2 | 67 | 573$\pm$88 |
SDSSp J134646.45$-$003150.4 | 47 | T7 | 197 | T6.5 | 61 | 69.2$\pm$2.3 | 516.0$\pm$3.3 | 76,1 | 1011$\pm$86 |
LHS 2803B (134802$-$134407) | 230 |  $\cdots$ |  $\cdots$ | T5.5 | 230 | 54.9973$\pm$0.0838 | 857.9$\pm$0.2 | 168aaThe astrometry listed is for the primary star in the system. | 939$\pm$88 |
WISE J140035.40$-$385013.5 | 8 |  $\cdots$ |  $\cdots$ | T4 | 8 | 61.7$\pm$3.6 | 231.5$\pm$2.1 | 0 | 1031$\pm$88 |
WISEPC J140518.40+553421.4 | 10 |  $\cdots$ |  $\cdots$ | Y0.5(pec ?) | 9,73 | 158.2$\pm$2.6 | 2345.8$\pm$1.6 | 0 | 411$\pm$88 |
WISE J140533.32+835030.5 | 119 | L8 | 119 | L9 | 119 | 103.1218$\pm$0.7054 | 840.9$\pm$1.7 | 168 | 1314$\pm$88 |
CWISE J141127.70$-$481153.4 | 0 |  $\cdots$ |  $\cdots$ | [T6.5] | 0 | 58.2$\pm$4.7 | 489.0$\pm$14.8 | 0 | 890$\pm$79 |
ULAS J141623.94+134836.3 | 49 |  $\cdots$ |  $\cdots$ | [(sd)T7.5] | 62 | 107.5599$\pm$0.2958 | 154.9$\pm$0.8 | 168aaThe astrometry listed is for the primary star in the system. | 656$\pm$54 | sd
SDSS J141624.08+134826.7 | 100,134 | sdL7 | 133 | sdL7 | 133 | 107.5599$\pm$0.2958 | 154.9$\pm$0.8 | 168 | 1586$\pm$88 | sd
Gl 547B (142320+011638) | 50 |  $\cdots$ |  $\cdots$ | sdT8,T8 | 50,8 | 57.3445$\pm$0.0362 | 528.0$\pm$0.1 | 168aaThe astrometry listed is for the primary star in the system. | 613$\pm$88 | sd
DENIS-P J142527.97-365023.4 | 137 | L3 | 150 | L4$\gamma$ | 175 | 84.5181$\pm$0.3435 | 548.5$\pm$0.8 | 168 | 1535$\pm$53 | yng
VHS J143311.46$-$083736.3 | 23 |  $\cdots$ |  $\cdots$ | T8 | 23 | 56.5$\pm$2.8 | 366.4$\pm$1.9 | 0 | 578$\pm$88 |
WISEPA J143602.19$-$181421.8 | 4 |  $\cdots$ |  $\cdots$ | T8pec | 4 | 50.9$\pm$2.0 | 116.5$\pm$1.3 | 0 | 686$\pm$79 |
2MASSW J1439284+192915 | 139 | L1 | 139 | L1 | 114 | 69.77$\pm$0.44 | 1295.0$\pm$0.2 | 172 | 2121$\pm$61 |
G 239-25B (J144221+660320) | 116 |  $\cdots$ |  $\cdots$ | L0 | 151 | 91.4776$\pm$0.0261 | 301.6$\pm$0.1 | 168aaThe astrometry listed is for the primary star in the system. | 2338$\pm$88 |
CWISEP J144606.62$-$231717.8 | 232,231 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 232 | 95.6$\pm$13.9 | 1211.3$\pm$54.5 | 0 | 367$\pm$79 | [86.4]
WISE J144806.48$-$253420.3 | 20 |  $\cdots$ |  $\cdots$ | T8 | 20 | 54.8$\pm$2.1 | 757.1$\pm$1.4 | 0 | 626$\pm$88 |
2MASSW J1448256+103159 | 109 | L5 | 117 | L7 | 124 | 71.2548$\pm$0.7233 | 251.3$\pm$1.5 | 168 | 1623$\pm$91 |
Gl 564B (145016+235441) | 152 |  $\cdots$ |  $\cdots$ | L4 | 153 | 54.9068$\pm$0.0684 | 148.0$\pm$0.2 | 168aaThe astrometry listed is for the primary star in the system. | 1722$\pm$134 |
Gl 564C (145016+235441) | 152 |  $\cdots$ |  $\cdots$ | L4 | 153 | 54.9068$\pm$0.0684 | 148.0$\pm$0.2 | 168aaThe astrometry listed is for the primary star in the system. | 1722$\pm$134 |
DENIS-P J1454078-660447 | 129 | L3.5 | 129 |  $\cdots$ |  $\cdots$ | 93.2242$\pm$0.3013 | 597.7$\pm$0.7 | 168 | 1793$\pm$88 |
WISEPC J145715.03+581510.2 | 4 | T8 | 4 | T7 | 4 | 55.0$\pm$2.3 | 502.0$\pm$1.1 | 1 | 923$\pm$88 |
Gl 570D (145715$-$212107) | 51 | T7 | 197 | T7.5 | 61 | 170.0112$\pm$0.0851 | 2008.7$\pm$0.2 | 168aaThe astrometry listed is for the primary star in the system. | 759$\pm$63 |
WISE J150115.92$-$400418.4 | 17 |  $\cdots$ |  $\cdots$ | T6 | 6 | 72.8$\pm$2.3 | 501.9$\pm$1.8 | 0 | 864$\pm$88 |
2MASS J15031961+2525196 | 52 | T6 | 197 | T5 | 61 | 154.9208$\pm$1.1025 | 566.1$\pm$3.0 | 168 | 1016$\pm$85 |
Gl 576B (150457+053759) | 54 |  $\cdots$ |  $\cdots$ | T6pec | 54 | 52.5873$\pm$0.0668 | 791.1$\pm$0.2 | 168aaThe astrometry listed is for the primary star in the system. | 875$\pm$88 | sd
WISEPC J150649.97+702736.0 | 4 | T6 | 214 | T6 | 4 | 193.5$\pm$0.6 | 1587.3$\pm$0.3 | 1 | 921$\pm$88 |
2MASSW J1506544+132106 | 142 | L3 | 142 | L4 | 124 | 85.5810$\pm$0.2883 | 1071.1$\pm$0.6 | 168 | 2004$\pm$75 |
2MASSW J1507476-162738 | 107 | L5 | 107 | L5 | 124 | 135.2332$\pm$0.3274 | 908.5$\pm$0.9 | 168 | 1607$\pm$70 |
2MASSW J1515008+484742 | 109 | L6 | 134 | L5.5 | 124 | 102.59$\pm$0.63 | 1744.2$\pm$0.2 | 172 | 1505$\pm$74 |
WISEPC J151906.64+700931.5 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 78.5$\pm$2.6 | 594.0$\pm$1.6 | 0 | 612$\pm$88 |
2MASS J15200224-4422419A | 111 |  $\cdots$ |  $\cdots$ | L1.5 | 154 | 54.4581$\pm$0.2465 | 736.7$\pm$0.6 | 168 | 2029$\pm$134 |
2MASS J15200224-4422419B | 111 |  $\cdots$ |  $\cdots$ | L4.5 | 154 | 53.6580$\pm$0.6308 | 753.4$\pm$1.8 | 168 | 1666$\pm$134 |
SDSS J152039.82+354619.8 | 53 |  $\cdots$ |  $\cdots$ | L7.5 | 124 | 57.4$\pm$4.8 | 499.8$\pm$7.6 | 237 | 1364$\pm$88 |
WISE J152305.10+312537.6 | 8 |  $\cdots$ |  $\cdots$ | T6.5pec | 8 | 65.0$\pm$3.5 | 522.5$\pm$2.5 | 0 | 612$\pm$88 | sd
Gl 584C (152322+301456) | 105 | L8 | 105 | L7.5 | 124 | 55.98$\pm$0.78 | 207.4$\pm$0.6 | 173 | 1295$\pm$76 |
2MASSI J1526140+204341 | 105 | L7 | 105 | L5.5 | 124 | 50.0002$\pm$1.4846 | 421.6$\pm$3.1 | 168 | 1518$\pm$157 |
CWISE J153143.38$-$330657.3 | 0 |  $\cdots$ |  $\cdots$ | [Y0] | 0 | [58.9] | 309.3$\pm$54.8 | 0 | 460$\pm$79 |
CWISE J153347.50+175306.7 | 0 |  $\cdots$ |  $\cdots$ | [T8] | 0 | 51.3$\pm$7.0 | 222.2$\pm$2.5 | 0 | 686$\pm$79 | [53.2]
2MASSI J1534498$-$295227A | 32 |  $\cdots$ |  $\cdots$ | T4.5 | 67 | 74.5$\pm$1.2 | 268.8$\pm$1.9 | 76ccThis object’s parallax has been converted from relative to absolute by adding 0.9$\pm$0.3 mas, per the discussion in section 8 of Kirkpatrick et al. (2019). | 1172$\pm$79 |
2MASSI J1534498$-$295227B | 189 |  $\cdots$ |  $\cdots$ | T5 | 67 | 74.5$\pm$1.2 | 268.8$\pm$1.9 | 76ccThis object’s parallax has been converted from relative to absolute by adding 0.9$\pm$0.3 mas, per the discussion in section 8 of Kirkpatrick et al. (2019). | 1125$\pm$79 |
DENIS-P J153941.96-052042.4 | 137 | L3.5 | 112 | L4 | 124 | 58.8245$\pm$0.4213 | 599.4$\pm$1.0 | 168 | 1753$\pm$85 |
WISEPA J154151.66$-$225025.2 | 10 |  $\cdots$ |  $\cdots$ | Y1 | 9 | 166.9$\pm$2.0 | 907.4$\pm$1.3 | 0 | 395$\pm$88 |
WISE J154214.00+223005.2 | 8 |  $\cdots$ |  $\cdots$ | T9.5 | 8 | 84.3$\pm$3.0 | 1053.2$\pm$1.8 | 0 | 472$\pm$88 |
2MASS J15461461+4932114 | 188 |  $\cdots$ |  $\cdots$ | T3 | 124 | 53.0$\pm$4.4 | 731.5$\pm$4.0 | 0 | 1261$\pm$88 |
2MASSI J1546291$-$332511 | 32 |  $\cdots$ |  $\cdots$ | T5.5 | 124 | 88.9$\pm$1.9 | 225.4$\pm$2.2 | 76ccThis object’s parallax has been converted from relative to absolute by adding 0.9$\pm$0.3 mas, per the discussion in section 8 of Kirkpatrick et al. (2019). | 1002$\pm$84 |
2MASSI J1553022+153236A | 32 |  $\cdots$ |  $\cdots$ | T6.5 | 61 | 75.1$\pm$0.9 | 420.1$\pm$0.7 | 67 | 890$\pm$79 |
2MASSI J1553022+153236B | 32 |  $\cdots$ |  $\cdots$ | T7.5 | 61 | 75.1$\pm$0.9 | 420.1$\pm$0.7 | 67 | 751$\pm$79 |
2MASSW J1555157-095605 | 135 | L1 | 135 | L1.6 | 106 | 73.6519$\pm$0.1870 | 1218.3$\pm$0.4 | 168 | 2102$\pm$64 |
WISE J160018.05$-$454332.7 | 16 |  $\cdots$ |  $\cdots$ | [L9:] | 0 | 74.7951$\pm$0.9190 | 885.9$\pm$2.9 | 168 | 1382$\pm$88 |
WISEPA J161215.94$-$342027.1 | 4 |  $\cdots$ |  $\cdots$ | T6.5 | 4 | 90.0$\pm$2.7 | 656.1$\pm$1.4 | 0 | 718$\pm$88 |
WISEPA J161441.45+173936.7 | 4 |  $\cdots$ |  $\cdots$ | T9 | 4 | 98.2$\pm$2.7 | 728.6$\pm$1.4 | 0 | 510$\pm$88 |
2MASS J16150413+1340079 | 24 |  $\cdots$ |  $\cdots$ | T6 | 24 | 55.4$\pm$2.1 | 436.6$\pm$1.4 | 0 | 906$\pm$87 |
2MASSW J1615441+355900 | 105 | L3 | 105 | L3.6 | 106 | 50.0611$\pm$0.3713 | 529.5$\pm$1.0 | 168 | 1793$\pm$88 |
WISEPA J161705.75+180714.3 | 4 | T8 | 4 | T8 | 4 | 78.0$\pm$3.1 | 101.9$\pm$5.5 | 237 | 618$\pm$88 |
WISEA J162341.27$-$740230.4 | 158 |  $\cdots$ |  $\cdots$ | L9 (sl. red) | 158 | 50.6$\pm$3.1 | 413.2$\pm$3.7 | 0 | 1202$\pm$88 |
SDSSp J162414.37+002915.6 | 55 | T6 | 197 | T6 | 61 | 91.8$\pm$1.2 | 373.0$\pm$1.6 | 76,1 | 936$\pm$78 |
WISEPA J162725.64+325525.5A | 4 |  $\cdots$ |  $\cdots$ | [T6] | 4 | 54.4$\pm$1.9 | 351.6$\pm$0.8 | 1 | 965$\pm$79 |
WISEPA J162725.64+325525.5[B] | 4 |  $\cdots$ |  $\cdots$ | [T6] | 4 | 54.4$\pm$1.9 | 351.6$\pm$0.8 | 1 | 965$\pm$79 |
SDSS J162838.77+230821.1 | 53 |  $\cdots$ |  $\cdots$ | T7 | 53 | 75.1$\pm$0.9 | 605.2$\pm$0.8 | 67 | 815$\pm$88 |
PSO J247.3273+03.5932 (162918+033537) | 99 | T3 | 214 | T2 | 8 | 81.2$\pm$3.0 | 276.3$\pm$1.6 | 0 | 1193$\pm$88 |
CWISE J163041.79$-$064338.3 | 0 |  $\cdots$ |  $\cdots$ | T5 | 0 | [55.3] | 580.0$\pm$28.6 | 0 | 1125$\pm$79 |
SDSS J163022.92+081822.0 | 53 |  $\cdots$ |  $\cdots$ | T5.5 | 53 | 55.8$\pm$3.4 | 124.4$\pm$1.4 | 0 | 970$\pm$88 |
2MASSW J1632291+190441 | 139 | L8 | 139 | L7 | 124 | 66.29$\pm$1.61 | 297.9$\pm$0.3 | 172 | 1279$\pm$81 |
WISEA J163932.75+184049.4 | 233 |  $\cdots$ |  $\cdots$ | [T9.5] | 233 | 61.9$\pm$4.7 | 547.9$\pm$12.8 | 0 | 511$\pm$79 |
WISE J163940.86$-$684744.6 | 17 |  $\cdots$ |  $\cdots$ | Y0pec | 9 | 219.6$\pm$2.3 | 3160.8$\pm$1.6 | 0 | 412$\pm$88 |
2MASSW J1645221-131951 | 135 | L1.5 | 135 |  $\cdots$ |  $\cdots$ | 88.8220$\pm$0.1444 | 885.7$\pm$0.3 | 168 | 2013$\pm$88 |
CWISE J165013.37+565257.0 | 0 |  $\cdots$ |  $\cdots$ | T0 | 0 | [68.1] | 115.4$\pm$5.9 | 0 | 1254$\pm$79 |
WISEPA J165311.05+444423.9 | 4 | T8 | 4 | T8 | 4 | 75.7$\pm$1.9 | 405.3$\pm$2.9 | 0 | 696$\pm$88 |
2MASSW J1658037+702701 | 142 | L1 | 142 |  $\cdots$ |  $\cdots$ | 54.1172$\pm$0.2058 | 344.9$\pm$0.5 | 168 | 2181$\pm$62 |
DENIS-P J170548.38-051645.7 | 137 | L0.5 | 117 | L1 | 124 | 52.6734$\pm$0.3516 | 167.6$\pm$0.7 | 168 | 2125$\pm$88 |
2MASS J17065487$-$1314396 | 176 |  $\cdots$ |  $\cdots$ | L5 pec | 176 | 51.4814$\pm$0.5128 | 188.2$\pm$1.2 | 168 | 1736$\pm$88 |
2MASS J17072343$-$0558249B | 156 |  $\cdots$ |  $\cdots$ | L3 | 156 | 85.0112$\pm$0.4386 | 89.2$\pm$0.7 | 168 | 1671$\pm$88 |
WISE J170745.85$-$174452.5 | 8 |  $\cdots$ |  $\cdots$ | T5: | 8 | 86.0$\pm$2.8 | 173.5$\pm$1.3 | 0 | 780$\pm$88 |
Gaia J171340.47$-$395211.8ffThe Gaia DR2 identifications for these sources are given in Table 17 and are: Gaia J041246.85$-$073416.8 = Gaia DR2 3195979005694112768, Gaia J171340.47$-$395211.8 = Gaia DR2 5972124644679705728, Gaia J183118.29$-$073227.6 = Gaia DR2 4159791176135290752, Gaia J183610.72+031524.6 = Gaia DR2 4283084190940885888, Gaia J195557.27+321518.2 = Gaia DR2 2034222547248988032. | 220 | [L0.5] | 220 |  $\cdots$ |  $\cdots$ | 51.4479$\pm$0.2749 | 305.9$\pm$0.5 | 168 | 2105$\pm$88 |
2MASSI J1721039+334415 | 115 | L3 | 115 | L5$\pm$1 (blue) | 132 | 61.3203$\pm$0.2050 | 1947.6$\pm$0.5 | 168 | 1840$\pm$88 |
WISE J172134.46+111739.4 | 8 |  $\cdots$ |  $\cdots$ | T6 | 8 | 50.4$\pm$2.9 | 160.6$\pm$2.6 | 0 | 1001$\pm$88 |
CWISE J172617.09-484424.9 | 0 |  $\cdots$ |  $\cdots$ | T2.5 | 0 | [90.6 ] | 200.0$\pm$7.1 | 0 | 1209$\pm$79 |
VVV J172640.2-273803 | 157 |  $\cdots$ |  $\cdots$ | L5$\pm$1 (blue) | 157 | 53.9938$\pm$0.3612 | 634.8$\pm$0.7 | 168 | 2050$\pm$88 |
2MASS J17312974+2721233 | 117 | L0 | 117 | L0 | 112 | 83.7364$\pm$0.1182 | 268.5$\pm$0.3 | 168 | 2190$\pm$88 |
DENIS-P J1733423-165449 | 129 | L1.0 | 129 | L0.9 | 106 | 55.3156$\pm$0.3564 | 80.9$\pm$0.8 | 168 | 1977$\pm$88 |
LSPM J1735+2634B | 215 |  $\cdots$ |  $\cdots$ | L0: | 180 | 64.7$\pm$0.8 | 352.5$\pm$0.8 | 67,180 | 2274$\pm$88 |
WISEA J173551.56$-$820900.3 | 6 |  $\cdots$ |  $\cdots$ | T6 | 6 | 76.1$\pm$3.2 | 368.0$\pm$2.3 | 0 | 804$\pm$88 |
WISEPA J173835.53+273258.9 | 10 |  $\cdots$ |  $\cdots$ | Y0 | 10 | 130.9$\pm$2.1 | 481.2$\pm$1.1 | 0 | 450$\pm$88 |
WISE J174102.78$-$464225.5 | 114 |  $\cdots$ |  $\cdots$ | L6-8 $\gamma$ | 175 | 50.5$\pm$2.9 | 357.7$\pm$3.0 | 0 | 1145$\pm$197 | yng
WISEPA J174124.26+255319.5 | 4,33,56 | T9 | 4 | T9 | 4 | 214.3$\pm$2.8 | 1556.9$\pm$1.3 | 1 | 570$\pm$88 |
WISE J174303.71+421150.0 | 8 |  $\cdots$ |  $\cdots$ | T4.5 | 8 | 59.2$\pm$3.3 | 514.5$\pm$1.8 | 0 | 1068$\pm$88 |
DENIS-P J1745346-164053 | 129 | L1.5 | 129 | L1.3 | 106 | 51.0274$\pm$0.2957 | 146.6$\pm$0.6 | 168 | 2019$\pm$88 |
2MASS J17502484$-$0016151 | 111 | L5 | 214 | L5.5 | 111 | 108.2676$\pm$0.2552 | 443.7$\pm$0.6 | 168 | 1600$\pm$88 |
WISEA J175328.55-590447.6 | 233 |  $\cdots$ |  $\cdots$ | [T8.5] | TBD | 60.2$\pm$3.7 | 332.6$\pm$13.7 | 0 | 624$\pm$79 |
2MASS J17534518-6559559 | 117 | L4 | 117 |  $\cdots$ |  $\cdots$ | 63.8219$\pm$0.3244 | 346.0$\pm$0.6 | 168 | 1751$\pm$88 |
2MASS J17545447+1649196 | 71 | T5.5 | 214 | T5.5 | 124 | 74.0$\pm$3.1 | 190.1$\pm$4.4 | 0 | 987$\pm$88 |
WISE J175510.28+180320.2 | 8 |  $\cdots$ |  $\cdots$ | T2 | 8 | 53.6$\pm$3.1 | 421.5$\pm$1.8 | 0 | 1235$\pm$88 |
GJ 4040B (175805+463311) | 57 |  $\cdots$ |  $\cdots$ | T6.5 | 61 | 71.4754$\pm$0.0354 | 578.5$\pm$0.1 | 168aaThe astrometry listed is for the primary star in the system. | 901$\pm$88 |
WISE J180001.15-155927.2 | 160 | L4.5 | 155 | L4.5 | 149 | 80.8967$\pm$0.3389 | 296.2$\pm$0.8 | 168 | 1778$\pm$88 |
WISEP J180026.60+013453.1 | 162 | L7.5 | 216 | L7.5 | 162 | 127.4450$\pm$0.6642 | 424.4$\pm$2.0 | 168 | 1291$\pm$88 |
WISEPA J180435.40+311706.1 | 4 |  $\cdots$ |  $\cdots$ | T9.5: | 4 | 62.2$\pm$2.7 | 254.1$\pm$1.3 | 0 | 578$\pm$88 |
2MASSI J1807159+501531 | 109 | L1.5 | 115 | L1 | 109 | 68.3317$\pm$0.1280 | 139.1$\pm$0.4 | 168 | 2065$\pm$88 |
WISE J180901.07+383805.4 | 41 |  $\cdots$ |  $\cdots$ | T7.5 | 8 | 52.4$\pm$2.3 | 778.0$\pm$3.4 | 237 | 780$\pm$88 |
WISEPA J181210.85+272144.3 | 4 |  $\cdots$ |  $\cdots$ | T8.5: | 10 | 98.5$\pm$4.4 | 351.4$\pm$8.8 | 1 | 536$\pm$88 |
WISE J181329.40+283533.3 | 8 |  $\cdots$ |  $\cdots$ | T8 | 8 | 73.6$\pm$2.0 | 512.5$\pm$3.5 | 237 | 734$\pm$88 |
WISEA J181849.59-470146.9 | 233 |  $\cdots$ |  $\cdots$ | [T8.5] | 233 | 94.6$\pm$3.9 | 511.9$\pm$13.7 | 0 | 624$\pm$79 |
2MASS J18212815+1414010 | 161 | L4.5 | 161 | L4 pec | 175 | 106.8740$\pm$0.2518 | 335.3$\pm$0.8 | 168 | 1613$\pm$88 |
WISEPA J182831.08+265037.8 | 10 |  $\cdots$ |  $\cdots$ |  $\geq$Y2 | 2 | 100.3$\pm$2.0 | 1030.5$\pm$1.1 | 0 | 406$\pm$88 |
2MASS J18283572$-$4849046 | 3 |  $\cdots$ |  $\cdots$ | T5.5 | 124 | 87.9$\pm$2.0 | 250.7$\pm$3.6 | 74 | 1060$\pm$103 |
Gaia J183118.29$-$073227.6ffThe Gaia DR2 identifications for these sources are given in Table 17 and are: Gaia J041246.85$-$073416.8 = Gaia DR2 3195979005694112768, Gaia J171340.47$-$395211.8 = Gaia DR2 5972124644679705728, Gaia J183118.29$-$073227.6 = Gaia DR2 4159791176135290752, Gaia J183610.72+031524.6 = Gaia DR2 4283084190940885888, Gaia J195557.27+321518.2 = Gaia DR2 2034222547248988032. | 229 | [L0::]eeAnalysis in section 7.7 shows that this object is probably a late-M dwarf. It has been dropped from subsequent analysis and not considered a member of the L, T, and Y dwarf census. | 229 |  $\cdots$ |  $\cdots$ | 53.9968$\pm$0.4015 | 206.7$\pm$1.0 | 168 |  $\cdots$ |
CWISE J183207.94$-$540943.3 | 0 |  $\cdots$ |  $\cdots$ | T7 | 0 | 57.0$\pm$4.3 | 215.1$\pm$15.1 | 0 | 819$\pm$79 |
Gaia J183610.72+031524.6ffThe Gaia DR2 identifications for these sources are given in Table 17 and are: Gaia J041246.85$-$073416.8 = Gaia DR2 3195979005694112768, Gaia J171340.47$-$395211.8 = Gaia DR2 5972124644679705728, Gaia J183118.29$-$073227.6 = Gaia DR2 4159791176135290752, Gaia J183610.72+031524.6 = Gaia DR2 4283084190940885888, Gaia J195557.27+321518.2 = Gaia DR2 2034222547248988032. | 224 | [L5:] | 229 | L6 v. red | 0 | 54.5934$\pm$0.8539 | 311.0$\pm$2.1 | 168 | 1606$\pm$88 |
SCR J1845$-$6357B (184505$-$635746) | 58 |  $\cdots$ |  $\cdots$ | T6 | 63 | 249.9187$\pm$0.1551 | 2650.6$\pm$0.2 | 168aaThe astrometry listed is for the primary star in the system. | 969$\pm$88 |
WISEPA J185215.78+353716.3 | 4 |  $\cdots$ |  $\cdots$ | T7 | 4 | 72.0$\pm$1.9 | 381.5$\pm$1.1 | 1 | 810$\pm$88 |
2MASS J19010601+4718136 | 3 |  $\cdots$ |  $\cdots$ | T5 | 124 | 67.3$\pm$3.4 | 423.9$\pm$2.0 | 0 | 1064$\pm$88 |
WISEPA J190624.75+450808.2 | 4 |  $\cdots$ |  $\cdots$ | T6 | 4 | 64.1$\pm$1.6 | 351.0$\pm$0.1 | 1 | 921$\pm$88 |
WISEP J190648.47+401106.8 | 162 |  $\cdots$ |  $\cdots$ | L1 | 162 | 59.5710$\pm$0.1363 | 473.9$\pm$0.4 | 168 | 2135$\pm$88 |
WISE J191915.54+304558.4 | 20 |  $\cdots$ |  $\cdots$ | L6 | 20 | 62.5$\pm$3.3 | 569.3$\pm$3.4 | 0 | 1308$\pm$88 |
Gl 758B (192334+331319) | 190 |  $\cdots$ |  $\cdots$ | T7: | 218 | 64.0623$\pm$0.0218 | 180.0$\pm$0.1 | 168aaThe astrometry listed is for the primary star in the system. | 581$\pm$88 |
2MASS J19251275+0700362 | 177 |  $\cdots$ |  $\cdots$ | L7 | 219 | 89.2606$\pm$0.6718 | 219.8$\pm$1.8 | 168 | 1345$\pm$88 |
CWISE J192537.88+290159.0 | 0 |  $\cdots$ |  $\cdots$ | [T8.5] | 0 | [76.2] | 258.4$\pm$29.4 | 0 | 624$\pm$79 |
CWISE J192636.29$-$342955.7 | 0 |  $\cdots$ |  $\cdots$ | [T5.5] | 0 | 51.6$\pm$3.90 | 211.3$\pm$2.1 | 0 | 1044$\pm$79 |
WISE J192841.35+235604.9 | 8 |  $\cdots$ |  $\cdots$ | T6 | 8 | 154.9$\pm$1.8 | 344.1$\pm$1.0 | 0 | 941$\pm$88 |
WISEA J193054.55-205949.4 | 233 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 233 | 106.3$\pm$4.9 | 1501.6$\pm$13.0 | 0 | 367$\pm$79 |
CWISEP J193518.59-154620.3 | 191 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 232 | 69.3$\pm$3.8 | 293.4$\pm$16.3 | 0 | 367$\pm$79 |
WISENF J193656.08+040801.2 | 232 |  $\cdots$ |  $\cdots$ | [Y0] | 232 | 113.9$\pm$3.8 | 1182.5$\pm$16.2 | 0 | 460$\pm$79 |
CWISE J193824.10+350025.0 | 0 |  $\cdots$ |  $\cdots$ | [T8] | 0 | [50.7] | 359.8$\pm$63.6 | 0 | 686$\pm$79 |
WISEPA J195246.66+724000.8 | 4 |  $\cdots$ |  $\cdots$ | T4 | 4 | [78.7] | 410.9$\pm$99.7 | 0,4 | 1181$\pm$79 |
Gaia J195557.27+321518.2ffThe Gaia DR2 identifications for these sources are given in Table 17 and are: Gaia J041246.85$-$073416.8 = Gaia DR2 3195979005694112768, Gaia J171340.47$-$395211.8 = Gaia DR2 5972124644679705728, Gaia J183118.29$-$073227.6 = Gaia DR2 4159791176135290752, Gaia J183610.72+031524.6 = Gaia DR2 4283084190940885888, Gaia J195557.27+321518.2 = Gaia DR2 2034222547248988032. | 229 | [L6.5::] | 229 |  $\cdots$ |  $\cdots$ | 59.3427$\pm$0.9291 | 678.0$\pm$2.1 | 168 | 1465$\pm$134 |
WISEPA J195905.66$-$333833.7 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 83.9$\pm$2.0 | 200.8$\pm$1.1 | 0 | 710$\pm$88 |
WISE J200050.19+362950.1 | 18 |  $\cdots$ |  $\cdots$ | T8 | 18 | 133.4$\pm$2.2 | 372.9$\pm$1.3 | 0 | 765$\pm$88 |
2MASS J20025073$-$0521524 | 25 | L5$\beta$ | 175 | L5-7$\gamma$ | 175 | 56.7162$\pm$1.4818 | 159.9$\pm$4.0 | 168 | 1388$\pm$197 | yng
Gl 779B (200406+170413) | 163 |  $\cdots$ |  $\cdots$ | L4.5$\pm$1.5 | 163 | 56.4256$\pm$0.0690 | 571.2$\pm$0.1 | 168aaThe astrometry listed is for the primary star in the system. | 1533$\pm$88 |
WISE J200520.38+542433.9 | 25 |  $\cdots$ |  $\cdots$ | sdT8 | 25 | 53.9$\pm$2.7 | 1467.9$\pm$1.4 | 0 | 750$\pm$150 | sd
WISE J200804.71$-$083428.5 | 8 |  $\cdots$ |  $\cdots$ | T5.5 | 8 | 57.8$\pm$3.3 | 342.4$\pm$1.7 | 0 | 896$\pm$88 |
CWISEP J201146.45-481259.7 | 232 |  $\cdots$ |  $\cdots$ | [Y0] | 232 | 71.0$\pm$3.7 | 409.3$\pm$15.2 | 0 | 460$\pm$79 |
WISEPA J201824.96-742325.9 | 4 |  $\cdots$ |  $\cdots$ | T7 | 4 | 83.2$\pm$1.9 | 1054.3$\pm$1.9 | 1 | 714$\pm$88 |
WISEA J201833.67-141720.3 | 233 |  $\cdots$ |  $\cdots$ | [T9] | 233 | [64.9] | 159.3$\pm$28.7 | 0 | 566$\pm$79 |
WISE J201920.76$-$114807.5 | 8 |  $\cdots$ |  $\cdots$ | T8: | 8 | 79.9$\pm$2.7 | 358.4$\pm$1.6 | 0 | 613$\pm$88 |
WISE J203042.79+074934.7 | 8 |  $\cdots$ |  $\cdots$ | T1.5 | 8 | 103.9664$\pm$0.9809 | 670.9$\pm$2.3 | 168 | 1323$\pm$88 |
Gl 802B (204319+552053) | 227 | [L5-L7] | 226 |  $\cdots$ |  $\cdots$ | 58.3160$\pm$0.1412 | 1897.0$\pm$1.0 | 168 | 1483$\pm$88 |
WISEPC J205628.90+145953.3 | 10 |  $\cdots$ |  $\cdots$ | Y0 | 10 | 140.8$\pm$2.0 | 980.6$\pm$1.1 | 0 | 464$\pm$88 |
CWISE J205701.64$-$170407.3 | 0 |  $\cdots$ |  $\cdots$ | [T8.5] | 0 | [51.0] | 344.6$\pm$31.3 | 0 | 624$\pm$79 |
DENIS-P J205754.1-025229 | 164 | L1.5 | 115 | L2$\beta$ | 175 | 64.4710$\pm$0.2365 | 102.3$\pm$0.4 | 168 | 2041$\pm$88 | yng
CWISEP J210007.87$-$293139.8 | 232 |  $\cdots$ |  $\cdots$ | [T9.5] | 232 | 43.8$\pm$18.0 | 425.8$\pm$53.5 | 0 | 511$\pm$79 | [52.7]
WISE J210200.15$-$442919.5 | 2 |  $\cdots$ |  $\cdots$ | T9 | 2 | 92.9$\pm$1.9 | 356.9$\pm$2.7 | 21,1 | 560$\pm$88 |
2MASSI J2104149-103736 | 115 | L2.5 | 103 | L2 | 124 | 58.1658$\pm$0.4051 | 664.1$\pm$0.8 | 168 | 1994$\pm$73 |
WISEA J211456.86-180519.0 | 233 |  $\cdots$ |  $\cdots$ | [T8] | 233 | 59.0$\pm$10.7 | 654.1$\pm$34.2 | 0 | 686$\pm$79 | [55.0]
PSO J319.3102$-$29.6682 (211714$-$294005) | 181 |  $\cdots$ |  $\cdots$ | T0: | 181 | 76.1$\pm$3.5 | 224.8$\pm$4.2 | 0 | 1218$\pm$88 |
WISE J212100.87$-$623921.6 | 149 |  $\cdots$ |  $\cdots$ | T2 | 149 | 74.9$\pm$3.2 | 460.9$\pm$3.5 | 0 | 1224$\pm$88 |
SDSS J212413.89+010000.3 | 57 |  $\cdots$ |  $\cdots$ | T5 | 124 | 57.0$\pm$3.2 | 321.5$\pm$3.5 | 237 | 1034$\pm$88 |
2MASS J21265916+7617440A | 133 |  $\cdots$ |  $\cdots$ | [L7] | 133 | 60.2775$\pm$0.8384 | 1120.1$\pm$2.3 | 168 | 1420$\pm$134 |
2MASS J21265916+7617440[B] | 133 |  $\cdots$ |  $\cdots$ | [T3.5] | 133 | 60.2775$\pm$0.8384 | 1120.1$\pm$2.3 | 168 | 1190$\pm$79 |
CWISEP J213249.05+690113.7 | 232 |  $\cdots$ |  $\cdots$ | [T8.5] | 232 | [56.2] | 274.4$\pm$15.3 | 0 | 624$\pm$79 |
WISEPA J213456.73$-$713743.6 | 4 |  $\cdots$ |  $\cdots$ | T9 pec | 4 | 109.7$\pm$3.7 | 1381.4$\pm$6.2 | 21,1 | 481$\pm$88 | sd
2MASS J21373742+0808463 | 112 | L5: | 112 | L5 | 124 | 66.0620$\pm$0.8664 | 695.8$\pm$2.2 | 168 | 1560$\pm$88 |
CWISEP J213838.74$-$313808.5 | 232 |  $\cdots$ |  $\cdots$ | T8 | 0 | [50.2] | 665.2$\pm$62.7 | 0 | 686$\pm$79 |
2MASS J21392676+0220226 | 112 | T2 | 214 | T1.5 | 61 | 101.5$\pm$2.0 | 501.7$\pm$3.4 | 74 | 1123$\pm$94 |
WISE J214155.85$-$511853.1 | 184 |  $\cdots$ |  $\cdots$ | L6 pec (blue) | 184 | 63.4787$\pm$0.9028 | 752.5$\pm$2.1 | 168 | 1415$\pm$88 |
GJ 836.7B (214431+144618) | 192 |  $\cdots$ |  $\cdots$ | T3 | 124 | 55.1631$\pm$0.0608 | 257.3$\pm$0.1 | 168aaThe astrometry listed is for the primary star in the system. | 1043$\pm$23 |
GJ 1263B (214638$-$001038) | 59 |  $\cdots$ |  $\cdots$ | T8.5 | 10 | 80.7724$\pm$0.1102 | 920.8$\pm$0.2 | 168aaThe astrometry listed is for the primary star in the system. | 568$\pm$88 |
WISE J214706.78$-$102924.0 | 8 |  $\cdots$ |  $\cdots$ | T7.5 | 8 | 51.8$\pm$2.4 | 172.7$\pm$2.1 | 0 | 774$\pm$88 |
2MASS J21481628+4003593 | 193 | L6 | 161 | L6.5 pec (red) | 161 | 123.2758$\pm$0.4557 | 898.8$\pm$1.1 | 168 | 1446$\pm$72 |
2MASS J21513839$-$4853542 | 195 |  $\cdots$ |  $\cdots$ | T4 | 124 | 57.46$\pm$2.31 | 465.0$\pm$2.8 | 200 | 1160$\pm$88 |
2MASS J21522609+0937575A | 112 | L6: | 117 |  $\cdots$ |  $\cdots$ | 51.3$\pm$3.4 | 301.9$\pm$1.3 | 0 | 1512$\pm$134 |
2MASS J21522609+0937575B | 112 | L6: | 117 |  $\cdots$ |  $\cdots$ | 51.3$\pm$3.4 | 301.9$\pm$1.3 | 0 | 1512$\pm$134 |
2MASS J21543318+5942187 | 24 |  $\cdots$ |  $\cdots$ | T6 | 24 | 71.0$\pm$2.3 | 493.4$\pm$1.0 | 0 | 981$\pm$88 |
WISEPC J215751.38+265931.4 | 4 |  $\cdots$ |  $\cdots$ | T7 | 4 | 61.2$\pm$2.0 | 119.5$\pm$1.1 | 0 | 762$\pm$88 |
WISEA J215949.54$-$480855.2 | 6 |  $\cdots$ |  $\cdots$ | T9 | 6 | 73.9$\pm$2.6 | 1279.6$\pm$1.6 | 0 | 549$\pm$88 |
WISEA J220304.18+461923.4 | 22 |  $\cdots$ |  $\cdots$ | T8 | 22 | 75.1$\pm$3.4 | 1317.3$\pm$4.6 | 0 | 686$\pm$79 |
Gl 845B (220410$-$564657) | 60 | T0-2 | 222 | T1 | 61 | 274.8048$\pm$0.2494 | 4708.2$\pm$0.6 | 168aaThe astrometry listed is for the primary star in the system. | 1236$\pm$79 |
Gl 845C (220410$-$564657) | 235 | T6-6.5 | 222 | T6 | 61 | 274.8048$\pm$0.2494 | 4708.2$\pm$0.6 | 168aaThe astrometry listed is for the primary star in the system. | 965$\pm$79 |
WISE J220905.73+271143.9 | 4 |  $\cdots$ |  $\cdots$ | Y0: | 18 | 161.7$\pm$2.0 | 1819.2$\pm$1.1 | 0 | 389$\pm$88 |
WISEPC J220922.10$-$273439.5 | 4 |  $\cdots$ |  $\cdots$ | T7 | 4 | 75.5$\pm$3.6 | 878.2$\pm$2.3 | 0 | 751$\pm$88 |
WISEA J221140.53$-$475826.7 | 6 |  $\cdots$ |  $\cdots$ | [T8] | 6 | 53.0$\pm$3.3 | 128.5$\pm$2.9 | 0 | 759$\pm$88 |
WISE J221216.33$-$693121.6 | 9 |  $\cdots$ |  $\cdots$ | T9 | 9 | 80.6$\pm$1.9 | 791.7$\pm$1.0 | 0 | 487$\pm$88 |
WISEPC J221354.69+091139.4 | 4 |  $\cdots$ |  $\cdots$ | T7 | 4 | 54.5$\pm$2.5 | 128.0$\pm$1.2 | 1 | 867$\pm$88 |
2MASS J22153705+2110554 | 196 |  $\cdots$ |  $\cdots$ | T1 pec | 196 | 57.6$\pm$3.6 | 197.1$\pm$4.2 | 0 | 1204$\pm$88 |
WISE J222055.31$-$362817.4 | 2 |  $\cdots$ |  $\cdots$ | Y0 | 2 | 95.5$\pm$2.1 | 305.9$\pm$1.3 | 0 | 452$\pm$88 |
2MASSW J2224438$-$015852 | 105 | L4.5 | 105 | L4.5 pec (red) | 166 | 87.50$\pm$0.54 | 984.4$\pm$0.1 | 172 | 1646$\pm$71 |
WISEPC J222623.05+044003.9 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 54.4$\pm$5.9 | 543.2$\pm$5.7 | 1 | 817$\pm$88 |
2MASS J22282889$-$4310262 | 34 |  $\cdots$ |  $\cdots$ | T6 | 61 | 92.1$\pm$2.6 | 305.7$\pm$3.6 | 74 | 891$\pm$82 |
CWISEP J223022.60+254907.5 | 232 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 232 | 71.3$\pm$16.0 | 735.5$\pm$47.7 | 0 | 367$\pm$79 | [62.2]
WISEA J223204.53$-$573010.4 | 6 |  $\cdots$ |  $\cdots$ | T9 | 6 | 51.7$\pm$3.4 | 426.1$\pm$2.4 | 0 | 611$\pm$88 |
WISE J223617.59+510551.9 | 8 |  $\cdots$ |  $\cdots$ | T5.5 | 8 | 102.8$\pm$1.9 | 780.3$\pm$3.3 | 237 | 1077$\pm$88 |
WISE J223720.39+722833.8 | 8 |  $\cdots$ |  $\cdots$ | T6 | 8 | 67.3$\pm$2.2 | 130.4$\pm$1.3 | 0 | 971$\pm$88 |
WISEA J224319.56-145857.3 | 233 |  $\cdots$ |  $\cdots$ | [Y0] | 233 | [68.3] | 626.1$\pm$22.1 | 0 | 460$\pm$79 |
2MASSW J2244316+204343 | 170 | L6.5 pec | 175 | L6-8$\gamma$ | 175 | 58.7$\pm$1.0 | 328.9$\pm$1.4 | 198 | 1184$\pm$10 | yng
DENIS-P J225210.73$-$173013.4A | 137 |  $\cdots$ |  $\cdots$ | [L4:] | 180 | 59.1461$\pm$0.8244 | 438.8$\pm$1.9 | 168 | 1722$\pm$134 |
DENIS-P J225210.73$-$173013.4B | 223 |  $\cdots$ |  $\cdots$ | [T3.5] | 180 | 59.1461$\pm$0.8244 | 438.8$\pm$1.9 | 168 | 1190$\pm$79 |
WISEA J225404.16-265257.5 | 233 |  $\cdots$ |  $\cdots$ | [T9.5] | 233 | [63.0] | 614.6$\pm$25.8 | 0 | 511$\pm$79 |
2MASSI J2254188+312349 | 32 | T5 | 214 | T4 | 124 | 72$\pm$3 | 199$\pm$8 | 77 | 1131$\pm$88 |
2MASS J22551861-5713056A | 111 | L6: | 167 | L5.5: | 167 | 58.8576$\pm$0.5866 | 327.4$\pm$1.2 | 168 | 1562$\pm$134 |
2MASS J22551861-5713056B | 167 |  $\cdots$ |  $\cdots$ | L8: | 167 | 58.8576$\pm$0.5866 | 327.4$\pm$1.2 | 168 | 1335$\pm$134 |
WISEPC J225540.74$-$311841.8 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 72.8$\pm$3.5 | 348.0$\pm$2.7 | 0 | 686$\pm$88 |
CWISEP J225628.97+400227.3 | 232 |  $\cdots$ |  $\cdots$ | [$\geq$Y1] | 232 | 101.8$\pm$11.2 | 720.0$\pm$32.1 | 0 | 367$\pm$79 |
CWISEP J230158.30$-$645858.3 | 232 |  $\cdots$ |  $\cdots$ | [T8.5] | 232 | [56.8] | 348.2$\pm$52.1 | 0 | 624$\pm$79 |
WISE J230133.32+021635.0 | 8 |  $\cdots$ |  $\cdots$ | T6.5 | 8 | 54.1$\pm$2.5 | 112.1$\pm$1.9 | 0 | 919$\pm$88 |
WISEA J230228.66$-$713441.7 | 6 |  $\cdots$ |  $\cdots$ | [T4.5] | 6 | 64.8$\pm$3.3 | 100.9$\pm$2.6 | 0 | 705$\pm$88 |
WISEPA J231336.40$-$803700.3 | 4 |  $\cdots$ |  $\cdots$ | T8 | 4 | 92.6$\pm$2.2 | 494.5$\pm$1.3 | 0 | 675$\pm$88 |
2MASS J23174712-4838501 | 112 | L4 pec | 133 | L6.5 pec (red) | 133 | 50.0212$\pm$1.2656 | 257.5$\pm$1.8 | 168 | 1537$\pm$197 | yng
2MASS J23185497$-$1301106 | 104 |  $\cdots$ |  $\cdots$ | T5 | 104 | 66.5$\pm$3.2 | 834.5$\pm$4.8 | 237 | 1120$\pm$88 |
WISEPC J231939.13$-$184404.3 | 4 |  $\cdots$ |  $\cdots$ | T7.5 | 4 | 80.9$\pm$2.7 | 154.8$\pm$1.6 | 0 | 632$\pm$88 |
ULAS J232123.79+135454.9 | 26 |  $\cdots$ |  $\cdots$ | T7.5 | 31 | 82.8$\pm$2.1 | 575.2$\pm$1.4 | 0 | 725$\pm$88 |
2MASS J23224684-3133231 | 112 | L0$\beta$ | 112 | L2$\beta$ | 118,175 | 50.3213$\pm$0.5576 | 577.4$\pm$0.8 | 168 | 1667$\pm$139 | yng
WISEPC J232519.54$-$410534.9 | 4 |  $\cdots$ |  $\cdots$ | T9 pec | 4 | 108.4$\pm$3.7 | 837.0$\pm$6.7 | 21,1 | 503$\pm$88 | sd
2MASS J23254530+4251488 | 120 | L8 | 120 | L7.5$\pm$1 | 124 | 67.6385$\pm$2.1054 | 289.3$\pm$5.0 | 168 | 1303$\pm$88 |
2MASS J23312378$-$4718274 | 3 |  $\cdots$ |  $\cdots$ | T5 | 124 | 56.5$\pm$7.5 | 101.1$\pm$2.9 | 0 | 1125$\pm$79 | [67.2]
WISE J233226.49$-$432510.6 | 2 |  $\cdots$ |  $\cdots$ | T9: | 2 | 61.1$\pm$2.1 | 362.6$\pm$1.2 | 0 | 555$\pm$88 |
2MASSI J2339101+135230 | 32 |  $\cdots$ |  $\cdots$ | T5 | 124 | 51.2$\pm$4.2 | 1028.2$\pm$7.8 | 0 | 1117$\pm$88 |
WISEPA J234351.20$-$741847.0 | 4 |  $\cdots$ |  $\cdots$ | T6 | 4 | 60.9$\pm$2.2 | 436.5$\pm$1.3 | 0 | 974$\pm$88 |
CWISE J234426.81$-$475502.6 | 0 |  $\cdots$ |  $\cdots$ | T5.5 | 0 | [59.8] | 119.6$\pm$13.0 | 0 | 1044$\pm$79 |
WISEPC J234446.25+103415.8 | 4 |  $\cdots$ |  $\cdots$ | T9 | 4,8 | 68.0$\pm$2.6 | 947.0$\pm$1.6 | 0 | 574$\pm$88 |
WISEPC J234841.10$-$102844.4 | 4 |  $\cdots$ |  $\cdots$ | T7 | 4 | 58.4$\pm$3.5 | 642.5$\pm$1.5 | 1 | 853$\pm$88 |
WISEA J235402.79+024014.1 | 9 |  $\cdots$ |  $\cdots$ | Y1 | 9 | 130.6$\pm$3.3 | 642.7$\pm$3.1 | 0 | 388$\pm$88 |
CWISEP J235644.78-481456.3 | 232 |  $\cdots$ |  $\cdots$ | [Y0.5] | 232 | [57.6] | 887.1$\pm$25.0 | 0 | 412$\pm$79 |
2MASSI J2356547$-$155310 | 32 |  $\cdots$ |  $\cdots$ | T5.5 | 124 | 68.97$\pm$3.42 | 746.2$\pm$2.9 | 68 | 1007$\pm$88 |
WISE J235716.49+122741.8 | 8 |  $\cdots$ |  $\cdots$ | T6 | 8 | 61.9$\pm$3.0 | 509.1$\pm$3.1 | 0 | 905$\pm$88 |
WISEPA J235941.07$-$733504.8 | 4 |  $\cdots$ |  $\cdots$ | T5.5 | 4 | 86.7$\pm$5.7 | 283.6$\pm$7.7 | 66 | 879$\pm$88 |

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Having now compiled the census, it is instructive to look back to previous
attempts at assembling lists of nearby L, T, and Y dwarfs. These comparisons
show how quickly our knowledge of this sample has evolved in just over fifteen
years.

Kendall, et al. (2004) published a list of the sixteen nearest L dwarfs, out
to $\sim$11 pc. Of those, fourteen appear in Table 11, the two exceptions
being objects now considered to be late-M dwarfs: SDSS J143808.31+640836.3,
which Cruz, et al. (2003) classify as M9.5 in the optical, and 2MASSW
J2306292$-$050227202020Kendall, et al. 2004 mistakenly list this as 2MASSW
J2306292+154905. (aka TRAPPIST 1), which Gizis, et al. (2000) type as an
optical M7.5.

Looper et al. (2008a) published a list of L dwarfs believed to fall within 10
pc. All ten of those objects appear in Table 11.

Reid et al. (2008) published a list of ninety-four L dwarf systems believed to
lie within 20 pc. Eighty-four of these appear in Table 11. The exceptions are
eight systems – 2MASS J01550354+0950003, 2MASS J02284243+1639329, DENIS
J061549.3$-$010041, SDSS J080531.84+481233.0, DENIS J082303.1$-$491201, 2MASS
J09111297+7401081, 2MASS J19360187$-$5502322, and 2MASS J20360316+1051295 –
that are now known to fall just outside of the 20-pc volume according to Gaia
DR2, and two objects – DENIS J065219.7$-$253450 (M9.2 near-infrared; Bardalez
Gagliuffi, et al. 2014) and 2MASSW J1421314+182740 (M8.9 near-infrared;
Bardalez Gagliuffi, et al. 2014) – that we consider to be late-M dwarfs.

Kirkpatrick et al. (2012) published the full stellar census within 8 pc, using
a combination of preliminary trigonometric parallaxes and spectrophotometric
distance estimates for the L, T, and Y dwarfs. All thirty-three of those L, T,
and Y dwarfs appear in Table 11.

Kirkpatrick et al. (2019) gave a listing of 235 L0-L5.5 and T6-Y1+ dwarfs
within 20 pc but missed a few objects, discovered prior to their paper, that
this new census now includes. In the L0-L5.5 range, a handful of component
objects in systems known to be binaries or triples were overlooked – DENIS
0205$-$1159A ([L5]; Bouy et al. 2005), 2MASS 1315$-$2649A (L5.5/L5; Burgasser
et al. 2011b), LSPM 1735+2634B (L0:; Law et al. 2006), Gl 802B ([L5-L7];
Ireland et al. 2008), and DENIS 2252$-$1730 ([L4:]; Reid et al. 2006b).
Several previously published objects near the L0 or L5.5 edges are now
considered to fall within the L0-L5.5 range based on published spectral types
– 2MASS 0413+3709 ([L1]; Kirkpatrick et al. 2010), 2MASS 0421$-$6306
(L5$\beta$; Cruz, et al. 2007), 2MASS 0835$-$0819 (L5; Cruz, et al. 2003),
2MASS 0908+5032 (L5/L6; Cruz, et al. 2003), and 2MASS 1010$-$0406 (L6/L5;
Cruz, et al. 2003). Two objects in the middle of the L0-L5.5 range were also
overlooked: WISE J0508+3319 (L2; Kirkpatrick et al. 2016) and DENIS
J1013$-$7842 (L3; Aberasturi et al. 2014). Finally, one object (2MASS
J21580457$-$1550098; L4:/L5; Gizis, et al. 2003) has now been dropped from the
Kirkpatrick et al. (2019) list because a definitive parallax from Smart et al.
(2018) shows that it likely lies beyond 20 pc. In the T6-Y1+ range, two
objects near T6 were overlooked – UGPS 0355+4743 (T6:; Smith et al. 2014) and
2MASS 2154+5942 (T6; Looper et al. 2007) – along with two later T dwarfs –
2MASS 1315$-$2649B (T7; Burgasser et al. 2011b) and Gl 758B (T7; Thalmann et
al. 2009).

Bardalez Gagliuffi et al. (2019) published a list of 472 dwarfs of type M7
through L5 within 25 pc, of which 283 fall within 1$\sigma$ of 20 pc. Three of
the L dwarfs do not appear in our Table 11 because we consider them to have
late-M spectral types: DENIS J065219.7$-$253450 (see above), 2MASS
J14213145+1827407 (see above), and 2MASSI J1438082+640836 (M9.5 optical; Cruz,
et al. 2003). Several other L dwarfs are now known (or are likely, within the
uncertainties) to be outside of the 20-pc volume based on accurate parallaxes:
DENIS J1228.2$-$1547AB (Dupuy, & Liu 2017), SDSS J133148.92$-$011651.4 (Smart
et al. 2018), SDSS J144600.59+002451.9 (Faherty et al. 2012), SDSS
J153453.33+121949.2 (Gaia Collaboration et al. 2018), 2MASS J21580457-1550098
(Smart et al. 2018), and 2MASS J23512200+3010540 (Liu et al. 2016). Two other
L dwarfs, 2MASS J04474307-1936045 ($\sim$26 pc; Faherty et al. 2012), and SDSS
J092308.70+234013.6 ($\sim$21pc; Schmidt, et al. 2010), have published
spectrophotometric distance estimates placing them outside of 20 pc, so they
are not included in our table.

Finally, there are two objects noted in Best et al. (2020) as falling within
20 pc that are nonetheless excluded from Table 11. 2MASS J05160945$-$0445499
has a parallax listed by Best et al. (2020) as 54.2$\pm$4.3 mas, but a more
accurate parallax of 47.83$\pm$2.85 mas from NPARSEC (Smart, priv. comm.),
places this object just outside of 20 pc. WISEA J055007.94+161051.9 has a Best
et al. (2020) parallax of 53.9$\pm$2.8 mas, but a more accurate Gaia DR2
parallax of 49.1169$\pm$0.8467 places it beyond 20 pc.

The above checks are illustrative of the fact that our knowledge of the nearby
census is constantly changing. New objects are still being discovered. Some
objects already known within the census are found to be binary (or triple),
and some higher mass stars within 20 pc are found to have L, T, or Y
companions. Some objects originally thought to lie within the volume are
found, once better astrometry is available, to fall outside. And objects are
sometimes discovered then forgotten simply because there does not exist a
living, publicly available database that adequately captures this information.
Nonetheless, our knowledge – and our completeness – of this census is
improving with time, thereby enabling a more robust look into the low-mass
products of star formation.

##  7 Characterizing the 20-pc Census

With the census of L, T, and Y dwarfs within 20 pc now compiled, we can begin
to study the field mass function. As described in section 8 below, we must
compute space densities binned by effective temperature so that we can compare
the empirical data to mass function simulations. This requires us to calculate
an effective temperature for each individual object. Most objects can be
assigned temperatures using relations typical of old, solar-metallicity field
objects, but some objects within the census are young or low metallicity. To
handle these properly, we first need to identify which objects they are.
Moreover, because we want to assign temperatures to individual objects, this
means recognizing when objects are unresolved multiple systems, to the extent
that our existing data can help to address that. In the next subsections we
delve into this characterization of the census, as a prelude to determining
the space densities we need.

###  7.1 Low-gravity (Young) Objects

Brown dwarfs with ages less than $\sim$100 Myr have not yet fully contracted
to their final, equilibrium radius (Kirkpatrick et al. 2008) and are
identifiable through spectroscopic and photometric signatures that indicate a
lower gravity than normal, old brown dwarfs that have fully contracted. These
young brown dwarfs represent a challenge to determining the mass function via
our methodology because the standard mapping of spectral type, absolute
magnitude, or color into effective temperature does not apply to them (Faherty
et al. 2016). Young objects that fall within the 20-pc census need to be
identified so that they can be placed into the correct bins of Teff.

On the other hand, these same objects also represent an opportunity to probe
the low-mass cutoff. Objects below a few Jupiter masses are generally very
difficult to find if formed billions of years ago because of the intrinsic
faintness resulting from their long cooling times. However, objects of similar
mass can be much more easily detected when they are younger because they will
be much warmer and brighter. An isolated brown dwarf that shows signs of low
gravity, if it can be associated kinematically to a moving group or young
association of known age, can be placed on theoretical isochrones to produce a
mass estimate. Although it was once believed that a large reservoir of rogue
planets – objects that escaped their original protoplanetary disks – existed
in the Milky Way (Sumi et al. 2011), microlensing results with more robust
statistics have shown that the population of field objects having masses down
to at least a few Jupiter masses appears to be drawn from the same population
as higher-mass brown dwarfs and stars (Mróz et al. 2017). Thus, such young
brown dwarfs can serve as independent probes of the low-mass cutoff value of
star formation itself.

Spectroscopic signatures of youth have been noted in late-M, L, and even some
T dwarfs (e.g., Cruz et al. 2009; Allers & Liu 2013; Gagné et al. 2015), and
classification systems have been developed to incorporate these. The most
commonly used system (Kirkpatrick 2005) assigns a suffix of $\beta$, $\gamma$,
or $\delta$ to the core type to indicate the degree to which low-gravity
signatures are evident, with the infrequently used $\alpha$ suffix assigned to
spectra with gravities typical of old field objects. Faherty et al. (2016)
note that a fraction of objects assigned $\beta$ designations seem not to
belong to any known, young moving groups, and some young associations of
presumably fixed age can contain objects with both $\beta$ and $\gamma$
designations. Sengupta & Marley (2010) point out that the rotation rates of
some brown dwarfs can make them oblate, but non-sphericity in an old object
seen equator-on is unlikely to produce the radius inflation needed to turn an
$\alpha$ classification into a $\beta$ classification, for example. The
differences between the two classifications is thought to be around 0.5 dex in
log($g$) (see Figure 9 of Burrows et al. 1997), so a simple calculation shows
that a radius increase of 10$\times$ would be needed to achieve the effect.
Gonzales et al. (2019) has further noted that the late-M dwarf TRAPPIST-1,
though presumably of field age, nonetheless has near-infrared spectral indices
indicating an intermediate gravity. If this star’s radius is truly inflated,
it could be due to magnetic activity or to tidal interactions by the numerous
planets in its solar system. (It has also been shown that low-gravity indices
can sometimes be incorrectly assigned in the near-infrared for subdwarfs
[Aganze et al. 2016], although a more careful analysis of the overall spectral
energy distribution can eliminate this problem.) For the remainder of our
analysis, we will regard $\beta$ designations to be true indicators of low
gravity even if youth cannot confidently be assigned through moving group
membership.

Several L, T, and Y dwarfs in the 20-pc census (Table 11) are known to have
low-gravity features. Given that our Spitzer monitoring has improved the
astrometry for many of these targets, we can now run analyses to determine if
there are any objects found to be high-probability members of any known moving
groups but lacking spectra or having spectra where gravity diagnostics are
less clear. For this exercise, we consider only those objects in the 20-pc
census having measured trigonometric parallaxes, and we use two separate tools
that can assess membership probabilities based on the subset of kinematic data
we have – positions, distances, and motions, but not radial velocities. The
first tool is Banyan $\Sigma$ (Gagné et al. 2018), which uses Bayesian
inference to compute the membership probabilities for twenty-nine different
associations within 150 pc of the Sun. For our set of input parameters (RA,
Dec, $\varpi_{abs}$, $\mu_{\alpha}$, $\mu_{\delta}$), Banyan $\Sigma$ uses
Bayes’ theorem to marginalize over radial velocity, and the Bayesian priors
are set so that a probability threshold of 90% will recover 82% of true