# Discovery of 34 low-mass comoving systems using NOIRLab Source Catalog DR2

Frank Kiwy Backyard Worlds: Planet 9  Jacqueline K. Faherty Department of
Astrophysics, American Museum of Natural History, Central Park West at 79th
Street, NY 10024, USA  Aaron Meisner NSF’s National Optical-Infrared Astronomy
Research Laboratory, 950 N. Cherry Ave., Tucson, AZ 85719, USA  Adam C.
Schneider United States Naval Observatory, Flagstaff Station, 10391 West Naval
Observatory Rd., Flagstaff, AZ 86005, USA  Department of Physics and
Astronomy, George Mason University, MS3F3, 4400 University Drive, Fairfax, VA
22030, USA  J. Davy Kirkpatrick IPAC, Mail Code 100-22, Caltech, 1200 E.
California Blvd., Pasadena, CA 91125, USA  Marc J. Kuchner NASA Goddard Space
Flight Center, Exoplanets and Stellar Astrophysics Laboratory, Code 667,
Greenbelt, MD 20771, USA  Adam J. Burgasser Center for Astrophysics and Space
Science, University of California, San Diego, La Jolla, CA 92093, USA  Sarah
Casewell School of Physics and Astronomy, University of Leicester, University
Road, Leicester, LE1 7RH, UK  Rocio Kiman Kavli Institute for Theoretical
Physics, University of California, Santa Barbara, CA 93106, USA  Emily
Calamari Department of Physics, Barnard College, Columbia University, New
York, NY 10027, USA  Christian Aganze Department of Physics, University of
California, San Diego, La Jolla, CA 92093  Chih-Chun Hsu Department of
Physics, University of California, San Diego, La Jolla, CA 92093  Arttu Sainio
Backyard Worlds: Planet 9  Vinod Thakur  Backyard Worlds: Planet 9  The
Backyard Worlds: Planet 9 Collaboration

###### Abstract

We present the discovery of 34 comoving systems containing an ultra-cool dwarf
found by means of the NOIRLab Source Catalog (NSC) DR2. NSC’s angular
resolution of $\sim 1\arcsec$ allows for the detection of small separation
binaries with significant proper motions. We used the catalog’s accurate
proper motion measurements to identify the companions by cross-matching a
previously compiled list of brown dwarf candidates with NSC DR2. The comoving
pairs consist of either a very low-mass star and an ultra-cool companion, or a
white dwarf and an ultra-cool companion. The estimated spectral types of the
primaries are in the K and M dwarf regimes, those of the secondaries in the M,
L and T dwarf regimes. We calculated angular separations between $\sim 2$ and
$\sim 56\arcsec$, parallactic distances between $\sim 43$ and $\sim 261$ pc
and projected physical separations between $\sim 169$ and $\sim 8487$ AU. The
lowest measured total proper motion is 97 mas yr-1, the highest 314 mas yr-1.
Tangential velocities range from $\sim 23$ to $\sim 187$ km s-1. We also
determined comoving probabilities, estimated mass ratios and calculated
binding energies for each system. We found no indication of possible binarity
for any component of the 34 systems in the published literature. The
discovered systems can contribute to the further study of the formation and
evolution of low-mass systems as well as to the characterization of cool
substellar objects.

Binary stars — Multiple stars — Low-mass stars — Brown dwarfs — White dwarf
stars

##  1 Introduction

Binary and multiple stellar systems have long been used to study the formation
and fundamental properties of stars. With the first discovery of brown dwarf
binary systems (Martín et al., 1998; Basri & Martín, 1999; Martín et al.,
1999), these investigations have been extended into the substellar regime.
Physical properties of individual brown dwarfs (e.g. mass, metallicity or
surface gravity) are difficult to determine due to the absence of main
sequence hydrogen burning, causing them to cool and fade over time. For brown
dwarfs in multiple systems, however, physical properties, age and composition
can be inferred from their stellar companions. Further, the binary fraction,
mass ratio distribution and separation of brown dwarf companion systems can
provide constraints on star formation and dynamical evolution (Goodwin &
Whitworth, 2007).

One valuable type of benchmark systems are those with a wide binary composed
of resolved companions, the primary being a main sequence star and the
secondary being an L or T dwarf. Because it is very difficult to determine
properties such as metallicity and age of L and T dwarfs, these properties can
be inferred from the primary since comoving systems are assumed to have formed
at the same time, from the same material and developed in the same
environment. However, benchmark systems involving L or T dwarf companions are
more difficult to find than systems composed of earlier type companions,
because often either the primary is saturated or the secondary remains
undetected. Moreover, the binary fraction seems to decrease from early to late
primary spectral types (Kraus & Hillenbrand, 2012). While the binary fraction
for solar type stars ranges within 50-60% (Duquennoy & Mayor, 1991; Raghavan
et al., 2010), it decreases to 30-40% for M stars (Fischer & Marcy, 1992;
Delfosse et al., 2004; Janson et al., 2014; Winters et al., 2019). For field
brown dwarfs, the resolved binary fraction for very low-mass systems is around
10-20% (Close et al., 2003; Burgasser et al., 2006; Gelino et al., 2011;
Huélamo et al., 2015; Fontanive et al., 2018).

Identifying comoving companions has become easier through the use of large,
multi-epoch surveys such as the Wide-field Infrared Survey Explorer (Wright et
al., 2010), the Gaia Mission (Gaia Collaboration et al., 2016), or the DESI
Legacy Imaging Surveys (Dey et al., 2019). Resulting catalogs like CatWISE2020
(Marocco et al., 2021), Gaia DR2 (Gaia Collaboration et al., 2018), Gaia EDR3
(Gaia Collaboration et al., 2021) or NSC DR2 (Nidever et al., 2021) are
excellent resources for finding late-type moving objects and their potential
companions by using the provided proper motions. Two objects sufficiently
close to each other on the sky and having comparable proper motions can
provide a basis for inferring a common origin.

This paper is outlined as follows. In Section 2, we briefly describe the NSC
and its key elements relevant to this work. In Section 3, we present our
search method, and in Section 4, we characterize the discovered systems. We
discuss some of the systems in more detail in Section 5.

##  2 NOIRLab Source Catalog DR2

NSC DR2 (Nidever et al., 2021) is based on public image data from the NOIRLab
Astro Data Archive. These images come from telescopes in both hemispheres
(CTIO-4m+DECam, KPNO-4m+Mosaic3 and Bok-2.3m+90Prime) and cover $\sim 35,000$
square degrees of the sky. A significant part of the images were obtained by
the Dark Energy Survey (Abbott et al., 2018) and the DESI Legacy Imaging
Surveys (Dey et al., 2019). NSC DR2 includes more than 3.9 billion single
objects with over 68 billion individual source measurements. It has depths of
$\sim 23rd$ magnitude in most broadband filters (u, g, r, i, z, Y and VR),
accurate proper motions and an astrometric accuracy of $\sim 7$ mas.

NSC provides proper motion measurements that push much fainter at optical
wavelengths than Gaia DR2 or EDR3. At g-band, NSC is $\sim 2.5$ magnitudes
deeper than Gaia and allows proper motion searches for distant stars with high
tangential velocities over a volume $\sim 25$ times larger than Gaia. NSC can
also measure motions for white dwarfs much fainter than those detected by
Gaia, expanding the census of white dwarfs in the solar neighborhood. NSC’s
accurate proper motions enable the discovery of ultra-cool white dwarf
binaries where metallicity and radial velocity can be derived from a main
sequence companion (Lam et al., 2020).

Due to its excellent red-optical sensitivity and sky coverage, NSC provides
many new possibilities to search for ultra-cool stars and brown dwarfs in the
solar neighborhood. CatWISE2020 (Marocco et al., 2021) represents one of the
best infrared proper motion catalogs currently available. However, at its
faint end, CatWISE motions are only significant above $\sim 150-200$ mas yr-1,
unlike NSC, which can measure motions many times smaller at high significance.
NSC’s Y-band depth (23.4 mag) and angular resolution ($\sim 1\arcsec$) allow
for motion searches of late-type objects not possible with WISE. This enables
queries for pairs of faint objects with consistent proper motions to find
closely spaced low-mass companion systems.

##  3 Search Method

In a first step, we searched for previously missed L and T dwarfs in the
NOIRLab Source Catalog using proper motion and photometry. We used the z, i
and Y magnitudes along with the relations described in Carnero Rosell et al.
(2019) to determine the color cut for our initial selection. We required all
objects having at least one detection in each of those three bands. The
adopted color cut ($1.4<(i-z)_{NSC}<3.5$ and $0.4<(z-Y)_{NSC}<1.5$) should
restrict the search to L and T dwarfs. However, it cannot be excluded that
some late M dwarfs are within the selected objects. Note that both color
constraints had to be satisfied for this selection. No quality cuts were
applied to the photometry to avoid eliminating more distant late-type/faint
objects with less accurate photometry. Candidates having proper motions below
100 mas yr-1 have been discarded from the selection to provide proper motions
significant enough to be visually confirmed by blinking images of different
epochs. We avoided the galactic plane ($\lvert b\rvert>15$°) to further reduce
the number of sources with spurious proper motions. We required a high
Star/Galaxy classifier of at least 0.7 to ensure that the search only returns
objects with a point-like morphology. The Star/Galaxy classifier is a NSC
catalog column which provides information on an object’s probability of being
either a galaxy or a star, based on its morphology. Selected objects had to
have a time baseline of at least six months between the first and last
observation. By applying these criteria, we obtained a total of 2896 candidate
ultracool dwarfs, mostly in the L and T regimes.

In a second step, we examined a $100\arcsec$ radius around all 2896 objects
using the NSC by comparing the proper motion components of each object to the
proper motion components of the objects found in the defined radius. We
applied a proper motion matching tolerance of 20 mas yr-1 to find potential
companions either of earlier or later type. Note that we exclusively used NSC
DR2 proper motions for this purpose. As in the first step, we excluded objects
having a Star/Galaxy classifier below 0.7 and a time baseline of less than six
months. To further reduce the number of false positives, each identified
companion was cross-matched with Gaia EDR3 to discard objects with a parallax
below 2 mas. This resulted in 46 pairs with similar proper motions.

Among those 46 potential companions, we found four false positives (no object
visible in WISE or DECaLS imagery), three likely false positives with
significant differences in their proper motion components, and thirteen known
pairs, one of which (NSC J2322-6151) is referenced in Smart et al. (2019) and
Calissendorff et al. (2019), the other twelve find mention in the SUPERWIDE
catalog (Hartman & Lépine, 2020). The known pairs, which are listed in Table 1
(Rediscovered systems), are not further described in this paper.

We repeated both steps described above using a slightly different color cut
than in the first selection ($i_{NSC}>99$ and $0.4<(z-Y)_{NSC}<1.5$). The goal
of this second selection was to target specifically substellar sources and not
more distant warmer stars. Since late-type brown dwarfs emit more radiation in
the near infrared, an i-band dropout is a strong signature for detecting a
cold compact source. We therefore dropped the $i-z$ color but used the same
constraints for the $z-Y$ color than in the first selection. We also required
selected objects explicitly to have no i-band photometry by adding a
corresponding constraint ($i>99$) to exclude any objects found in the first
selection. After applying the first step of our search method, we obtained a
total of 2520 objects. Step two resulted in three additional systems, #2, #21
and #24, having secondaries with estimated spectral types of T5, T3 and T0,
respectively.

Each object has been visually inspected to determine whether its proper motion
components are consistent with those of its comoving companion by blinking
images of different epochs. For this, we used AstroToolBox (Kiwy, 2022), which
is a Java tool set with a graphical user interface allowing us to blink either
unWISE coadds (Meisner et al., 2017, 2018) of epochs 2010 and 2014-2020, or
DECaLS cutouts (Dey et al., 2019) from DR5, DR7, DR8 and DR9. DECaLS cutouts
have a resolution $10\times$ higher than unWISE coadds (0.27″/pixel vs.
2.75″/pixel), making it possible to identify the components of binary systems
down to an angular separation of $\sim 1\arcsec$. All objects have been
carefully checked against at least one background star, showing no visible
motion, to eliminate false positives produced by misaligned images.

To assess the effect of the photometric uncertainties on the selection, we
calculated the mean photometric error associated with the $(i-z)_{NSC}$ and
$(z-Y)_{NSC}$ colors of the secondaries in our sample, which is 0.035 mag for
both of these colors (Table 8). The used color cut ($1.4<i-z<3.5$ and
$0.4<z-Y<1.5$) was determined by the means of the Carnero Rosell et al. (2019)
relations with the following color values for the given spectral types: {L0,
T9} = {($i-z=1.48,z-Y=0.43$), ($i-z=3.39,z-Y=1.5$)}. Note that the Carnero
Rosell relations do not give uncertainties on their color values. When we
subtract the mean photometric errors from the color values for spectral type
L0, we obtain the following values: $i-z=1.48-0.035=1.445$ and
$z-Y=0.43-0.035=0.395$. While the value for the $i-z$ color is still above the
lower limit of our color cut, that for the $z-Y$ color is 0.005 mag below the
limit. Given this small color value difference, we conclude that it has
minimal, if any, effect on the selection. As for the upper limits of the used
color cut, the photometric errors do not affect the selection since our sample
does not contain objects with estimated spectral types later than T5. This
corresponds to the color values $i-z=3.25$ and $z-Y=1.02$ from the Carnero
Rosell relations, which both are well below the upper bounds of the employed
color cut ($i-z=3.5,z-Y=1.5$), and stay well below even if we add the mean
photometric uncertainties ($i-z=3.25+0.035=3.285$ and $z-Y=1.02+0.035=1.055$).

Aside from the 29 new systems discovered through the method described above,
an additional five new systems (#3, #11, #16, #25 and #27) were recovered
serendipitously when visually checking a list of objects from a previous NSC
DR2 search focused on high proper motion ultra-cool dwarf candidates. The
color and proper motion cuts used in that search were somewhat different from
those applied in step one of this work. In each of these cases, the companion
could be identified through AstroToolBox’s image blinker. For those five
systems, either the primary or the secondary did not satisfy all the
constraints defined in the search method of this work.

At the same time these searches were on-going, several members of the Backyard
Worlds: Planet 9 citizen science project (Kuchner et al., 2017) were searching
for similar cold compact objects via the Zooniverse portal or via a research
scientist guided side project. Arttu Sainio recovered system #21, Vinod Thakur
recovered systems #13, #20, and Sam Goodman recovered systems #1 and #35.
Details on those searches and additional discoveries by the larger Backyard
Worlds team will be reported in a forthcoming paper.

We identified a total of 34 new candidate binary systems, most of which are
located in the DES footprint (Abbott et al., 2021). The general properties of
these systems are given in Table 1 (Newly discovered systems) with additional
astrometry from NSC DR2 in Table 2 and relevant photometry in Table 7.
Histograms showing the distribution of distances, angular and physical
separations, total proper motions and tangential velocities can be found in
Figure 2.

##  4 Characterizing Systems

###  4.1 Spectral Type Estimates

We evaluated the photometric quality of our sample by calculating the weighted
mean of all photometric errors in all bands of the employed photometric
systems. Since the secondaries are generally fainter and often blended by the
primaries, we calculated the weighted mean separately and found that it is
0.015 mag for the primaries and 0.078 mag for the secondaries (Table 8). We
deduce that the overall photometric quality of our sample is good and even
excellent for most of the primaries but degrades for the secondaries (with
regard to the primaries).

We plotted different types of color-magnitude diagrams (CMDs), using Gaia EDR3
G-band versus $G-G_{RP}$ color, Pan-STARRS DR2 z-band versus $z-y$ color, NSC
DR2 z-band versus $z-Y$ color, and VISTA VHS DR5 J-band versus $J-Ks$ color
(Figure 3). For the Gaia CMD, we plotted the primaries on a comparative sample
composed of late K and M dwarfs (K8-M9) and DA white dwarfs extracted from the
SIMBAD database (Wenger et al., 2000). For the Pan-STARRS, NSC and VISTA VHS
CMDs, we used as a comparative sample the M dwarfs from Best et al. (2018) and
the L & T dwarfs from Best et al. (2020). The M dwarfs were cross-matched with
Gaia EDR3 to obtain the parallaxes to calculate the absolute magnitudes. M, L
and T dwarfs were cross-matched with NSC and VISTA VHS to get the
corresponding photometry. A radius of $2\arcsec$ was used for both cross-
matches. We split the comparative sample into early and late-type M, L and T
dwarfs and used a different color for each of these categories. We always
plotted all the systems having the corresponding photometry on each of those
CMDs.

According to our color-magnitude diagrams, we found 31 systems composed of a
main sequence star and an ultra-cool companion, and 3 systems composed of a
white dwarf and an ultra-cool companion. The estimated spectral types of the
main-sequence stars are in the late-K and M dwarf regimes, those of the ultra-
cool companions in the late-M, L and early-T dwarf regimes. Our search
resulted in 1 K+L, 11 M+M, 16 M+L, 3 M+T, 1 WD+M and 2 WD+L systems. More
accurate spectral type estimates can be found in Table 1.

The spectral type estimates were obtained from AstroToolBox’s Photometric
Classifier, which uses the available photometry along with the relations from
Kiman et al. (2019), Carnero Rosell et al. (2019), Best et al. (2018) and
Mamajek (2021) to establish a spectral type classification by counting the
occurrences of each determined spectral type. Kiman et al. (2019) relates to
Gaia photometry for spectral types M0 to L7, Carnero Rosell et al. (2019)
relates to DES, VHS and AllWISE photometry for spectral types M1 to T9, and
Best et al. (2018) relates to Pan-STARRS, 2MASS and WISE photometry for
spectral types M0 to T9. The Mamajek (2021) relations are using Gaia
photometry for spectral types B9-L8, Sloan photometry for spectral types
M0-T8, 2MASS photometry for spectral types O9-Y1, and WISE photometry for
spectral types B5-K5 and M5-Y4. AstroToolBox does not account for photometric
uncertainties, but relies on the number of equal spectral type estimates from
the various photometric systems and corresponding relations. For each object,
we retained the spectral type with the most occurrences. In case there were
two or more distinct spectral types with the same number of occurrences, we
kept the one whose photometric distance best fits the Gaia parallax. When
considering the mean photometric error of our sample in each of the used
colors (Table 8), we infer a spectral type uncertainty of about one sub-type
for the primaries and two sub-types for the secondaries.

###  4.2 Spectroscopy

####  4.2.1 Kast Optical Spectrograph

Optical spectroscopy was obtained for the primary of system #8 (NSC
J0153$-$0015A) using the Kast Double Spectrograph mounted on the Lick 3m Shane
Telescope on 2021 Dec 12 (UT). Conditions were cloudy with average seeing of
1$\farcs$3\. Two exposures of 1500 s each were obtained in the red channel
using the 600/7500 grating and 1$\farcs$5-wide slit, providing 6000–9000 Å at
an average resolution of $\lambda/\Delta\lambda$ = 1900. Only one of the
exposures was used due to the deteriorating weather conditions. The flux
standard Feige 110 was observed at the start of the night for flux
calibration, and the G2 V star HD 13043 was observed after NSC J0153$-$0015A
to measure telluric absorption. Data were reduced and analyzed using the
kastredux package111https://github.com/aburgasser/kastredux with default
settings. The reduced spectrum, shown in Figure 4 (bottom left panel), has an
average signal-to-noise of $\approx$25, due to the poor transparency.
Nevertheless, we detect an overall red spectral energy distribution and weak
molecular features consistent with an early-type M dwarf. We compared this
spectrum to M dwarf optical template spectra from Bochanski et al. (2007),
finding a best match to the M1 template, which we adopt for the classification
of this primary.

####  4.2.2 SpeX Infrared Prism Spectroscopy

We observed the secondary in system #21 using the SpeX spectrograph on NASA’s
IRTF telescope. The spectrum was taken on the night of 23 October 2021 (UT),
under good conditions with minimal cloud coverage, in prism mode using the
0.8$\arcsec$ slit to achieve a resolving power of $\sim$100 - 500 over the 0.8
- 2.5 $\mu$m coverage. We obtained 7 AB nods using 180 s exposures on the
target and then acquired the A0 star HD 32855 for telluric correction using 1
s exposures and 10 AB nods. All data were reduced using the Spextool package
(Cushing et al., 2004) with telluric correction and flux calibration of the A0
stars following the technique described in Vacca et al. (2003). In Figure 4
(top right panel) we compare this spectrum to several T dwarf standards from
Burgasser et al. (2004) and find a good agreement with the T3 standard, which
confirms our spectral type estimate for this object.

###  4.3 Distance Estimates

Photometric distances were calculated for the secondaries by employing
relevant spectro-photometric distance conversions. We used the spectral type
estimates from AstroToolBox and derived the corresponding absolute magnitudes
from Table 4 in Kiman et al. (2019) and Table 6 in Best et al. (2018). For
each photometric system, we calculated distances using the bands covered by
the above relations and retained the minimum and maximum values of the
photometric system with the best match. For a given magnitude, we estimated an
average distance difference between a given sub-type (e.g. L5) and its lower
and upper neighbors (L4, L6) of $\sim 20\%$ of the sub-type’s (L5) photometric
distance. These estimations were done by comparing the distances of the lower
and upper neighbors of a given sub-type at different magnitudes and in
different bands. Since we assume a spectral type uncertainty of two sub-types
for the secondaries, this can lead to distance discrepancies of up to $\sim
40\%$ of the secondary’s photometric distance, depending on the quality of the
photometry used for the spectral type estimates. A comparison between the
parallactic distance of the primaries and the mean photometric distance of the
secondaries is presented in Table 3, which also contains the bands used to
calculate the minimum and maximum photometric distances as well as the
spectral types employed to derive the absolute magnitudes for those
calculations. We have illustrated the distance difference between the
primaries and the secondaries in Figure 1. Note that for systems #9 and #15,
the parallactic distance of the primary is about twice the photometric
distance of the secondary, which we discuss further in Section 5.

Figure 1: Secondary mean photometric distance versus primary parallactic
distance.

###  4.4 Chance Alignment

We determined comoving probabilities using the CoMover code from Gagné et al.
(2021), which uses the sky position, proper motion, parallax and optionally
the heliocentric radial velocity of the host star with their respective
errors, and compares these with the observables of the potential companion on
the basis of various star models.

We executed the code once without a distance constraint and once with a
distance constraint on the secondaries, since most photometric distances of
our secondaries are based on spectral type estimates only. Also, the blending
caused by some of the primaries can lead to inaccurate photometry, affecting
spectral type and photometric distance estimates.

The resulting comoving probabilities are shown in Table 3. Those without a
distance constraint are all $>=$ 99.3% except for system #13, which only has a
comoving probability of 73.6%. Those with a distance constraint are $>=$ 99.8%
except for three systems (#9, #13 and #15), which all have comoving
probabilities significantly lower than 100% (59.8, 87.0 and 4.5%
respectively).

We used the sky positions and proper motions with their respective errors from
NSC DR2 for the primaries and secondaries. The parallax and associated error
of the primaries are from Gaia EDR3. The parallax and corresponding error of
the secondaries were inferred from their mean photometric distance, based on
the spectral type estimates from AstroToolBox. As seen previously, a
difference of two sub-types corresponds to a distance discrepancy of $\sim
40\%$. To determine how much the comoving probabilities change with a
difference of two sub-types, we increased the photometric distance of the
secondaries by 40% and re-ran the CoMover code. We found that most systems,
which already had a high comoving probability, still have a high one after
increasing the distance (see Table 3 columns 3 vs. 4).

###  4.5 Literature Information

We searched the literature for any derived physical properties for the
primaries and secondaries of the newly discovered systems. All of these
properties are from either Stassun et al. (2019) or Gentile Fusillo et al.
(2021) and are given in Table 4 along with all other literature references.
Fundamental parameters were not available for any of the secondaries in our
new systems. However, two of them find mention in Skrzypek et al. (2016),
which does not contain physical properties. Some of our primaries are
referenced by one or more of the following literary sources: Reylé (2018),
Pokorny et al. (2003), Luyten (1995), Eggen (1976a), Eggen (1976b), Salim &
Gould (2003), Wroblewski & Torres (1996), Kirkpatrick et al. (2016). None of
these works include fundamental parameters.

###  4.6 Astrometry

We calculated distances and tangential velocities for all our systems using
the Gaia EDR3 astrometry of the primaries (Table 1). Position angles, angular
and physical separations were calculated by correcting the position of the
primary for proper motion to the epoch of the secondary. NSC DR2 positions and
mean observation epochs were used for this purpose. All separations were
calculated using the general case equation
$\theta=\cos^{-1}\left[\sin\delta_{A}\sin\delta_{B}+\cos\delta_{A}\cos\delta_{B}\cos(\alpha_{A}-\alpha_{B})\right]$
to account for systems having larger RA coordinate separations at high
declination. In Table 2, we computed the difference in proper motion between
the primaries and secondaries, taking into account the errors in
$\mu_{\alpha}$ and $\mu_{\delta}$. We also found that there is good agreement
between the Gaia and NSC proper motions of the primaries (see Gaia proper
motions in Table 1 versus NSC proper motions in Table 2). Note that none of
our secondaries has proper motions in Gaia.

###  4.7 Mass Ratios and Binding Energies

To compute total masses, mass ratios and binding energies for each systems
(Table 5), we estimated component masses using a combination of literature
references and relations described below. Table 4 lists masses for the primary
stars. For mass estimates of the secondaries we used either the Mamajek (2021)
relation for sources with absolute G magnitude $<$ 17, or we extrapolated from
the spectral type to dynamical mass values computed in Dupuy & Liu (2017). In
Figure 5, we overplotted our systems with the collection of very low-mass
systems compiled in Faherty et al. (2020) as well as the collection of
binaries from Faherty et al. (2021). We have omitted any system with a
comoving probability $<$ 98% (#9, #13 and #15). The majority of our sources
lie near the locus of field comoving sources as they have estimated total
masses $>$ 0.2 M⊙. Three systems (#2, #11 and #14) have estimated total masses
$<$ 0.2 M⊙ as they contain low-mass secondaries (T5, L8, L4 respectively) with
low-mass host stars ($\sim M7$). These three systems are at the low end of the
binding energy distribution for field companion systems but still well
contained within the locus of known sources.

###  4.8 Age and Mass Estimates for the White Dwarfs

We performed age, initial and final mass estimates for the three white dwarf
primaries (systems #25, #27 and #33) included in our sample. We used
wdwarfdate222https://github.com/rkiman/wdwarfdate (Kiman et al. in prep.),
which is an open source code that estimates ages of white dwarfs in a Bayesian
framework. It runs a chain of models to estimate the ages and their
uncertainties from an effective temperature and a surface gravity. The code
determines the age of the progenitor star, the cooling age of the white dwarf,
and the total age. The age of the ultra-cool companion can be inferred
directly from the total age of the white dwarf, provided that both formed at
the same time. wdwarfdate also estimates the initial mass (that of the
progenitor star) and the final mass (that of the white dwarf). The code uses
the cooling tracks from (Bédard et al., 2020) to estimate the parameters of
the white dwarfs, and MIST stellar evolutionary tracks computed with the
Modules for Experiments in Stellar Astrophysics (MESA) (Paxton et al., 2011,
2013, 2015; Dotter, 2016; Choi et al., 2016). See also Lu et al. (2021) who
used the code to estimate the age of main sequence stars comoving with a white
dwarf, to compare with the results of their age-dating method.

Since our three white dwarfs are in Gentile Fusillo et al. (2021), we had the
required parameters to run the code using Cummings et al. (2018) initial-to-
final mass relation. As we don’t know the composition of our white dwarfs (we
are only working from the photometry), we ran the code using the derived Teff
and log g for DA and DB white dwarfs, provided by Gentile Fusillo. The results
are presented in Table 6. The final mass estimates are more or less consistent
with those from Gentile Fusillo. Since the white dwarf of system #25 has a
very low-mass (0.256$\pm$0.159 M⊙), which is outside the range of the initial-
to-final mass relation described in Cummings et al. (2018), wdwarfdate cannot
estimate the main sequence age and mass of the progenitor star. However, the
code can estimate the mass and cooling age of the white dwarf using Bédard et
al. (2020) cooling tracks.

###  4.9 Finder Charts

Figure 6 compares color composites from unWISE NEO7 with DESI Legacy Imaging
Surveys (LS) DR9. The purpose of these images is to show the difference
between low-resolution surveys such as WISE (FWHM $\sim 6\arcsec$ for the
short channels, Wright et al. 2010) compared to high-resolution surveys such
as DES (FWHM $\sim 1\arcsec$, Abbott et al. 2018) or VISTA VHS (FWHM $\sim
0.9\arcsec$, Sutherland et al. 2015) when it comes to identifying binary
systems that are less widely separated, in which case WISE would only show one
blended source rather than the resolved pair.

Figure 2: Distributions of parallactic distance, angular separation, projected
physical separation, total proper motion and $\upsilon_{tan}$ from Tables 1
and 2. Figure 3: Top left panel: Gaia CMD of the primaries. Top right panel:
Pan-STARRS CMD; Bottom left panel: NSC CMD; Bottom right panel: VHS CMD. Five-
pointed star symbols: the blue stars represent the white dwarf (WD) primaries,
the red stars correspond to the main sequence (MS) primaries, and the black
stars refer to the secondaries. We used the parallax of the primaries to
calculate the absolute magnitude of the secondaries.

Figure 4: Top left panel: Optical spectrum of NSC J015340.10-001550.34 A
(primary of system #8) compared to three M dwarf standards from Bochanski et
al. (2007). The spectrum of our primary (smoothed for a better comparison)
fits best with the M1 standard. Bottom left panel: Unsmoothed version of the
same spectrum with the M1 standard overplotted. Top right panel: Near-infrared
spectrum of NSC J045724.25-230012.74 B (secondary of system #21) compared to
three T dwarf standards from Burgasser et al. (2004). The spectrum of our
secondary (smoothed for a better comparison) fits best with the T3 standard.
Bottom right panel: Unsmoothed version of the same spectrum with the T3
standard overplotted.

Figure 5: Mass ratio (secondary/primary) versus projected separation for
literature sources taken from Faherty et al. 2020 and Faherty et al. 2021
(various color coded filled circles) and companions from this paper (black
five-pointed stars). We have color coded the exoplanet detections (as defined
by the Exoplanet Archive) by the detection method of the source. Figure 6:
unWISE NEO7 versus LS DR9 images (north up, east to the left). We used VISTA
VHS DR6 images for systems #27 and #28 since there is no corresponding LS DR9
imagery. The primaries are in the center of the images, the secondaries were
marked by a white dash. White lettering indicates the system number and name
followed by the size of the field of view ($50\arcsec\times
50\arcsec,80\arcsec\times 80\arcsec$ or $120\arcsec\times 120\arcsec$,
depending on the angular separation of the system components).

Figure 6 (Continued)

=1.5cm

Table 1: Discovered systems

Sys. | System name | Short name | $\varpi$ | $\mu_{\alpha}$ | $\mu_{\delta}$ | Dist.a |  $\upsilon_{tan}$b | Sep.c | Sep.d | Pos.e | Sys.f | Ref.g
---|---|---|---|---|---|---|---|---|---|---|---|---
# |  |  | (mas) | (mas yr-1) | (mas yr-1) | (pc) | (km $s^{-1}$) | (″) | (AU) | (deg) | type |
| Newly discovered systems |  |  |  |  |  |  |  |  |  |  |  |  |  |  |  |
1 | NSC J000456.31+045117.22 AB | NSC J0004+0451 | 9.2747$\pm$ | 0.1585 | 100.538$\pm$ | 0.206 | 10.524$\pm$ | 0.146 | 107.821$\pm$ | 1.843 | 51.663$\pm$ | 0.889 | 14.548 | 1568.531 | 15.4 | M6+L2 |  $\cdots$
2 | NSC J004058.68-294212.37 AB | NSC J0040-2942 | 18.1726$\pm$ | 0.1292 | 84.313$\pm$ | 0.128 | -124.955$\pm$ | 0.143 | 55.028$\pm$ | 0.391 | 39.318$\pm$ | 0.282 | 19.906 | 1095.379 | 181.2 | M7+T5 |  $\cdots$
3 | NSC J004239.82-250714.01 AB | NSC J0042-2507 | 3.8355$\pm$ | 0.8464 | 109.022$\pm$ | 0.936 | -17.709$\pm$ | 0.846 | 260.725$\pm$ | 57.535 | 136.499$\pm$ | 30.144 | 3.000 | 782.216 | 237.1 | M6+M6 |  $\cdots$
4 | NSC J004509.91-285557.20 AB | NSC J0045-2855 | 6.8596$\pm$ | 0.0544 | 93.307$\pm$ | 0.055 | -24.9$\pm$ | 0.061 | 145.78$\pm$ | 1.156 | 66.732$\pm$ | 0.531 | 5.447 | 794.110 | 286.4 | M4+M9 |  $\cdots$
5 | NSC J010717.67-265848.32 AB | NSC J0107-2658 | 11.5915$\pm$ | 0.0202 | 115.191$\pm$ | 0.021 | -119.037$\pm$ | 0.027 | 86.27$\pm$ | 0.15 | 67.736$\pm$ | 0.118 | 5.846 | 504.352 | 333.8 | M1+M8 |  $\cdots$
6 | NSC J012629.63-262023.18 AB | NSC J0126-2620 | 6.8549$\pm$ | 0.0307 | 101.256$\pm$ | 0.04 | -51.201$\pm$ | 0.027 | 145.882$\pm$ | 0.653 | 78.459$\pm$ | 0.352 | 7.921 | 1155.583 | 215.7 | M3+M8 |  $\cdots$
7 | NSC J014827.71-035716.63 AB | NSC J0148-0357 | 8.4201$\pm$ | 0.0628 | 52.933$\pm$ | 0.081 | -175.686$\pm$ | 0.042 | 118.764$\pm$ | 0.886 | 103.292$\pm$ | 0.771 | 11.752 | 1395.736 | 131.3 | M4+L4 |  $\cdots$
8 | NSC J015340.10-001550.34 AB | NSC J0153-0015 | 5.4188$\pm$ | 0.0236 | 83.398$\pm$ | 0.029 | -105.841$\pm$ | 0.02 | 184.544$\pm$ | 0.804 | 117.871$\pm$ | 0.514 | 4.206 | 776.150 | 359.0 | M1+M8 |  $\cdots$
9 | NSC J020029.71-125451.00 AB | NSC J0200-1254 | 4.3019$\pm$ | 0.0211 | 146.841$\pm$ | 0.021 | -84.873$\pm$ | 0.018 | 232.455$\pm$ | 1.14 | 186.876$\pm$ | 0.917 | 36.509 | 8486.735 | 260.8 | K7+L9 |  $\cdots$
10 | NSC J020048.45-470755.84 AB | NSC J0200-4707 | 13.2326$\pm$ | 0.0145 | 107.904$\pm$ | 0.013 | -4.801$\pm$ | 0.014 | 75.571$\pm$ | 0.083 | 38.69$\pm$ | 0.043 | 22.380 | 1691.254 | 213.5 | M2+L4 |  $\cdots$
11 | NSC J020541.24+020249.66 AB | NSC J0205+0202 | 8.7286$\pm$ | 0.736 | -81.262$\pm$ | 0.898 | -73.003$\pm$ | 0.67 | 114.566$\pm$ | 9.66 | 59.321$\pm$ | 5.021 | 5.561 | 637.127 | 95.9 | M7+L8 |  $\cdots$
12 | NSC J022132.42-633807.41 AB | NSC J0221-6338 | 6.4144$\pm$ | 0.1885 | 101.832$\pm$ | 0.25 | 43.48$\pm$ | 0.237 | 155.9$\pm$ | 4.581 | 81.823$\pm$ | 2.411 | 37.757 | 5886.303 | 140.4 | M6+L1 |  $\cdots$
13 | NSC J022821.48-532004.36 AB | NSC J0228-5320 | 10.8681$\pm$ | 0.0441 | 127.645$\pm$ | 0.045 | 27.171$\pm$ | 0.049 | 92.012$\pm$ | 0.373 | 56.918$\pm$ | 0.232 | 5.962 | 548.533 | 185.2 | M3+M8 |  $\cdots$
14 | NSC J023113.30-031147.09 AB | NSC J0231-0311 | 12.3836$\pm$ | 0.2079 | 24.676$\pm$ | 0.236 | -128.072$\pm$ | 0.195 | 80.752$\pm$ | 1.356 | 49.923$\pm$ | 0.841 | 5.246 | 423.614 | 341.3 | M7+L4 |  $\cdots$
15 | NSC J024433.27-051711.10 AB | NSC J0244-0517 | 3.8755$\pm$ | 0.0509 | 27.951$\pm$ | 0.051 | -104.003$\pm$ | 0.049 | 258.033$\pm$ | 3.389 | 131.717$\pm$ | 1.731 | 3.905 | 1007.524 | 265.6 | M1+L0 |  $\cdots$
16 | NSC J024507.25-123726.57 AB | NSC J0245-1237 | 6.0612$\pm$ | 0.0295 | 34.715$\pm$ | 0.033 | -141.047$\pm$ | 0.034 | 164.983$\pm$ | 0.803 | 113.593$\pm$ | 0.554 | 5.808 | 958.154 | 234.1 | M2+M7 |  $\cdots$
17 | NSC J025450.03-085252.25 AB | NSC J0254-0852 | 8.2213$\pm$ | 0.0638 | 115.448$\pm$ | 0.078 | -48.647$\pm$ | 0.064 | 121.635$\pm$ | 0.944 | 72.23$\pm$ | 0.562 | 6.095 | 741.364 | 14.9 | M3+L0 |  $\cdots$
18 | NSC J041239.68-262105.02 AB | NSC J0412-2621 | 6.3603$\pm$ | 0.24 | -10.497$\pm$ | 0.189 | -164.793$\pm$ | 0.27 | 157.225$\pm$ | 5.933 | 123.06$\pm$ | 4.648 | 2.617 | 411.436 | 36.3 | M6+M8 |  $\cdots$
19 | NSC J041641.96-215248.86 AB | NSC J0416-2152 | 7.4598$\pm$ | 0.0326 | 117.348$\pm$ | 0.027 | -219.012$\pm$ | 0.032 | 134.052$\pm$ | 0.586 | 157.878$\pm$ | 0.69 | 8.411 | 1127.526 | 306.3 | M3+M9 |  $\cdots$
20 | NSC J043503.99-355911.42 AB | NSC J0435-3559 | 9.3695$\pm$ | 0.0287 | -8.94$\pm$ | 0.027 | -96.481$\pm$ | 0.034 | 106.729$\pm$ | 0.327 | 49.018$\pm$ | 0.151 | 23.948 | 2555.901 | 299.7 | M4+L5 |  $\cdots$
21 | NSC J045724.25-230012.74 AB | NSC J0457-2300 | 18.187$\pm$ | 0.0217 | -128.657$\pm$ | 0.015 | 7.236$\pm$ | 0.02 | 54.984$\pm$ | 0.066 | 33.584$\pm$ | 0.04 | 16.970 | 933.096 | 317.3 | M4+T3 |  $\cdots$
22 | NSC J050456.74-482240.01 AB | NSC J0504-4822 | 12.574$\pm$ | 0.0199 | -3.188$\pm$ | 0.023 | 132.932$\pm$ | 0.029 | 79.529$\pm$ | 0.126 | 50.126$\pm$ | 0.08 | 7.175 | 570.648 | 248.1 | M3+L0 |  $\cdots$
23 | NSC J050506.28-475035.19 AB | NSC J0505-4750 | 6.3997$\pm$ | 0.1196 | 70.225$\pm$ | 0.131 | 88.813$\pm$ | 0.184 | 156.256$\pm$ | 2.92 | 83.858$\pm$ | 1.572 | 7.787 | 1216.806 | 208.4 | M6+M9 |  $\cdots$
24 | NSC J052307.20-565522.36 AB | NSC J0523-5655 | 18.3926$\pm$ | 0.0234 | -28.942$\pm$ | 0.029 | 156.764$\pm$ | 0.029 | 54.37$\pm$ | 0.069 | 41.083$\pm$ | 0.053 | 12.995 | 706.547 | 333.2 | M5+T0 |  $\cdots$
25 | NSC J053232.31-512450.75 AB | NSC J0532-5124 | 5.9143$\pm$ | 0.3818 | 102.804$\pm$ | 0.432 | 138.888$\pm$ | 0.479 | 169.081$\pm$ | 10.915 | 138.487$\pm$ | 8.948 | 3.003 | 507.731 | 80.4 | WD+L3 |  $\cdots$
26 | NSC J123900.73-005433.72 AB | NSC J1239-0054 | 23.3826$\pm$ | 0.0281 | -103.965$\pm$ | 0.036 | -47.8$\pm$ | 0.032 | 42.767$\pm$ | 0.051 | 23.196$\pm$ | 0.029 | 8.817 | 377.062 | 39.8 | M4+L4 |  $\cdots$
27 | NSC J130527.23-224728.44 AB | NSC J1305-2247 | 6.9608$\pm$ | 0.7951 | -140.208$\pm$ | 1.111 | 2.719$\pm$ | 0.754 | 143.661$\pm$ | 16.41 | 95.493$\pm$ | 10.934 | 4.983 | 715.907 | 358.1 | WD+L3 |  $\cdots$
28 | NSC J132017.47-401258.27 AB | NSC J1320-4012 | 14.9605$\pm$ | 0.0182 | -17.48$\pm$ | 0.016 | -117.831$\pm$ | 0.016 | 66.843$\pm$ | 0.081 | 37.742$\pm$ | 0.046 | 55.312 | 3697.213 | 300.0 | M1+L1 |  $\cdots$
29 | NSC J202349.63-484435.01 AB | NSC J2023-4844 | 10.4053$\pm$ | 0.0331 | 13.143$\pm$ | 0.032 | -132.182$\pm$ | 0.028 | 96.105$\pm$ | 0.306 | 60.511$\pm$ | 0.193 | 11.382 | 1093.871 | 225.4 | M4+L0 |  $\cdots$
30 | NSC J220852.71-551054.25 AB | NSC J2208-5510 | 10.4478$\pm$ | 0.0612 | -136.283$\pm$ | 0.061 | 5$\pm$ | 0.055 | 95.714$\pm$ | 0.561 | 61.871$\pm$ | 0.363 | 4.498 | 430.541 | 113.1 | M5+M9 |  $\cdots$
31 | NSC J224101.90-450026.44 AB | NSC J2241-4500 | 17.1738$\pm$ | 0.6061 | 273.035$\pm$ | 0.404 | -154.157$\pm$ | 0.509 | 58.228$\pm$ | 2.055 | 86.54$\pm$ | 3.057 | 7.183 | 418.277 | 144.5 | M5+L2 |  $\cdots$
32 | NSC J232703.65-524727.94 AB | NSC J2327-5247 | 8.6324$\pm$ | 0.0161 | 108.844$\pm$ | 0.013 | -32.352$\pm$ | 0.016 | 115.842$\pm$ | 0.216 | 62.349$\pm$ | 0.117 | 56.005 | 6487.802 | 243.5 | M1+L1 |  $\cdots$
33 | NSC J233302.51-634721.39 AB | NSC J2333-6347 | 8.8339$\pm$ | 0.4268 | 48.71$\pm$ | 0.376 | -162.431$\pm$ | 0.422 | 113.2$\pm$ | 5.469 | 90.99$\pm$ | 4.402 | 2.851 | 322.740 | 26.5 | WD+M9 |  $\cdots$
34 | NSC J234443.91+003112.41 AB | NSC J2344+0031 | 8.1622$\pm$ | 0.175 | -92.89$\pm$ | 0.188 | -103.067$\pm$ | 0.127 | 122.516$\pm$ | 2.627 | 80.575$\pm$ | 1.73 | 8.414 | 1030.796 | 270.9 | M6+L2 |  $\cdots$
| Rediscovered systems |  |  |  |  |  |  |  |  |  |  |  |  |  |  |  |
$\cdots$ | NSC J002111.11-424540.39 AB | NSC J0021-4245 | 37.3319$\pm$ | 0.0378 | 255.184$\pm$ | 0.031 | -12.475$\pm$ | 0.039 | 26.787$\pm$ | 0.027 | 32.439$\pm$ | 0.033 | 77.840 | 2085.087 | 316.9 | M6+L0 | 1
$\cdots$ | NSC J003011.68-374049.20 AB | NSC J0030-3740 | 21.0552$\pm$ | 0.0576 | -86.91$\pm$ | 0.042 | -65.42$\pm$ | 0.059 | 47.494$\pm$ | 0.13 | 24.489$\pm$ | 0.068 | 89.057 | 4229.675 | 312.3 | WD+M9 | 1
$\cdots$ | NSC J003320.53-422726.41 AB | NSC J0033-4227 | 16.4251$\pm$ | 0.0183 | 320.573$\pm$ | 0.015 | -46.16$\pm$ | 0.014 | 60.883$\pm$ | 0.068 | 93.466$\pm$ | 0.104 | 29.065 | 1769.531 | 125.2 | M3+L0 | 1
$\cdots$ | NSC J013609.18-255613.81 AB | NSC J0136-2556 | 13.7237$\pm$ | 0.1623 | 203.037$\pm$ | 0.184 | 17.952$\pm$ | 0.095 | 72.867$\pm$ | 0.862 | 70.4$\pm$ | 0.835 | 7.074 | 515.438 | 34.5 | WD+L0 | 1
$\cdots$ | NSC J014953.56-612919.67 AB | NSC J0149-6129 | 13.0666$\pm$ | 0.0544 | 3.697$\pm$ | 0.06 | -161.535$\pm$ | 0.063 | 76.531$\pm$ | 0.319 | 58.613$\pm$ | 0.245 | 12.321 | 942.972 | 338.5 | WD+L0 | 1
$\cdots$ | NSC J020640.61-222439.29 AB | NSC J0206-2224 | 7.525$\pm$ | 0.0578 | 88.629$\pm$ | 0.049 | -61.198$\pm$ | 0.045 | 132.89$\pm$ | 1.021 | 67.843$\pm$ | 0.522 | 9.978 | 1325.982 | 336.8 | M3+M7 | 1
$\cdots$ | NSC J023508.17-041443.11 AB | NSC J0235-0414 | 17.7429$\pm$ | 0.0284 | 114.207$\pm$ | 0.032 | -22.807$\pm$ | 0.029 | 56.36$\pm$ | 0.09 | 31.113$\pm$ | 0.051 | 11.587 | 653.049 | 340.0 | M4+M9 | 1
$\cdots$ | NSC J044142.59-304256.75 AB | NSC J0441-3042 | 14.7129$\pm$ | 0.0408 | 63.624$\pm$ | 0.038 | 83.713$\pm$ | 0.045 | 67.968$\pm$ | 0.188 | 33.875$\pm$ | 0.095 | 17.664 | 1200.582 | 53.6 | M5+M9 | 1
$\cdots$ | NSC J124428.51-011900.40 AB | NSC J1244-0119 | 12.0087$\pm$ | 0.0502 | -57.115$\pm$ | 0.066 | -171.286$\pm$ | 0.047 | 83.273$\pm$ | 0.348 | 71.269$\pm$ | 0.299 | 3.080 | 256.494 | 252.4 | WD+M9 | 1
$\cdots$ | NSC J203439.06-541247.73 AB | NSC J2034-5412 | 9.3785$\pm$ | 0.0857 | 3.973$\pm$ | 0.078 | -105.771$\pm$ | 0.083 | 106.626$\pm$ | 0.974 | 53.495$\pm$ | 0.491 | 30.371 | 3238.356 | 212.2 | M5+M9 | 1
$\cdots$ | NSC J211810.50-472110.21 AB | NSC J2118-4721 | 15.117$\pm$ | 0.0219 | 153.639$\pm$ | 0.02 | -216.018$\pm$ | 0.016 | 66.151$\pm$ | 0.096 | 83.118$\pm$ | 0.121 | 3.333 | 220.509 | 176.7 | M3+M9 | 1
$\cdots$ | NSC J232028.36-495545.70 AB | NSC J2320-4955 | 13.1006$\pm$ | 0.1154 | 75.9$\pm$ | 0.081 | -75.051$\pm$ | 0.09 | 76.332$\pm$ | 0.672 | 38.62$\pm$ | 0.342 | 7.363 | 562.070 | 2.7 | M7+M8 | 1
$\cdots$ | NSC J232252.60-615112.77 AB | NSC J2322-6151 | 23.5626$\pm$ | 0.0296 | 78.122$\pm$ | 0.028 | -78.252$\pm$ | 0.033 | 42.44$\pm$ | 0.053 | 22.244$\pm$ | 0.029 | 16.589 | 704.027 | 165.6 | M5+L2 | 2,3

Note— The parallaxes and proper motions are from Gaia EDR3. The primary of
system #8 and the secondary of system #21 have confirmed spectral types of M0
and T3, respectively (see spectra in Figure 4). (a)Distance, derived from the
Gaia EDR3 parallax of the primary; (b)Tangential velocity, calculated using
the Gaia EDR3 astrometry of the primary; (c)Angular separation; (d)Projected
physical separation, calculated using the Gaia EDR3 parallax of the primary;
(e)Position angle (east of north) of the secondary with respect to the
primary; (f)System type, based on spectral type estimates (A+B); (g)Binary
system references: (1) Hartman & Lépine (2020), (2) Smart et al. (2019), (3)
Calissendorff et al. (2019) (c,e)Calculated using NSC DR2 positions,
translating the position of the primary to the epoch of the secondary.

=1cm

Table 2: NSC DR2 astrometry

Sys. | C.a | $\alpha$ | $\delta$ | Epoch | $\mu_{\alpha}$ | $\mu_{\delta}$ | $\mu_{tot}$ |  $\Delta\mu_{\alpha}$b |  $\Delta\mu_{\delta}$c |  $\Delta\mu_{tot}$d
---|---|---|---|---|---|---|---|---|---|---
# |  | (deg) | (deg) |  | (mas yr-1) | (mas yr-1) | (mas yr-1) | (mas yr-1) | (mas yr-1) | (mas yr-1)
1 | A | 1.2346196$\pm$ | 0$\farcs$002078 | 4.8547833$\pm$ | 0$\farcs$002548 | 2017-02-17 | 101.586$\pm$ | 2.081 | 16.224$\pm$ | 2.243 | 102.873$\pm$ | 2.085 |  |  |  |  |  |
| B | 1.2356978$\pm$ | 0$\farcs$008701 | 4.8586783$\pm$ | 0$\farcs$008999 | 2017-01-31 | 103.442$\pm$ | 10.176 | 8.665$\pm$ | 10.271 | 103.804$\pm$ | 10.177 | 1.856$\pm$ | 10.387 | 7.559$\pm$ | 10.513 | 7.784$\pm$ | 10.506
2 | A | 10.2445114$\pm$ | 0$\farcs$002146 | -29.703435$\pm$ | 0$\farcs$002093 | 2016-09-23 | 85.588$\pm$ | 1.684 | -127.509$\pm$ | 1.637 | 153.57$\pm$ | 1.652 |  |  |  |  |  |
| B | 10.2443636$\pm$ | 0$\farcs$015625 | -29.7089511$\pm$ | 0$\farcs$015601 | 2016-05-22 | 76.615$\pm$ | 11.596 | -137.72$\pm$ | 11.576 | 157.596$\pm$ | 11.581 | 8.973$\pm$ | 11.718 | 10.211$\pm$ | 11.691 | 13.593$\pm$ | 11.703
3 | A | 10.6659165$\pm$ | 0$\farcs$002078 | -25.1205574$\pm$ | 0$\farcs$002254 | 2017-06-23 | 110.017$\pm$ | 1.081 | -18.631$\pm$ | 1.168 | 111.583$\pm$ | 1.084 |  |  |  |  |  |
| B | 10.6651479$\pm$ | 0$\farcs$002717 | -25.1210108$\pm$ | 0$\farcs$002906 | 2017-08-07 | 114.399$\pm$ | 1.451 | -16.276$\pm$ | 1.542 | 115.551$\pm$ | 1.453 | 4.382$\pm$ | 1.809 | 2.355$\pm$ | 1.934 | 4.975$\pm$ | 1.838
4 | A | 11.2912826$\pm$ | 0$\farcs$002091 | -28.9325546$\pm$ | 0$\farcs$002165 | 2016-10-10 | 91.114$\pm$ | 1.456 | -24.391$\pm$ | 1.525 | 94.322$\pm$ | 1.461 |  |  |  |  |  |
| B | 11.2896207$\pm$ | 0$\farcs$002027 | -28.9321265$\pm$ | 0$\farcs$002127 | 2016-08-29 | 98.791$\pm$ | 1.421 | -25.35$\pm$ | 1.474 | 101.992$\pm$ | 1.424 | 7.677$\pm$ | 2.034 | 0.959$\pm$ | 2.121 | 7.737$\pm$ | 2.036
5 | A | 16.8236365$\pm$ | 0$\farcs$010278 | -26.9800885$\pm$ | 0$\farcs$008563 | 2017-02-24 | 120.909$\pm$ | 13.555 | -114.787$\pm$ | 11.718 | 166.718$\pm$ | 12.717 |  |  |  |  |  |
| B | 16.822841$\pm$ | 0$\farcs$003846 | -26.978638$\pm$ | 0$\farcs$003594 | 2017-05-15 | 123.797$\pm$ | 3.129 | -132.236$\pm$ | 2.945 | 181.141$\pm$ | 3.032 | 2.888$\pm$ | 13.911 | 17.449$\pm$ | 12.082 | 17.686$\pm$ | 12.135
6 | A | 21.6234552$\pm$ | 0$\farcs$003409 | -26.3397711$\pm$ | 0$\farcs$003143 | 2015-08-16 | 94.787$\pm$ | 4.24 | -53.296$\pm$ | 3.25 | 108.743$\pm$ | 4.024 |  |  |  |  |  |
| B | 21.6220425$\pm$ | 0$\farcs$004235 | -26.341568$\pm$ | 0$\farcs$00456 | 2016-04-26 | 104.433$\pm$ | 2.991 | -39.322$\pm$ | 3.367 | 111.591$\pm$ | 3.04 | 9.646$\pm$ | 5.189 | 13.974$\pm$ | 4.68 | 16.98$\pm$ | 4.85
7 | A | 27.1154771$\pm$ | 0$\farcs$002914 | -3.9546199$\pm$ | 0$\farcs$002943 | 2016-02-23 | 49.302$\pm$ | 1.912 | -171.409$\pm$ | 2.122 | 178.358$\pm$ | 2.107 |  |  |  |  |  |
| B | 27.1179324$\pm$ | 0$\farcs$023287 | -3.9567589$\pm$ | 0$\farcs$023424 | 2015-11-05 | 68.828$\pm$ | 16.381 | -168.594$\pm$ | 16.504 | 182.102$\pm$ | 16.486 | 19.526$\pm$ | 16.492 | 2.815$\pm$ | 16.64 | 19.728$\pm$ | 16.495
8 | A | 28.4171021$\pm$ | 0$\farcs$004829 | -0.2639823$\pm$ | 0$\farcs$006201 | 2015-02-22 | 85.484$\pm$ | 2.781 | -109.777$\pm$ | 4.129 | 139.135$\pm$ | 3.679 |  |  |  |  |  |
| B | 28.4171034$\pm$ | 0$\farcs$004138 | -0.2628419$\pm$ | 0$\farcs$004276 | 2016-01-19 | 85.823$\pm$ | 2.704 | -110.007$\pm$ | 2.7 | 139.525$\pm$ | 2.702 | 0.339$\pm$ | 3.879 | 0.23$\pm$ | 4.933 | 0.41$\pm$ | 4.24
9 | A | 30.1238025$\pm$ | 0$\farcs$004582 | -12.9141655$\pm$ | 0$\farcs$004964 | 2015-10-30 | 146.547$\pm$ | 4.654 | -85.844$\pm$ | 4.933 | 169.839$\pm$ | 4.727 |  |  |  |  |  |
| B | 30.1135648$\pm$ | 0$\farcs$017378 | -12.9158077$\pm$ | 0$\farcs$017444 | 2016-08-11 | 163.476$\pm$ | 11.532 | -85.838$\pm$ | 11.596 | 184.642$\pm$ | 11.546 | 16.929$\pm$ | 12.436 | 0.006$\pm$ | 12.602 | 16.929$\pm$ | 12.436
10 | A | 30.2018838$\pm$ | 0$\farcs$006962 | -47.1321787$\pm$ | 0$\farcs$005139 | 2015-03-28 | 108.767$\pm$ | 3.213 | -5.923$\pm$ | 2.803 | 108.928$\pm$ | 3.212 |  |  |  |  |  |
| B | 30.1968786$\pm$ | 0$\farcs$012833 | -47.1373651$\pm$ | 0$\farcs$01282 | 2016-01-17 | 109.414$\pm$ | 7.503 | -7.568$\pm$ | 7.513 | 109.675$\pm$ | 7.503 | 0.647$\pm$ | 8.162 | 1.645$\pm$ | 8.019 | 1.768$\pm$ | 8.038
11 | A | 31.421821$\pm$ | 0$\farcs$003174 | 2.0471276$\pm$ | 0$\farcs$003597 | 2016-02-05 | -79.908$\pm$ | 1.652 | -72.908$\pm$ | 1.83 | 108.171$\pm$ | 1.735 |  |  |  |  |  |
| B | 31.4233605$\pm$ | 0$\farcs$048468 | 2.0469716$\pm$ | 0$\farcs$048787 | 2016-01-06 | -79.81$\pm$ | 27.969 | -79.694$\pm$ | 28.054 | 112.786$\pm$ | 28.011 | 0.098$\pm$ | 28.018 | 6.786$\pm$ | 28.114 | 6.787$\pm$ | 28.114
12 | A | 35.3850943$\pm$ | 0$\farcs$002373 | -63.635391$\pm$ | 0$\farcs$002409 | 2016-05-01 | 99.186$\pm$ | 1.589 | 40.524$\pm$ | 1.59 | 107.145$\pm$ | 1.589 |  |  |  |  |  |
| B | 35.4001583$\pm$ | 0$\farcs$011979 | -63.6434698$\pm$ | 0$\farcs$012019 | 2016-05-15 | 94.643$\pm$ | 7.404 | 57.983$\pm$ | 7.437 | 110.992$\pm$ | 7.413 | 4.543$\pm$ | 7.573 | 17.459$\pm$ | 7.605 | 18.04$\pm$ | 7.603
13 | A | 37.0895103$\pm$ | 0$\farcs$005066 | -53.3345431$\pm$ | 0$\farcs$004095 | 2015-08-01 | 128.523$\pm$ | 2.28 | 25.6$\pm$ | 2.016 | 131.048$\pm$ | 2.27 |  |  |  |  |  |
| B | 37.0892954$\pm$ | 0$\farcs$003524 | -53.3361878$\pm$ | 0$\farcs$003471 | 2016-03-18 | 135.364$\pm$ | 1.736 | 44.364$\pm$ | 1.681 | 142.449$\pm$ | 1.731 | 6.841$\pm$ | 2.866 | 18.764$\pm$ | 2.625 | 19.972$\pm$ | 2.654
14 | A | 37.8054288$\pm$ | 0$\farcs$00155 | -3.1964142$\pm$ | 0$\farcs$00168 | 2014-10-19 | 27.345$\pm$ | 0.764 | -126.129$\pm$ | 0.875 | 129.059$\pm$ | 0.87 |  |  |  |  |  |
| B | 37.8049613$\pm$ | 0$\farcs$019263 | -3.195033$\pm$ | 0$\farcs$019493 | 2014-10-12 | 23.43$\pm$ | 8.058 | -122.34$\pm$ | 8.252 | 124.563$\pm$ | 8.245 | 3.915$\pm$ | 8.094 | 3.789$\pm$ | 8.298 | 5.448$\pm$ | 8.193
15 | A | 41.1386057$\pm$ | 0$\farcs$002152 | -5.2864157$\pm$ | 0$\farcs$002432 | 2015-12-06 | 28.081$\pm$ | 1.252 | -103.368$\pm$ | 1.425 | 107.114$\pm$ | 1.414 |  |  |  |  |  |
| B | 41.1375166$\pm$ | 0$\farcs$009645 | -5.2864883$\pm$ | 0$\farcs$009866 | 2015-07-16 | 33.115$\pm$ | 5.409 | -95.38$\pm$ | 5.519 | 100.965$\pm$ | 5.507 | 5.034$\pm$ | 5.552 | 7.988$\pm$ | 5.7 | 9.442$\pm$ | 5.658
16 | A | 41.2802081$\pm$ | 0$\farcs$003752 | -12.624046$\pm$ | 0$\farcs$003647 | 2015-11-18 | 31.967$\pm$ | 3.213 | -142.653$\pm$ | 3.03 | 146.191$\pm$ | 3.039 |  |  |  |  |  |
| B | 41.2788699$\pm$ | 0$\farcs$003593 | -12.6249969$\pm$ | 0$\farcs$003506 | 2016-01-07 | 35.216$\pm$ | 2.566 | -139.192$\pm$ | 2.569 | 143.578$\pm$ | 2.569 | 3.249$\pm$ | 4.112 | 3.461$\pm$ | 3.972 | 4.747$\pm$ | 4.038
17 | A | 43.7084538$\pm$ | 0$\farcs$002476 | -8.8811802$\pm$ | 0$\farcs$002285 | 2016-04-25 | 117.81$\pm$ | 1.636 | -47.432$\pm$ | 1.418 | 127$\pm$ | 1.607 |  |  |  |  |  |
| B | 43.7088891$\pm$ | 0$\farcs$005807 | -8.8795421$\pm$ | 0$\farcs$005976 | 2016-03-04 | 122.706$\pm$ | 4.318 | -50.082$\pm$ | 4.482 | 132.533$\pm$ | 4.342 | 4.896$\pm$ | 4.618 | 2.65$\pm$ | 4.701 | 5.567$\pm$ | 4.637
18 | A | 63.1653339$\pm$ | 0$\farcs$00273 | -26.3513948$\pm$ | 0$\farcs$002554 | 2016-02-12 | -11.367$\pm$ | 1.854 | -171.564$\pm$ | 1.774 | 171.94$\pm$ | 1.774 |  |  |  |  |  |
| B | 63.1658141$\pm$ | 0$\farcs$006391 | -26.3508035$\pm$ | 0$\farcs$006278 | 2016-01-03 | -21.539$\pm$ | 4.404 | -165.401$\pm$ | 4.288 | 166.798$\pm$ | 4.29 | 10.172$\pm$ | 4.778 | 6.163$\pm$ | 4.64 | 11.893$\pm$ | 4.742
19 | A | 64.1748361$\pm$ | 0$\farcs$005138 | -21.8802396$\pm$ | 0$\farcs$004524 | 2017-10-14 | 126.736$\pm$ | 6.728 | -211.923$\pm$ | 5.893 | 246.928$\pm$ | 6.124 |  |  |  |  |  |
| B | 64.1727738$\pm$ | 0$\farcs$004377 | -21.8788069$\pm$ | 0$\farcs$004248 | 2016-12-06 | 116.722$\pm$ | 3.622 | -223.551$\pm$ | 3.549 | 252.189$\pm$ | 3.565 | 10.014$\pm$ | 7.641 | 11.628$\pm$ | 6.879 | 15.346$\pm$ | 7.213
20 | A | 68.7666169$\pm$ | 0$\farcs$004239 | -35.9865056$\pm$ | 0$\farcs$003406 | 2015-09-16 | -7.196$\pm$ | 3.604 | -99.253$\pm$ | 3.035 | 99.514$\pm$ | 3.038 |  |  |  |  |  |
| B | 68.7594779$\pm$ | 0$\farcs$018314 | -35.9832042$\pm$ | 0$\farcs$018233 | 2015-08-06 | -19.485$\pm$ | 11.443 | -100.729$\pm$ | 11.386 | 102.596$\pm$ | 11.388 | 12.289$\pm$ | 11.997 | 1.476$\pm$ | 11.784 | 12.377$\pm$ | 11.994
21 | A | 74.3510223$\pm$ | 0$\farcs$003104 | -23.0035376$\pm$ | 0$\farcs$003016 | 2016-12-31 | -122.647$\pm$ | 2.746 | 3.851$\pm$ | 2.62 | 122.707$\pm$ | 2.746 |  |  |  |  |  |
| B | 74.3475712$\pm$ | 0$\farcs$009615 | -23.0000735$\pm$ | 0$\farcs$009499 | 2016-06-02 | -117.71$\pm$ | 7.21 | 8.87$\pm$ | 7.089 | 118.044$\pm$ | 7.209 | 4.937$\pm$ | 7.715 | 5.019$\pm$ | 7.558 | 7.04$\pm$ | 7.636
22 | A | 76.2364019$\pm$ | 0$\farcs$004426 | -48.3777799$\pm$ | 0$\farcs$003606 | 2015-02-28 | -6.873$\pm$ | 2.628 | 131.213$\pm$ | 2.716 | 131.393$\pm$ | 2.716 |  |  |  |  |  |
| B | 76.2336175$\pm$ | 0$\farcs$004861 | -48.3785139$\pm$ | 0$\farcs$004749 | 2015-06-14 | -3.561$\pm$ | 3.02 | 129.436$\pm$ | 3.031 | 129.485$\pm$ | 3.031 | 3.312$\pm$ | 4.003 | 1.777$\pm$ | 4.07 | 3.759$\pm$ | 4.018
23 | A | 76.2761717$\pm$ | 0$\farcs$002213 | -47.8431073$\pm$ | 0$\farcs$002096 | 2014-07-23 | 71.531$\pm$ | 1.131 | 89.929$\pm$ | 1.069 | 114.908$\pm$ | 1.093 |  |  |  |  |  |
| B | 76.2746353$\pm$ | 0$\farcs$003374 | -47.8450102$\pm$ | 0$\farcs$003375 | 2014-07-09 | 72.705$\pm$ | 1.733 | 88.922$\pm$ | 1.709 | 114.861$\pm$ | 1.719 | 1.174$\pm$ | 2.069 | 1.007$\pm$ | 2.016 | 1.547$\pm$ | 2.047
24 | A | 80.7800047$\pm$ | 0$\farcs$003103 | -56.9228765$\pm$ | 0$\farcs$003141 | 2013-05-15 | -20.786$\pm$ | 7.213 | 160.34$\pm$ | 7.203 | 161.682$\pm$ | 7.203 |  |  |  |  |  |
| B | 80.7770104$\pm$ | 0$\farcs$017716 | -56.9196198$\pm$ | 0$\farcs$017769 | 2014-03-04 | -33.032$\pm$ | 9.194 | 160.116$\pm$ | 9.229 | 163.488$\pm$ | 9.228 | 12.246$\pm$ | 11.686 | 0.224$\pm$ | 11.707 | 12.248$\pm$ | 11.686
25 | A | 83.1346048$\pm$ | 0$\farcs$003653 | -51.4140969$\pm$ | 0$\farcs$003674 | 2015-02-21 | 106.814$\pm$ | 2.48 | 137.433$\pm$ | 2.484 | 174.061$\pm$ | 2.482 |  |  |  |  |  |
| B | 83.1359277$\pm$ | 0$\farcs$032688 | -51.4139545$\pm$ | 0$\farcs$032751 | 2015-03-25 | 83.45$\pm$ | 23.761 | 158.756$\pm$ | 23.832 | 179.353$\pm$ | 23.817 | 23.364$\pm$ | 23.89 | 21.323$\pm$ | 23.961 | 31.631$\pm$ | 23.922
26 | A | 189.7530615$\pm$ | 0$\farcs$002337 | -0.9093664$\pm$ | 0$\farcs$002861 | 2014-03-13 | -109.464$\pm$ | 1.666 | -46.147$\pm$ | 2.013 | 118.794$\pm$ | 1.723 |  |  |  |  |  |
| B | 189.7546283$\pm$ | 0$\farcs$005759 | -0.9074848$\pm$ | 0$\farcs$006148 | 2014-03-22 | -109.687$\pm$ | 5.431 | -61.573$\pm$ | 5.766 | 125.787$\pm$ | 5.513 | 0.223$\pm$ | 5.681 | 15.426$\pm$ | 6.107 | 15.428$\pm$ | 6.107
27 | A | 196.3634786$\pm$ | 0$\farcs$00336 | -22.7912345$\pm$ | 0$\farcs$003236 | 2017-07-09 | -137.418$\pm$ | 2.968 | 2.063$\pm$ | 3.02 | 137.433$\pm$ | 2.968 |  |  |  |  |  |
| B | 196.3634238$\pm$ | 0$\farcs$004029 | -22.7898509$\pm$ | 0$\farcs$004017 | 2017-08-31 | -146.575$\pm$ | 14.522 | -20.231$\pm$ | 15.312 | 147.965$\pm$ | 14.537 | 9.157$\pm$ | 14.822 | 22.294$\pm$ | 15.607 | 24.101$\pm$ | 15.496
28 | A | 200.0728026$\pm$ | 0$\farcs$00611 | -40.2161851$\pm$ | 0$\farcs$006481 | 2014-10-18 | -14.727$\pm$ | 14.628 | -129.167$\pm$ | 16.618 | 130.004$\pm$ | 16.594 |  |  |  |  |  |
| B | 200.0553734$\pm$ | 0$\farcs$00314 | -40.2084978$\pm$ | 0$\farcs$00343 | 2014-05-20 | -23.624$\pm$ | 2.603 | -120.376$\pm$ | 2.712 | 122.672$\pm$ | 2.708 | 8.897$\pm$ | 14.858 | 8.791$\pm$ | 16.838 | 12.508$\pm$ | 15.867
29 | A | 305.9567781$\pm$ | 0$\farcs$003761 | -48.7430579$\pm$ | 0$\farcs$004199 | 2016-02-24 | 14.067$\pm$ | 2.045 | -135.67$\pm$ | 2.292 | 136.397$\pm$ | 2.29 |  |  |  |  |  |
| B | 305.9533633$\pm$ | 0$\farcs$006408 | -48.7452881$\pm$ | 0$\farcs$006845 | 2016-06-21 | 17.981$\pm$ | 5.364 | -127.904$\pm$ | 5.744 | 129.162$\pm$ | 5.737 | 3.914$\pm$ | 5.741 | 7.766$\pm$ | 6.184 | 8.697$\pm$ | 6.097
30 | A | 332.2196288$\pm$ | 0$\farcs$002378 | -55.1817348$\pm$ | 0$\farcs$002615 | 2015-10-03 | -136.067$\pm$ | 1.465 | 6.288$\pm$ | 1.529 | 136.212$\pm$ | 1.465 |  |  |  |  |  |
| B | 332.2216314$\pm$ | 0$\farcs$004927 | -55.1822256$\pm$ | 0$\farcs$005096 | 2015-11-26 | -135.249$\pm$ | 2.78 | 9.723$\pm$ | 2.781 | 135.598$\pm$ | 2.78 | 0.818$\pm$ | 3.142 | 3.435$\pm$ | 3.174 | 3.531$\pm$ | 3.172
31 | A | 340.2579184$\pm$ | 0$\farcs$002945 | -45.007344$\pm$ | 0$\farcs$0032 | 2015-03-19 | 270.602$\pm$ | 1.938 | -150.33$\pm$ | 2.114 | 309.555$\pm$ | 1.981 |  |  |  |  |  |
| B | 340.2595948$\pm$ | 0$\farcs$00365 | -45.0089825$\pm$ | 0$\farcs$003825 | 2015-07-23 | 271.007$\pm$ | 1.724 | -146.575$\pm$ | 1.809 | 308.106$\pm$ | 1.744 | 0.405$\pm$ | 2.594 | 3.755$\pm$ | 2.782 | 3.777$\pm$ | 2.78
32 | A | 351.7652028$\pm$ | 0$\farcs$005126 | -52.7910943$\pm$ | 0$\farcs$005375 | 2014-05-10 | 102.662$\pm$ | 3.5 | -31.86$\pm$ | 3.634 | 107.492$\pm$ | 3.512 |  |  |  |  |  |
| B | 351.7421728$\pm$ | 0$\farcs$002748 | -52.7980402$\pm$ | 0$\farcs$002734 | 2014-02-19 | 109.78$\pm$ | 2.967 | -30.027$\pm$ | 2.953 | 113.812$\pm$ | 2.966 | 7.118$\pm$ | 4.588 | 1.833$\pm$ | 4.683 | 7.35$\pm$ | 4.594
33 | A | 353.26044$\pm$ | 0$\farcs$003137 | -63.7892751$\pm$ | 0$\farcs$003392 | 2015-12-30 | 43.408$\pm$ | 2.348 | -161.641$\pm$ | 2.417 | 167.368$\pm$ | 2.412 |  |  |  |  |  |
| B | 353.2612406$\pm$ | 0$\farcs$004994 | -63.7885657$\pm$ | 0$\farcs$005257 | 2015-12-23 | 44.617$\pm$ | 3.447 | -156.7$\pm$ | 3.555 | 162.928$\pm$ | 3.547 | 1.209$\pm$ | 4.171 | 4.941$\pm$ | 4.299 | 5.087$\pm$ | 4.292
34 | A | 356.1829712$\pm$ | 0$\farcs$00207 | 0.5201146$\pm$ | 0$\farcs$002457 | 2015-06-30 | -93.08$\pm$ | 1.302 | -103.922$\pm$ | 1.565 | 139.512$\pm$ | 1.454 |  |  |  |  |  |
| B | 356.180629$\pm$ | 0$\farcs$008729 | 0.5201466$\pm$ | 0$\farcs$009094 | 2015-09-14 | -82.033$\pm$ | 5.105 | -100.468$\pm$ | 5.33 | 129.704$\pm$ | 5.241 | 11.047$\pm$ | 5.268 | 3.454$\pm$ | 5.555 | 11.574$\pm$ | 5.295

Note— (a)Component, where A is the primary and B the secondary of the system;
(b)Proper motion difference in right ascension; (c)Proper motion difference in
declination; (d)Difference in total proper motion.

=1cm

Table 3: Comoving probabilities and photometric distances of the secondaries

Sys. | Comoving | Comoving | Comoving | $\Delta\mu_{\alpha}$ | $\Delta\mu_{\delta}$ | Sep. | Parallactic | Mean phot. | $\Delta_{dist.}$ | Min. phot. | Max. phot. | Band min. | Band max. | SpT
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
# | prob. (%) | prob. (%) | prob. (%) | (mas yr-1) | (mas yr-1) | (AU) | dist. (pc) | dist. (pc) | (pc) | dist. (pc) | dist. (pc) | phot. dist. | phot. dist. | phot. dist.
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10) | (11) | (12) | (13) | (14) | (15)
1 | 99.8 | 100.0 | 98.5 | 1.856$\pm$ | 10.387 | 7.559$\pm$ | 10.513 | 1569 | 107.8$\pm$ | 1.8 | 101.9$\pm$ | 8.4 | 6$\pm$ | 8.6 | 99.5$\pm$ | 11 | 104.3$\pm$ | 12.6 | $z_{NSC}$ | $i_{NSC}$ | L2
2 | 99.8 | 100.0 | 100.0 | 8.973$\pm$ | 11.718 | 10.211$\pm$ | 11.691 | 1095 | 55$\pm$ | 0.4 | 42.4$\pm$ | 3.5 | 12.6$\pm$ | 3.5 | 40.8$\pm$ | 4.9 | 44.1$\pm$ | 5 | $W1_{CWISE}$ | $W2_{CWISE}$ | T5
3 | 100.0 | 100.0 | 100.0 | 4.382$\pm$ | 1.809 | 2.355$\pm$ | 1.934 | 782 | 260.7$\pm$ | 57.5 | 282.5$\pm$ | 29.9 | 21.8$\pm$ | 64.8 | 263.4$\pm$ | 36.5 | 301.7$\pm$ | 47.3 | $y_{PS1}$ | $i_{PS1}$ | M6
4 | 100.0 | 100.0 | 99.9 | 7.677$\pm$ | 2.034 | 0.959$\pm$ | 2.121 | 794 | 145.8$\pm$ | 1.2 | 148.9$\pm$ | 25 | 3.1$\pm$ | 25 | 148.7$\pm$ | 34.2 | 149.2$\pm$ | 36.4 | $RP_{EDR3}$ | $G_{EDR3}$ | M9
5 | 99.8 | 99.9 | 99.8 | 2.888$\pm$ | 13.911 | 17.449$\pm$ | 12.082 | 504 | 86.3$\pm$ | 0.2 | 81.6$\pm$ | 12.4 | 4.7$\pm$ | 12.4 | 80$\pm$ | 17.7 | 83.2$\pm$ | 17.3 | $i_{DES}$ | $z_{DES}$ | M8
6 | 99.6 | 99.8 | 99.1 | 9.646$\pm$ | 5.189 | 13.974$\pm$ | 4.68 | 1156 | 145.9$\pm$ | 0.7 | 147.2$\pm$ | 21.1 | 1.3$\pm$ | 21.1 | 145.1$\pm$ | 28.8 | 149.2$\pm$ | 30.9 | $y_{PS1}$ | $z_{PS1}$ | M8
7 | 100.0 | 98.8 | 100.0 | 19.526$\pm$ | 16.492 | 2.815$\pm$ | 16.64 | 1396 | 118.8$\pm$ | 0.9 | 72.3$\pm$ | 14.4 | 46.4$\pm$ | 14.4 | 71$\pm$ | 25.4 | 73.7$\pm$ | 13.5 | $r_{DES}$ | $i_{DES}$ | L4
8 | 100.0 | 100.0 | 100.0 | 0.339$\pm$ | 3.879 | 0.23$\pm$ | 4.933 | 776 | 184.5$\pm$ | 0.8 | 129.3$\pm$ | 19.6 | 55.2$\pm$ | 19.6 | 125.5$\pm$ | 27.8 | 133.1$\pm$ | 27.6 | $i_{DES}$ | $z_{DES}$ | M8
9 | 100.0 | 59.8 | 100.0 | 16.929$\pm$ | 12.436 | 0.006$\pm$ | 12.602 | 8487 | 232.5$\pm$ | 1.1 | 121.8$\pm$ | 30.2 | 110.6$\pm$ | 30.2 | 119.8$\pm$ | 43.1 | 123.9$\pm$ | 42.4 | $W2_{CWISE}$ | $W1_{CWISE}$ | L9
10 | 99.9 | 100.0 | 99.9 | 0.647$\pm$ | 8.162 | 1.645$\pm$ | 8.019 | 1691 | 75.6$\pm$ | 0.1 | 72.3$\pm$ | 17.3 | 3.2$\pm$ | 17.3 | 60.5$\pm$ | 9.2 | 84.2$\pm$ | 33.3 | $z_{DES}$ | $r_{DES}$ | L4
11 | 99.6 | 99.9 | 99.1 | 0.098$\pm$ | 28.018 | 6.786$\pm$ | 28.114 | 637 | 114.6$\pm$ | 9.7 | 115.6$\pm$ | 12 | 1$\pm$ | 15.4 | 115.4$\pm$ | 18.1 | 115.8$\pm$ | 15.7 | $W2_{CWISE}$ | $W1_{CWISE}$ | L8
12 | 99.8 | 99.9 | 89.0 | 4.543$\pm$ | 7.573 | 17.459$\pm$ | 7.605 | 5886 | 155.9$\pm$ | 4.6 | 153.3$\pm$ | 12.1 | 2.6$\pm$ | 12.9 | 152.6$\pm$ | 16.2 | 153.9$\pm$ | 17.9 | $z_{NSC}$ | $i_{NSC}$ | L1
13 | 73.6 | 87.0 | 25.7 | 6.841$\pm$ | 2.866 | 18.764$\pm$ | 2.625 | 549 | 92$\pm$ | 0.4 | 100.8$\pm$ | 14 | 8.8$\pm$ | 14 | 100$\pm$ | 19.3 | 101.6$\pm$ | 20.1 | $J_{VHS}$ | $K_{VHS}$ | M8
14 | 99.9 | 100.0 | 100.0 | 3.915$\pm$ | 8.094 | 3.789$\pm$ | 8.298 | 424 | 80.8$\pm$ | 1.4 | 67.3$\pm$ | 8 | 13.5$\pm$ | 8.2 | 65.5$\pm$ | 10 | 69$\pm$ | 12.6 | $z_{DES}$ | $i_{DES}$ | L4
15 | 100.0 | 4.5 | 5.7 | 5.034$\pm$ | 5.552 | 7.988$\pm$ | 5.7 | 1008 | 258$\pm$ | 3.4 | 128.4$\pm$ | 10.7 | 129.6$\pm$ | 11.3 | 127.5$\pm$ | 15.4 | 129.3$\pm$ | 14.9 | $i_{NSC}$ | $z_{NSC}$ | L0
16 | 100.0 | 100.0 | 100.0 | 3.249$\pm$ | 4.112 | 3.461$\pm$ | 3.972 | 958 | 165$\pm$ | 0.8 | 154.4$\pm$ | 17.8 | 10.6$\pm$ | 17.8 | 150.8$\pm$ | 21.5 | 157.9$\pm$ | 28.4 | $y_{PS1}$ | $i_{PS1}$ | M7
17 | 100.0 | 100.0 | 99.7 | 4.896$\pm$ | 4.618 | 2.65$\pm$ | 4.701 | 741 | 121.6$\pm$ | 0.9 | 121.8$\pm$ | 11.5 | 0.2$\pm$ | 11.5 | 111.7$\pm$ | 14 | 132$\pm$ | 18.2 | $z_{SDSS}$ | $i_{SDSS}$ | L0
18 | 100.0 | 100.0 | 100.0 | 10.172$\pm$ | 4.778 | 6.163$\pm$ | 4.64 | 411 | 157.2$\pm$ | 5.9 | 191.5$\pm$ | 29.4 | 34.3$\pm$ | 29.9 | 185.2$\pm$ | 43.7 | 197.9$\pm$ | 39.2 | $i_{PS1}$ | $y_{PS1}$ | M8
19 | 100.0 | 100.0 | 100.0 | 10.014$\pm$ | 7.641 | 11.628$\pm$ | 6.879 | 1128 | 134.1$\pm$ | 0.6 | 108.6$\pm$ | 13.5 | 25.4$\pm$ | 13.5 | 106.3$\pm$ | 18.2 | 110.9$\pm$ | 20 | $z_{PS1}$ | $i_{PS1}$ | M9
20 | 99.8 | 99.8 | 99.9 | 12.289$\pm$ | 11.997 | 1.476$\pm$ | 11.784 | 2556 | 106.7$\pm$ | 0.3 | 75.6$\pm$ | 19.7 | 31.2$\pm$ | 19.7 | 59.7$\pm$ | 8.1 | 91.5$\pm$ | 38.6 | $z_{DES}$ | $r_{DES}$ | L5
21 | 100.0 | 100.0 | 100.0 | 4.937$\pm$ | 7.715 | 5.019$\pm$ | 7.558 | 933 | 55$\pm$ | 0.1 | 48.9$\pm$ | 8.5 | 6.1$\pm$ | 8.5 | 47.6$\pm$ | 13.4 | 50.2$\pm$ | 10.4 | $W1_{UWISE}$ | $W2_{UWISE}$ | T3
22 | 100.0 | 100.0 | 100.0 | 3.312$\pm$ | 4.003 | 1.777$\pm$ | 4.07 | 571 | 79.5$\pm$ | 0.1 | 71.6$\pm$ | 10.8 | 8$\pm$ | 10.8 | 64.5$\pm$ | 9.3 | 78.7$\pm$ | 19.4 | $r_{DES}$ | $g_{DES}$ | L0
23 | 100.0 | 100.0 | 100.0 | 1.174$\pm$ | 2.069 | 1.007$\pm$ | 2.016 | 1217 | 156.3$\pm$ | 2.9 | 103.3$\pm$ | 12.9 | 52.9$\pm$ | 13.2 | 92.7$\pm$ | 16.7 | 114$\pm$ | 19.7 | $i_{NSC}$ | $r_{NSC}$ | M9
24 | 100.0 | 100.0 | 100.0 | 12.246$\pm$ | 11.686 | 0.224$\pm$ | 11.707 | 707 | 54.4$\pm$ | 0.1 | 55.7$\pm$ | 7.6 | 1.4$\pm$ | 7.6 | 55$\pm$ | 10 | 56.4$\pm$ | 11.4 | $K_{VHS}$ | $J_{VHS}$ | T0
25 | 100.0 | 100.0 | 100.0 | 23.364$\pm$ | 23.89 | 21.323$\pm$ | 23.961 | 508 | 169.1$\pm$ | 10.9 | 150$\pm$ | 17.4 | 19.1$\pm$ | 20.5 | 145.5$\pm$ | 21 | 154.4$\pm$ | 27.7 | $z_{NSC}$ | $i_{NSC}$ | L3
26 | 99.3 | 100.0 | 99.9 | 0.223$\pm$ | 5.681 | 15.426$\pm$ | 6.107 | 377 | 42.8$\pm$ | 0.1 | 37.6$\pm$ | 4.3 | 5.2$\pm$ | 4.3 | 36.7$\pm$ | 6.5 | 38.5$\pm$ | 5.7 | $i_{PS1}$ | $y_{PS1}$ | L4
27 | 99.9 | 99.9 | 99.9 | 9.157$\pm$ | 14.822 | 22.294$\pm$ | 15.607 | 716 | 143.7$\pm$ | 16.4 | 112.3$\pm$ | 13.6 | 31.4$\pm$ | 21.3 | 111.3$\pm$ | 19.6 | 113.2$\pm$ | 18.8 | $W2_{CWISE}$ | $W1_{CWISE}$ | L3
28 | 100.0 | 100.0 | 91.6 | 8.897$\pm$ | 14.858 | 8.791$\pm$ | 16.838 | 3697 | 66.8$\pm$ | 0.1 | 70.7$\pm$ | 5.8 | 3.9$\pm$ | 5.8 | 68.6$\pm$ | 7.2 | 72.9$\pm$ | 9.1 | $H_{2MASS}$ | $K_{2MASS}$ | L1
29 | 100.0 | 100.0 | 99.4 | 3.914$\pm$ | 5.741 | 7.766$\pm$ | 6.184 | 1094 | 96.1$\pm$ | 0.3 | 96.6$\pm$ | 9.8 | 0.5$\pm$ | 9.8 | 93.9$\pm$ | 11.3 | 99.4$\pm$ | 16.1 | $i_{DES}$ | $r_{DES}$ | L0
30 | 100.0 | 100.0 | 100.0 | 0.818$\pm$ | 3.142 | 3.435$\pm$ | 3.174 | 431 | 95.7$\pm$ | 0.6 | 111$\pm$ | 12.5 | 15.3$\pm$ | 12.5 | 109.6$\pm$ | 17.2 | 112.4$\pm$ | 18.1 | $J_{VHS}$ | $H_{VHS}$ | M9
31 | 100.0 | 100.0 | 99.9 | 0.405$\pm$ | 2.594 | 3.755$\pm$ | 2.782 | 418 | 58.2$\pm$ | 2.1 | 60$\pm$ | 5 | 1.8$\pm$ | 5.4 | 59.8$\pm$ | 5.8 | 60.2$\pm$ | 8 | $J_{VHS}$ | $K_{VHS}$ | L2
32 | 100.0 | 100.0 | 99.7 | 7.118$\pm$ | 4.588 | 1.833$\pm$ | 4.683 | 6488 | 115.8$\pm$ | 0.2 | 112.6$\pm$ | 10 | 3.2$\pm$ | 10 | 95.2$\pm$ | 13.1 | 130$\pm$ | 15 | $r_{NSC}$ | $i_{NSC}$ | L1
33 | 100.0 | 100.0 | 100.0 | 1.209$\pm$ | 4.171 | 4.941$\pm$ | 4.299 | 323 | 113.2$\pm$ | 5.5 | 135.5$\pm$ | 16.4 | 22.3$\pm$ | 17.3 | 134.9$\pm$ | 23 | 136$\pm$ | 23.3 | $W1_{CWISE}$ | $W2_{CWISE}$ | M9
34 | 100.0 | 100.0 | 98.1 | 11.047$\pm$ | 5.268 | 3.454$\pm$ | 5.555 | 1031 | 122.5$\pm$ | 2.6 | 119.3$\pm$ | 9.2 | 3.2$\pm$ | 9.5 | 115.8$\pm$ | 11.4 | 122.8$\pm$ | 14.3 | $J_{VHS}$ | $H_{VHS}$ | L2

Column descriptions:
(1) System number
(2) Comoving probability without a distance constraint on the secondary
(3) Comoving probability with a distance constraint on the secondary
(4) Comoving probability calculated by increasing the secondary’s distance by
40% (see Section 4.4)
(5) Proper motion difference in right ascension
(6) Proper motion difference in declination
(7) Projected physical separation
(8) Parallactic distance of the primary
(9) Mean photometric distance of the secondary
(10) Distance difference between the primary (parallactic distance) and
secondary (mean photometric distance)
(11) Minimum photometric distance of the secondary for a given photometric
system
(12) Maximum photometric distance of the secondary for a given photometric
system
(13) Band from which the minimum photometric distance of the secondary was
inferred (CWISE and UWISE stand for CatWISE2020 and unWISE DR1, respectively)
(14) Band from which the maximum photometric distance of the secondary was
inferred
(15) Spectral type estimate used to derive the absolute magnitude for the
photometric distance calculations

Table 4: Fundamental parameters and literature references

Sys. | Component | Teff | log g | Mass | Radius | Luminosity | Param. | Other
---|---|---|---|---|---|---|---|---
# | name | (K) |  | (M⊙) | (R⊙) | (L⊙) | ref.c | ref.d
1 | NSC J0004+0451 A | 2900$\pm$ | 157 | 5.0627$\pm$ | 0.0207 | 0.17$\pm$ | 0.021 | 0.201$\pm$ | 0.007 | 0.00257$\pm$ | 0.00075 | 1 |
1 | NSC J0004+0451 B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  | 3
2 | NSC J0040-2942 A | 2823$\pm$ | 157 | 5.2584$\pm$ | 0.0648 | 0.097$\pm$ | 0.02 | 0.121$\pm$ | 0.004 | 0.00084$\pm$ | 0.00024 | 1 | 4,5
4 | NSC J0045-2855 A | 3326$\pm$ | 157 | 4.9128$\pm$ | 0.0029 | 0.29$\pm$ | 0.021 | 0.312$\pm$ | 0.01 | 0.01073$\pm$ | 0.00273 | 1 |
5 | NSC J0107-2658 A | 3677$\pm$ | 157 | 4.7644$\pm$ | 0.007 | 0.467$\pm$ | 0.02 | 0.469$\pm$ | 0.014 | 0.03627$\pm$ | 0.0084 | 1 | 5,6,7,8
6 | NSC J0126-2620 A | 3435$\pm$ | 157 | 4.7987$\pm$ | 0.0058 | 0.426$\pm$ | 0.021 | 0.431$\pm$ | 0.013 | 0.02327$\pm$ | 0.00573 | 1 |
7 | NSC J0148-0357 A | 3343$\pm$ | 158 | 4.9799$\pm$ | 0.0109 | 0.226$\pm$ | 0.02 | 0.255$\pm$ | 0.008 | 0.00731$\pm$ | 0.00187 | 1 | 6,9
8 | NSC J0153-0015 A | 3962$\pm$ | 157 | 4.6746$\pm$ | 0.0102 | 0.565$\pm$ | 0.02 | 0.572$\pm$ | 0.017 | 0.07275$\pm$ | 0.01593 | 1 |
9 | NSC J0200-1254 A | 4205$\pm$ | 122 | 4.6726$\pm$ | $\cdots$ | 0.66$\pm$ | $\cdots$ | 0.62$\pm$ | $\cdots$ | 0.10834$\pm$ | $\cdots$ | 1 | 10
10 | NSC J0200-4707 A | 3577$\pm$ | 157 | 4.7872$\pm$ | 0.0058 | 0.44$\pm$ | 0.02 | 0.444$\pm$ | 0.013 | 0.02903$\pm$ | 0.00686 | 1 |
12 | NSC J0221-6338 A | 3028$\pm$ | 166 | 5.1495$\pm$ | 0.0159 | 0.131$\pm$ | 0.022 | 0.159$\pm$ | 0.01 | 0.00192$\pm$ | 0.00068 | 1 |
13 | NSC J0228-5320 A | 3383$\pm$ | 157 | 4.8175$\pm$ | 0.0042 | 0.403$\pm$ | 0.02 | 0.41$\pm$ | 0.012 | 0.01984$\pm$ | 0.00491 | 1 |
14 | NSC J0231-0311 A | 2900$\pm$ | 158 | 5.1218$\pm$ | 0.0274 | 0.141$\pm$ | 0.021 | 0.171$\pm$ | 0.007 | 0.00187$\pm$ | 0.00057 | 1 |
15 | NSC J0244-0517 A | 3734$\pm$ | 157 | 4.8153$\pm$ | 0.0063 | 0.405$\pm$ | 0.022 | 0.412$\pm$ | 0.014 | 0.0298$\pm$ | 0.00707 | 1 |
16 | NSC J0245-1237 A | 3665$\pm$ | 157 | 4.7833$\pm$ | 0.0064 | 0.444$\pm$ | 0.021 | 0.448$\pm$ | 0.014 | 0.03262$\pm$ | 0.00762 | 1 |
17 | NSC J0254-0852 A | 3410$\pm$ | 158 | 4.9829$\pm$ | 0.0112 | 0.224$\pm$ | 0.02 | 0.253$\pm$ | 0.008 | 0.00777$\pm$ | 0.00196 | 1 |
18 | NSC J0412-2621 A | 3116$\pm$ | 165 | 5.2027$\pm$ | 0.0176 | 0.113$\pm$ | 0.022 | 0.139$\pm$ | 0.011 | 0.00165$\pm$ | 0.00061 | 1 |
19 | NSC J0416-2152 A | 3453$\pm$ | 157 | 4.8909$\pm$ | 0.0013 | 0.315$\pm$ | 0.02 | 0.333$\pm$ | 0.01 | 0.0142$\pm$ | 0.00348 | 1 | 6,9
20 | NSC J0435-3559 A | 3406$\pm$ | 157 | 4.9323$\pm$ | 0.0062 | 0.27$\pm$ | 0.02 | 0.294$\pm$ | 0.009 | 0.01049$\pm$ | 0.00259 | 1 |
21 | NSC J0457-2300 A | 3351$\pm$ | 157 | 4.9899$\pm$ | 0.0137 | 0.218$\pm$ | 0.02 | 0.247$\pm$ | 0.008 | 0.00695$\pm$ | 0.00174 | 1 |
22 | NSC J0504-4822 A | 3400$\pm$ | 157 | 4.8947$\pm$ | 0.0024 | 0.31$\pm$ | 0.02 | 0.329$\pm$ | 0.01 | 0.01305$\pm$ | 0.00321 | 1 |
23 | NSC J0505-4750 A | 3085$\pm$ | 160 | 5.1279$\pm$ | 0.0257 | 0.139$\pm$ | 0.021 | 0.168$\pm$ | 0.008 | 0.00232$\pm$ | 0.0007 | 1 |
24 | NSC J0523-5655 A | 3221$\pm$ | 157 | 5.022$\pm$ | 0.0185 | 0.195$\pm$ | 0.02 | 0.225$\pm$ | 0.007 | 0.00492$\pm$ | 0.00127 | 1 | 11
25 | NSC J0532-5124 A | 4960$\pm$ | 422a | 7.2249$\pm$ | 0.5067a | 0.256$\pm$ | 0.159a |  $\cdots$ |  |  $\cdots$ |  | 2 |
25 | NSC J0532-5124 A | 5043$\pm$ | 337b | 7.3208$\pm$ | 0.3934b | 0.283$\pm$ | 0.133b |  $\cdots$ |  |  $\cdots$ |  | 2 |
26 | NSC J1239-0054 A | 3245$\pm$ | 157 | 4.9843$\pm$ | 0.0132 | 0.222$\pm$ | 0.02 | 0.251$\pm$ | 0.008 | 0.00632$\pm$ | 0.00161 | 1 |
26 | NSC J1239-0054 B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  | 3
27 | NSC J1305-2247 A | 5373$\pm$ | 786a | 8.076$\pm$ | 0.6699a | 0.63$\pm$ | 0.383a |  $\cdots$ |  |  $\cdots$ |  | 2 |
27 | NSC J1305-2247 A | 5266$\pm$ | 720b | 8.0029$\pm$ | 0.6323b | 0.571$\pm$ | 0.355b |  $\cdots$ |  |  $\cdots$ |  | 2 |
28 | NSC J1320-4012 A | 3601$\pm$ | 157 | 4.737$\pm$ | 0.0082 | 0.499$\pm$ | 0.02 | 0.5$\pm$ | 0.015 | 0.03795$\pm$ | 0.00892 | 1 |
29 | NSC J2023-4844 A | 3250$\pm$ | 157 | 4.9134$\pm$ | 0.0037 | 0.29$\pm$ | 0.02 | 0.311$\pm$ | 0.01 | 0.00974$\pm$ | 0.0025 | 1 |
30 | NSC J2208-5510 A | 3055$\pm$ | 157 | 5.0057$\pm$ | 0.0142 | 0.206$\pm$ | 0.02 | 0.236$\pm$ | 0.008 | 0.00438$\pm$ | 0.0012 | 1 |
31 | NSC J2241-4500 A | 3014$\pm$ | 157 | 4.9062$\pm$ | 0.0089 | 0.297$\pm$ | 0.026 | 0.318$\pm$ | 0.017 | 0.00753$\pm$ | 0.00241 | 1 | 5
32 | NSC J2327-5247 A | 3620$\pm$ | 157 | 4.7416$\pm$ | 0.0081 | 0.493$\pm$ | 0.02 | 0.495$\pm$ | 0.015 | 0.03794$\pm$ | 0.0089 | 1 |
33 | NSC J2333-6347 A | 5243$\pm$ | 318a | 8.0675$\pm$ | 0.2821a | 0.623$\pm$ | 0.175a |  $\cdots$ |  |  $\cdots$ |  | 2 |
33 | NSC J2333-6347 A | 5147$\pm$ | 285b | 8.0023$\pm$ | 0.2531b | 0.57$\pm$ | 0.143b |  $\cdots$ |  |  $\cdots$ |  | 2 |
34 | NSC J2344+0031 A | 2987$\pm$ | 160 | 5.0783$\pm$ | 0.0229 | 0.161$\pm$ | 0.02 | 0.192$\pm$ | 0.007 | 0.00265$\pm$ | 0.00077 | 1 |

(a)Teff, log g and mass for DA white dwarfs
(b)Teff, log g and mass for DB white dwarfs
(c)Parameter references: (1) Stassun et al. (2019), (2) Gentile Fusillo et al.
(2021)
(d)Other literature references: (3) Skrzypek et al. (2016), (4) Reylé (2018),
(5) Pokorny et al. (2003), (6) Luyten (1995), (7) Eggen (1976a), (8) Eggen
(1976b), (9) Salim & Gould (2003), (10) Wroblewski & Torres (1996), (11)
Kirkpatrick et al. (2016)

Table 5: Total masses, mass ratios and binding energies

Sys. | Sys. | Sep.a | M1b | M2c | Mtotd | M2/M1e | Ebinf | SpT2g
---|---|---|---|---|---|---|---|---
# | name | (AU) | (M⊙) | (M⊙) | (M⊙) |  | ($\times 10^{41}$ erg) |
1 | NSC J0004+0451 | 1568.531 | 0.170 | 0.073 | 0.243 | 0.427 | 1.11 | L2
2 | NSC J0040-2942 | 1095.379 | 0.097 | 0.034 | 0.131 | 0.354 | 0.42 | T5
3 | NSC J0042-2507 | 782.216 | 0.128 | 0.115 | 0.243 | 0.901 | 2.64 | M6
4 | NSC J0045-2855 | 794.110 | 0.290 | 0.079 | 0.369 | 0.273 | 4.04 | M9
5 | NSC J0107-2658 | 504.352 | 0.467 | 0.090 | 0.557 | 0.192 | 11.67 | M8
6 | NSC J0126-2620 | 1155.583 | 0.426 | 0.090 | 0.516 | 0.211 | 4.65 | M8
7 | NSC J0148-0357 | 1395.736 | 0.226 | 0.055 | 0.281 | 0.245 | 1.25 | L4
8 | NSC J0153-0015 | 776.150 | 0.565 | 0.090 | 0.655 | 0.159 | 9.18 | M8
9 | NSC J0200-1254 | 8486.735 | 0.660 | 0.046 | 0.706 | 0.069 | 0.50 | L9
10 | NSC J0200-4707 | 1691.254 | 0.440 | 0.055 | 0.495 | 0.126 | 2.00 | L4
11 | NSC J0205+0202 | 637.127 | 0.084 | 0.055 | 0.139 | 0.659 | 1.02 | L8
12 | NSC J0221-6338 | 5886.303 | 0.131 | 0.073 | 0.204 | 0.554 | 0.23 | L1
13 | NSC J0228-5320 | 548.533 | 0.403 | 0.090 | 0.493 | 0.223 | 9.26 | M8
14 | NSC J0231-0311 | 423.614 | 0.141 | 0.055 | 0.196 | 0.393 | 2.56 | L4
15 | NSC J0244-0517 | 1007.524 | 0.405 | 0.077 | 0.482 | 0.191 | 4.34 | L0
16 | NSC J0245-1237 | 958.154 | 0.444 | 0.097 | 0.541 | 0.219 | 6.30 | M7
17 | NSC J0254-0852 | 741.364 | 0.224 | 0.077 | 0.301 | 0.345 | 3.26 | L0
18 | NSC J0412-2621 | 411.436 | 0.113 | 0.090 | 0.203 | 0.795 | 3.46 | M8
19 | NSC J0416-2152 | 1127.526 | 0.315 | 0.079 | 0.394 | 0.251 | 3.09 | M9
20 | NSC J0435-3559 | 2555.901 | 0.270 | 0.055 | 0.325 | 0.205 | 0.81 | L5
21 | NSC J0457-2300 | 933.096 | 0.218 | 0.046 | 0.264 | 0.210 | 1.50 | T3
22 | NSC J0504-4822 | 570.648 | 0.310 | 0.077 | 0.387 | 0.249 | 5.86 | L0
23 | NSC J0505-4750 | 1216.806 | 0.139 | 0.079 | 0.218 | 0.569 | 1.26 | M9
24 | NSC J0523-5655 | 706.547 | 0.195 | 0.046 | 0.241 | 0.235 | 1.78 | T0
25 | NSC J0532-5124 | 507.731 | 0.256 | 0.073 | 0.329 | 0.285 | 5.16 | L3
26 | NSC J1239-0054 | 377.062 | 0.222 | 0.055 | 0.277 | 0.250 | 4.54 | L4
27 | NSC J1305-2247 | 715.907 | 0.630 | 0.073 | 0.703 | 0.116 | 9.00 | L3
28 | NSC J1320-4012 | 3697.213 | 0.499 | 0.073 | 0.572 | 0.145 | 1.38 | L1
29 | NSC J2023-4844 | 1093.871 | 0.290 | 0.077 | 0.367 | 0.267 | 2.86 | L0
30 | NSC J2208-5510 | 430.541 | 0.206 | 0.079 | 0.285 | 0.384 | 5.29 | M9
31 | NSC J2241-4500 | 418.277 | 0.297 | 0.073 | 0.370 | 0.244 | 7.26 | L2
32 | NSC J2327-5247 | 6487.802 | 0.493 | 0.073 | 0.566 | 0.147 | 0.78 | L1
33 | NSC J2333-6347 | 322.740 | 0.570 | 0.079 | 0.649 | 0.139 | 19.54 | M9
34 | NSC J2344+0031 | 1030.796 | 0.161 | 0.073 | 0.234 | 0.451 | 1.60 | L2

Note— (a)Projected physical separation; (b)Primary mass estimate from either
Stassun et al. (2019) or Gentile Fusillo et al. (2021); (c)Secondary mass
estimate from either Mamajek (2021) for sources with MG $<$ 17 mag, or from
the SpT to dynamical mass values computed in Dupuy & Liu (2017); (d)Total mass
(primary mass + secondary mass); (e)Mass ratio (secondary/primary); (f)Binding
energy, calculated by multiplying the physical separation by 1.26 to account
for inclination angle and eccentricity of the binary orbits (Fischer & Marcy,
1992); (g)Spectral type used to derive the secondary’s mass.

Table 6: Age, initial and final mass estimates of the white dwarfs

Sys. | WD | Teffa | log gb | Massc | MS aged | WD agee | Tot. agef | Init. massg | Final massh
---|---|---|---|---|---|---|---|---|---
# | type | (K) |  | (M⊙) | (Gyr) | (Gyr) | (Gyr) | (M⊙) | (M⊙)
(1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) | (9) | (10)
25 | DA | 4960$\pm$ | 422 | 7.225$\pm$ | 0.507 | 0.256$\pm$ | 0.159 |  $\cdots$ |  | 2.34 | ${}_{-0.91}^{+2.04}$ |  $\cdots$ |  |  $\cdots$ |  | 0.33 | ${}_{-0.11}^{+0.21}$
25 | DB | 5043$\pm$ | 337 | 7.321$\pm$ | 0.393 | 0.283$\pm$ | 0.133 |  $\cdots$ |  | 2.04 | ${}_{-0.65}^{+1.62}$ |  $\cdots$ |  |  $\cdots$ |  | 0.32 | ${}_{-0.1}^{+0.16}$
27 | DA | 5373$\pm$ | 786 | 8.076$\pm$ | 0.670 | 0.63$\pm$ | 0.383 | 1.42 | ${}_{-1.01}^{+2.15}$ | 5.25 | ${}_{-2.07}^{+2.27}$ | 7.41 | ${}_{-2.06}^{+1.75}$ | 1.93 | ${}_{-0.53}^{+1.18}$ | 0.65 | ${}_{-0.05}^{+0.12}$
27 | DB | 5266$\pm$ | 720 | 8.003$\pm$ | 0.632 | 0.571$\pm$ | 0.355 | 1.46 | ${}_{-1.0}^{+2.14}$ | 5.39 | ${}_{-2.05}^{+2.22}$ | 7.57 | ${}_{-2.01}^{+1.65}$ | 1.91 | ${}_{-0.51}^{+1.09}$ | 0.65 | ${}_{-0.05}^{+0.1}$
33 | DA | 5243$\pm$ | 318 | 8.067$\pm$ | 0.282 | 0.623$\pm$ | 0.175 | 1.65 | ${}_{-0.98}^{+2.05}$ | 5.52 | ${}_{-1.62}^{+1.84}$ | 7.79 | ${}_{-1.59}^{+1.4}$ | 1.82 | ${}_{-0.42}^{+0.83}$ | 0.64 | ${}_{-0.05}^{+0.07}$
33 | DB | 5147$\pm$ | 285 | 8.002$\pm$ | 0.253 | 0.57$\pm$ | 0.143 | 1.73 | ${}_{-0.94}^{+1.92}$ | 5.73 | ${}_{-1.58}^{+1.7}$ | 8.05 | ${}_{-1.5}^{+1.25}$ | 1.78 | ${}_{-0.38}^{+0.71}$ | 0.63 | ${}_{-0.04}^{+0.06}$

Note— (a,b,c)Effective temperature, surface gravity and mass estimates from
Gentile Fusillo et al. (2021); (d)Main sequence age (age of the progenitor
star); (e)Cooling age of the white dwarf; (f)Total age (main sequence age +
cooling age); (g)Initial mass (mass of the progenitor star); (h)Final mass
(mass of the white dwarf).

##  5 Discussion

Systems #9 and #19 have high tangential velocities of $\sim 187$ and $\sim
158$ km s-1 respectively, suggesting a possible thick disk or halo membership
(Carollo et al., 2010; Dupuy & Liu, 2012; Belokurov et al., 2018; Amarante et
al., 2020). Further study of these systems is required to determine how old or
metal-poor these objects really are.

Systems #13, #14 and #31 have a primary with a high Gaia RUWE333Re-normalized
Unit Weight Error of $\sim 1.9$, $\sim 14$ and $\sim 2.7$ respectively. A RUWE
significantly greater than 1.0 (e.g. $>$1.4) could indicate that the source is
non-single and thus might be an unresolved binary (Belokurov et al., 2020;
Penoyre et al., 2020). Given past work suggesting that widely separated
ultracool dwarfs from higher mass companions are likely to be found in
hierarchical systems, there is an increased probability of finding more hidden
companions. (e.g. Burgasser et al. 2003, Faherty et al. 2010, Law et al.
2010). System #31, which is likely a triple system (M+M+L), has already been
analyzed in more detail (Kiwy et al., 2021).

Systems #9, #13 and #15 have comoving probabilities well below 100%, when we
use a distance constraint in these calculations, indicating that they are
likely chance alignments. Systems #9 and #15 also show the largest
discrepancies between the primary’s parallactic and the secondary’s
photometric distance (232.5$\pm$1.1 pc vs. 121.8$\pm$30.2 pc and 258$\pm$3.4
pc vs. 128.4$\pm$10.7 pc, respectively), implying that these systems (provided
the photometric distance is reasonably correct) cannot be physically bound.
Whereas system #13 has a much smaller distance difference of only 8.8$\pm$14
pc between the primary and the secondary as well as a higher comoving
probability (87.0%) compared to systems #9 and #15 (59.8 and 4.5%,
respectively), but still well below that of the majority of the systems ($>$
99%).

##  6 Conclusion

We presented the discovery of 34 new, potential comoving systems found by the
means of NSC DR2 and demonstrated that the catalog’s proper motions are well
suited for the discovery of comoving systems including late-type objects such
as brown dwarfs in the L and T regimes. We also showed that the catalog can be
used to find close late-type comoving companions to white dwarfs, providing
valuable benchmark systems for the difficult task of estimating brown dwarf
ages.

According to the literature, none of the 34 identified objects were previously
known to have a comoving companion. Some of the systems stand out as having
high tangential velocities, suggesting that they could be candidates for low
metallicity benchmark systems. The newly discovered systems expand the known
sample of benchmark systems involving L and T dwarfs and thus contribute to
the further characterization of cool substellar objects.

Spectroscopic follow-up on individual interesting systems is warranted, for
instance, to find out how low the metallicity of the high tangential velocity
systems actually is, or to clarify the potential binarity of the primaries
with a high Gaia RUWE value.

##  7 Acknowledgements

This work has made use of data and/or services provided by:

  * •

The Astro Data Lab at NSF’s National Optical-Infrared Astronomy Research
Laboratory. NOIRLab is operated by the Association of Universities for
Research in Astronomy (AURA), Inc. under a cooperative agreement with the
National Science Foundation.

  * •

The DESI Legacy Imaging Surveys (https://www.legacysurvey.org/acknowledgment)

  * •

The VISTA Science Archive (VSA) holding the image and catalogue data products
generated by VIRCAM on the Visible and Infrared Survey Telescope for Astronomy
(VISTA)

  * •

The European Space Agency (ESA) mission Gaia
(https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and
Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has
been provided by national institutions, in particular the institutions
participating in the Gaia Multilateral Agreement.

  * •

The European Southern Observatory under ESO program VHS 179.A-2010

  * •

The SIMBAD database (Wenger et al., 2000), operated at CDS, Strasbourg, France

  * •

The VizieR catalogue access tool, CDS, Strasbourg, France (DOI :
10.26093/cds/vizier). The original description of the VizieR service was
published in Ochsenbein et al. (2000).

  * •

The Infrared Telescope Facility, which is operated by the University of Hawaii
under contract 80HQTR19D0030 with the National Aeronautics and Space
Administration

  * •

The SpeX Prism Spectral Libraries, maintained by Adam Burgasser at
http://pono.ucsd.edu/~adam/browndwarfs/spexprism

  * •

The UltracoolSheet, maintained by Will Best, Trent Dupuy, Michael Liu, Rob
Siverd, and Zhoujian Zhang, and developed from compilations by Dupuy & Liu
(2012), Dupuy & Kraus (2013), Liu et al. (2016), Best et al. (2018), and Best
et al. (2021).

  * •

wdwarfdate, an open source code which estimates ages of white dwarfs in a
Bayesian framework from effective temperature and surface gravity
https://github.com/rkiman/wdwarfdate

  * •

AstroToolBox, a Java tool set for the identification and classification of
astronomical objects with a focus on very low-mass and ultra-cool dwarfs
https://github.com/fkiwy/AstroToolBox

  * •

This research was supported by National Science Foundation Grant No.’s
2007068, 2009136, and 2009177 and J.F. acknowledge support from the Heising-
Simons Foundation.

## References

  * Abbott et al. (2018) Abbott, T. M. C., Abdalla, F. B., Allam, S., et al. 2018, ApJS, 239, 18, doi: 10.3847/1538-4365/aae9f0
  * Abbott et al. (2021) Abbott, T. M. C., Adamów, M., Aguena, M., et al. 2021, ApJS, 255, 20, doi: 10.3847/1538-4365/ac00b3
  * Amarante et al. (2020) Amarante, J. A. S., Smith, M. C., & Boeche, C. 2020, MNRAS, 492, 3816, doi: 10.1093/mnras/staa077
  * Basri & Martín (1999) Basri, G., & Martín, E. L. 1999, AJ, 118, 2460, doi: 10.1086/301079
  * Bédard et al. (2020) Bédard, A., Bergeron, P., Brassard, P., & Fontaine, G. 2020, ApJ, 901, 93, doi: 10.3847/1538-4357/abafbe
  * Belokurov et al. (2018) Belokurov, V., Erkal, D., Evans, N. W., Koposov, S. E., & Deason, A. J. 2018, MNRAS, 478, 611, doi: 10.1093/mnras/sty982
  * Belokurov et al. (2020) Belokurov, V., Penoyre, Z., Oh, S., et al. 2020, MNRAS, 496, 1922, doi: 10.1093/mnras/staa1522
  * Best et al. (2020) Best, W. M. J., Dupuy, T. J., Liu, M. C., Siverd, R. J., & Zhang, Z. 2020, The UltracoolSheet: Photometry, Astrometry, Spectroscopy, and Multiplicity for 3000+ Ultracool Dwarfs and Imaged Exoplanets, doi: 10.5281/zenodo.4169085
  * Best et al. (2021) Best, W. M. J., Liu, M. C., Magnier, E. A., & Dupuy, T. J. 2021, AJ, 161, 42, doi: 10.3847/1538-3881/abc893
  * Best et al. (2018) Best, W. M. J., Magnier, E. A., Liu, M. C., et al. 2018, ApJS, 234, 1, doi: 10.3847/1538-4365/aa9982
  * Bochanski et al. (2007) Bochanski, J. J., West, A. A., Hawley, S. L., & Covey, K. R. 2007, AJ, 133, 531, doi: 10.1086/510240
  * Burgasser et al. (2006) Burgasser, A. J., Kirkpatrick, J. D., Cruz, K. L., et al. 2006, ApJS, 166, 585, doi: 10.1086/506327
  * Burgasser et al. (2003) Burgasser, A. J., Kirkpatrick, J. D., Reid, I. N., et al. 2003, ApJ, 586, 512, doi: 10.1086/346263
  * Burgasser et al. (2004) Burgasser, A. J., McElwain, M. W., Kirkpatrick, J. D., et al. 2004, AJ, 127, 2856, doi: 10.1086/383549
  * Calissendorff et al. (2019) Calissendorff, P., Janson, M., Asensio-Torres, R., & Köhler, R. 2019, A&A, 627, A167, doi: 10.1051/0004-6361/201935319
  * Carnero Rosell et al. (2019) Carnero Rosell, A., Santiago, B., dal Ponte, M., et al. 2019, MNRAS, 489, 5301, doi: 10.1093/mnras/stz2398
  * Carollo et al. (2010) Carollo, D., Beers, T. C., Chiba, M., et al. 2010, ApJ, 712, 692, doi: 10.1088/0004-637X/712/1/692
  * Choi et al. (2016) Choi, J., Dotter, A., Conroy, C., et al. 2016, ApJ, 823, 102, doi: 10.3847/0004-637X/823/2/102
  * Close et al. (2003) Close, L. M., Siegler, N., Freed, M., & Biller, B. 2003, ApJ, 587, 407, doi: 10.1086/368177
  * Cummings et al. (2018) Cummings, J. D., Kalirai, J. S., Tremblay, P. E., Ramirez-Ruiz, E., & Choi, J. 2018, ApJ, 866, 21, doi: 10.3847/1538-4357/aadfd6
  * Cushing et al. (2004) Cushing, M. C., Vacca, W. D., & Rayner, J. T. 2004, PASP, 116, 362, doi: 10.1086/382907
  * Delfosse et al. (2004) Delfosse, X., Beuzit, J. L., Marchal, L., et al. 2004, in Astronomical Society of the Pacific Conference Series, Vol. 318, Spectroscopically and Spatially Resolving the Components of the Close Binary Stars, ed. R. W. Hilditch, H. Hensberge, & K. Pavlovski, 166–174
  * Dey et al. (2019) Dey, A., Schlegel, D. J., Lang, D., et al. 2019, AJ, 157, 168, doi: 10.3847/1538-3881/ab089d
  * Dotter (2016) Dotter, A. 2016, ApJS, 222, 8, doi: 10.3847/0067-0049/222/1/8
  * Dupuy & Kraus (2013) Dupuy, T. J., & Kraus, A. L. 2013, Science, 341, 1492, doi: 10.1126/science.1241917
  * Dupuy & Liu (2012) Dupuy, T. J., & Liu, M. C. 2012, ApJS, 201, 19, doi: 10.1088/0067-0049/201/2/19
  * Dupuy & Liu (2017) —. 2017, ApJS, 231, 15, doi: 10.3847/1538-4365/aa5e4c
  * Duquennoy & Mayor (1991) Duquennoy, A., & Mayor, M. 1991, A&A, 500, 337
  * Eggen (1976a) Eggen, O. J. 1976a, ApJS, 30, 351, doi: 10.1086/190366
  * Eggen (1976b) —. 1976b, ApJ, 204, 101, doi: 10.1086/154154
  * Faherty et al. (2010) Faherty, J. K., Burgasser, A. J., West, A. A., et al. 2010, AJ, 139, 176, doi: 10.1088/0004-6256/139/1/176
  * Faherty et al. (2020) Faherty, J. K., Goodman, S., Caselden, D., et al. 2020, ApJ, 889, 176, doi: 10.3847/1538-4357/ab5303
  * Faherty et al. (2021) Faherty, J. K., Gagné, J., Popinchalk, M., et al. 2021, ApJ, 923, 48, doi: 10.3847/1538-4357/ac2499
  * Fischer & Marcy (1992) Fischer, D. A., & Marcy, G. W. 1992, ApJ, 396, 178, doi: 10.1086/171708
  * Fontanive et al. (2018) Fontanive, C., Biller, B., Bonavita, M., & Allers, K. 2018, MNRAS, 479, 2702, doi: 10.1093/mnras/sty1682
  * Gagné et al. (2021) Gagné, J., Faherty, J. K., Schneider, A. C., & Meisner, A. M. 2021, CoMover: Bayesian probability of co-moving stars.  http://ascl.net/2106.007
  * Gelino et al. (2011) Gelino, C. R., Kirkpatrick, J. D., Cushing, M. C., et al. 2011, AJ, 142, 57, doi: 10.1088/0004-6256/142/2/57
  * Gentile Fusillo et al. (2021) Gentile Fusillo, N. P., Tremblay, P. E., Cukanovaite, E., et al. 2021, MNRAS, 508, 3877, doi: 10.1093/mnras/stab2672
  * Goodwin & Whitworth (2007) Goodwin, S. P., & Whitworth, A. 2007, A&A, 466, 943, doi: 10.1051/0004-6361:20066745
  * Hartman & Lépine (2020) Hartman, Z. D., & Lépine, S. 2020, ApJS, 247, 66, doi: 10.3847/1538-4365/ab79a6
  * Huélamo et al. (2015) Huélamo, N., Ivanov, V. D., Kurtev, R., et al. 2015, A&A, 578, A1, doi: 10.1051/0004-6361/201525634
  * Gaia Collaboration et al. (2016) Gaia Collaboration, Prusti, T., de Bruijne, J. H. J., et al. 2016, A&A, 595, A1, doi: 10.1051/0004-6361/201629272
  * Gaia Collaboration et al. (2018) Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2018, A&A, 616, A1, doi: 10.1051/0004-6361/201833051
  * Gaia Collaboration et al. (2021) —. 2021, A&A, 649, A1, doi: 10.1051/0004-6361/202039657
  * Janson et al. (2014) Janson, M., Bergfors, C., Brandner, W., et al. 2014, ApJ, 789, 102, doi: 10.1088/0004-637X/789/2/102
  * Kiman et al. (2019) Kiman, R., Schmidt, S. J., Angus, R., et al. 2019, AJ, 157, 231, doi: 10.3847/1538-3881/ab1753
  * Kirkpatrick et al. (2016) Kirkpatrick, J. D., Kellogg, K., Schneider, A. C., et al. 2016, ApJS, 224, 36, doi: 10.3847/0067-0049/224/2/36
  * Kiwy (2022) Kiwy, F. 2022, AstroToolBox: Java toolkit for identifying and classifying astronomical objects.  http://ascl.net/2201.002
  * Kiwy et al. (2021) Kiwy, F., Faherty, J., Meisner, A., et al. 2021, Research Notes of the American Astronomical Society, 5, 196, doi: 10.3847/2515-5172/ac1f9c
  * Kraus & Hillenbrand (2012) Kraus, A. L., & Hillenbrand, L. A. 2012, ApJ, 757, 141, doi: 10.1088/0004-637X/757/2/141
  * Kuchner et al. (2017) Kuchner, M. J., Faherty, J. K., Schneider, A. C., et al. 2017, ApJ, 841, L19, doi: 10.3847/2041-8213/aa7200
  * Lam et al. (2020) Lam, M. C., Hambly, N. C., Lodieu, N., et al. 2020, MNRAS, 493, 6001, doi: 10.1093/mnras/staa584
  * Law et al. (2010) Law, N. M., Dhital, S., Kraus, A., Stassun, K. G., & West, A. A. 2010, ApJ, 720, 1727, doi: 10.1088/0004-637X/720/2/1727
  * Liu et al. (2016) Liu, M. C., Dupuy, T. J., & Allers, K. N. 2016, ApJ, 833, 96, doi: 10.3847/1538-4357/833/1/96
  * Lu et al. (2021) Lu, Y. L., Angus, R., Curtis, J. L., David, T. J., & Kiman, R. 2021, AJ, 161, 189, doi: 10.3847/1538-3881/abe4d6
  * Luyten (1995) Luyten, W. J. 1995, VizieR Online Data Catalog, I/98A
  * Mamajek (2021) Mamajek, E. E. 2021, A Modern Mean Dwarf Stellar Color and Effective Temperature Sequence, 2021.03.02.  https://www.pas.rochester.edu/~emamajek/EEM_dwarf_UBVIJHK_colors_Teff.txt
  * Marocco et al. (2021) Marocco, F., Eisenhardt, P. R. M., Fowler, J. W., et al. 2021, ApJS, 253, 8, doi: 10.3847/1538-4365/abd805
  * Martín et al. (1999) Martín, E. L., Brandner, W., & Basri, G. 1999, Science, 283, 1718, doi: 10.1126/science.283.5408.1718
  * Martín et al. (1998) Martín, E. L., Basri, G., Brandner, W., et al. 1998, ApJ, 509, L113, doi: 10.1086/311775
  * Meisner et al. (2017) Meisner, A. M., Lang, D., & Schlegel, D. J. 2017, AJ, 154, 161, doi: 10.3847/1538-3881/aa894e
  * Meisner et al. (2018) —. 2018, AJ, 156, 69, doi: 10.3847/1538-3881/aacbcd
  * Nidever et al. (2021) Nidever, D. L., Dey, A., Fasbender, K., et al. 2021, AJ, 161, 192, doi: 10.3847/1538-3881/abd6e1
  * Ochsenbein et al. (2000) Ochsenbein, F., Bauer, P., & Marcout, J. 2000, A&AS, 143, 23, doi: 10.1051/aas:2000169
  * Paxton et al. (2011) Paxton, B., Bildsten, L., Dotter, A., et al. 2011, ApJS, 192, 3, doi: 10.1088/0067-0049/192/1/3
  * Paxton et al. (2013) Paxton, B., Cantiello, M., Arras, P., et al. 2013, ApJS, 208, 4, doi: 10.1088/0067-0049/208/1/4
  * Paxton et al. (2015) Paxton, B., Marchant, P., Schwab, J., et al. 2015, ApJS, 220, 15, doi: 10.1088/0067-0049/220/1/15
  * Penoyre et al. (2020) Penoyre, Z., Belokurov, V., Wyn Evans, N., Everall, A., & Koposov, S. E. 2020, MNRAS, 495, 321, doi: 10.1093/mnras/staa1148
  * Pokorny et al. (2003) Pokorny, R. S., Jones, H. R. A., & Hambly, N. C. 2003, A&A, 397, 575, doi: 10.1051/0004-6361:20021385
  * Raghavan et al. (2010) Raghavan, D., McAlister, H. A., Henry, T. J., et al. 2010, ApJS, 190, 1, doi: 10.1088/0067-0049/190/1/1
  * Reylé (2018) Reylé, C. 2018, A&A, 619, L8, doi: 10.1051/0004-6361/201834082
  * Salim & Gould (2003) Salim, S., & Gould, A. 2003, ApJ, 582, 1011, doi: 10.1086/344822
  * Skrzypek et al. (2016) Skrzypek, N., Warren, S. J., & Faherty, J. K. 2016, A&A, 589, A49, doi: 10.1051/0004-6361/201527359
  * Smart et al. (2019) Smart, R. L., Marocco, F., Sarro, L. M., et al. 2019, MNRAS, 485, 4423, doi: 10.1093/mnras/stz678
  * Stassun et al. (2019) Stassun, K. G., Oelkers, R. J., Paegert, M., et al. 2019, AJ, 158, 138, doi: 10.3847/1538-3881/ab3467
  * Sutherland et al. (2015) Sutherland, W., Emerson, J., Dalton, G., et al. 2015, A&A, 575, A25, doi: 10.1051/0004-6361/201424973
  * Vacca et al. (2003) Vacca, W. D., Cushing, M. C., & Rayner, J. T. 2003, PASP, 115, 389, doi: 10.1086/346193
  * Wenger et al. (2000) Wenger, M., Ochsenbein, F., Egret, D., et al. 2000, A&AS, 143, 9, doi: 10.1051/aas:2000332
  * Winters et al. (2019) Winters, J. G., Henry, T. J., Jao, W.-C., et al. 2019, AJ, 157, 216, doi: 10.3847/1538-3881/ab05dc
  * Wright et al. (2010) Wright, E. L., Eisenhardt, P. R. M., Mainzer, A. K., et al. 2010, AJ, 140, 1868, doi: 10.1088/0004-6256/140/6/1868
  * Wroblewski & Torres (1996) Wroblewski, H., & Torres, C. 1996, A&AS, 115, 481

=1cm

Table 7: Optical and infrared photometry

Sys. | C.a | GBP | G | GRP | rPS1 | iPS1 | zPS1 | yPS1 | rNSC | iNSC | zNSC | YNSC
---|---|---|---|---|---|---|---|---|---|---|---|---
# |  | J2M | H2M | Ks2M | JVHS | HVHS | KsVHS | W1A | W2A | W3A | W1C | W2C
|  | (mag) | (mag) | (mag) | (mag) | (mag) | (mag) | (mag) | (mag) | (mag) | (mag) | (mag)
1 | A | 20.314$\pm$ | 0.065 | 17.904$\pm$ | 0.003 | 16.491$\pm$ | 0.005 | 19.221$\pm$ | 0.008 | 17.174$\pm$ | 0.004 | 16.203$\pm$ | 0.003 | 15.702$\pm$ | 0.004 | 19.031$\pm$ | 0.003 | 16.947$\pm$ | 0.002 | 16.005$\pm$ | 0.001 | 15.643$\pm$ | 0.002
|  | 14.301$\pm$ | 0.029 | 13.688$\pm$ | 0.04 | 13.381$\pm$ | 0.034 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 13.208$\pm$ | 0.025 | 12.995$\pm$ | 0.03 |  $>$12.226 |  | 13.2$\pm$ | 0.013 | 12.995$\pm$ | 0.011
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 22.159$\pm$ | 0.343 | 21.797$\pm$ | 0.183 | 20.609$\pm$ | 0.129 | 19.641$\pm$ | 0.052 |  $\cdots$ |  | 21.821$\pm$ | 0.033 | 20.288$\pm$ | 0.015 | 19.696$\pm$ | 0.03
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.278$\pm$ | 0.039 | 15.137$\pm$ | 0.1 |  $>$12.551 |  | 15.373$\pm$ | 0.021 | 15.138$\pm$ | 0.031
2 | A | 20.79$\pm$ | 0.103 | 17.983$\pm$ | 0.003 | 16.495$\pm$ | 0.006 | 19.822$\pm$ | 0.015 | 17.256$\pm$ | 0.005 | 16.147$\pm$ | 0.003 | 15.566$\pm$ | 0.004 | 19.519$\pm$ | 0.004 | 16.944$\pm$ | 0.002 | 15.879$\pm$ | 0.001 | 15.528$\pm$ | 0.002
|  | 14.118$\pm$ | 0.03 | 13.576$\pm$ | 0.029 | 13.307$\pm$ | 0.033 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 13.004$\pm$ | 0.025 | 12.788$\pm$ | 0.026 |  $>$12.514 |  |  $\cdots$ |  |  $\cdots$ |
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.238$\pm$ | 0.033 | 20.145$\pm$ | 0.044
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.575$\pm$ | 0.075 | 15.91$\pm$ | 0.057
3 | A | 21.476$\pm$ | 0.216 | 20.34$\pm$ | 0.006 | 19.048$\pm$ | 0.045 | 21.698$\pm$ | 0.041 | 19.564$\pm$ | 0.015 | 18.613$\pm$ | 0.018 | 18.174$\pm$ | 0.018 | 21.477$\pm$ | 0.014 | 19.415$\pm$ | 0.003 | 18.484$\pm$ | 0.002 | 18.128$\pm$ | 0.011
|  | 16.766$\pm$ | 0.144 |  $>$15.939 |  |  $>$15.37 |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.465$\pm$ | 0.043 | 15.231$\pm$ | 0.104 |  $>$12.139 |  | 15.824$\pm$ | 0.081 | 15.684$\pm$ | 0.098
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 20.648$\pm$ | 0.018 | 19.405$\pm$ | 0.035 | 18.863$\pm$ | 0.02 | 22.883$\pm$ | 0.045 | 20.408$\pm$ | 0.005 | 19.229$\pm$ | 0.004 | 18.827$\pm$ | 0.019
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.479$\pm$ | 0.037 | 16.281$\pm$ | 0.085
4 | A | 18.001$\pm$ | 0.011 | 16.487$\pm$ | 0.003 | 15.289$\pm$ | 0.004 | 17.13$\pm$ | 0.002 | 15.771$\pm$ | 0.006 | 15.168$\pm$ | 0.005 | 14.853$\pm$ | 0.006 | 17.021$\pm$ | 0.001 |  $\cdots$ |  | 15.059$\pm$ | 0.001 | 14.796$\pm$ | 0.001
|  | 13.599$\pm$ | 0.026 | 12.968$\pm$ | 0.023 | 12.804$\pm$ | 0.027 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 12.585$\pm$ | 0.024 | 12.47$\pm$ | 0.024 | 12.619$\pm$ | 0.526 | 12.66$\pm$ | 0.014 | 12.511$\pm$ | 0.013
| B | 21.562$\pm$ | 0.183 | 21.128$\pm$ | 0.021 | 19.481$\pm$ | 0.167 |  $\cdots$ |  | 20.572$\pm$ | 0.036 | 19.169$\pm$ | 0.017 | 18.328$\pm$ | 0.019 | 22.863$\pm$ | 0.045 | 20.189$\pm$ | 0.005 | 18.781$\pm$ | 0.002 | 18.203$\pm$ | 0.005
|  | 16.586$\pm$ | 0.114 | 15.862$\pm$ | 0.181 |  $>$14.405 |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.245$\pm$ | 0.049 | 15.234$\pm$ | 0.052
5 | A | 14.78$\pm$ | 0.003 | 13.697$\pm$ | 0.003 | 12.662$\pm$ | 0.004 | 13.958$\pm$ | 0.003 | 13.104$\pm$ | 0.022 | 12.712$\pm$ | $\cdots$ | 12.475$\pm$ | 0.001 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |
|  | 11.348$\pm$ | 0.021 | 10.753$\pm$ | 0.022 | 10.535$\pm$ | 0.021 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 10.395$\pm$ | 0.023 | 10.307$\pm$ | 0.019 | 10.185$\pm$ | 0.064 | 10.414$\pm$ | 0.012 | 10.312$\pm$ | 0.008
| B | 21.549$\pm$ | 0.261 | 20.745$\pm$ | 0.01 | 19.128$\pm$ | 0.048 |  $\cdots$ |  |  $\cdots$ |  | 18.614$\pm$ | 0.05 | 17.557$\pm$ | 0.042 | 23.131$\pm$ | 0.042 | 19.676$\pm$ | 0.006 | 18.18$\pm$ | 0.004 | 17.674$\pm$ | 0.007
|  | 15.996$\pm$ | 0.12 | 15.418$\pm$ | 0.269 | 14.854$\pm$ | 0.137 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |
6 | A | 16.744$\pm$ | 0.005 | 15.396$\pm$ | 0.003 | 14.252$\pm$ | 0.004 | 15.908$\pm$ | 0.002 | 14.717$\pm$ | 0.002 | 14.183$\pm$ | 0.003 | 13.926$\pm$ | 0.004 | 15.81$\pm$ | 0.003 | 14.629$\pm$ | 0.003 | 14.086$\pm$ | 0.002 | 13.859$\pm$ | 0.002
|  | 12.88$\pm$ | 0.03 | 12.178$\pm$ | 0.035 | 11.902$\pm$ | 0.029 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 11.669$\pm$ | 0.023 | 11.595$\pm$ | 0.022 | 11.477$\pm$ | 0.193 | 11.633$\pm$ | 0.011 | 11.591$\pm$ | 0.008
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 20.815$\pm$ | 0.053 | 19.479$\pm$ | 0.016 | 18.618$\pm$ | 0.027 | 22.797$\pm$ | 0.166 | 20.541$\pm$ | 0.014 | 19.098$\pm$ | 0.007 | 18.546$\pm$ | 0.023
|  | 17.153$\pm$ | 0.235 | 16.388$\pm$ | 0.248 | 15.454$\pm$ | 0.205 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.351$\pm$ | 0.039 | 15.312$\pm$ | 0.051
7 | A | 18.023$\pm$ | 0.008 | 16.489$\pm$ | 0.003 | 15.281$\pm$ | 0.004 | 17.19$\pm$ | 0.004 | 15.782$\pm$ | 0.002 | 15.157$\pm$ | 0.002 | 14.857$\pm$ | 0.002 | 17.034$\pm$ | 0.002 | 15.661$\pm$ | 0.002 | 15.06$\pm$ | 0.001 | 14.811$\pm$ | 0.001
|  | 13.679$\pm$ | 0.03 | 13.141$\pm$ | 0.031 | 12.905$\pm$ | 0.031 | 13.598$\pm$ | 0.002 | 13.154$\pm$ | 0.002 | 12.892$\pm$ | 0.003 | 12.732$\pm$ | 0.023 | 12.504$\pm$ | 0.024 | 12.237$\pm$ | 0.413 | 12.707$\pm$ | 0.014 | 12.524$\pm$ | 0.01
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.095$\pm$ | 0.139 | 19.593$\pm$ | 0.134 |  $\cdots$ |  | 22.865$\pm$ | 0.095 | 21.032$\pm$ | 0.039 | 20.29$\pm$ | 0.071
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 18.359$\pm$ | 0.046 | 17.933$\pm$ | 0.066 | 17.176$\pm$ | 0.085 | 16.213$\pm$ | 0.062 | 16.274$\pm$ | 0.217 | 12.404$\pm$ | 0.454 | 16.656$\pm$ | 0.043 | 16.998$\pm$ | 0.168
8 | A | 15.326$\pm$ | 0.004 | 14.455$\pm$ | 0.003 | 13.532$\pm$ | 0.004 | 14.554$\pm$ | 0.004 | 13.931$\pm$ | 0.002 | 13.653$\pm$ | 0.003 | 13.486$\pm$ | 0.001 | 14.513$\pm$ | 0.002 |  $\cdots$ |  |  $\cdots$ |  | 13.413$\pm$ | 0.002
|  | 12.378$\pm$ | 0.023 | 11.739$\pm$ | 0.022 | 11.545$\pm$ | 0.019 | 12.467$\pm$ | 0.001 | 12.007$\pm$ | 0.001 | 11.63$\pm$ | 0.001 | 11.466$\pm$ | 0.023 | 11.434$\pm$ | 0.022 | 11.601$\pm$ | 0.186 | 11.483$\pm$ | 0.013 | 11.443$\pm$ | 0.009
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.001$\pm$ | 0.01 | 19.302$\pm$ | 0.006 | 18.486$\pm$ | 0.011
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.181$\pm$ | 0.012 | 16.635$\pm$ | 0.015 | 16.322$\pm$ | 0.025 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |
9 | A | 15.105$\pm$ | 0.003 | 14.36$\pm$ | 0.003 | 13.514$\pm$ | 0.004 | 14.388$\pm$ | 0.001 | 13.903$\pm$ | 0.002 | 13.689$\pm$ | 0.004 | 13.559$\pm$ | 0.002 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 13.502$\pm$ | 0.001
|  | 12.467$\pm$ | 0.024 | 11.813$\pm$ | 0.022 | 11.661$\pm$ | 0.021 | 12.484$\pm$ | 0.001 |  $\cdots$ |  | 11.672$\pm$ | 0.001 | 11.632$\pm$ | 0.023 | 11.633$\pm$ | 0.022 | 11.344$\pm$ | 0.151 | 11.618$\pm$ | 0.012 | 11.629$\pm$ | 0.009
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.343$\pm$ | 0.197 | 20.17$\pm$ | 0.144 |  $\cdots$ |  | 22.896$\pm$ | 0.056 | 21.084$\pm$ | 0.029 | 20.623$\pm$ | 0.057
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 18.781$\pm$ | 0.053 |  $\cdots$ |  | 17.728$\pm$ | 0.121 | 17.589$\pm$ | 0.168 | 16.659$\pm$ | 0.274 |  $>$12.722 |  | 17.405$\pm$ | 0.071 | 16.842$\pm$ | 0.131
10 | A | 14.843$\pm$ | 0.003 | 13.666$\pm$ | 0.003 | 12.587$\pm$ | 0.004 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 12.344$\pm$ | 0.002
|  | 11.212$\pm$ | 0.022 | 10.607$\pm$ | 0.027 | 10.384$\pm$ | 0.021 | 12.176$\pm$ | 0.001 | 12.859$\pm$ | 0.002 | 11.559$\pm$ | 0.001 | 10.218$\pm$ | 0.023 | 10.114$\pm$ | 0.02 | 9.924$\pm$ | 0.049 | 10.235$\pm$ | 0.012 | 10.128$\pm$ | 0.008
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 22.485$\pm$ | 0.049 | 20.613$\pm$ | 0.022 | 20.126$\pm$ | 0.048
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.928$\pm$ | 0.045 | 17.092$\pm$ | 0.039 | 16.499$\pm$ | 0.044 | 15.677$\pm$ | 0.042 | 15.302$\pm$ | 0.077 |  $>$12.542 |  | 15.754$\pm$ | 0.02 | 15.538$\pm$ | 0.037
11 | A | 21.161$\pm$ | 0.244 | 20.374$\pm$ | 0.007 | 18.853$\pm$ | 0.043 | 18.805$\pm$ | $\cdots$ | 19.7$\pm$ | 0.009 | 18.519$\pm$ | 0.016 | 17.877$\pm$ | 0.011 | 22.205$\pm$ | 0.018 | 19.411$\pm$ | 0.005 | 18.27$\pm$ | 0.003 | 17.859$\pm$ | 0.013
|  | 16.219$\pm$ | 0.095 | 15.645$\pm$ | 0.114 | 15.432$\pm$ | 0.16 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.312$\pm$ | 0.038 | 15.079$\pm$ | 0.077 |  $>$12.66 |  | 15.293$\pm$ | 0.02 | 15.116$\pm$ | 0.033
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 22.094$\pm$ | 0.062 |  $\cdots$ |
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.519$\pm$ | 0.092 | 16.971$\pm$ | 0.163
12 | A | 20.823$\pm$ | 0.146 | 19.099$\pm$ | 0.004 | 17.703$\pm$ | 0.014 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 20.01$\pm$ | 0.005 | 18.048$\pm$ | 0.002 | 17.203$\pm$ | 0.002 | 16.944$\pm$ | 0.003
|  | 15.693$\pm$ | 0.062 | 15.243$\pm$ | 0.098 | 14.685$\pm$ | 0.122 | 15.575$\pm$ | 0.005 |  $\cdots$ |  | 14.766$\pm$ | 0.01 | 14.564$\pm$ | 0.028 | 14.355$\pm$ | 0.036 |  $>$12.835 |  | 14.516$\pm$ | 0.014 | 14.346$\pm$ | 0.014
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 22.347$\pm$ | 0.04 | 20.848$\pm$ | 0.022 | 20.367$\pm$ | 0.044
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 18.494$\pm$ | 0.051 |  $\cdots$ |  | 17.375$\pm$ | 0.092 | 17.014$\pm$ | 0.079 | 16.698$\pm$ | 0.202 |  $>$12.674 |  | 16.898$\pm$ | 0.034 | 16.678$\pm$ | 0.082
13 | A | 16.142$\pm$ | 0.005 | 14.725$\pm$ | 0.003 | 13.551$\pm$ | 0.004 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.151$\pm$ | 0.001 |  $\cdots$ |  |  $\cdots$ |  | 13.137$\pm$ | 0.002
|  | 11.964$\pm$ | 0.026 | 11.372$\pm$ | 0.025 | 11.108$\pm$ | 0.021 | 11.949$\pm$ | 0.001 |  $\cdots$ |  | 11.188$\pm$ | 0.001 | 10.943$\pm$ | 0.022 | 10.783$\pm$ | 0.02 | 10.653$\pm$ | 0.081 | 10.884$\pm$ | 0.01 | 10.777$\pm$ | 0.007
| B | 21.516$\pm$ | 0.188 | 20.975$\pm$ | 0.012 | 19.365$\pm$ | 0.117 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 22.223$\pm$ | 0.045 | 19.867$\pm$ | 0.005 | 18.313$\pm$ | 0.004 | 17.432$\pm$ | 0.007
|  | 16.127$\pm$ | 0.112 | 15.417$\pm$ | 0.128 | 15.01$\pm$ | 0.121 | 16.149$\pm$ | 0.006 |  $\cdots$ |  | 15.066$\pm$ | 0.01 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.037$\pm$ | 0.036 | 14.63$\pm$ | 0.034
14 | A | 19.859$\pm$ | 0.064 | 17.536$\pm$ | 0.007 | 16.044$\pm$ | 0.008 | 18.838$\pm$ | 0.003 | 16.711$\pm$ | 0.003 | 15.765$\pm$ | 0.003 | 15.281$\pm$ | 0.005 | 18.63$\pm$ | 0.002 | 16.509$\pm$ | 0.001 | 15.582$\pm$ | 0.001 | 15.225$\pm$ | 0.001
|  | 13.914$\pm$ | 0.03 | 13.352$\pm$ | 0.029 | 13.013$\pm$ | 0.033 | 13.824$\pm$ | 0.002 | 13.332$\pm$ | 0.002 | 13.004$\pm$ | 0.003 | 12.778$\pm$ | 0.023 | 12.547$\pm$ | 0.025 | 11.877$\pm$ | 0.203 | 12.788$\pm$ | 0.011 | 12.56$\pm$ | 0.01
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 20.784$\pm$ | 0.202 | 19.466$\pm$ | 0.176 |  $\cdots$ |  | 22.787$\pm$ | 0.091 | 20.742$\pm$ | 0.026 | 20.023$\pm$ | 0.055
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 18.07$\pm$ | 0.036 | 17.403$\pm$ | 0.04 | 16.787$\pm$ | 0.048 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.173$\pm$ | 0.052 | 15.958$\pm$ | 0.077
15 | A | 17.371$\pm$ | 0.01 | 16.332$\pm$ | 0.003 | 15.325$\pm$ | 0.005 | 16.543$\pm$ | 0.002 | 15.737$\pm$ | 0.003 | 15.363$\pm$ | 0.002 | 15.162$\pm$ | 0.005 | 16.507$\pm$ | 0.002 | 15.698$\pm$ | 0.001 | 15.331$\pm$ | 0.001 | 15.14$\pm$ | 0.001
|  | 14.024$\pm$ | 0.028 | 13.47$\pm$ | 0.03 | 13.312$\pm$ | 0.034 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 13.152$\pm$ | 0.023 | 13.007$\pm$ | 0.029 |  $>$12.254 |  | 13.15$\pm$ | 0.013 | 13.04$\pm$ | 0.011
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.527$\pm$ | 0.038 | 20.078$\pm$ | 0.016 | 19.657$\pm$ | 0.04
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |
16 | A | 16.233$\pm$ | 0.005 | 15.141$\pm$ | 0.003 | 14.099$\pm$ | 0.004 | 15.432$\pm$ | 0.002 | 14.525$\pm$ | 0.003 | 14.098$\pm$ | 0.004 | 13.89$\pm$ | 0.003 | 15.37$\pm$ | 0.002 |  $\cdots$ |  | 14.039$\pm$ | 0.002 | 13.857$\pm$ | 0.001
|  | 12.749$\pm$ | 0.022 | 12.196$\pm$ | 0.026 | 12.031$\pm$ | 0.023 | 12.73$\pm$ | 0.001 |  $\cdots$ |  | 11.981$\pm$ | 0.002 | 11.871$\pm$ | 0.023 | 11.729$\pm$ | 0.021 | 11.679$\pm$ | 0.164 | 11.799$\pm$ | 0.011 | 11.73$\pm$ | 0.009
| B | 19.444$\pm$ | 1.812 | 20.911$\pm$ | 0.018 | 19.237$\pm$ | 0.079 |  $\cdots$ |  | 20.172$\pm$ | 0.024 | 18.907$\pm$ | 0.017 | 18.202$\pm$ | 0.008 | 22.37$\pm$ | 0.061 | 19.876$\pm$ | 0.007 | 18.631$\pm$ | 0.005 | 18.158$\pm$ | 0.011
|  | 16.651$\pm$ | 0.178 |  $>$14.644 |  |  $>$14.182 |  | 16.737$\pm$ | 0.01 |  $\cdots$ |  | 15.97$\pm$ | 0.035 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |
17 | A | 17.794$\pm$ | 0.012 | 16.382$\pm$ | 0.003 | 15.226$\pm$ | 0.005 | 16.938$\pm$ | 0.002 | 15.691$\pm$ | 0.002 | 15.13$\pm$ | 0.003 | 14.856$\pm$ | 0.006 | 16.842$\pm$ | 0.002 | 15.58$\pm$ | 0.001 | 15.051$\pm$ | 0.001 | 14.82$\pm$ | 0.001
|  | 13.705$\pm$ | 0.029 | 13.156$\pm$ | 0.03 | 12.956$\pm$ | 0.033 | 13.615$\pm$ | 0.002 |  $\cdots$ |  | 12.915$\pm$ | 0.002 | 12.764$\pm$ | 0.024 | 12.545$\pm$ | 0.023 | 12.255$\pm$ | 0.256 | 12.809$\pm$ | 0.016 | 12.6$\pm$ | 0.012
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.261$\pm$ | 0.037 | 19.878$\pm$ | 0.02 | 18.913$\pm$ | 0.042 |  $\cdots$ |  | 20.983$\pm$ | 0.021 | 19.419$\pm$ | 0.009 | 18.654$\pm$ | 0.021
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.137$\pm$ | 0.013 |  $\cdots$ |  | 16.283$\pm$ | 0.032 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.58$\pm$ | 0.042 | 15.292$\pm$ | 0.05
18 | A | 21.215$\pm$ | 0.1 | 19.343$\pm$ | 0.003 | 17.989$\pm$ | 0.013 | 20.681$\pm$ | 0.039 | 18.589$\pm$ | 0.007 | 17.692$\pm$ | 0.005 | 17.28$\pm$ | 0.013 | 20.474$\pm$ | 0.007 | 18.383$\pm$ | 0.003 | 17.548$\pm$ | 0.002 | 17.238$\pm$ | 0.005
|  | 16.007$\pm$ | 0.087 | 15.324$\pm$ | 0.097 | 15.199$\pm$ | 0.181 | 15.902$\pm$ | 0.005 |  $\cdots$ |  | 15.174$\pm$ | 0.011 | 14.816$\pm$ | 0.03 | 14.453$\pm$ | 0.044 |  $>$12.711 |  | 14.793$\pm$ | 0.02 | 14.578$\pm$ | 0.024
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.338$\pm$ | 0.179 |  $\cdots$ |  | 19.292$\pm$ | 0.016 |  $\cdots$ |  | 21.485$\pm$ | 0.022 | 19.79$\pm$ | 0.01 | 19.252$\pm$ | 0.024
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.504$\pm$ | 0.016 |  $\cdots$ |  | 16.703$\pm$ | 0.041 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.845$\pm$ | 0.051 | 16.738$\pm$ | 0.13
19 | A | 17.12$\pm$ | 0.005 | 15.791$\pm$ | 0.003 | 14.653$\pm$ | 0.004 | 16.315$\pm$ | 0.004 | 15.112$\pm$ | 0.002 | 14.544$\pm$ | 0.003 | 14.309$\pm$ | 0.002 | 16.219$\pm$ | 0.002 | 15.016$\pm$ | 0.004 | 14.508$\pm$ | 0.002 | 14.266$\pm$ | 0.002
|  | 13.206$\pm$ | 0.029 | 12.655$\pm$ | 0.029 | 12.478$\pm$ | 0.027 | 13.137$\pm$ | 0.001 |  $\cdots$ |  | 12.484$\pm$ | 0.002 | 12.244$\pm$ | 0.062 | 12.065$\pm$ | 0.022 | 11.976$\pm$ | 0.262 | 12.256$\pm$ | 0.012 | 12.094$\pm$ | 0.009
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 20.845$\pm$ | 0.036 | 19.303$\pm$ | 0.027 | 18.401$\pm$ | 0.064 | 23.34$\pm$ | 0.077 | 20.535$\pm$ | 0.012 | 18.984$\pm$ | 0.006 | 18.446$\pm$ | 0.018
|  | 16.631$\pm$ | 0.148 | 15.883$\pm$ | 0.195 |  $>$15.028 |  | 16.794$\pm$ | 0.009 |  $\cdots$ |  | 15.972$\pm$ | 0.024 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.509$\pm$ | 0.031 | 15.043$\pm$ | 0.037
20 | A | 17.208$\pm$ | 0.005 | 15.813$\pm$ | 0.003 | 14.656$\pm$ | 0.004 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.209$\pm$ | 0.002 |  $\cdots$ |  |  $\cdots$ |  | 14.288$\pm$ | 0.001
|  | 13.096$\pm$ | 0.026 | 12.533$\pm$ | 0.022 | 12.287$\pm$ | 0.023 | 13.081$\pm$ | 0.001 |  $\cdots$ |  | 12.333$\pm$ | 0.002 | 12.139$\pm$ | 0.214 | 11.941$\pm$ | 0.022 | 11.873$\pm$ | 0.204 | 12.15$\pm$ | 0.013 | 11.987$\pm$ | 0.009
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 22.723$\pm$ | 0.064 | 20.934$\pm$ | 0.034 | 20.393$\pm$ | 0.059
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 18.268$\pm$ | 0.033 |  $\cdots$ |  | 17.08$\pm$ | 0.062 | 16.12$\pm$ | 0.524 | 16.166$\pm$ | 0.145 |  $>$12.897 |  | 16.353$\pm$ | 0.028 | 16.209$\pm$ | 0.064
21 | A | 16.38$\pm$ | 0.004 | 14.902$\pm$ | 0.003 | 13.718$\pm$ | 0.004 | 15.493$\pm$ | 0.004 | 14.204$\pm$ | 0.004 | 13.622$\pm$ | 0.004 | 13.33$\pm$ | 0.003 | 15.383$\pm$ | 0.002 | 14.047$\pm$ | 0.003 | 13.504$\pm$ | 0.002 | 13.242$\pm$ | 0.002
|  | 12.138$\pm$ | 0.023 | 11.6$\pm$ | 0.028 | 11.299$\pm$ | 0.025 | 12.072$\pm$ | 0.001 |  $\cdots$ |  | 11.295$\pm$ | 0.001 | 11.125$\pm$ | 0.023 | 10.947$\pm$ | 0.02 | 10.866$\pm$ | 0.081 | 11.125$\pm$ | 0.012 | 10.957$\pm$ | 0.009
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 19.657$\pm$ | 0.159 |  $\cdots$ |  |  $\cdots$ |  | 20.563$\pm$ | 0.017 | 19.641$\pm$ | 0.027
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.482$\pm$ | 0.016 |  $\cdots$ |  | 16.864$\pm$ | 0.053 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.121$\pm$ | 0.028 | 15.247$\pm$ | 0.031
22 | A | 16.287$\pm$ | 0.004 | 14.888$\pm$ | 0.003 | 13.728$\pm$ | 0.004 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.306$\pm$ | 0.003 |  $\cdots$ |  |  $\cdots$ |  | 13.343$\pm$ | 0.001
|  | 12.177$\pm$ | 0.023 | 11.643$\pm$ | 0.022 | 11.343$\pm$ | 0.019 | 12.44$\pm$ | 0.001 |  $\cdots$ |  | 11.646$\pm$ | 0.001 | 11.205$\pm$ | 0.023 | 11.041$\pm$ | 0.021 | 11.02$\pm$ | 0.079 | 11.142$\pm$ | 0.01 | 11.032$\pm$ | 0.008
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 22.87$\pm$ | 0.074 | 20.439$\pm$ | 0.012 | 18.955$\pm$ | 0.008 | 18.089$\pm$ | 0.014
|  | 16.516$\pm$ | 0.145 | 15.77$\pm$ | 0.147 | 15.314$\pm$ | 0.157 | 16.466$\pm$ | 0.007 |  $\cdots$ |  | 15.4$\pm$ | 0.015 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.098$\pm$ | 0.027 | 14.808$\pm$ | 0.028
23 | A | 20.287$\pm$ | 0.111 | 18.405$\pm$ | 0.003 | 17.092$\pm$ | 0.011 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 19.248$\pm$ | 0.003 | 17.446$\pm$ | 0.001 | 16.676$\pm$ | 0.001 | 16.447$\pm$ | 0.002
|  | 15.219$\pm$ | 0.049 | 14.59$\pm$ | 0.057 | 14.487$\pm$ | 0.081 | 15.071$\pm$ | 0.003 |  $\cdots$ |  | 14.335$\pm$ | 0.006 | 14.156$\pm$ | 0.025 | 13.924$\pm$ | 0.033 |  $>$13.003 |  | 14.182$\pm$ | 0.014 | 13.977$\pm$ | 0.012
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 23.424$\pm$ | 0.06 | 20.455$\pm$ | 0.005 | 19.041$\pm$ | 0.005 | 18.622$\pm$ | 0.011
|  | 17.193$\pm$ | 0.217 | 16.583$\pm$ | 0.261 | 15.615$\pm$ | 0.218 | 16.911$\pm$ | 0.011 |  $\cdots$ |  | 15.984$\pm$ | 0.025 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.813$\pm$ | 0.02 | 15.587$\pm$ | 0.031
24 | A | 17.021$\pm$ | 0.006 | 15.334$\pm$ | 0.003 | 14.091$\pm$ | 0.004 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.968$\pm$ | $\cdots$ |  $\cdots$ |  |  $\cdots$ |  | 13.566$\pm$ | 0.001
|  | 12.333$\pm$ | 0.023 | 11.782$\pm$ | 0.024 | 11.501$\pm$ | 0.025 | 12.295$\pm$ | 0.001 |  $\cdots$ |  | 11.543$\pm$ | 0.001 | 11.336$\pm$ | 0.024 | 11.142$\pm$ | 0.02 | 11.047$\pm$ | 0.082 | 11.297$\pm$ | 0.01 | 11.141$\pm$ | 0.008
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.09$\pm$ | 0.026 | 20.484$\pm$ | 0.066
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 18.318$\pm$ | 0.037 |  $\cdots$ |  | 16.782$\pm$ | 0.054 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.818$\pm$ | 0.021 | 15.46$\pm$ | 0.03
25 | A | 20.505$\pm$ | 0.077 | 20.017$\pm$ | 0.006 | 19.405$\pm$ | 0.08 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 20.044$\pm$ | 0.005 | 19.879$\pm$ | 0.007 | 19.876$\pm$ | 0.012 | 19.952$\pm$ | 0.042
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 19.009$\pm$ | 0.052 | 18.695$\pm$ | 0.088 | 18.521$\pm$ | 0.196 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 23.344$\pm$ | 0.189 | 21.694$\pm$ | 0.047 | 20.859$\pm$ | 0.12
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 18.922$\pm$ | 0.049 | 18.206$\pm$ | 0.057 | 17.432$\pm$ | 0.073 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.892$\pm$ | 0.031 | 16.485$\pm$ | 0.062
26 | A | 16.154$\pm$ | 0.005 | 14.517$\pm$ | 0.003 | 13.285$\pm$ | 0.004 | 15.275$\pm$ | 0.003 | 13.79$\pm$ | 0.002 | 13.132$\pm$ | 0.001 | 12.832$\pm$ | 0.003 | 15.107$\pm$ | 0.001 | 13.636$\pm$ | 0.001 | 13.027$\pm$ | 0.003 | 12.738$\pm$ | 0.002
|  | 11.588$\pm$ | 0.023 | 10.978$\pm$ | 0.024 | 10.704$\pm$ | 0.021 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 10.549$\pm$ | 0.022 | 10.379$\pm$ | 0.02 | 10.225$\pm$ | 0.079 | 10.428$\pm$ | 0.01 | 10.335$\pm$ | 0.007
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.172$\pm$ | 0.05 | 19.602$\pm$ | 0.025 | 18.586$\pm$ | 0.018 | 22.875$\pm$ | 0.173 | 20.639$\pm$ | 0.029 | 19.118$\pm$ | 0.007 | 18.468$\pm$ | 0.041
|  | 16.563$\pm$ | 0.147 | 15.566$\pm$ | 0.113 | 14.754$\pm$ | 0.127 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 14.074$\pm$ | 0.138 | 13.963$\pm$ | 0.141 |  $>$12.058 |  | 14.272$\pm$ | 0.02 | 14.077$\pm$ | 0.02
27 | A | 20.964$\pm$ | 0.155 | 20.459$\pm$ | 0.008 | 19.939$\pm$ | 0.115 | 20.366$\pm$ | 0.027 | 20.154$\pm$ | 0.023 | 20.021$\pm$ | 0.03 | 19.827$\pm$ | 0.07 | 20.476$\pm$ | 0.006 | 20.241$\pm$ | 0.005 | 20.151$\pm$ | 0.008 | 20.004$\pm$ | 0.016
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 19.203$\pm$ | 0.144 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.451$\pm$ | 0.053 | 20.208$\pm$ | 0.035 | 19.195$\pm$ | 0.028 |  $\cdots$ |  | 21.279$\pm$ | 0.013 | 19.732$\pm$ | 0.006 | 19.117$\pm$ | 0.008
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.379$\pm$ | 0.028 |  $\cdots$ |  | 16.329$\pm$ | 0.053 | 15.862$\pm$ | 0.049 | 15.51$\pm$ | 0.109 |  $>$12.796 |  | 15.929$\pm$ | 0.026 | 15.623$\pm$ | 0.048
28 | A | 14.234$\pm$ | 0.003 | 13.083$\pm$ | 0.003 | 12.017$\pm$ | 0.004 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 13.328$\pm$ | 0.008 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |
|  | 10.633$\pm$ | 0.026 | 10$\pm$ | 0.026 | 9.768$\pm$ | 0.021 | 11.202$\pm$ | 0.001 |  $\cdots$ |  | 10.49$\pm$ | 0.001 | 9.639$\pm$ | 0.022 | 9.576$\pm$ | 0.021 | 9.406$\pm$ | 0.036 | 9.645$\pm$ | 0.013 | 9.586$\pm$ | 0.009
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 22.795$\pm$ | 0.033 | 20.189$\pm$ | 0.007 | 18.7$\pm$ | 0.003 | 18.196$\pm$ | 0.011
|  | 16.322$\pm$ | 0.105 | 15.412$\pm$ | 0.092 | 15.023$\pm$ | 0.128 | 16.137$\pm$ | 0.013 |  $\cdots$ |  | 14.9$\pm$ | 0.016 | 14.516$\pm$ | 0.03 | 14.387$\pm$ | 0.045 |  $>$12.574 |  | 14.493$\pm$ | 0.017 | 14.324$\pm$ | 0.019
29 | A | 17.269$\pm$ | 0.008 | 15.645$\pm$ | 0.003 | 14.418$\pm$ | 0.004 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.264$\pm$ | 0.001 |  $\cdots$ |  |  $\cdots$ |  | 13.914$\pm$ | 0.003
|  | 12.657$\pm$ | 0.024 | 12.162$\pm$ | 0.022 | 11.889$\pm$ | 0.027 | 12.646$\pm$ | 0.001 | 12.221$\pm$ | 0.001 | 11.929$\pm$ | 0.001 | 11.708$\pm$ | 0.022 | 11.568$\pm$ | 0.021 | 11.594$\pm$ | 0.224 |  $\cdots$ |  |  $\cdots$ |
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 23.413$\pm$ | 0.068 | 20.94$\pm$ | 0.018 | 19.395$\pm$ | 0.01 | 18.86$\pm$ | 0.03
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.939$\pm$ | 0.018 | 16.211$\pm$ | 0.02 | 15.764$\pm$ | 0.021 | 16.226$\pm$ | 0.056 | 15.824$\pm$ | 0.137 |  $>$12.081 |  | 15.364$\pm$ | 0.021 | 15.579$\pm$ | 0.055
30 | A | 18.678$\pm$ | 0.019 | 16.716$\pm$ | 0.003 | 15.398$\pm$ | 0.004 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.533$\pm$ | 0.001 | 15.777$\pm$ | 0.001 | 14.98$\pm$ | 0.001 | 14.729$\pm$ | 0.001
|  | 13.465$\pm$ | 0.029 | 12.875$\pm$ | 0.032 | 12.584$\pm$ | 0.037 | 13.341$\pm$ | 0.001 | 12.85$\pm$ | 0.002 | 12.544$\pm$ | 0.002 | 12.262$\pm$ | 0.023 | 12.083$\pm$ | 0.023 | 11.634$\pm$ | 0.249 | 12.223$\pm$ | 0.01 | 12.081$\pm$ | 0.008
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 22.81$\pm$ | 0.056 | 20.423$\pm$ | 0.013 | 18.995$\pm$ | 0.008 | 18.395$\pm$ | 0.014
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.61$\pm$ | 0.012 | 15.971$\pm$ | 0.014 | 15.472$\pm$ | 0.015 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |
31 | A | 17.61$\pm$ | 0.007 | 15.668$\pm$ | 0.004 | 14.245$\pm$ | 0.004 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.452$\pm$ | 0.001 |  $\cdots$ |  | 13.795$\pm$ | 0.001 | 13.516$\pm$ | 0.001
|  | 16.168$\pm$ | 0.105 | 15.371$\pm$ | 0.126 | 14.611$\pm$ | 0.084 | 12.267$\pm$ | 0.001 |  $\cdots$ |  | 11.417$\pm$ | 0.001 | 11.103$\pm$ | 0.025 | 10.928$\pm$ | 0.023 | 10.827$\pm$ | 0.102 | 11.136$\pm$ | 0.014 | 10.967$\pm$ | 0.01
| B |  $\cdots$ |  | 21.101$\pm$ | 0.023 | 19.38$\pm$ | 0.089 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 22.336$\pm$ | 0.036 | 20.117$\pm$ | 0.008 | 18.684$\pm$ | 0.005 | 18.154$\pm$ | 0.014
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 16.136$\pm$ | 0.006 |  $\cdots$ |  | 14.761$\pm$ | 0.008 | 13.993$\pm$ | 0.135 | 13.714$\pm$ | 0.134 |  $>$12.362 |  | 14.622$\pm$ | 0.027 | 14.554$\pm$ | 0.031
32 | A | 15.375$\pm$ | 0.003 | 14.247$\pm$ | 0.003 | 13.181$\pm$ | 0.004 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 14.501$\pm$ | 0.003 | 13.513$\pm$ | 0.003 | 13.064$\pm$ | 0.001 | 12.919$\pm$ | 0.001
|  | 11.815$\pm$ | 0.024 | 11.169$\pm$ | 0.022 | 10.964$\pm$ | 0.023 | 12.205$\pm$ | 0.001 | 11.801$\pm$ | 0.001 | 11.357$\pm$ | 0.001 | 10.814$\pm$ | 0.023 | 10.755$\pm$ | 0.021 | 10.534$\pm$ | 0.085 | 10.836$\pm$ | 0.011 | 10.75$\pm$ | 0.008
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 23.633$\pm$ | 0.106 | 21.98$\pm$ | 0.013 | 20.483$\pm$ | 0.004 | 19.949$\pm$ | 0.025
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.81$\pm$ | 0.022 | 17.08$\pm$ | 0.026 | 16.449$\pm$ | 0.031 | 16.197$\pm$ | 0.05 | 15.895$\pm$ | 0.109 |  $>$12.271 |  | 16.146$\pm$ | 0.026 | 15.779$\pm$ | 0.043
33 | A | 20.477$\pm$ | 0.057 | 19.994$\pm$ | 0.005 | 19.467$\pm$ | 0.053 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 19.968$\pm$ | 0.005 | 19.775$\pm$ | 0.007 | 19.656$\pm$ | 0.01 | 19.62$\pm$ | 0.029
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 18.616$\pm$ | 0.055 |  $\cdots$ |  | 18.372$\pm$ | 0.249 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 23.359$\pm$ | 0.155 | 21.013$\pm$ | 0.017 | 19.483$\pm$ | 0.009 | 18.977$\pm$ | 0.016
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.125$\pm$ | 0.015 |  $\cdots$ |  | 16.009$\pm$ | 0.029 | 15.752$\pm$ | 0.043 | 15.268$\pm$ | 0.079 |  $>$12.223 |  | 15.6$\pm$ | 0.019 | 15.348$\pm$ | 0.031
34 | A | 20.057$\pm$ | 0.088 | 18.006$\pm$ | 0.003 | 16.641$\pm$ | 0.008 | 19.131$\pm$ | 0.006 | 17.269$\pm$ | 0.002 | 16.396$\pm$ | 0.003 | 15.931$\pm$ | 0.004 | 18.929$\pm$ | 0.003 | 17.147$\pm$ | 0.001 | 16.219$\pm$ | 0.001 | 15.878$\pm$ | 0.002
|  | 14.557$\pm$ | 0.031 | 14.051$\pm$ | 0.051 | 13.637$\pm$ | 0.032 | 14.523$\pm$ | 0.003 | 14.033$\pm$ | 0.004 | 13.713$\pm$ | 0.004 | 13.432$\pm$ | 0.025 | 13.219$\pm$ | 0.035 |  $>$11.68 |  | 13.494$\pm$ | 0.013 | 13.313$\pm$ | 0.012
| B |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 21.832$\pm$ | 0.087 | 20.714$\pm$ | 0.061 | 19.823$\pm$ | 0.035 |  $\cdots$ |  | 21.883$\pm$ | 0.029 | 20.379$\pm$ | 0.016 | 19.754$\pm$ | 0.044
|  |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 17.639$\pm$ | 0.039 | 16.856$\pm$ | 0.042 | 16.168$\pm$ | 0.031 |  $\cdots$ |  |  $\cdots$ |  |  $\cdots$ |  | 15.607$\pm$ | 0.024 | 15.331$\pm$ | 0.043

Note— (a)Component, where A is the primary and B the secondary of the system.
Gaia photometry is from EDR3, Pan-STARRS and NSC photometry is from DR2, VHS
photometry is from DR5.
The photometric band subscripts _2M_ , _A_ and _C_ stand for 2MASS, AllWISE
and CatWISE, respectively.

Table 8: Mean photometric uncertainties per band and color

| Primary photometric uncertainties | Secondary photometric uncertainties
---|---|---
Catalog | Band | Number | Mean | Min | Median | Max | Number | Mean | Min | Median | Max
| Color | of objects | (mag) | (mag) | (mag) | (mag) | of objects | (mag) | (mag) | (mag) | (mag)
Gaia EDR3 | BP | 34 | 0.046 | 0.003 | 0.009 | 0.244 |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |
Gaia EDR3 | G | 34 | 0.004 | 0.003 | 0.003 | 0.008 | 5 | 0.017 | 0.010 | 0.018 | 0.023
Gaia EDR3 | RP | 34 | 0.014 | 0.004 | 0.004 | 0.115 | 5 | 0.100 | 0.048 | 0.089 | 0.167
SDSS DR16 | g | 10 | 0.050 | 0.003 | 0.017 | 0.378 |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |
SDSS DR16 | r | 10 | 0.019 | 0.003 | 0.010 | 0.119 |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |
SDSS DR16 | i | 10 | 0.006 | 0.001 | 0.005 | 0.021 | 5 | 0.156 | 0.051 | 0.150 | 0.330
SDSS DR16 | z | 10 | 0.007 | 0.003 | 0.005 | 0.024 | 5 | 0.114 | 0.064 | 0.101 | 0.198
PS1 DR2 | g | 18 | 0.012 | 0.001 | 0.007 | 0.047 |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |
PS1 DR2 | r | 19 | 0.009 | 0.001 | 0.004 | 0.041 | 1 | 0.343 | 0.343 | 0.343 | 0.343
PS1 DR2 | i | 20 | 0.006 | 0.002 | 0.004 | 0.023 | 11 | 0.069 | 0.018 | 0.050 | 0.183
PS1 DR2 | z | 19 | 0.006 | 0.001 | 0.003 | 0.030 | 14 | 0.069 | 0.016 | 0.043 | 0.202
PS1 DR2 | y | 20 | 0.008 | 0.001 | 0.004 | 0.070 | 16 | 0.061 | 0.008 | 0.042 | 0.176
NSC DR2 | g | 33 | 0.009 | 0.001 | 0.003 | 0.093 |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |
NSC DR2 | r | 30 | 0.004 | 0.001 | 0.003 | 0.018 | 16 | 0.078 | 0.033 | 0.065 | 0.173
NSC DR2 | i | 21 | 0.003 | 0.001 | 0.002 | 0.007 | 30 | 0.031 | 0.005 | 0.018 | 0.189
NSC DR2 | z | 24 | 0.003 | 0.001 | 0.002 | 0.012 | 34 | 0.015 | 0.002 | 0.009 | 0.062
NSC DR2 | y | 32 | 0.005 | 0.001 | 0.002 | 0.042 | 33 | 0.031 | 0.005 | 0.024 | 0.120
DES DR1 | g | 30 | 0.014 | 0.000 | 0.001 | 0.204 |  $\cdots$ |  $\cdots$ |  $\cdots$ |  $\cdots$ |
DES DR1 | r | 30 | 0.005 | 0.000 | 0.001 | 0.053 | 29 | 0.374 | 0.020 | 0.148 | 2.487
DES DR1 | i | 30 | 0.003 | 0.000 | 0.003 | 0.009 | 29 | 0.115 | 0.010 | 0.024 | 1.571
DES DR1 | z | 30 | 0.004 | 0.000 | 0.003 | 0.015 | 29 | 0.026 | 0.004 | 0.012 | 0.114
DES DR1 | y | 30 | 0.005 | 0.000 | 0.001 | 0.054 | 29 | 0.047 | 0.007 | 0.026 | 0.186
2MASS | J | 31 | 0.038 | 0.021 | 0.028 | 0.144 | 10 | 0.152 | 0.105 | 0.147 | 0.235
2MASS | H | 30 | 0.040 | 0.022 | 0.029 | 0.126 | 9 | 0.182 | 0.092 | 0.181 | 0.269
2MASS | K | 30 | 0.043 | 0.019 | 0.028 | 0.181 | 7 | 0.156 | 0.121 | 0.137 | 0.218
VHS DR5 | J | 25 | 0.012 | 0.001 | 0.001 | 0.144 | 25 | 0.024 | 0.006 | 0.016 | 0.053
VHS DR5 | H | 9 | 0.011 | 0.001 | 0.002 | 0.088 | 9 | 0.035 | 0.014 | 0.039 | 0.066
VHS DR5 | K | 24 | 0.021 | 0.001 | 0.002 | 0.249 | 25 | 0.042 | 0.008 | 0.032 | 0.121